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"title": "First X-Ray Polarization Measurement Confirms the Low Black Hole Spin in LMC X-3",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "
© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
\n\nThe Imaging X-ray Polarimetry Explorer (IXPE) is a joint US and Italian mission. The US contribution is supported by the National Aeronautics and Space Administration (NASA) and led and managed by its Marshall Space Flight Center (MSFC), with industry partner Ball Aerospace (contract NNM15AA18C). The Italian contribution is supported by the Italian Space Agency (Agenzia Spaziale Italiana, ASI) through contract ASI-OHBI-2022-13-I.0, agreements ASI-INAF-2022-19-HH.0 and ASI-INFN-2017.13-H0, and its Space Science Data Center (SSDC) with agreements ASI-INAF-2022-14-HH.0 and ASI-INFN 2021-43-HH.0, and by the Istituto Nazionale di Astrofisica (INAF) and the Istituto Nazionale di Fisica Nucleare (INFN) in Italy. This research used data products provided by the IXPE Team (MSFC, SSDC, INAF, and INFN) and distributed with additional software tools by the High-Energy Astrophysics Science Archive Research Center (HEASARC), at NASA Goddard Space Flight Center (GSFC). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.
\nThe authors thank the referee for insightful comments and suggestions. J.S., M.D., J.P., M.B., and V.K. thank GACR project 21-06825X for the support and institutional support from RVO:67985815. A.Y. and M.B. acknowledge the support from GAUK project No. 102323. A.I. acknowledges support from the Royal Society. A.V. thanks the Academy of Finland grant 355672 for support. P.-O.P. acknowledges financial support from the French Space Agency (CNES) and the French High Energy National Programme (PNHE) of CNRS. N.R.C., M.R.M., H.K., K.H., and S.C. acknowledge support by NASA grants 80NSSC22K1291, 80NSSC23K1041, and 80NSSC20K0329.
\n\nIXPE - , NICER - , NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission
",
"abstract": "\n
X-ray polarization is a powerful tool to investigate the geometry of accreting material around black holes, allowing independent measurements of the black hole spin and orientation of the innermost parts of the accretion disk. We perform X-ray spectropolarimetric analysis of an X-ray binary system in the Large Magellanic Cloud, LMC X-3, that hosts a stellar-mass black hole, known to be persistently accreting since its discovery. We report the first detection of the X-ray polarization in LMC X-3 with the Imaging X-ray Polarimetry Explorer, and find the average polarization degree (PD) of 3.2% ± 0.6% and a constant polarization angle of −42° ± 6° over the 2–8 keV range. Using accompanying spectroscopic observations by NICER, NuSTAR, and the Neil Gehrels Swift observatories, we confirm previous measurements of the black hole spin via the X-ray continuum method, a ≈ 0.2. From polarization analysis only, we found consistent results with low black hole spin, with an upper limit of a < 0.7 at a 90% confidence level. A slight increase in the PD with energy, similar to other black hole X-ray binaries in the soft state, is suggested from the data but with a low statistical significance.
\n
",
"date": "2024-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "960",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "3",
"issn": "0004-637X",
"official_url": "https://authors.library.caltech.edu/records/jntd1-93p75",
"funders": {
"items": [
{
"grant_number": "NNM15AA18C"
},
{
"grant_number": "ASI-OHBI-2022-13-I.0"
},
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"grant_number": "ASI-INAF-2022-19-HH.0"
},
{
"grant_number": "ASI-INFN-2017.13-H0"
},
{
"grant_number": "ASI-INAF-2022-14-HH.0"
},
{
"grant_number": "ASI-INFN 2021-43-HH.0"
},
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{},
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},
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},
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{},
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"grant_number": "80NSSC22K1291"
},
{
"grant_number": "80NSSC23K1041"
},
{
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}
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"doi": "10.3847/1538-4357/ad0842",
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"pub_year": "2024",
"author_list": "Svoboda, Ji\u0159\u00ed; Dov\u010diak, Michal; et el."
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"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "Marianne"
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta"
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Lazzarini-Margaret",
"name": {
"family": "Lazzarini",
"given": "Margaret"
},
"orcid": "0000-0003-3252-352X"
},
{
"id": "Middleton-Matthew-J",
"name": {
"family": "Middleton",
"given": "Matthew J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Weaver-Kimberly-A",
"name": {
"family": "Weaver",
"given": "Kimberly A."
}
}
]
},
"title": "A New Sample of Transient Ultraluminous X-Ray Sources Serendipitously Discovered by Swift/XRT",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nWe wish to thank the Swift PI, Brad Cenko, for approving the target of opportunity requests we made to observe these transient sources, as well as the rest of the Swift team for carrying them out. We also acknowledge the use of public data from the Swift data archive. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. \n\nWe also wish to thank Patrick Slane, Director of the Chandra X-ray Center, for approving the DDT requests to observe Swift J130456.1-493158, Swift J095520.7+690401, and Swift J235749.9-323526, and the Chandra team for carrying out the observations. \n\nIn addition we wish to thank the NuSTAR PI, Fiona Harrison, for approving the DDT request we made to observe Swift J235749.9-323526 as well as the NuSTAR SOC for carrying out the observation. This work was also supported under NASA Contract No. NNG08FD60C. NuSTAR is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nThis research has made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. \n\nThis work was also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. \n\nThis research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. \n\nBased on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESAC/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). The Hubble Source Catalog can be accessed via doi:10.17909/T97P46, and the specific observations used can be accessed via doi:10.17909/jmva-dc49. \n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nJ.M.C.'s research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. M.H. acknowledges support from an ESO fellowship and J.-P.L. was supported in part by a grant from the French Space Agency CNES. \n\nFacilities: Swift (XRT - , UVOT) - , CXO - , NuSTAR - , XMM - , VLA - Very Large Array. \n\nSoftware: CIAO (Fruscione et al. 2006), XSPEC (Arnaud1996).\n\nPublished - Brightman_2023_ApJ_951_51.pdf
",
"abstract": "Ultraluminous X-ray sources (ULXs) are our best laboratories for studying extreme super-Eddington accretion. Most studies of these objects are of relatively persistent sources; however, there is growing evidence to suggest a large fraction of these sources are transient. Here we present a sample of five newly reported transient ULXs in the galaxies NGC 4945, NGC 7793, and M81 serendipitously discovered in Swift/XRT observations. Swift monitoring of these sources have provided well-sampled lightcurves, allowing for us to model the lightcurves with the disk-instability model of Hameury & Lasota, which implies durations of 60\u2013400 days and that the mass-accretion rate through the disk is close to or greater than the Eddington rate. Of the three source regions with prior Hubble Space Telescope imaging, color\u2013magnitude diagrams of the potential stellar counterparts show varying ages of the possible stellar counterparts. Our estimation of the rates of these sources in these three galaxies is 0.4\u20131.3 yr\u207b\u00b9. We find that, while persistent ULXs dominate the high end of galaxy luminosity functions, the number of systems that produce ULX luminosities are likely dominated by transient sources.",
"date": "2023-07-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "951",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 51",
"id_number": "CaltechAUTHORS:20230717-55375900.15",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230717-55375900.15",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "European Southern Observatory (ESO)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/acd18a",
"primary_object": {
"basename": "Brightman_2023_ApJ_951_51.pdf",
"url": "https://authors.library.caltech.edu/records/pzn87-vvg25/files/Brightman_2023_ApJ_951_51.pdf"
},
"pub_year": "2023",
"author_list": "Brightman, Murray; Hameury, Jean-Marie; et el."
},
{
"id": "https://authors.library.caltech.edu/records/mzyac-qyh22",
"eprint_id": 122126,
"eprint_status": "archive",
"datestamp": "2023-08-22 21:04:13",
"lastmod": "2023-10-20 19:00:04",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lefkir-Mehdy",
"name": {
"family": "Lefkir",
"given": "Mehdy"
},
"orcid": "0000-0002-6972-2429"
},
{
"id": "Kammoun-Elias",
"name": {
"family": "Kammoun",
"given": "Elias"
},
"orcid": "0000-0002-0273-218X"
},
{
"id": "Barret-Didier",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Boorman-Peter",
"name": {
"family": "Boorman",
"given": "Peter"
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Matzeu-Gabriele",
"name": {
"family": "Matzeu",
"given": "Gabriele"
},
"orcid": "0000-0003-1994-5322"
},
{
"id": "Miller-Jon-M",
"name": {
"family": "Miller",
"given": "Jon M."
},
"orcid": "0000-0003-2869-7682"
},
{
"id": "Nardini-Emanuele",
"name": {
"family": "Nardini",
"given": "Emanuele"
},
"orcid": "0000-0001-9226-8992"
},
{
"id": "Zoghbi-Abderahmen",
"name": {
"family": "Zoghbi",
"given": "Abderahmen"
},
"orcid": "0000-0002-0572-9613"
}
]
},
"title": "A hard look at the X-ray spectral variability of NGC 7582",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nWe thank the anonymous referee for their comments and suggestions. ML acknowledges useful discussions with Johannes Buchner on the UXCLUMPY model. DB/ESK/ML acknowledge financial support from the Centre National d'Etudes Spatiales (CNES). ML acknowledges financial support through the UK Science and Technology Facilities Council (STFC). AZ is supported by NASA under award number 80GSFC21M0002. \n\nThis research has made use of data and/or software provided by the heasarc, which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research made use of Astropy, a community-developed core python package for Astronomy (Astropy Collaboration et al. 2013, 2018), numpy (Harris et al. 2020), and matplotlib, a python library for publication quality graphics (Hunter 2007). This work has made use of GetDist (Lewis 2019), a python library for analysing Monte Carlo samples. This research made use of xspec (Arnaud 1996). We have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. NuSTAR data was reduced with the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We have also made use of data based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. \n\nData Availability: The data used in this paper are publicly available to access and download from the High Energy Astrophysics Science Archive Research Center (heasarc) for NuSTAR and from the XMM\u2013Newton Science Archive. Final data products from this study can be provided on reasonable request to the corresponding author.\n\nPublished - stad995.pdf
",
"abstract": "NGC 7582 (z = 0.005264; D = 22.5\u2009Mpc) is a highly variable, changing-look AGN. In this work, we explore the X-ray properties of this source using XMM\u2013Newton and NuSTAR archival observations in the 3 \u2013 40\u2009keV range, from 2001 to 2016. NGC 7582 exhibits a long-term variability between observations but also a short-term variability in two observations that has not been studied before. To study the variability, we perform a time-resolved spectral analysis using a phenomenological model and a physically motivated model (uxclumpy). The spectral fitting is achieved using a nested sampling Monte Carlo method. uxclumpy enables testing various geometries of the absorber that may fit AGN spectra. We find that the best model is composed of a fully covering clumpy absorber. From this geometry, we estimate the velocity, size, and distance of the clumps. The column density of the absorber in the line of sight varies from Compton-thin to Compton-thick between observations. Variability over the time-scale of a few tens of kiloseconds is also observed within two observations. The obscuring clouds are consistent with being located at a distance not larger than 0.6\u2009pc, moving with a transverse velocity exceeding \u223c700\u2009km\u2009s\u207b\u00b9. We could put only a lower limit on the size of the obscuring cloud being larger than 10\u00b9\u00b3 cm. Given the sparsity of the observations, and the limited exposure time per observation available, we cannot determine the exact structure of the obscuring clouds. The results are broadly consistent with comet-like obscuring clouds or spherical clouds with a non-uniform density profile.",
"date": "2023-06",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "522",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1169-1182",
"id_number": "CaltechAUTHORS:20230705-942391700.8",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230705-942391700.8",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "80GSFC21M0002"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stad995",
"primary_object": {
"basename": "stad995.pdf",
"url": "https://authors.library.caltech.edu/records/mzyac-qyh22/files/stad995.pdf"
},
"pub_year": "2023",
"author_list": "Lefkir, Mehdy; Kammoun, Elias; et el."
},
{
"id": "https://authors.library.caltech.edu/records/426w2-6p371",
"eprint_id": 121689,
"eprint_status": "archive",
"datestamp": "2023-08-22 20:59:24",
"lastmod": "2023-10-20 15:46:55",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Zhang-Zuobin",
"name": {
"family": "Zhang",
"given": "Zuobin"
},
"orcid": "0000-0003-0847-1299"
},
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
},
"orcid": "0000-0002-9639-4352"
},
{
"id": "Liu-Honghui",
"name": {
"family": "Liu",
"given": "Honghui"
},
"orcid": "0000-0003-2845-1009"
},
{
"id": "Bambi-Cosimo",
"name": {
"family": "Bambi",
"given": "Cosimo"
},
"orcid": "0000-0002-3180-9502"
},
{
"id": "Reynolds-Christopher-S",
"name": {
"family": "Reynolds",
"given": "Christopher S."
},
"orcid": "0000-0002-1510-4860"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Dauser-Thomas",
"name": {
"family": "Dauser",
"given": "Thomas"
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Young-Andrew-J",
"name": {
"family": "Young",
"given": "Andrew J."
},
"orcid": "0000-0003-3626-9151"
},
{
"id": "Gallo-Luigi-C",
"name": {
"family": "Gallo",
"given": "Luigi C."
}
},
{
"id": "Yu-Zhibo",
"name": {
"family": "Yu",
"given": "Zhibo"
}
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
}
]
},
"title": "The Low-temperature Corona in ESO 511-G030 Revealed by NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nThis work was supported by the National Natural Science Foundation of China (NSFC), grant No. 11973019; the Natural Science Foundation of Shanghai, grant No. 22ZR1403400; the Shanghai Municipal Education Commission, grant No. 2019-01-07-00-07-E00035; and Fudan University, grant No. JIH1512604. J.J. acknowledges support from the Leverhulme Trust, the Isaac Newton Trust, and St Edmund's College, University of Cambridge.\n\nPublished - Zhang_2023_ApJ_949_4.pdf
",
"abstract": "We present the results from a coordinated XMM-Newton + NuSTAR observation of the Seyfert 1 galaxy ESO 511\u2212G030. With this joint monitoring program, we conduct a detailed variability and spectral analysis. The source remained in a low flux and very stable state throughout the observation period, although there are slight fluctuations of flux over long timescales. The broadband (0.3\u201378 keV) spectrum shows the presence of a power-law continuum with a soft excess below 2 keV, a relatively narrow iron K\u03b1 emission (\u223c6.4 keV), and an obvious cutoff at high energies. We find that the soft excess can be modeled by two different possible scenarios: a warm (kT\u2091 \u223c 0.19 keV) and optically thick (\u03c4 = 18\u201325) Comptonizing corona or a relativistic reflection from a high-density (log[n\u2091_/cm}\u207b\u00b3] = 17.1-18.5) inner disk. All models require a low temperature (kT\u2091 \u223c 13 keV) for the hot corona.",
"date": "2023-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "949",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 4",
"id_number": "CaltechAUTHORS:20230602-251659000.31",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230602-251659000.31",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11973019"
},
{
"agency": "Natural Science Foundation of Shanghai",
"grant_number": "22ZR1403400"
},
{
"agency": "Shanghai Municipal Education Commission",
"grant_number": "2019-01-07-00-07-E00035"
},
{
"agency": "Fudan University",
"grant_number": "JIH1512604"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Isaac Newton Trust"
},
{
"agency": "St. Edmund's College, University of Cambridge"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/acc38f",
"primary_object": {
"basename": "Zhang_2023_ApJ_949_4.pdf",
"url": "https://authors.library.caltech.edu/records/426w2-6p371/files/Zhang_2023_ApJ_949_4.pdf"
},
"pub_year": "2023",
"author_list": "Zhang, Zuobin; Jiang, Jiachen; et el."
},
{
"id": "https://authors.library.caltech.edu/records/6zqjb-6fm13",
"eprint_id": 121397,
"eprint_status": "archive",
"datestamp": "2023-08-22 20:42:34",
"lastmod": "2023-10-20 15:27:05",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Yun-S-B",
"name": {
"family": "Yun",
"given": "S. B."
}
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Brumback-McKinley-C",
"name": {
"family": "Brumback",
"given": "M. C."
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "Buisson-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "D. J. K."
},
"orcid": "0000-0002-5341-6929"
},
{
"id": "Mastroserio-Guglielmo",
"name": {
"family": "Mastroserio",
"given": "G."
},
"orcid": "0000-0003-4216-7936"
},
{
"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "S. N."
},
"orcid": "0000-0002-8403-0041"
}
]
},
"title": "Revealing the Spectral State Transition of the Clocked Burster, GS 1826-238, with NuSTAR StrayCats",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nThis work was supported by the National Aeronautics and Space Administration (NASA) under grant number 80NSSC19K1023 issued through the NNH18ZDA001N Astrophysics Data Analysis Program (ADAP). This research was performed at the California Institute of Technology (Caltech) under the Summer Undergraduate Research Fellowship (SURF) program. \n\nAdditionally, this work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for their support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC.\n\nPublished - Yun_2023_ApJ_947_81.pdf
",
"abstract": "We present the long-term analysis of GS 1826-238, a neutron star X-ray binary known as the Clocked Burster, using data from NuSTAR StrayCats. StrayCats, a catalog of NuSTAR stray light data, contains data from bright, off-axis X-ray sources that have not been focused by the NuSTAR optics. We obtained stray light observations of the source from 2014\u20132021, reduced and analyzed the data using nustar-gen-utils Python tools, demonstrating the transition of the source from the island atoll state to a banana branch. We also present the light-curve analysis of Type I X-ray bursts from the Clocked Burster and show that the bursts from the banana/soft state are systematically shorter in duration than those from the island/hard state and have a higher burst fluence. From our analysis, we note an increase in the mass accretion rate of the source, and a decrease in burst frequency with the transition.",
"date": "2023-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "947",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 81",
"id_number": "CaltechAUTHORS:20230515-138512000.10",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230515-138512000.10",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC19K1023"
},
{
"agency": "NASA",
"grant_number": "NNH18ZDA001N"
},
{
"agency": "Caltech Summer Undergraduate Research Fellowship (SURF)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/acb689",
"primary_object": {
"basename": "Yun_2023_ApJ_947_81.pdf",
"url": "https://authors.library.caltech.edu/records/6zqjb-6fm13/files/Yun_2023_ApJ_947_81.pdf"
},
"pub_year": "2023",
"author_list": "Yun, S. B.; Grefenstette, B. W.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ssmp9-me185",
"eprint_id": 121132,
"eprint_status": "archive",
"datestamp": "2023-08-22 20:16:21",
"lastmod": "2023-10-18 18:09:45",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Paterson-Sarah-J",
"name": {
"family": "Paterson",
"given": "Sarah"
},
"orcid": "0000-0003-2147-9586"
},
{
"id": "Hannah-Iain-G",
"name": {
"family": "Hannah",
"given": "Iain G."
},
"orcid": "0000-0003-1193-8603"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hudson-Hugh-S",
"name": {
"family": "Hudson",
"given": "Hugh S."
},
"orcid": "0000-0001-5685-1283"
},
{
"id": "Krucker-S\u00e4m",
"name": {
"family": "Krucker",
"given": "S\u00e4m"
},
"orcid": "0000-0002-2002-9180"
},
{
"id": "Glesener-Lindsay",
"name": {
"family": "Glesener",
"given": "Lindsay"
},
"orcid": "0000-0001-7092-2703"
},
{
"id": "White-Stephen-M",
"name": {
"family": "White",
"given": "Stephen M."
},
"orcid": "0000-0002-8574-8629"
},
{
"id": "Smith-David-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
}
]
},
"title": "The First Survey of Quiet Sun Features Observed in Hard X-Rays with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 The Author(s) 2023. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/. \n\nThis paper made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and UKSA as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). AIA on the Solar Dynamics Observatory is part of NASA's Living with a Star program. This research has made use of SunPy, an open-source and free community-developed solar data analysis package written in Python (SunPy Community et al., 2015). This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al., 2018, 2013). The authors would also like to thank Kathy Reeves for co-ordinating the Hinode/XRT observations. \n\nSP acknowledges support from the UK's Science and Technology Facilities Council (STFC) doctoral training grant (ST/T506102/1). IGH acknowledges support from a Royal Society University Fellowship (URF/R/180010) and STFC grant (ST/T000422/1). \n\nContributions. SP did the data processing and applied the analysis techniques described and wrote the manuscript text. IGH developed the demreg analysis techniques and helped with the spectral analysis. All authors revised the manuscript. \n\nThe authors declare no competing interests.\n\nPublished - s11207-023-02135-4.pdf
",
"abstract": "We present the first survey of quiet Sun features observed in hard X-rays (HXRs), using the Nuclear Spectroscopic Telescope ARray (NuSTAR), a HXR focusing optics telescope. The recent solar minimum, combined with NuSTAR's high sensitivity, has presented a unique opportunity to perform the first HXR imaging spectroscopy on a range of features in the quiet Sun. By studying the HXR emission of these features, we can detect or constrain the presence of high temperature (>\u20095 MK) or non-thermal sources, to help understand how they relate to larger, more energetic solar phenomena, and determine their contribution to heating the solar atmosphere. We report on several features observed in the 28 September 2018 NuSTAR full-disk quiet Sun mosaics, the first of the NuSTAR quiet Sun observing campaigns, which mostly include steady features of X-ray bright points and an emerging flux region, which later evolved into an active region, as well as a short-lived jet. We find that the features' HXR spectra are well fitted with isothermal models with temperatures ranging between 2.0\u2009\u2013\u20093.2 MK. Combining the NuSTAR data with softer X-ray emission from Hinode/XRT and EUV from SDO/AIA, we recover the differential emission measures, confirming little significant emission above 4 MK. The NuSTAR HXR spectra allow us to constrain the possible non-thermal emission that would still be consistent with a null HXR detection. We found that for only one of the features (the jet) was there a potential non-thermal upper limit capable of powering the heating observed. However, even here, the non-thermal electron distribution had to be very steep (effectively mono-energetic) with a low energy cut-off between 3\u2009\u2013\u20094\u00a0keV.",
"date": "2023-03",
"date_type": "published",
"publication": "Solar Physics",
"volume": "298",
"number": "3",
"publisher": "Springer",
"pagerange": "Art. No. 47",
"id_number": "CaltechAUTHORS:20230420-956212500.5",
"issn": "0038-0938",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230420-956212500.5",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/T506102/1"
},
{
"agency": "Royal Society",
"grant_number": "URF/R/180010"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/T000422/1"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
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},
"doi": "10.1007/s11207-023-02135-4",
"primary_object": {
"basename": "s11207-023-02135-4.pdf",
"url": "https://authors.library.caltech.edu/records/ssmp9-me185/files/s11207-023-02135-4.pdf"
},
"pub_year": "2023",
"author_list": "Paterson, Sarah; Hannah, Iain G.; et el."
},
{
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"datestamp": "2023-08-20 09:01:21",
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{
"id": "Roach-Brandon-M",
"name": {
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{
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"name": {
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"family": "Perez",
"given": "Kerstin"
},
"orcid": "0000-0002-6404-4737"
},
{
"id": "Beacom-John-F",
"name": {
"family": "Beacom",
"given": "John F."
},
"orcid": "0000-0002-0005-2631"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Horiuchi-Shunsaku",
"name": {
"family": "Horiuchi",
"given": "Shunsaku"
},
"orcid": "0000-0001-6142-6556"
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{
"id": "Krivonos-Roman-A",
"name": {
"family": "Krivonos",
"given": "Roman"
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Wik-Daniel-R",
"name": {
"family": "Wik",
"given": "Daniel R."
},
"orcid": "0000-0001-9110-2245"
}
]
},
"title": "Long-exposure NuSTAR constraints on decaying dark matter in the Galactic halo",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2023 American Physical Society. \n\nWe are grateful to the NuSTAR team for the excellent performance of the observatory and their assistance with data processing. We also thank Alexey Boyarsky, Josh Foster, Nick Rodd, Field Rogers, Mengjiao Xiao, and the anonymous reviewer for helpful comments and discussions. B.\u2009M.\u2009R. and K.\u2009P. thank Paul Acosta, Gabriel Collin, and the MIT Laboratory for Nuclear Science for computing support. B.\u2009M.\u2009R. and K.\u2009P. were supported by the Cottrell Scholar Award, Research Corporation for Science Advancement (RCSA), ID No. 25928. S.\u2009R. and D.\u2009R.\u2009W. were supported by NASA Grant No. 80NSSC18K0686. K.\u2009C.\u2009Y.\u2009N. was supported by the Research Grants Council (RGC) of HKSAR, Project No. 24302721. J.\u2009F.\u2009B. was supported by U.S. National Science Foundation (NSF) Grant No. PHY-2012955. B.\u2009W.\u2009G. was supported by NASA Contract No. NNG08FD60C.\u2009S.\u2009H. was supported by the U.S. Department of Energy Office of Science under Award No. DE-SC0020262, NSF Grants No. AST-1908960 and No. PHY-1914409, JSPS KAKENHI Grant No. JP22K03630, and the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. R.\u2009K. was supported by Russian Science Foundation Grant No. 22-12-00271. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC.\n\nPublished - PhysRevD.107.023009.pdf
",
"abstract": "We present two complementary NuSTAR x-ray searches for keV-scale dark matter decaying to monoenergetic photons in the Milky Way halo. In the first, we utilize the known intensity pattern of unfocused stray light across the detector planes\u2014the dominant source of photons from diffuse sources\u2014to separate astrophysical emission from internal instrument backgrounds using ~7-Ms/detector deep blank-sky exposures. In the second, we present an updated parametric model of the full NuSTAR instrument background, allowing us to leverage the statistical power of an independent ~20-Ms/detector stacked exposures spread across the sky. Finding no evidence of anomalous x-ray lines using either method, we set limits on the active-sterile mixing angle sin\u00b2 (2\u03b8) for sterile-neutrino masses 6\u201340 keV. The first key result is that we strongly disfavor a ~7-keV sterile neutrino decaying into a 3.5-keV photon. The second is that we derive leading limits on sterile neutrinos with masses ~15-18 keV and ~25-40 KeV, reaching or extending below the big bang nucleosynthesis limit. In combination with previous results, the parameter space for the neutrino minimal standard model is now nearly closed.",
"date": "2023-01-15",
"date_type": "published",
"publication": "Physical Review D",
"volume": "107",
"number": "2",
"publisher": "American Physical Society",
"pagerange": "Art. No. 023009",
"id_number": "CaltechAUTHORS:20230301-701033500.15",
"issn": "2470-0010",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230301-701033500.15",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Cottrell Scholar of Research Corporation",
"grant_number": "25928"
},
{
"agency": "NASA",
"grant_number": "80NSSC18K0686"
},
{
"agency": "Research Grants Council of Hong Kong",
"grant_number": "24302721"
},
{
"agency": "NSF",
"grant_number": "PHY-2012955"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-SC0020262"
},
{
"agency": "NSF",
"grant_number": "AST-1908960"
},
{
"agency": "NSF",
"grant_number": "PHY-1914409"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "JP22K03630"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)"
},
{
"agency": "Russian Science Foundation",
"grant_number": "22-12-00271"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
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{
"id": "NuSTAR"
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},
"doi": "10.1103/physrevd.107.023009",
"primary_object": {
"basename": "PhysRevD.107.023009.pdf",
"url": "https://authors.library.caltech.edu/records/eegpe-hmh46/files/PhysRevD.107.023009.pdf"
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"pub_year": "2023",
"author_list": "Roach, Brandon M.; Rossland, Steven; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-22 18:37:48",
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"items": [
{
"id": "Diaz-Yaherlyn",
"name": {
"family": "Diaz",
"given": "Y."
},
"orcid": "0000-0002-8604-1158"
},
{
"id": "Hern\u00e1ndez-Garc\u00eda-Lorena",
"name": {
"family": "Hern\u00e1ndez-Garc\u00eda",
"given": "L."
},
"orcid": "0000-0002-8606-6961"
},
{
"id": "Ar\u00e9valo-Patricia",
"name": {
"family": "Ar\u00e9valo",
"given": "P."
},
"orcid": "0000-0001-8503-9809"
},
{
"id": "L\u00f3pez-Navas-E",
"name": {
"family": "L\u00f3pez-Navas",
"given": "E."
}
},
{
"id": "Ricci-Claudio",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Koss-Michael-J",
"name": {
"family": "Koss",
"given": "M."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Gonz\u00e1lez-Mart\u00edn-Omaira",
"name": {
"family": "Gonz\u00e1lez-Mart\u00edn",
"given": "O."
},
"orcid": "0000-0002-2356-8358"
},
{
"id": "Balokovi\u0107-Mislav",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Osorio-Clavijo-Natalia",
"name": {
"family": "Osorio-Clavijo",
"given": "N."
},
"orcid": "0000-0002-3467-8077"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
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{
"id": "Malizia-Angela",
"name": {
"family": "Malizia",
"given": "A."
},
"orcid": "0000-0002-6558-1163"
}
]
},
"title": "Constraining the X-ray reflection in low accretion-rate active galactic nuclei using XMM-Newton, NuSTAR, and Swift",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 The Authors 2023. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. This article is published in open access under the Subscribe-to-Open model. Subscribe to A&A to support open access publication. \n\nWe thank the referee for the valuable comments that improved the manuscript. D.Y. acknowledges financial support from the Doctorate Fellowship program FIB-UV of the Universidad de Valpara\u00edso and the Max Planck Society by a Max Planck partner group. LHG acknowledges funds by ANID \u2013 Millennium Science Initiative Program \u2013 ICN12_009 awarded to the Millennium Institute of Astrophysics (MAS). ELN acknowledges financial support from ANID Beca 21200718. CR acknowledges support from the Fondecyt Iniciacion grant 11190831 and ANID BASAL project FB210003. MB acknowledges support from the YCAA Prize Postdoctoral Fellowship. NOC acknowledges support from CONACyT. J.A.G. acknowledges support from NASA grant 80NSSC21K1567.\n\nPublished - aa44678-22.pdf
",
"abstract": "An interesting feature of active galactic nuclei (AGN) accreting at low rates is the weakness of the reflection features in their X-ray spectra, which may result from the gradual disappearance of the torus with decreasing accretion rates. It has been suggested that low-luminosity AGN (LLAGN) would exhibit a different reflector configuration than high-luminosity AGN, covering a smaller fraction of the sky or simply having less material. Additionally, we note that the determination of the spectral index (\u0393) and the cut-off energy of the primary power-law emission is affected by the inclusion of reflection models, showing their importance in studying accretion mechanisms. This is especially valid in the case of the LLAGN which has previously shown a high dispersion in the relation between \u0393 and the accretion rate. \n\nAims. Our purpose is to constrain the geometry and column density of the reflector in a sample of LLAGN covering a broad X-ray range of energy by combining data from XMM-Newton+ NuSTAR + Swift. The spectral analysis also allows us to investigate the accretion mechanism in LLAGN. \n\nMethods. We used XMM-Newton+ NuSTAR + Swift observations of a hard X-ray flux-limited sample of 17 LLAGN from BASS/DR2 with accretion rates of \u03bb_(Edd)\u2004=\u2004L_(Bol)/L_(Edd)\u2004< 10\u207b\u00b3. We fit all spectra using the reflection model for torus (BORUS) and accretion disk (XILLVER) reflectors. \n\nResults. We found a tentative correlation between the torus column density and the accretion rate, with LLAGN showing a lower column density than the high-luminosity objects. We also confirm the relation between \u0393 and \u03bb_(Edd), with a smaller scatter than previously reported, thanks to the inclusion of high-energy data and the reflection models. Our results are consistent with a break at \u03bb_(Edd)\u2004\u223c\u200410\u207b\u00b3, which is suggestive of a different accretion mechanism compared with higher accretion AGN.",
"date": "2023-01",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "669",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A114",
"id_number": "CaltechAUTHORS:20230314-844891400.8",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230314-844891400.8",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Universidad de Valpara\u00edso"
},
{
"agency": "Max Planck Society"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ICN12_009"
},
{
"agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)",
"grant_number": "21200718"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "11190831"
},
{
"agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)",
"grant_number": "FB210003"
},
{
"agency": "Yale Center for Astronomy and Astrophysics"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)"
},
{
"agency": "NASA",
"grant_number": "80NSSC21K1567"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/202244678",
"primary_object": {
"basename": "aa44678-22.pdf",
"url": "https://authors.library.caltech.edu/records/rnp3v-80k61/files/aa44678-22.pdf"
},
"pub_year": "2023",
"author_list": "Diaz, Y.; Hern\u00e1ndez-Garc\u00eda, L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/5x05z-f7d06",
"eprint_id": 121348,
"eprint_status": "archive",
"datestamp": "2023-08-22 18:39:36",
"lastmod": "2023-10-23 20:16:05",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Violette-Daniel-P",
"name": {
"family": "Violette",
"given": "Daniel P."
},
"orcid": "0000-0002-5943-4730"
},
{
"id": "Allen-Branden",
"name": {
"family": "Allen",
"given": "Branden"
}
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "Jaesub"
},
"orcid": "0000-0002-6089-5390"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Grindlay-Jonathan-E",
"name": {
"family": "Grindlay",
"given": "Jonathan"
},
"orcid": "0000-0002-1323-5314"
}
]
},
"title": "Tuning of nuclear spectroscopic telescope array application specific integrated circuits to improve low energy threshold of future hard x-ray imaging detectors",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Mechanical Engineering; Astronomy and Astrophysics; Instrumentation; Control and Systems Engineering; Electronic, Optical and Magnetic Materials",
"note": "\u00a9 2023 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nWe would like to thank Fiona A. Harrison, Jill A. Burnham, and W. Rick Cook of the California Institute of Technology along with the rest of the NuSTAR Team for developing the NuASIC and providing valuable information to facilitate its operation and testing. DPV is grateful to MA and KV for useful advice. This work was supported by NASA APRA (Grant No. NNX17AE62G). DPV is supported by the NASA FINESST Fellowship (Grant No. 80NSSC20K1537).\n\nPublished - 016001_1.pdf
",
"abstract": "Detector commanding, processing and readout of spaceborne instrumentation is often accomplished with application specific integrated circuits (ASICs). The ASIC designed for the nuclear spectroscopic telescope array (NuSTAR) mission enables future tiled CdZnTe (CZT) detector array readout for x-ray detectors, such as the high resolution energetic x-ray imager (HREXI). Modified NuSTAR ASIC (NuASIC) gain settings have been implemented for HREXI's broader targeted imaging energy range (3 to 300 keV) compared with NuSTAR (2 to 79 keV), which may require updated NuASIC internal parameters for optimal energy resolution. To reach HREXI's targeted low energy threshold, we have also enabled the NuASIC's \"charge pump mode,\" which introduces an additional tuning parameter. We describe the mechanics of the NuASIC's adjustable parameters and use our recently developed ASIC test stand to probe a \"bare\" NuASIC using its internal test pulser. We record the effects of parameter tuning on the device's electronics noise and low energy threshold and report the optimal set of parameters for HREXI's updated gain setting. We detail a semiautomated procedure to derive the optimal parameters for each of HREXI's large area closely tiled NuASIC/CZT detectors to expedite instrument integration.",
"date": "2023-01",
"date_type": "published",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"volume": "9",
"number": "1",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"pagerange": "Art. No. 016001",
"id_number": "CaltechAUTHORS:20230509-880670200.5",
"issn": "2329-4124",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230509-880670200.5",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX17AE62G"
},
{
"agency": "NASA Earth and Space Science and Technology Fellowship",
"grant_number": "80NSSC20K1537"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1117/1.jatis.9.1.016001",
"primary_object": {
"basename": "016001_1.pdf",
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"pub_year": "2023",
"author_list": "Violette, Daniel P.; Allen, Branden; et el."
},
{
"id": "https://authors.library.caltech.edu/records/mb3ja-v5e51",
"eprint_id": 119018,
"eprint_status": "archive",
"datestamp": "2023-08-22 18:27:27",
"lastmod": "2023-10-24 23:48:13",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Mastroserio-Guglielmo",
"name": {
"family": "Mastroserio",
"given": "G."
},
"orcid": "0000-0003-4216-7936"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Thalhammer-Philipp",
"name": {
"family": "Thalhammer",
"given": "P."
},
"orcid": "0000-0001-6269-2821"
},
{
"id": "Buisson-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "D. J. K."
},
"orcid": "0000-0002-5341-6929"
},
{
"id": "Brumback-McKinley-C",
"name": {
"family": "Brumback",
"given": "M. C."
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Connors-Riley-M-T",
"name": {
"family": "Connors",
"given": "R. M. T."
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Grinberg-Victoria",
"name": {
"family": "Grinberg",
"given": "V."
},
"orcid": "0000-0003-2538-0188"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "H."
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wilms-J\u00f6rn",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "NuSTAR Spectral Analysis beyond 79 keV with Stray Light",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "G.M. would like to thank Lorenzo Natalucci for the helpful comments. J.A.G. acknowledges support from NASA grant 80NSSC19K1020 and from the Alexander von Humboldt Foundation. The material is based upon work supported by NASA under award No. 80GSFC21M0002. This work was supported by NASA under grant No. 80NSSC19K1023 issued through the NNH18ZDA001N Astrophysics Data Analysis Program (ADAP). This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).",
"abstract": "Due to the structure of the NuSTAR telescope, photons at a large off axis (>1\u00b0) can reach the detectors directly (stray light), without passing through the instrument optics. At these off-axis angles NuSTAR essentially turns into a collimated instrument and the spectrum can extend to energies above the Pt K edge (79 keV) of the multilayers, which limits the effective area bandpass of the optics. We present the first scientific spectral analysis beyond 79 keV using a Cygnus X-1 observation in StrayCats: the catalog of stray light observations. This serendipitous stray light observation occurred simultaneously with an INTEGRAL observation. When the spectra are modeled together in the 30\u2013120 keV energy band, we find that the NuSTAR stray light flux is well calibrated and constrained to be consistent with the INTEGRAL flux at the 90% confidence level. Furthermore, we explain how to treat the background of the stray light spectral analysis, which is especially important at high energies.",
"date": "2022-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "941",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 35",
"id_number": "CaltechAUTHORS:20230203-893210800.24",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230203-893210800.24",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC19K1020"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA",
"grant_number": "80GSFC21M0002"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1023"
},
{
"agency": "NASA",
"grant_number": "NNH18ZDA001N"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ac8c94",
"pub_year": "2022",
"author_list": "Mastroserio, G.; Grefenstette, B. W.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/47qwz-pzq56",
"eprint_id": 118892,
"eprint_status": "archive",
"datestamp": "2023-08-22 18:20:09",
"lastmod": "2023-10-24 23:31:49",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Chalise-Sulov",
"name": {
"family": "Chalise",
"given": "S."
},
"orcid": "0000-0002-5641-0442"
},
{
"id": "Lohfink-Anne-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Chauhan-Jaiverdhan",
"name": {
"family": "Chauhan",
"given": "J."
},
"orcid": "0000-0003-0330-1901"
},
{
"id": "Russell-Thomas-D",
"name": {
"family": "Russell",
"given": "T. D."
},
"orcid": "0000-0001-6958-8891"
},
{
"id": "Buisson-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "D. J. K."
},
"orcid": "0000-0002-5341-6929"
},
{
"id": "Mallick-Labani",
"name": {
"family": "Mallick",
"given": "L."
},
"orcid": "0000-0001-8624-9162"
}
]
},
"title": "Broad-band spectral analysis of Mrk\u2009926 using multi-epoch X-ray observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has also made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. We would like to thank Javier Garc\u00eda and Andy Fabian for helpful discussions.",
"abstract": "The X-ray spectra of some active galactic nuclei (AGNs) show a soft X-ray excess, emission in excess to the extrapolated primary X-ray continuum below 2\u2009keV. Recent studies have shown that this soft excess can be described well as originating from either a relativistic ionized reflection, the extreme blurring of the reprocessed emission from the innermost region of the accretion disc, or Comptonization from an optically thick and warm region called the 'warm corona', in which electron scattering is the dominant source of opacity. To constrain the origin of the soft excess in the Seyfert 1 galaxy Mrk\u2009926, we carry out a multi-epoch X-ray spectral study using observations from Suzaku (2009), XMM\u2013Newton and NuSTAR (2016), and NuSTAR and Swift-XRT (2021). The broad-band X-ray spectra of Mrk\u2009926 contains a thermally Comptonized primary continuum, a variable soft excess, and distant reflection. We find that in Mrk\u2009926 as in so many sources, it is difficult to make a definite statement as to what is causing the observed soft excess. A warm coronal-like component is slightly preferred by the data but a reflection origin is also possible. Using archival radio data, we detect an optically thin radio component in our broad-band study of Mrk\u2009926. While this component is consistent with an optically thin radio jet, future multiwavelength observations including high spatial resolution radio observations at multiple frequencies are required to probe the origin of the radio emission in more detail.",
"date": "2022-12",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "517",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4788-4794",
"id_number": "CaltechAUTHORS:20230123-451320900.19",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230123-451320900.19",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stac2953",
"pub_year": "2022",
"author_list": "Chalise, S.; Lohfink, A. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/8fvrg-vfn93",
"eprint_id": 118079,
"eprint_status": "archive",
"datestamp": "2023-08-22 18:10:26",
"lastmod": "2023-10-24 23:13:48",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lewin-Collin",
"name": {
"family": "Lewin",
"given": "Collin"
},
"orcid": "0000-0002-8671-1190"
},
{
"id": "Kara-Erin",
"name": {
"family": "Kara",
"given": "Erin"
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Wilkins-Dan",
"name": {
"family": "Wilkins",
"given": "Dan"
},
"orcid": "0000-0002-4794-5998"
},
{
"id": "Mastroserio-Guglielmo",
"name": {
"family": "Mastroserio",
"given": "Guglielmo"
},
"orcid": "0000-0003-4216-7936"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Zhang-Rachel-C",
"name": {
"family": "Zhang",
"given": "Rachel C."
},
"orcid": "0000-0002-2905-9239"
},
{
"id": "Alston-William-N",
"name": {
"family": "Alston",
"given": "William N."
},
"orcid": "0000-0003-2658-6559"
},
{
"id": "Connors-Riley-M-T",
"name": {
"family": "Connors",
"given": "Riley"
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Dauser-Thomas",
"name": {
"family": "Dauser",
"given": "Thomas"
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "Andrew"
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Ingram-Adam",
"name": {
"family": "Ingram",
"given": "Adam"
},
"orcid": "0000-0002-5311-9078"
},
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
},
"orcid": "0000-0002-9639-4352"
},
{
"id": "Lohfink-Anne-M",
"name": {
"family": "Lohfink",
"given": "Anne M."
}
},
{
"id": "Lucchini-Matteo",
"name": {
"family": "Lucchini",
"given": "Matteo"
},
"orcid": "0000-0002-2235-3347"
},
{
"id": "Reynolds-Christopher-S",
"name": {
"family": "Reynolds",
"given": "Christopher S."
},
"orcid": "0000-0002-1510-4860"
},
{
"id": "Tombesi-Francesco",
"name": {
"family": "Tombesi",
"given": "Francesco"
},
"orcid": "0000-0002-6562-8654"
},
{
"id": "van-der-Klis-Michiel",
"name": {
"family": "van der Klis",
"given": "Michiel"
},
"orcid": "0000-0003-0070-9872"
},
{
"id": "Wang-Jingyi",
"name": {
"family": "Wang",
"given": "Jingyi"
},
"orcid": "0000-0002-1742-2125"
}
]
},
"title": "X-Ray Reverberation Mapping of Ark 564 Using Gaussian Process Regression",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "E.K., G.M., and J.A.G. acknowledge support from NASA grant 80NSSC20K0575. J.J. acknowledges support from the Leverhulme Trust, the Isaac Newton Trust, and St Edmund's College, University of Cambridge. A.I. acknowledges support from the Royal Society. G.M. and J.A.G. acknowledge support from NASA grant 80NSSC19K1020. J.A.G. also acknowledges support from the Alexander von Humboldt Foundation. This work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for their support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (nustardas), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). M.K. acknowledges support through an NWO (Nederlandse Organisatie voor Wetenschappelijk Onderzoek) Spinoza grant. C.S.R. thanks the UK Science and Technology Facilities Council (STFC) for support under the Consolidated Grant ST/S000623/1, as well as the European Research Council (ERC) for support under the European Union\u00e2s Horizon 2020 research and innovation program (grant 834203).",
"abstract": "Ark 564 is an extreme high-Eddington narrow-line Seyfert 1 galaxy, known for being one of the brightest, most rapidly variable soft X-ray active galactic nuclei (AGN), and for having one of the lowest temperature coronae. Here, we present a 410 ks NuSTAR observation and two 115 ks XMM-Newton observations of this unique source, which reveal a very strong, relativistically broadened iron line. We compute the Fourier-resolved time lags by first using Gaussian processes to interpolate the NuSTAR gaps, implementing the first employment of multitask learning for application in AGN timing. By simultaneously fitting the time lags and the flux spectra with the relativistic reverberation model reltrans, we constrain the mass at 2.3_(-1.3)^(+2.6) x 10^(6)M_(\u2299), although additional components are required to describe the prominent soft excess in this source. These results motivate future combinations of machine learning, Fourier-resolved timing, and the development of reverberation models.",
"date": "2022-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "939",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 109",
"id_number": "CaltechAUTHORS:20221128-494241100.41",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221128-494241100.41",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC20K0575"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1020"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/S000623/1"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "834203"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Isaac Newton Trust"
},
{
"agency": "St. Edmund's College, University of Cambridge"
},
{
"agency": "Royal Society"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ac978f",
"pub_year": "2022",
"author_list": "Lewin, Collin; Kara, Erin; et el."
},
{
"id": "https://authors.library.caltech.edu/records/me5qz-qs841",
"eprint_id": 117469,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:53:30",
"lastmod": "2023-10-24 22:32:12",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "Marianne"
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Maccarone-Thomas-J",
"name": {
"family": "Maccarone",
"given": "Thomas"
},
"orcid": "0000-0003-0976-4755"
},
{
"id": "Huppenkothen-Daniela",
"name": {
"family": "Huppenkothen",
"given": "Daniela"
},
"orcid": "0000-0002-1169-7486"
},
{
"id": "Israel-Gian-Luca",
"name": {
"family": "Israel",
"given": "Gian Luca"
},
"orcid": "0000-0001-5480-6438"
},
{
"id": "Barret-Didier",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Brumback-McKinley-C",
"name": {
"family": "Brumback",
"given": "McKinley"
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah P."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Forster-Karl",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "F\u00fcrst-Felix",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta D."
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Middleton-Matthew-J",
"name": {
"family": "Middleton",
"given": "Matthew"
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "Sean N."
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Pilla-Maura",
"name": {
"family": "Pilia",
"given": "Maura"
},
"orcid": "0000-0001-7397-8091"
},
{
"id": "Poutanen-Juri",
"name": {
"family": "Poutanen",
"given": "Juri"
},
"orcid": "0000-0002-0983-0049"
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Webb-Natalie-A",
"name": {
"family": "Webb",
"given": "Natalie"
}
},
{
"id": "Wilms-J\u00f6rn",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Orbital Decay in M82 X-2",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "The authors wish to thank Victoria Grinberg, W\u0142odek Klu\u017aniak, and Alessandro Ridolfi for useful discussions, and the staff at the NuSTAR Science Operations Center at Caltech for the help in scheduling the observations and the frequent clock-correction file updates, which allowed a prompt analysis of the data. We would also wish to thank the anonymous referee, and the three referees of a previous submission, who provided very insightful feedback that led to a substantial improvement of the quality of the analysis. M.B. was funded in part by PRIN TEC INAF 2019 \"SpecTemPolar!\u2014Timing analysis in the era of high-throughput photon detectors\". M.H. is supported by an ESO fellowship. G.L.I. and M.B. acknowledge funding from the Italian MIUR PRIN grant No. 2017LJ39LM. A.D.J. was funded in part by the Chandra grant No. 803-0000-716015-404H00-6100-2723-4210-40716015HH83121. J.P. was supported by the grant No. 14.W03.31.0021 of the Ministry of Science and Higher Education of the Russian Federation and the Academy of Finland grant No. 333112. D.J.W. acknowledges support from STFC in the form of an Ernest Rutherford Fellowship. H.P.E. acknowledges support under NASA Contract No. NNG08FD60C.\n\nAll the analysis of this paper was done using open-source software, Astropy, Stingray, HENDRICS, PINT, emcee, corner, and scinum, and can easily be verified using the solutions in Tables 1 and 2. The implementation of the Pletsch & Clark (2015) method can be found in the github repository https://github.com/matteobachetti/ell1fit. Figures were produced using the Matplotlib library and the Veusz software. The data used for this work come from the NuSTAR and XMM-Newton missions and are usually held private for one year, and made public on the High Energy Astrophysics Science archive (HEASARC) and the XMM-Newton Science Archive (XSA) afterwards. NuSTAR is a Small Explorer mission led by Caltech and managed by the JPL for NASA's Science Mission Directorate in Washington. NuSTAR was developed in partnership with the Danish Technical University and the Italian Space Agency (ASI). The spacecraft was built by Orbital Sciences Corp., Dulles, Virginia. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.",
"abstract": "M82 X-2 is the first pulsating ultraluminous X-ray source discovered. The luminosity of these extreme pulsars, if isotropic, implies an extreme mass transfer rate. An alternative is to assume a much lower mass transfer rate, but with an apparent luminosity boosted by geometrical beaming. Only an independent measurement of the mass transfer rate can help discriminate between these two scenarios. In this paper, we follow the orbit of the neutron star for 7 yr, measure the decay of the orbit (\u1e56_(orb) / P_(orb) \u2248 -8 \u2022 10\u207b\u2076 yr\u207b\u00b9), and argue that this orbital decay is driven by extreme mass transfer of more than 150 times the mass transfer limit set by the Eddington luminosity. If this is true, the mass available to the accretor is more than enough to justify its luminosity, with no need for beaming. This also strongly favors models where the accretor is a highly magnetized neutron star.",
"date": "2022-10-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "937",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 125",
"id_number": "CaltechAUTHORS:20221017-15547800.31",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221017-15547800.31",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN-TEC 2019"
},
{
"agency": "European Southern Observatory (ESO)"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "2017LJ39LM"
},
{
"agency": "NASA",
"grant_number": "803-0000-716015-404H00-6100-2723-4210-40716015HH 83121"
},
{
"agency": "Ministry of Science and Higher Education of the Russian Federation",
"grant_number": "14.W03.31.0021"
},
{
"agency": "Academy of Finland",
"grant_number": "333112"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "ESA Member States"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ac8d67",
"pub_year": "2022",
"author_list": "Bachetti, Matteo; Heida, Marianne; et el."
},
{
"id": "https://authors.library.caltech.edu/records/84d9r-p0f91",
"eprint_id": 119368,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:52:18",
"lastmod": "2023-10-23 20:12:50",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Zoglauer-Andreas",
"name": {
"family": "Zoglauer",
"given": "Andreas"
},
"orcid": "0000-0001-9067-3150"
}
]
},
"title": "NuSTAR non-x-ray background",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Mechanical Engineering; Astronomy and Astrophysics; Instrumentation; Control and Systems Engineering; Electronic, Optical and Magnetic Materials",
"note": "CC BY: \u00a9 2023 The Authors. Published by SPIE under a Creative Commons Attribution 4.0 International License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC, Italy) and the California Institute of Technology (USA). This material is based upon work supported by NASA under award number 80GSFC21M0002. We thank Dan Stern for constructive comments on this manuscript and to the anonymous referees for their feedback. The authors have no relevant financial interests in the manuscript and no other potential conflicts of interest to disclose. \n\nCode, Data, and Materials Availability. All data for this paper are publicly accessible via the NuSTAR repository in the High Energy Astrophysics Archive at NASA GSFC. Data were processed using the publicly available nustardas FTOOLs as described in this paper. All of the filtering and sorting steps are described in the text. Plots were produced using matpotlib in Python.\n\nPublished - 047001_1.pdf
",
"abstract": "We present an overview of the NuSTAR non x-ray background. This is dominated by proton scattering in the detector and surrounding material as well as activation lines from of material in the detector and its housing. We also discuss contributions from the solar component (when the Sun is active), and the impact of short-lived radiation belts on the NuSTAR background and activation in the detectors.",
"date": "2022-10",
"date_type": "published",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"volume": "8",
"number": "4",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"pagerange": "Art. No. 047001",
"id_number": "CaltechAUTHORS:20230221-18374200.17",
"issn": "2329-4124",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230221-18374200.17",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "80GSFC21M0002"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1117/1.jatis.8.4.047001",
"primary_object": {
"basename": "047001_1.pdf",
"url": "https://authors.library.caltech.edu/records/84d9r-p0f91/files/047001_1.pdf"
},
"pub_year": "2022",
"author_list": "Grefenstette, Brian W.; Madsen, Kristin K.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ycme0-wxv30",
"eprint_id": 119373,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:52:23",
"lastmod": "2023-10-25 14:39:06",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "Sean N."
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Mandigo-Stoba-Milan-Sharma",
"name": {
"family": "Mandigo-Stoba",
"given": "Milan Sharma"
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Cook-W-R",
"name": {
"family": "Cook",
"given": "Walter R., III"
}
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian"
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
}
]
},
"title": "Properties of Redlen cadmium zinc telluride with respect to x-ray spectroscopy",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Mechanical Engineering; Astronomy and Astrophysics; Instrumentation; Control and Systems Engineering; Electronic, Optical and Magnetic Materials",
"note": "\u00a9 2022 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nWe would like to thank the anonymous reviewers for their suggestions, which have significantly improved the quality of this work. This work was supported by NASA (Grant No. NNX13AC55G). Milan Sharma Mandigo-Stoba also acknowledges support from the Larson Fellowship via the Caltech Summer Undergraduate Research Fellowships program. To the best of our knowledge, there exist no conflicts of interest with regards to this manuscript.\n\nPublished - 046002_1.pdf
",
"abstract": "We present a study of a sample pixelated cadmium zinc telluride (CZT) detector using CZT purchased from Redlen Technologies. We demonstrate that the material shows good uniformity across the 2 cm \u00d7 2 cm \u00d7 3 mm crystal in terms of leakage current, gain, and spectral resolution. We find that the detector produces very good spectral resolution for energies up to at least 105 keV, achieving a full-width at half-maxima of 450 eV at 14 keV up to 880 eV at 105 keV using only single-pixel events. Though our analysis of spectra including multiple-pixel events is somewhat limited, we also produce a spectrum including events in which photon energy is deposited across two adjacent pixels. We find that this degrades the energy resolution by up to 30%, but this result can likely be improved using more rigorous calibrations. Additionally, we investigate depth-of-interaction effects, showing that spectral resolution can be improved by 3% to 7% for energies between 86 and 105 keV by removing events beyond a certain depth. Performing this cut reduces efficiency, removing 13% to 21% of photons from the resulting spectral lines.",
"date": "2022-10",
"date_type": "published",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"volume": "8",
"number": "4",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"pagerange": "Art. No. .046002",
"id_number": "CaltechAUTHORS:20230221-18374200.20",
"issn": "2329-4124",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230221-18374200.20",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX13AC55G"
},
{
"agency": "Caltech Summer Undergraduate Research Fellowship (SURF)"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1117/1.jatis.8.4.046002",
"primary_object": {
"basename": "046002_1.pdf",
"url": "https://authors.library.caltech.edu/records/ycme0-wxv30/files/046002_1.pdf"
},
"pub_year": "2022",
"author_list": "Pike, Sean N.; Mandigo-Stoba, Milan Sharma; et el."
},
{
"id": "https://authors.library.caltech.edu/records/htqqk-vr305",
"eprint_id": 117548,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:34:13",
"lastmod": "2023-10-23 20:06:59",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Forster-Karl",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
}
]
},
"title": "Effective area calibration of the Nuclear Spectroscopic Telescope Array",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Mechanical Engineering; Astronomy and Astrophysics; Instrumentation; Control and Systems Engineering; Electronic, Optical and Magnetic Materials",
"note": "\u00a9 The Authors. Published by SPIE under a Creative Commons Attribution 4.0 International License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. \n\nThis work was supported under NASA (Contract No. NNG08FD60C), and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC, Italy) and the California Institute of Technology (USA). This material is based upon work supported by NASA (award number 80GSFC21M0002). We thank Murray Brightman, Renee Ludlam, Guglielmo Mastroserio, and Riley Connors for performing the case study re-analyses in Sec. 7.2.\n\nPublished - 034003_1.pdf
",
"abstract": "We present here the updated calibration of the Nuclear Spectroscopic Telescope Array, which was performed using data on the Crab accumulated over the last nine years in orbit. The basis for this new calibration contains over 250 ks of focused Crab observations (imaged through the optics) and over 500 ks of stray-light (SL) Crab observations (not imaged through optics). We measured an epoch averaged spectrum of the SL Crab data and define a canonical Crab spectrum of \u0393 = 2.103 \u00b1 0.001 and N = 9.69 \u00b1 0.02 keV\u207b\u00b9 cm\u207b\u00b2\u2009s\u207b\u00b9 at 1 keV, which we use as our calibration standard. This calibration released in the Calibration Data Base update 20211020 provides significant updates to: (1) the detector absorption component, (2) the detector response function, and (3) the effective area vignetting function. The calibration improves agreement between FPMA and FPMB across detectors with a standard deviation of 1.7% for repeat observations between off-axis angles of 1' to 4'. As a consequence of the measured SL observations, the absolute flux of the instrument has increased by 5% to 15%, with 5% below 1' off-axis angle, 10% between 1 and 2', and 15% above 4'.",
"date": "2022-09",
"date_type": "published",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"volume": "8",
"number": "3",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"pagerange": "Art. No. 034003",
"id_number": "CaltechAUTHORS:20221024-125854800.17",
"issn": "2329-4124",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221024-125854800.17",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "80GSFC21M0002"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1117/1.jatis.8.3.034003",
"primary_object": {
"basename": "034003_1.pdf",
"url": "https://authors.library.caltech.edu/records/htqqk-vr305/files/034003_1.pdf"
},
"pub_year": "2022",
"author_list": "Madsen, Kristin K.; Forster, Karl; et el."
},
{
"id": "https://authors.library.caltech.edu/records/1azpx-42142",
"eprint_id": 114944,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:19:09",
"lastmod": "2023-10-24 15:16:08",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "De-Kishalay",
"name": {
"family": "De",
"given": "Kishalay"
},
"orcid": "0000-0002-8989-0542"
},
{
"id": "Mereminskiy-Ilya-A",
"name": {
"family": "Mereminskiy",
"given": "Ilya"
},
"orcid": "0000-0001-8931-1320"
},
{
"id": "Soria-Roberto",
"name": {
"family": "Soria",
"given": "Roberto"
},
"orcid": "0000-0002-4622-796X"
},
{
"id": "Conroy-Charlie",
"name": {
"family": "Conroy",
"given": "Charlie"
},
"orcid": "0000-0002-1590-8551"
},
{
"id": "Kara-Erin",
"name": {
"family": "Kara",
"given": "Erin"
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Anand-Shreya-G",
"name": {
"family": "Anand",
"given": "Shreya"
},
"orcid": "0000-0003-3768-7515"
},
{
"id": "Ashley-Michael-C-B",
"name": {
"family": "Ashley",
"given": "Michael C. B."
},
"orcid": "0000-0003-1412-2028"
},
{
"id": "Boyer-Martha-L",
"name": {
"family": "Boyer",
"given": "Martha L."
},
"orcid": "0000-0003-4850-9589"
},
{
"id": "Chakrabarty-Deepto",
"name": {
"family": "Chakrabarty",
"given": "Deepto"
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian"
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hankins-Matthew-J",
"name": {
"family": "Hankins",
"given": "Matthew J."
},
"orcid": "0000-0001-9315-8437"
},
{
"id": "Hillenbrand-L-A",
"name": {
"family": "Hillenbrand",
"given": "Lynne A."
}
},
{
"id": "Jencson-Jacob-E",
"name": {
"family": "Jencson",
"given": "Jacob E."
},
"orcid": "0000-0001-5754-4007"
},
{
"id": "Karambelkar-Viraj-R",
"name": {
"family": "Karambelkar",
"given": "Viraj"
},
"orcid": "0000-0003-2758-159X"
},
{
"id": "Kasliwal-M-M",
"name": {
"family": "Kasliwal",
"given": "Mansi M."
},
"orcid": "0000-0002-5619-4938"
},
{
"id": "Lau-Ryan-M",
"name": {
"family": "Lau",
"given": "Ryan M."
},
"orcid": "0000-0003-0778-0321"
},
{
"id": "Lutovinov-Alexander-A",
"name": {
"family": "Lutovinov",
"given": "Alexander"
},
"orcid": "0000-0002-6255-9972"
},
{
"id": "Moore-Anna-M",
"name": {
"family": "Moore",
"given": "Anna M."
},
"orcid": "0000-0002-2894-6936"
},
{
"id": "Ng-Mason",
"name": {
"family": "Ng",
"given": "Mason"
},
"orcid": "0000-0002-0940-6563"
},
{
"id": "Panagiotou-Christos",
"name": {
"family": "Panagiotou",
"given": "Christos"
}
},
{
"id": "Pasham-Dheeraj-R",
"name": {
"family": "Pasham",
"given": "Dheeraj R."
},
"orcid": "0000-0003-1386-7861"
},
{
"id": "Semena-Andrey-N",
"name": {
"family": "Semena",
"given": "Andrey"
}
},
{
"id": "Simcoe-Robert-A",
"name": {
"family": "Simcoe",
"given": "Robert"
},
"orcid": "0000-0003-3769-9559"
},
{
"id": "Soon-Jamie",
"name": {
"family": "Soon",
"given": "Jamie"
}
},
{
"id": "Srinivasaragavan-Gokul-P",
"name": {
"family": "Srinivasaragavan",
"given": "Gokul P."
}
},
{
"id": "Travouillon-Tony-D",
"name": {
"family": "Travouillon",
"given": "Tony"
},
"orcid": "0000-0002-7279-3658"
},
{
"id": "Yao-Yuhan",
"name": {
"family": "Yao",
"given": "Yuhan"
},
"orcid": "0000-0001-6747-8509"
}
]
},
"title": "SRGA J181414.6-225604: A New Galactic Symbiotic X-Ray Binary Outburst Triggered by an Intense Mass-loss Episode of a Heavily Obscured Mira Variable",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-ray surveys; Near infrared astronomy; Symbiotic binary stars; Asymptotic giant branch stars; Bondi accretion; Circumstellar dust",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 March 7; revised 2022 May 15; accepted 2022 May 17; published 2022 August 10. \n\nWe thank the anonymous referee for a careful reading of the manuscript and for providing valuable feedback that helped to improve its contents. We thank T. Maccarone, D. Rogantini, P. Pradhan, R. Remillard, and M Guenther for valuable discussions. We thank the Swift, NICER, and NuSTAR teams for approving the Target of Opportunity observations of the transient. Support for this work was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51477.001, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. \n\nPGIR is generously funded by Caltech, Australian National University, the Mt Cuba Foundation, the Heising-Simons Foundation, and the Bi-national Science Foundation. PGIR is a collaborative project among Caltech, Australian National University, University of New South Wales, Columbia University, and the Weizmann Institute of Science. This work is based on data from the Mikhail Pavlinsky ART-XC X-ray telescope on board the SRG observatory. The SRG observatory was built by Roskosmos in the interests of the Russian Academy of Sciences, represented by its Space Research Institute (IKI) in the framework of the Russian Federal Space Program, with the participation of the Deutsches Zentrum f\u00fcr Luft und Raumfahrt (DLR). The SRG spacecraft was designed, built, launched, and is operated by the Lavochkin Association and its subcontractors. The science data are downlinked via the Deep Space Network Antennae in Bear Lakes, Ussurijsk, and Baykonur, funded by Roskosmos. The ART-XC team thank the Russian Space Agency, the Russian Academy of Sciences, and State Corporation Rosatom, for the support for the SRG project and the ART-XC telescope, and the Lavochkin Association (NPOL) and partners for the creation and operation of the SRG spacecraft (Navigator). This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. We acknowledge the Visiting Astronomer Facility at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. \n\nThe work of I.M., A.L., and A.S. was supported by the Russian Science Foundation grant 19-12-00423. R.S. acknowledges grant No. 12073029 from the National Science Foundation of China. C.P. acknowledges financial support from the Swiss National Science Foundation (SNF). \n\nFacilities: ROSAT, INTEGRAL, XMM Newton, SRG: ART-XC, NICER, Swift, NuSTAR, PO: 0.3 m (PGIR), PO: 1.2 m (ZTF), PO: 1.5 m (SED Machine), PO: Hale (DBSP, TripleSpec), PanSTARRS, NEOWISE, IRTF (SpeX), Magellan: Baade (FIRE), SSO: ATT (WiFeS). \n\nSoftware: spextool (Cushing et al. 2004), xtellcor (Vacca et al. 2003), pypeit (Prochaska et al. 2020), nustardas (V2.1), Stingray (V0.3; Bachetti et al. 2021), xspec (Arnaud 1996), emcee (Foreman-Mackey et al. 2013), DUSTY (Ivezic & Elitzur 1997), HEAsoft (v6.29c; HEASARC 2014).\n\nPublished - De_2022_ApJ_935_36.pdf
Accepted Version - 2205.09139.pdf
",
"abstract": "We present the discovery and multiwavelength characterization of SRGA J181414.6-225604, a Galactic hard X-ray transient discovered during the ongoing SRG/ART-XC sky survey. Using data from the Palomar Gattini-IR survey, we identify a spatially and temporally coincident variable infrared (IR) source, IRAS 18111-2257, and classify it as a very-late-type (M7\u2013M8), long-period (1502 \u00b1 24 days), and luminous (M_K \u2248 \u22129.9 \u00b1 0.2) O-rich Mira donor star located at a distance of \u224814.6^(+2.9)_(\u22122.3) kpc. Combining multicolor photometric data over the last \u224825 yr, we show that the IR counterpart underwent a recent (starting \u2248800 days before the X-ray flare) enhanced mass-loss (reaching \u22482.1 \u00d7 10\u207b\u2075 M_\u2299 yr\u207b\u00b9) episode, resulting in an expanding dust shell obscuring the underlying star. Multi-epoch follow-up observations from Swift, NICER, and NuSTAR reveal a \u2248200 day long X-ray outburst reaching a peak luminosity of L_\u2093 \u2248 2.5 \u00d7 10\u00b3\u2076 erg s\u207b\u00b9, characterized by a heavily absorbed (N_H \u2248 6 \u00d7 10\u00b2\u00b2 cm\u207b\u00b2) X-ray spectrum consistent with an optically thick Comptonized plasma. The X-ray spectral and timing behavior suggest the presence of clumpy wind accretion, together with a dense ionized nebula overabundant in silicate material surrounding the compact object. Together, we show that SRGA J181414.6-225604 is a new symbiotic X-ray binary in outburst, triggered by an intense dust-formation episode of a highly evolved donor. Our results offer the first direct confirmation for the speculated connection between enhanced late-stage donor mass loss and the active lifetimes of symbiotic X-ray binaries.",
"date": "2022-08-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "935",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 36",
"id_number": "CaltechAUTHORS:20220526-173308925",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220526-173308925",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51477.001"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "Caltech"
},
{
"agency": "Australian National University"
},
{
"agency": "Mt. Cuba Astronomical Foundation"
},
{
"agency": "Heising-Simons Foundation"
},
{
"agency": "Binational Science Foundation (USA-Israel)"
},
{
"agency": "Roskosmos"
},
{
"agency": "Russian Space Agency"
},
{
"agency": "Russian Academy of Sciences"
},
{
"agency": "RosAtom"
},
{
"agency": "NASA",
"grant_number": "NNX-08AE38A"
},
{
"agency": "Russian Science Foundation",
"grant_number": "19-12-00423"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "12073029"
},
{
"agency": "Swiss National Science Foundation (SNSF)"
}
]
},
"local_group": {
"items": [
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"id": "Astronomy-Department"
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"doi": "10.3847/1538-4357/ac7c6e",
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"pub_year": "2022",
"author_list": "De, Kishalay; Mereminskiy, Ilya; et el."
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"items": [
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
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"orcid": "0000-0002-9639-4352"
},
{
"id": "Buisson-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "Douglas J. K."
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"orcid": "0000-0002-5341-6929"
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{
"id": "Dauser-Thomas",
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"family": "Dauser",
"given": "Thomas"
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"orcid": "0000-0003-4583-9048"
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"orcid": "0000-0002-9378-4072"
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"family": "F\u00fcrst",
"given": "Felix"
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"orcid": "0000-0003-0388-0560"
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{
"id": "Gallo-Luigi-C",
"name": {
"family": "Gallo",
"given": "Luigi C."
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"family": "Harrison",
"given": "Fiona A."
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"orcid": "0000-0003-2992-8024"
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"id": "Parker-Michael-L",
"name": {
"family": "Parker",
"given": "Michael L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Steiner-James-F",
"name": {
"family": "Steiner",
"given": "James F."
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"orcid": "0000-0002-5872-6061"
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"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
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{
"id": "Ubach-Santiago",
"name": {
"family": "Ubach",
"given": "Santiago"
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"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
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},
"title": "A NuSTAR and Swift view of the hard state of MAXI J1813\u2212095",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs, black hole physics, X-rays: binaries; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) \n\nReceived: 19 September 2021. Revision received: 15 May 2022. Accepted: 15 May 2022. Published: 20 May 2022. \n\nThis paper was written during the worldwide COVID-19 pandemic in 2020\u20132022. We acknowledge the hard work of all the health care workers around the world. We would not be able to finish this paper without their protection. JJ acknowledges support from the Leverhulme Trust, the Isaac Newton Trust, and St Edmund's College, University of Cambridge. \n\nDATA AVAILABILITY. All the data can be downloaded from the HEASARC website at https://heasarc.gsfc.nasa.gov. The reflionx and relxill models used in this work are available for downloads at https://www.michaelparker.space/reflionx-models and http://www.sternwarte.uni-erlangen.de/dauser/research/relxill.\n\nPublished - stac1401.pdf
Accepted Version - 2205.08227.pdf
",
"abstract": "We present an analysis of the NuSTAR and Swift spectra of the black hole candidate MAXI\u00a0J1813\u2212095 in a failed-transition outburst in 2018. The NuSTAR observations show evidence of reflected emission from the inner region of the accretion disc. By modelling the reflection component in the spectra, we find a disc inner radius of R\u1d62\u2099 < 7\u2009r\u2089. This result suggests that either a slightly truncated disc or a non-truncated disc forms at a few\u00a0per\u2009cent of the Eddington limit in MAXI\u00a0J1813\u2212095. Our best-fitting reflection models indicate that the geometry of the innermost accretion remains consistent during the period of NuSTAR observations. The spectral variability of MAXI\u00a0J1813\u2212095 from multi-epoch observations is dominated by the variable photon index of the Comptonization emission.",
"date": "2022-08",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "514",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1952-1960",
"id_number": "CaltechAUTHORS:20220712-629762000",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220712-629762000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Leverhulme Trust"
},
{
"agency": "Isaac Newton Trust"
},
{
"agency": "University of Cambridge"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
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"id": "NuSTAR"
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]
},
"doi": "10.1093/mnras/stac1401",
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"author_list": "Jiang, Jiachen; Buisson, Douglas J. K.; et el."
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"items": [
{
"id": "Masterson-Megan",
"name": {
"family": "Masterson",
"given": "Megan"
},
"orcid": "0000-0003-4127-0739"
},
{
"id": "Kara-Erin",
"name": {
"family": "Kara",
"given": "Erin"
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Ricci-Claudio",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "Ciro"
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Kosec-Peter",
"name": {
"family": "Kosec",
"given": "Peter"
},
"orcid": "0000-0003-4511-8427"
},
{
"id": "Remillard-Ronald-A",
"name": {
"family": "Remillard",
"given": "Ronald A."
},
"orcid": "0000-0003-4815-0481"
},
{
"id": "Loewenstein-Michael",
"name": {
"family": "Loewenstein",
"given": "Michael"
},
"orcid": "0000-0002-1661-4029"
},
{
"id": "Trakhtenbrot-Benny",
"name": {
"family": "Trakhtenbrot",
"given": "Benny"
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"orcid": "0000-0002-3683-7297"
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{
"id": "Arcavi-Iair",
"name": {
"family": "Arcavi",
"given": "Iair"
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"orcid": "0000-0001-7090-4898"
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]
},
"title": "Evolution of a Relativistic Outflow and X-Ray Corona in the Extreme Changing-look AGN 1ES 1927+654",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Active galactic nuclei; High energy astrophysics; Seyfert galaxies; Supermassive black holes; X-ray transient sources; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 March 9; revised 2022 May 23; accepted 2022 June 6; published 2022 July 22. \n\nWe thank the anonymous referee for the helpful comments that improved this manuscript. M.M. thanks Ruancun Li, Christos Panagiotou, and Brenna Mockler for their useful comments and discussions. E.K. thanks Daniel Proga and John Raymond for insightful discussions. M.M. and E.K. acknowledge support from NASA grant 80NSSC21K0661. M.M., E.K., B.T., and I.A. acknowledge support from the MISTI Global Seed Funds and the MIT-Israel Zuckerman STEM Fund. C.R. acknowledges support from the Fondecyt Iniciacion grant 11190831 and ANID BASAL project FB210003. R.R. acknowledges support from NASA grant 80NSSC19K1287. I.A. is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe Program and acknowledges support from that program, from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement No. 852097), from the Israel Science Foundation (grant No. 2752/19), from the United States\u2013Israel Binational Science Foundation (BSF), and from the Israeli Council for Higher Education Alon Fellowship. \n\nFacilities: XMM-Newton - , NuSTAR - , NICER. - \n\nSoftware: XSPEC (Arnaud 1996), Astropy (Astropy Collaboration et al. 2013, 2018), xillver (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), relxill (v1.4.0; Garc\u00eda et al. 2014; Dauser et al. 2014).\n\nPublished - Masterson_2022_ApJ_934_35.pdf
Accepted Version - 2206.05140.pdf
",
"abstract": "1ES 1927+654 is a paradigm-defying active galactic nucleus (AGN) and one of the most peculiar X-ray nuclear transients. In early 2018, this well-known AGN underwent a changing-look event, in which broad optical emission lines appeared and the optical flux increased. Yet, by 2018 July, the X-ray flux had dropped by over two orders of magnitude, indicating a dramatic change in the inner accretion flow. With three years of observations with NICER, XMM-Newton, and NuSTAR, we present the X-ray evolution of 1ES 1927+654, which can be broken down into three phases: (1) an early super-Eddington phase with rapid variability in X-ray luminosity and spectral parameters, (2) a stable super-Eddington phase at the peak X-ray luminosity, and (3) a steady decline back to the pre-outburst luminosity and spectral parameters. For the first time, we witnessed the formation of the X-ray corona, as the X-ray spectrum transitioned from thermally dominated to primarily Comptonized. We also track the evolution of the prominent, broad 1 keV feature in the early X-ray spectra and show that this feature can be modeled with blueshifted reflection (z = \u22120.33) from a single-temperature blackbody irradiating spectrum using xillverTDE, a new flavor of the xillver models. Thus, we propose that the 1 keV feature could arise from reflected emission off the base of an optically thick outflow from a geometrically thick, super-Eddington inner accretion flow, connecting the inner accretion flow with outflows launched during extreme accretion events (e.g., tidal disruption events). Lastly, we compare 1ES 1927+654 to other nuclear transients and discuss applications of xillverTDE to super-Eddington accretors.",
"date": "2022-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "934",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 35",
"id_number": "CaltechAUTHORS:20220726-998023000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220726-998023000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC21K0661"
},
{
"agency": "Massachusetts Institute of Technology (MIT)"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "11190831"
},
{
"agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)",
"grant_number": "FB210003"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1287"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "852097"
},
{
"agency": "Israel Science Foundation",
"grant_number": "2752/19"
},
{
"agency": "Binational Science Foundation (USA-Israel)"
},
{
"agency": "Israeli Council for Higher Education"
}
]
},
"local_group": {
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"doi": "10.3847/1538-4357/ac76c0",
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"pub_year": "2022",
"author_list": "Masterson, Megan; Kara, Erin; et el."
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"items": [
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah P."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "Marianne"
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta"
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Middleton-Matthew-J",
"name": {
"family": "Middleton",
"given": "Matthew J."
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"orcid": "0000-0002-8183-2970"
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{
"id": "Roberts-Timothy-P",
"name": {
"family": "Roberts",
"given": "Timothy P."
},
"orcid": "0000-0001-8252-6337"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
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"orcid": "0000-0001-5819-3552"
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},
"title": "The Variability Behavior of NGC 925 ULX-3",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Ultraluminous x-ray sources; X-ray sources; Neutron stars; Accretion; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 May 10; revised 2022 June 14; accepted 2022 June 15; published 2022 July 25. \n\nWe thank our anonymous referee for useful suggestions to improve this paper. We wish to thank Dan Stern for useful comments on this work. This work was supported by NASA grants 80NSSC20K1496 and 80NSSC21K0873, as well as by NASA contract NNG08FD60C. T.P.R. acknowledges funding from STFC consolidated grant ST/000244/1. \n\nWe wish to thank the Swift PI, Brad Cenko, for approving the target-of-opportunity requests we made to monitor NGC 925. We also wish to thank the NuSTAR PI, Fiona Harrison, for approving the DDT request to observe NGC 925 ULX-3 in 2019 December. The scientific results reported in this article are based on observations made by XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; observations by the NuSTAR mission, a project led by the California Institute of Technology, managed by JPL, and funded by NASA; and observations by the Swift mission, as well as public data from the Swift data archive provided by the UK Swift Science Data Centre at the University of Leicester. We thank the observing teams for these missions for carrying out these observations. \n\nFacilities: XMM - Newton X-Ray Multimirror Mission satellite, CXO - Chandra X-ray Observatory satellite, Swift(XRT) - Swift Gamma-Ray Burst Mission, NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission \n\nSoftware: astropy (Astropy Collaboration et al. 2013), CIAO (Fruscione et al. 2006), FTOOLS (Nasa High Energy Astrophysics Science Archive Research Center (Heasarc), 2014), XMM-Newton SAS, PIMMS, HENDRICS (Bachetti 2018; Huppenkothen et al. 2019).\n\nPublished - Earnshaw_2022_ApJ_934_42.pdf
Accepted Version - 2206.08397.pdf
",
"abstract": "We report the results of a 2019\u20132021 monitoring campaign with Swift and associated target-of-opportunity observations with XMM-Newton and NuSTAR, examining the spectral and timing behavior of the highly variable ultraluminous X-ray source (ULX) NGC 925 ULX-3. We find that the source exhibits a 127\u2013128-day periodicity, with fluxes typically ranging from 1 \u00d7 10\u207b\u00b9\u00b3 to 8 \u00d7 10\u207b\u00b9\u00b3 erg s\u207b\u00b9 cm\u207b\u00b2. We do not find strong evidence for a change in period over the time that NGC 925 ULX-3 has been observed, although the source may have been in a much lower flux state when first observed with Chandra in 2005. We do not detect pulsations, and we place an upper limit on the pulsed fraction of \u223c40% in the XMM-Newton band, consistent with some previous pulsation detections at low energies in other ULXs. The source exhibits a typical ULX spectrum that turns over in the NuSTAR band and can be fitted using two thermal components. These components have a high temperature ratio that may indicate the lack of extreme inner disk truncation by a magnetar-level magnetic field. We examine the implications for a number of different models for superorbital periods in ULXs, finding that a neutron star with a magnetic field of \u223c10\u00b9\u00b2 G may be plausible for this source. The future detection of pulsations from this source would allow for the further testing and constraining of such models.",
"date": "2022-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "934",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 42",
"id_number": "CaltechAUTHORS:20220726-997967000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220726-997967000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC20K1496"
},
{
"agency": "NASA",
"grant_number": "80NSSC21K0873"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/000244/1"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
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"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
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},
"doi": "10.3847/1538-4357/ac79b0",
"primary_object": {
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"title": "StrayCats. II. An Updated Catalog of NuSTAR Stray Light Observations",
"ispublished": "pub",
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"keywords": "X-ray surveys; Astrophysical black holes; Neutron stars; Low-mass x-ray binary stars; High mass x-ray binary stars; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 April 29; revised 2022 June 10; accepted 2022 June 20; published 2022 July 26. \n\nSupport for this work was provided by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51440.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work was additionally supported by NASA under grant No. 80NSSC19K1023 issued through the NNH18ZDA001N Astrophysics Data Analysis Program (ADAP). This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Ludlam_2022_ApJ_934_59.pdf
Accepted Version - 2206.09930.pdf
",
"abstract": "We present an updated catalog of StrayCats (a catalog of NuSTAR stray light observations of X-ray sources) that includes nearly 18 additional months of observations. StrayCats v2 has an added 53 sequence IDs, 106 rows, and three new identified stray light (SL) sources in comparison to the original catalog. The total catalog now has 489 unique sequence IDs, 862 entries, and 83 confirmed StrayCats sources. Additionally, we provide new resources for the community to gauge the utility and spectral state of the source in a given observation. We have created long-term light curves for each identified SL source using MAXI and Swift/BAT data when available. Further, source extraction regions for 632 identified SL observations were created and are available to the public. In this paper we present an overview of the updated catalog and new resources for each identified StrayCats SL source.",
"date": "2022-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "934",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 59",
"id_number": "CaltechAUTHORS:20220726-997906000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220726-997906000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA",
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},
{
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{
"agency": "NASA",
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}
]
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"title": "First Sagittarius A* Event Horizon Telescope Results. II. EHT and Multiwavelength Observations, Data Processing, and Calibration",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Black holes; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 February 28; revised 2022 April 4; accepted 2022 April 10; published 2022 May 12. \n\nWe thank an anonymous referee for their insight and helpful suggestions that have improved this paper. \n\nThe Event Horizon Telescope Collaboration thanks the following organizations and programs: the Academia Sinica; the Academy of Finland (projects 274477, 284495, 312496, 315721); the Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID), Chile via NCN19_058 (TITANs) and Fondecyt 1221421, the Alexander von Humboldt Stiftung; an Alfred P. Sloan Research Fellowship; Allegro, the European ALMA Regional Centre node in the Netherlands, the NL astronomy research network NOVA and the astronomy institutes of the University of Amsterdam, Leiden University and Radboud University; the ALMA North America Development Fund; the Black Hole Initiative, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation (although the opinions expressed in this work are those of the author(s) and do not necessarily reflect the views of these Foundations); Chandra DD7-18089X and TM6-17006X; the China Scholarship Council; China Postdoctoral Science Foundation fellowship (2020M671266); Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT, Mexico, projects U0004-246083, U0004-259839, F0003-272050, M0037-279006, F0003-281692, 104497, 275201, 263356); the Consejer\u00eda de Econom\u00eda, Conocimiento, Empresas y Universidad of the Junta de Andaluc\u00eda (grant P18-FR-1769), the Consejo Superior de Investigaciones Cient\u00edficas (grant 2019AEP112); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Direcci\u00f3n General de Asuntos del Personal Acad\u00e9mico-Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM, projects IN112417 and IN112820); the Dutch Organization for Scientific Research (NWO) VICI award (grant 639.043.513) and grant OCENW.KLEIN.113; the Dutch National Supercomputers, Cartesius and Snellius (NWO Grant 2021.013); the EACOA Fellowship awarded by the East Asia Core Observatories Association, which consists of the Academia Sinica Institute of Astronomy and Astrophysics, the National Astronomical Observatory of Japan, Center for Astronomical Mega-Science, Chinese Academy of Sciences, and the Korea Astronomy and Space Science Institute; the European Research Council (ERC) Synergy Grant \"BlackHoleCam: Imaging the Event Horizon of Black Holes\" (grant 610058); the European Union Horizon 2020 research and innovation programme under grant agreements RadioNet (No 730562) and M2FINDERS (No 101018682); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177 and GenT Program (project CIDEGENT/2018/021); MICINN Research Project PID2019-108995GB-C22; the European Research Council for advanced grant \"JETSET: Launching, propagation and emission of relativistic jets from binary mergers and across mass scales\" (Grant No. 884631); the Institute for Advanced Study; the Istituto Nazionale di Fisica Nucleare (INFN) sezione di Napoli, iniziative specifiche TEONGRAV; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; DFG research grant \"Jet physics on horizon scales and beyond\" (Grant No. FR 4069/2-1); Joint Princeton/Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships, research at the Flatiron Institute is supported by the Simons Foundation; the Japan Ministry of Education, Culture, Sports, Science and Technology (MEXT; grant JPMXP1020200109); the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship (JP17J08829); the Joint Institute for Computational Fundamental Science, Japan; the Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057, QYZDJSSW-SYS008, ZDBS-LY-SLH011); the Leverhulme Trust Early Career Research Fellowship; the Max-Planck-Gesellschaft (MPG); the Max Planck Partner Group of the MPG and the CAS; the MEXT/JSPS KAKENHI (grants 18KK0090, JP21H01137, JP18H03721, JP18K13594, 18K03709, JP19K14761, 18H01245, 25120007); the Malaysian Fundamental Research Grant Scheme (FRGS) FRGS/1/2019/STG02/UM/02/6; the MIT International Science and Technology Initiatives (MISTI) Funds; the Ministry of Science and Technology (MOST) of Taiwan (103-2119-M-001-010-MY2, 105-2112-M-001-025-MY3, 105-2119-M-001-042, 106-2112-M-001-011, 106-2119-M-001-013, 106-2119-M-001-027, 106-2923-M-001-005, 107-2119-M-001-017, 107-2119-M-001-020, 107-2119-M-001-041, 107-2119-M-110-005, 107-2923-M-001-009, 108-2112-M-001-048, 108-2112-M-001-051, 108-2923-M-001-002, 109-2112-M-001-025, 109-2124-M-001-005, 109-2923-M-001-001, 110-2112-M-003-007-MY2, 110-2112-M-001-033, 110-2124-M-001-007, and 110-2923-M-001-001); the Ministry of Education (MoE) of Taiwan Yushan Young Scholar Program; the Physics Division, National Center for Theoretical Sciences of Taiwan; the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC20K1567, NASA Astrophysics Theory Program grant 80NSSC20K0527, NASA NuSTAR award 80NSSC20K0645); NASA Hubble Fellowship grant HST-HF2-51431.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555; the National Institute of Natural Sciences (NINS) of Japan; the National Key Research and Development Program of China (grant 2016YFA0400704, 2017YFA0402703, 2016YFA0400702); the National Science Foundation (NSF, grants AST-0096454, AST-0352953, AST-0521233, AST-0705062, AST-0905844, AST-0922984, AST-1126433, AST-1140030, DGE-1144085, AST-1207704, AST-1207730, AST-1207752, MRI-1228509, OPP-1248097, AST-1310896, AST-1440254, AST-1555365, AST-1614868, AST-1615796, AST-1715061, AST-1716327, AST-1716536, OISE-1743747, AST-1816420, AST-1935980, AST-2034306); NSF Astronomy and Astrophysics Postdoctoral Fellowship (AST-1903847); the Natural Science Foundation of China (grants 11650110427, 10625314, 11721303, 11725312, 11873028, 11933007, 11991052, 11991053, 12192220, 12192223); the Natural Sciences and Engineering Research Council of Canada (NSERC, including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral Program); the National Youth Thousand Talents Program of China; the National Research Foundation of Korea (the Global PhD Fellowship Grant: grants NRF-2015H1A2A1033752, the Korea Research Fellowship Program: NRF-2015H1D3A1066561, Brain Pool Program: 2019H1D3A1A01102564, Basic Research Support Grant 2019R1F1A1059721, 2021R1A6A3A01086420, 2022R1C1C1005255); Netherlands Research School for Astronomy (NOVA) Virtual Institute of Accretion (VIA) postdoctoral fellowships; Onsala Space Observatory (OSO) national infrastructure, for the provisioning of its facilities/observational support (OSO receives funding through the Swedish Research Council under grant 2017-00648); the Perimeter Institute for Theoretical Physics (research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science and Economic Development and by the Province of Ontario through the Ministry of Research, Innovation and Science); the Spanish Ministerio de Ciencia e Innovaci\u00f3n (grants PGC2018-098915-B-C21, AYA2016-80889-P, PID2019-108995GB-C21, PID2020-117404GB-C21); the University of Pretoria for financial aid in the provision of the new Cluster Server nodes and SuperMicro (USA) for a SEEDING GRANT approved towards these nodes in 2020; the Shanghai Pilot Program for Basic Research, Chinese Academy of Science, Shanghai Branch (JCYJ-SHFY-2021-013); the State Agency for Research of the Spanish MCIU through the \"Center of Excellence Severo Ochoa\" award for the Instituto de Astrof\u00edsica de Andaluc\u00eda (SEV-2017- 0709); the Spinoza Prize SPI 78-409; the South African Research Chairs Initiative, through the South African Radio Astronomy Observatory (SARAO, grant ID 77948), which is a facility of the National Research Foundation (NRF), an agency of the Department of Science and Innovation (DSI) of South Africa; the Toray Science Foundation; Swedish Research Council (VR); the US Department of Energy (USDOE) through the Los Alamos National Laboratory (operated by Triad National Security, LLC, for the National Nuclear Security Administration of the USDOE (Contract 89233218CNA000001); and the YCAA Prize Postdoctoral Fellowship. \n\nWe thank the staff at the participating observatories, correlation centers, and institutions for their enthusiastic support. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.01154.V. ALMA is a partnership of the European Southern Observatory (ESO; Europe, representing its member states), NSF, and National Institutes of Natural Sciences of Japan, together with National Research Council (Canada), Ministry of Science and Technology (MOST; Taiwan), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA; Taiwan), and Korea Astronomy and Space Science Institute (KASI; Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities, Inc. (AUI)/NRAO, and the National Astronomical Observatory of Japan (NAOJ). The NRAO is a facility of the NSF operated under cooperative agreement by AUI. This research used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC05-00OR22725. We also thank the Center for Computational Astrophysics, National Astronomical Observatory of Japan. The computing cluster of Shanghai VLBI correlator supported by the Special Fund for Astronomy from the Ministry of Finance in China is acknowledged. \n\nAPEX is a collaboration between the Max-Planck-Institut f\u00fcr Radioastronomie (Germany), ESO, and the Onsala Space Observatory (Sweden). The SMA is a joint project between the SAO and ASIAA and is funded by the Smithsonian Institution and the Academia Sinica. The JCMT is operated by the East Asian Observatory on behalf of the NAOJ, ASIAA, and KASI, as well as the Ministry of Finance of China, Chinese Academy of Sciences, and the National Key Research and Development Program (No. 2017YFA0402700) of China and Natural Science Foundation of China grant 11873028. Additional funding support for the JCMT is provided by the Science and Technologies Facility Council (UK) and participating universities in the UK and Canada. The LMT is a project operated by the Instituto Nacional de Astr\u00f3fisica, \u00d3ptica, y Electr\u00f3nica (Mexico) and the University of Massachusetts at Amherst (USA). The IRAM 30-m telescope on Pico Veleta, Spain is operated by IRAM and supported by CNRS (Centre National de la Recherche Scientifique, France), MPG (Max-Planck-Gesellschaft, Germany) and IGN (Instituto Geogr\u00e1fico Nacional, Spain). The SMT is operated by the Arizona Radio Observatory, a part of the Steward Observatory of the University of Arizona, with financial support of operations from the State of Arizona and financial support for instrumentation development from the NSF. Support for SPT participation in the EHT is provided by the National Science Foundation through award OPP-1852617 to the University of Chicago. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago. The SPT hydrogen maser was provided on loan from the GLT, courtesy of ASIAA. \n\nThis work used the Extreme Science and Engineering Discovery Environment (XSEDE), supported by NSF grant ACI-1548562, and CyVerse, supported by NSF grants DBI-0735191, DBI-1265383, and DBI-1743442. XSEDE Stampede2 resource at TACC was allocated through TG-AST170024 and TG-AST080026N. XSEDE JetStream resource at PTI and TACC was allocated through AST170028. This research is part of the Frontera computing project at the Texas Advanced Computing Center through the Frontera Large-Scale Community Partnerships allocation AST20023. Frontera is made possible by National Science Foundation award OAC-1818253. This research was carried out using resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy Office of Science. Additional work used ABACUS2.0, which is part of the eScience center at Southern Denmark University. Simulations were also performed on the SuperMUC cluster at the LRZ in Garching, on the LOEWE cluster in CSC in Frankfurt, on the HazelHen cluster at the HLRS in Stuttgart, and on the Pi2.0 and Siyuan Mark-I at Shanghai Jiao Tong University. The computer resources of the Finnish IT Center for Science (CSC) and the Finnish Computing Competence Infrastructure (FCCI) project are acknowledged. This research was enabled in part by support provided by Compute Ontario (http://computeontario.ca), Calcul Quebec (http://www.calculquebec.ca) and Compute Canada (http://www.computecanada.ca). \n\nThe EHTC has received generous donations of FPGA chips from Xilinx Inc., under the Xilinx University Program. The EHTC has benefited from technology shared under open-source license by the Collaboration for Astronomy Signal Processing and Electronics Research (CASPER). The EHT project is grateful to T4Science and Microsemi for their assistance with Hydrogen Masers. This research has made use of NASA's Astrophysics Data System. We gratefully acknowledge the support provided by the extended staff of the ALMA, both from the inception of the ALMA Phasing Project through the observational campaigns of 2017 and 2018. We would like to thank A. Deller and W. Brisken for EHT-specific support with the use of DiFX. We thank Martin Shepherd for the addition of extra features in the Difmap software that were used for the CLEAN imaging results presented in this paper. We acknowledge the significance that Maunakea, where the SMA and JCMT EHT stations are located, has for the indigenous Hawaiian people. \n\nThe scientific results reported here are also based in part on observations made by the East Asian VLBI Network (EAVN), the Global 3 mm VLBI Array (GMVA), the Very Large Telescope (VLT), the Neil Gehrels Swift Observatory, the Chandra X-ray Observatory, and the Nuclear Spectroscopic Telescope (NuSTAR). We thank the scheduling, data processing, and archive teams from these facilities for making these observations possible. IMV acknowledges the use of LLuis Vives HPC resources of the University of Valencia. \n\nFacility: EHT, ALMA, APEX, IRAM:30 m, JCMT, LMT, SMA, ARO:SMT, SPT, Chandra, EAVN, GMVA, NuSTAR, Swift, VLT. \n\nSoftware: DiFX (Deller et al. 2011), CALC, PolConvert (Mart\u00ed-Vidal et al. 2016), HOPS (Whitney et al. 2004), EHT-HOPS Pipeline (Blackburn et al. 2019), CASA (McMullin et al. 2007), rPICARD (Janssen et al. 2018, 2019b).\n\nPublished - Akiyama_2022_ApJL_930_L13.pdf
",
"abstract": "We present Event Horizon Telescope (EHT) 1.3 mm measurements of the radio source located at the position of the supermassive black hole Sagittarius A* (Sgr A*), collected during the 2017 April 5\u201311 campaign. The observations were carried out with eight facilities at six locations across the globe. Novel calibration methods are employed to account for Sgr A*'s flux variability. The majority of the 1.3 mm emission arises from horizon scales, where intrinsic structural source variability is detected on timescales of minutes to hours. The effects of interstellar scattering on the image and its variability are found to be subdominant to intrinsic source structure. The calibrated visibility amplitudes, particularly the locations of the visibility minima, are broadly consistent with a blurred ring with a diameter of \u223c50 \u03bcas, as determined in later works in this series. Contemporaneous multiwavelength monitoring of Sgr A* was performed at 22, 43, and 86 GHz and at near-infrared and X-ray wavelengths. Several X-ray flares from Sgr A* are detected by Chandra, one at low significance jointly with Swift on 2017 April 7 and the other at higher significance jointly with NuSTAR on 2017 April 11. The brighter April 11 flare is not observed simultaneously by the EHT but is followed by a significant increase in millimeter flux variability immediately after the X-ray outburst, indicating a likely connection in the emission physics near the event horizon. We compare Sgr A*'s broadband flux during the EHT campaign to its historical spectral energy distribution and find that both the quiescent emission and flare emission are consistent with its long-term behavior.",
"date": "2022-05-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "930",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L13",
"id_number": "CaltechAUTHORS:20220721-8952000",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220721-8952000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Academia Sinica"
},
{
"agency": "Academy of Finland",
"grant_number": "274477"
},
{
"agency": "Academy of Finland",
"grant_number": "284495"
},
{
"agency": "Academy of Finland",
"grant_number": "312496"
},
{
"agency": "Academy of Finland",
"grant_number": "315721"
},
{
"agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)",
"grant_number": "NCN19_058"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1221421"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "Alfred P. Sloan Foundation"
},
{
"agency": "Allegro"
},
{
"agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)"
},
{
"agency": "ALMA North America Development Fund"
},
{
"agency": "Black Hole Initiative"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "Gordon and Betty Moore Foundation"
},
{
"agency": "NASA",
"grant_number": "DD7-18089X"
},
{
"agency": "NASA",
"grant_number": "TM6-17006X"
},
{
"agency": "China Scholarship Council"
},
{
"agency": "China Postdoctoral Science Foundation",
"grant_number": "2020M671266"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "U0004-246083"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "U0004-259839"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "F0003-272050"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "M0037-279006"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "F0003-281692"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "104497"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "275201"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "263356"
},
{
"agency": "Junta de Andaluc\u00eda",
"grant_number": "P18-FR-1769"
},
{
"agency": "Consejo Superior de Investigaciones Cient\u00edficas",
"grant_number": "2019AEP112"
},
{
"agency": "Perimeter Institute for Theoretical Physics"
},
{
"agency": "Direcci\u00f3n General de Asuntos del Personal Acad\u00e9mico-Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)",
"grant_number": "IN112417"
},
{
"agency": "Direcci\u00f3n General de Asuntos del Personal Acad\u00e9mico-Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)",
"grant_number": "IN112820"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)",
"grant_number": "639.043.513"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)",
"grant_number": "OCENW.KLEIN.113"
},
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"title": "An 8.56 keV Absorption Line in the Hyperluminous X-Ray Source in NGC 4045: Ultrafast Outflow or Cyclotron Line?",
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"keywords": "Ultraluminous x-ray sources; X-ray sources; X-ray transient sources; Neutron stars; Black holes; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 January 14; revised 2022 March 8; accepted 2022 March 14; published 2022 April 21. \n\nWe thank the anonymous referee for their review of this manuscript and for their constructive input. \n\nWe wish to thank the Swift PI, Brad Cenko, for approving the target of opportunity requests we made to observe NGC 4045 ULX, as well as the rest of the Swift team for carrying them out. We also acknowledge the use of public data from the Swift data archive. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. \n\nWe also wish to thank the NuSTAR PI, Fiona Harrison, for approving the DDT request we made to observe NGC 4045 ULX, as well as the NuSTAR SOC for carrying out the observation. This work was also supported under NASA contract No. NNG08FD60C. NuSTAR is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nIn addition, we wish to thank Belinda Wilkes, Director of the Chandra X-ray Center for approving the DDT request to observe NGC 4045 ULX and the Chandra team for carrying out the observation. \n\nFinally, we wish to thank Timothy Kallman for help in generating XSTAR models for XSPEC that were used in the analysis. \n\nThis work was also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. \n\nThis research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. \n\nThe work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. \n\nFacilities: Swift - Swift Gamma-Ray Burst Mission, NuSTAR - , CXO - , XMM. - \n\nSoftware: NuSTARDAS, XMMSAS (Gabriel et al. 2004), XSPEC (Arnaud 1996), spex, (Kaastra et al. 1996), hendrics (Bachetti 2015).\n\nPublished - Brightman_2022_ApJ_929_138.pdf
Accepted Version - 2203.11955.pdf
",
"abstract": "We report on the discovery of an absorption line at E 8.56_(-0.11)^(+0.05) keV detected with a significance of >3.3\u03c3 in the NuSTAR and XMM-Newton spectra of a newly discovered hyperluminous X-ray source (L\u2093 > 10\u2074\u00b9 erg s\u207b\u00b9) in the galaxy NGC 4045 at a distance of 32 Mpc. The source was first discovered serendipitously in a Swift/XRT observation of the galaxy, and Swift monitoring reveals a highly variable source changing by over an order of magnitude from maximum to minimum. The origin of the absorption line appears likely to be from highly ionized iron with a blueshift of 0.19c, indicating an ultrafast outflow. However, the large equivalent width of the line (EW = -0.22_(-0.09)^(+0.08) keV) paired with the lack of other absorption lines detected is difficult to reconcile with models. An alternative explanation is that the line is due to a cyclotron resonance scattering feature produced by the interaction of X-ray photons with the powerful magnetic field of a neutron star.",
"date": "2022-04-20",
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"publication": "Astrophysical Journal",
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"pagerange": "Art. No. 138",
"id_number": "CaltechAUTHORS:20220525-90131000",
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"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220525-90131000",
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{
"name": {
"family": "Gendreau",
"given": "K."
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{
"id": "Granot-Jonathan",
"name": {
"family": "Granot",
"given": "J."
},
"orcid": "0000-0001-8530-8941"
},
{
"name": {
"family": "Hailey",
"given": "C."
},
"orcid": "0000-0002-3681-145X"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
},
{
"name": {
"family": "Hartmann",
"given": "D."
},
"orcid": "0000-0002-8028-0991"
},
{
"name": {
"family": "Kaper",
"given": "L."
},
"orcid": "0000-0001-8025-8981"
},
{
"name": {
"family": "Kutyrev",
"given": "A."
},
"orcid": "0000-0002-2715-8460"
},
{
"name": {
"family": "Slane",
"given": "P. O."
},
"orcid": "0000-0002-6986-6756"
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"name": {
"family": "Troja",
"given": "E."
},
"orcid": "0000-0002-1869-7817"
},
{
"name": {
"family": "van der Horst",
"given": "A. J."
},
"orcid": "0000-0001-9149-6707"
},
{
"name": {
"family": "Wijers",
"given": "R. A. M. J."
},
"orcid": "0000-0002-3101-1808"
},
{
"name": {
"family": "Woudt",
"given": "P."
},
"orcid": "0000-0002-6896-1655"
}
]
},
"title": "Identification of an X-Ray Pulsar in the BeXRB System IGR J18219\u22121347",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-ray astronomy; High mass x-ray binary stars; Pulsars; Neutron stars",
"note": "\u00a9 2022 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 November 24; revised 2022 January 21; accepted 2022 January 24; published 2022 March 10. \n\nThe authors acknowledge useful discussions with Matteo Bachetti, Tomaso Belloni, and Oleg Kargaltsev. B.O., C.K., and N.G. acknowledge supported under NASA Grants 80NSSC20K0389 and 80NSSC19K091. L.J.T. is supported by the South African National Research Foundation. J.G. acknowledges support by the ISF-NSFC joint research program (grant No. 3296/19). \n\nThis work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC, Italy) and the California Institute of Technology (Caltech, USA). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. These results also made use of Lowell Observatory's Lowell Discovery Telescope (LDT), formerly the Discovery Channel Telescope. Lowell operates the LDT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the LDT was provided by Discovery Communications. LMI was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) under program 2018-2-LSP-001. We additionally made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). \n\nFacilities: Swift - Swift Gamma-Ray Burst Mission, NuSTAR - , NICER - , SALT - , LDT - , UKIRT - , ZTF - , PS1. - \n\nSoftware: HEASoft v6.27.2, XRTDAS, NuSTARDAS v1.9.2, NICERDAS v7a, XSPEC v12.11.0 (Arnaud 1996), IRAF (Tody 1986), DAOPHOT (Stetson 1987), SExtractor (Bertin & Arnouts 1996), Swarp (Bertin 2010), SCAMP (Bertin 2006), astrometry.net (Lang et al. 2010), Stingray (Huppenkothen et al. 2019), Astropy (Astropy Collaboration et al. 2013).\n\nPublished - OConnor_2022_ApJ_927_139.pdf
Submitted - 2111-12592.pdf
",
"abstract": "We report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219\u22121347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with P_(spin) = 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10\u201315 kpc for the source. The broadband X-ray spectrum (1.5\u201350 keV) of the source is described by an absorbed power law with a photon index \u0393 \u223c 0.5 and a cutoff energy at \u223c13 keV.",
"date": "2022-03-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "927",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 139",
"id_number": "CaltechAUTHORS:20220119-233939590",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220119-233939590",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC20K0389"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K091"
},
{
"agency": "National Research Foundation (South Africa)"
},
{
"agency": "Israel Science Foundation"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "3296/19"
},
{
"agency": "NSF",
"grant_number": "AST-1005313"
},
{
"agency": "Southern African Large Telescope (SALT)",
"grant_number": "2018-2-LSP-001"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
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{
"id": "NuSTAR"
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]
},
"doi": "10.3847/1538-4357/ac5032",
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"basename": "2111-12592.pdf",
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"basename": "OConnor_2022_ApJ_927_139.pdf",
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}
],
"pub_year": "2022",
"author_list": "O'Connor, B.; G\u00f6\u011f\u00fc\u015f, E.; et el."
},
{
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"eprint_id": 113722,
"eprint_status": "archive",
"datestamp": "2023-08-22 14:32:51",
"lastmod": "2023-10-23 19:11:17",
"type": "article",
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"creators": {
"items": [
{
"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "Sean N."
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Negoro-Hitoshi",
"name": {
"family": "Negoro",
"given": "Hitoshi"
},
"orcid": "0000-0003-0939-1178"
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Brumback-McKinley-C",
"name": {
"family": "Brumback",
"given": "McKinley"
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "Connors-Riley-M-T",
"name": {
"family": "Connors",
"given": "Riley M. T."
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian"
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hare-Jeremy",
"name": {
"family": "Hare",
"given": "Jeremy"
},
"orcid": "0000-0002-8548-482X"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta"
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Mastroserio-Guglielmo",
"name": {
"family": "Mastroserio",
"given": "Guglielmo"
},
"orcid": "0000-0003-4216-7936"
},
{
"id": "Mihara-Tatehiro",
"name": {
"family": "Mihara",
"given": "Tatehiro"
},
"orcid": "0000-0002-6337-7943"
},
{
"id": "Shidatsu-Megumi",
"name": {
"family": "Shidatsu",
"given": "Megumi"
},
"orcid": "0000-0001-8195-6546"
},
{
"id": "Sugizaka-Mutsumi",
"name": {
"family": "Sugizaki",
"given": "Mutsumi"
},
"orcid": "0000-0002-1190-0720"
},
{
"id": "Takagi-Ryohei",
"name": {
"family": "Takagi",
"given": "Ryohei"
}
}
]
},
"title": "MAXI and NuSTAR Observations of the Faint X-Ray Transient MAXI J1848-015 in the GLIMPSE-C01 Cluster",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Black holes; High energy astrophysics; Compact objects; Stellar mass black holes; X-ray binary stars; Accretion; Neutron stars",
"note": "\u00a9 2022 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 November 9; revised 2022 January 20; accepted 2022 February 5; published 2022 March 15. \n\nThis work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nR.M.L. acknowledges the support of NASA through Hubble Fellowship Program grant HST-HF2-51440.001. J.H. acknowledges support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the Universities Space Research Association under contract with NASA. A.J. would like to acknowledge support from Chandra X-ray Observatory Center's grant GO0-21067X. \n\nThis work also made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. Part of this work was financially supported by Grants-in-Aid for Scientific Research 21K03620 (H.N.), 17H06362 (H.N.), and 19K14762 (M.S.) from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. \n\nFinally, we would like to thank the anonymous reviewer, whose comments and suggestions significantly improved the quality of this work. \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018), Corner (Foreman-Mackey 2016), DS9 (Joye & Mandel 2003), Matplotlib (Hunter 2007), Scipy (Virtanen et al. 2020), Stingray (Huppenkothen et al. 2019), relxill (Dauser et al. 2014; Garc\u00eda et al. 2014), XSpec (Arnaud 1996).\n\nPublished - Pike_2022_ApJ_927_190.pdf
Accepted Version - 2202.02883.pdf
",
"abstract": "We present the results of Monitor of All-sky X-ray Image (MAXI) monitoring and two Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the recently discovered faint X-ray transient MAXI J1848015. Analysis of the MAXI light curve shows that the source underwent a rapid flux increase beginning on 2020 December 20, followed by a rapid decrease in flux after only \u223c5 days. NuSTAR observations reveal that the source transitioned from a bright soft state with unabsorbed, bolometric (0.1\u2013100 keV) flux F = 6.9 \u00b1 0.1 \u00d7 10\u207b\u00b9\u2070 erg cm\u207b\u00b2 s\u207b\u00b9, to a low hard state with flux F = 2.85 \u00b1 0.04 \u00d7 10\u207b\u00b9\u2070 erg cm\u207b\u00b2 s\u207b\u00b9. Given a distance of 3.3 kpc, inferred via association of the source with the GLIMPSE-C01 cluster, these fluxes correspond to an Eddington fraction of the order of 10\u207b\u00b3 for an accreting neutron star (NS) of mass M = 1.4M\u2299, or even lower for a more massive accretor. However, the source spectra exhibit strong relativistic reflection features, indicating the presence of an accretion disk that extends close to the accretor, for which we measure a high spin, a = 0.967 \u00b1 0.013. In addition to a change in flux and spectral shape, we find evidence for other changes between the soft and hard states, including moderate disk truncation with the inner disk radius increasing from R_(in) \u2248 3 R_g to R_(in) \u2248 8 R_g, narrow Fe emission whose centroid decreases from 6.8 \u00b1 0.1 keV to 6.3 \u00b1 0.1 keV, and an increase in low-frequency (10\u207b\u00b3\u201310\u207b\u00b9 Hz) variability. Due to the high spin, we conclude that the source is likely to be a black hole rather than an NS, and we discuss physical interpretations of the low apparent luminosity as well as the narrow Fe emission.",
"date": "2022-03-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "927",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 190",
"id_number": "CaltechAUTHORS:20220304-000054911",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220304-000054911",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "NASA",
"grant_number": "GO0-21067X"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)",
"grant_number": "21K03620"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)",
"grant_number": "17H06362"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)",
"grant_number": "19K14762"
},
{
"agency": "NASA Einstein Fellowship"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
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]
},
"doi": "10.3847/1538-4357/ac5258",
"primary_object": {
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"basename": "Pike_2022_ApJ_927_190.pdf",
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}
],
"pub_year": "2022",
"author_list": "Pike, Sean N.; Negoro, Hitoshi; et el."
},
{
"id": "https://authors.library.caltech.edu/records/3mzv9-ab577",
"eprint_id": 113812,
"eprint_status": "archive",
"datestamp": "2023-08-22 14:28:42",
"lastmod": "2023-10-23 23:14:46",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Cackett-Edward-M",
"name": {
"family": "Cackett",
"given": "E. M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Miller-Jon-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Stevens-Abigail-L",
"name": {
"family": "Stevens",
"given": "A. L."
},
"orcid": "0000-0002-5041-3079"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Homan-Jeroen",
"name": {
"family": "Homan",
"given": "J."
},
"orcid": "0000-0001-8371-2713"
},
{
"id": "Ng-Mason",
"name": {
"family": "Ng",
"given": "M."
},
"orcid": "0000-0002-0940-6563"
},
{
"id": "Guillot-Sebastien",
"name": {
"family": "Guillot",
"given": "S."
},
"orcid": "0000-0002-6449-106X"
},
{
"id": "Buisson-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "D. J. K."
}
},
{
"id": "Chakrabarty-Deepto",
"name": {
"family": "Chakrabarty",
"given": "D."
},
"orcid": "0000-0001-8804-8946"
}
]
},
"title": "Radius Constraints from Reflection Modeling of Cygnus X-2 with NuSTAR and NICER",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Neutron stars; Low-mass x-ray binary stars; Accretion; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 October 20; revised 2022 January 6; accepted 2022 January 27; published 2022 March 9. \n\nSupport for this work was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51440.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). \n\nJ.A.G. acknowledges support from NASA grant 80NSSC20K0540 and from the Alexander von Humboldt Foundation. S.G. acknowledges the support of the Centre National d'Etudes Spatiales (CNES).\n\nPublished - Ludlam_2022_ApJ_927_112.pdf
Accepted Version - 2201.11767.pdf
",
"abstract": "We present a spectral analysis of NuSTAR and NICER observations of the luminous, persistently accreting neutron star (NS) low-mass X-ray binary Cygnus X-2. The data were divided into different branches that the source traces out on the Z-track of the X-ray color\u2013color diagram; namely, the horizontal branch, the normal branch, and the vertex between the two. The X-ray continuum spectrum was modeled in two different ways that produced comparable quality fits. The spectra showed clear evidence of a reflection component in the form of a broadened Fe K line, as well as a lower-energy emission feature near 1 keV likely due to an ionized plasma located far from the innermost accretion disk. We account for the reflection spectrum with two independent models (relxillns and rdblur*rfxconv). The inferred inclination is in agreement with earlier estimates from optical observations of ellipsoidal lightcurve modeling (relxillns: i = 67\u00b0 \u00b1 4\u00b0; rdblur*rfxconv: i = 60\u00b0 \u00b1 10\u00b0). The inner disk radius remains close to the NS (R_(in) \u2264 1.15 R_(ISCO)) regardless of the source position along the Z-track or how the 1 keV feature is modeled. Given the optically determined NS mass of 1.71 \u00b1 0.21 M_\u2299, this corresponds to a conservative upper limit of R_(in) \u2264 19.5 km for M = 1.92 M_\u2299 or R_(in) \u2264 15.3 km for M = 1.5 M_\u2299. We compare these radius constraints to those obtained from NS gravitational wave merger events and recent NICER pulsar lightcurve modeling measurements.",
"date": "2022-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "927",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 112",
"id_number": "CaltechAUTHORS:20220309-982137000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220309-982137000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "NASA",
"grant_number": "80NSSC20K0540"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
"local_group": {
"items": [
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"doi": "10.3847/1538-4357/ac5028",
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"pub_year": "2022",
"author_list": "Ludlam, R. M.; Cackett, E. M.; et el."
},
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"eprint_id": 113715,
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"datestamp": "2023-08-22 14:27:54",
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"items": [
{
"id": "Kamraj-Nikita",
"name": {
"family": "Kamraj",
"given": "Nikita"
},
"orcid": "0000-0002-3233-2451"
},
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Balokovi\u0107-Mislav",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Ricci-Claudio",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Koss-Michael-J",
"name": {
"family": "Koss",
"given": "Michael J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Mej\u00eda-Restrepo-Julian-E",
"name": {
"family": "Mej\u00eda-Restrepo",
"given": "Julian E."
},
"orcid": "0000-0001-8450-7463"
},
{
"id": "Oh-Kyuseok",
"name": {
"family": "Oh",
"given": "Kyuseok"
},
"orcid": "0000-0002-5037-951X"
},
{
"id": "Powell-Meredith-C",
"name": {
"family": "Powell",
"given": "Meredith C."
},
"orcid": "0000-0003-2284-8603"
},
{
"id": "Urry-C-Megan",
"name": {
"family": "Urry",
"given": "C. Megan"
},
"orcid": "0000-0002-0745-9792"
}
]
},
"title": "X-Ray Coronal Properties of Swift/BAT-selected Seyfert 1 Active Galactic Nuclei",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Active galactic nuclei; Black holes; X-ray sources; Seyfert galaxies; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 July 20; revised 2021 November 2; accepted 2021 November 20; published 2022 March 3. \n\nWe have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the following resources: NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA); online Swift data processing services provided by the SSDC; the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center; NASA's Astrophysics Data System; Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018). Some of the optical spectra used for determining black hole masses used in this work were taken with the Doublespec (DBSP) instrument at Palomar via Yale (PI: M. Powell, 2017\u20132019, 16 nights) as well as Caltech (PI: F. Harrison) and JPL (PI: D. Stern) from programs from 2013 to 2020. \n\nM. Balokovi\u0107 acknowledges support from the Black Hole Initiative at Harvard University, which is funded in part by the Gordon and Betty Moore Foundation (grant GBMF8273) and in part by the John Templeton Foundation, as well as support from the YCAA Prize Postdoctoral Fellowship. M.K. acknowledges support from NASA through ADAP award NNH16CT03C. K.O. acknowledges support from the National Research Foundation of Korea (NRF-2020R1C1C1005462). C.R. acknowledges support from the CONICYT+PAI Convocatoria Nacional subvencion a instalacion en la academia convocatoria a\u00f1o 2017 PAI77170080. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - , XMM-Newton - , Palomar Hale(DBSP). - \n\nSoftware: TBabs (Wilms et al. 2000), pexrav (Magdziarz & Zdziarski 1995), nthComp (Zdziarski et al. 1996), xillverCp (Garc\u00eda & Kallman 2010), NuSTARDAS (v2.17.1), HEASOFT (v6.24), XMM SAS (v16.1.0), XSPEC (v12.8.2), Astropy (Astropy Collaboration et al. 2013, 2018), NumPy, Matplotlib (Hunter 2007).\n\nPublished - Kamraj_2022_ApJ_927_42.pdf
Accepted Version - 2202.00895.pdf
",
"abstract": "The corona is an integral component of active galactic nuclei (AGNs) which produces the bulk of the X-ray emission above 1\u20132 keV. However, many of its physical properties and the mechanisms powering this emission remain a mystery. In particular, the temperature of the coronal plasma has been difficult to constrain for large samples of AGNs, as constraints require high-quality broadband X-ray spectral coverage extending above 10 keV in order to measure the high-energy cutoff, which provides constraints on the combination of coronal optical depth and temperature. We present constraints on the coronal temperature for a large sample of Seyfert 1 AGNs selected from the Swift/BAT survey using high-quality hard X-ray data from the NuSTAR observatory combined with simultaneous soft X-ray data from Swift/XRT or XMM-Newton. When applying a physically motivated, nonrelativistic disk-reflection model to the X-ray spectra, we find a mean coronal temperature kT_e = 84 \u00b1 9 keV. We find no significant correlation between the coronal cutoff energy and accretion parameters such as the Eddington ratio and black hole mass. We also do not find a statistically significant correlation between the X-ray photon index, \u0393, and Eddington ratio. This calls into question the use of such relations to infer properties of supermassive black hole systems.",
"date": "2022-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "927",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 42",
"id_number": "CaltechAUTHORS:20220303-225982929",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220303-225982929",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Harvard University"
},
{
"agency": "Gordon and Betty Moore Foundation",
"grant_number": "GBMF8273"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "Yale Center for Astronomy and Astrophysics"
},
{
"agency": "NASA",
"grant_number": "NNH16CT03C"
},
{
"agency": "National Research Foundation of Korea",
"grant_number": "NRF-2020R1C1C1005462"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "PAI77170080"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
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"id": "NuSTAR"
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"doi": "10.3847/1538-4357/ac45f6",
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}
],
"pub_year": "2022",
"author_list": "Kamraj, Nikita; Brightman, Murray; et el."
},
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{
"id": "Brumback-McKinley-C",
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"family": "Brumback",
"given": "McKinley C."
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"orcid": "0000-0002-4024-6967"
},
{
"id": "Grefenstette-Brian-W",
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"family": "Grefenstette",
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{
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"family": "Buisson",
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"orcid": "0000-0002-5341-6929"
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{
"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Connors-Riley-M-T",
"name": {
"family": "Connors",
"given": "Riley"
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta"
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Krivonos-Roman-A",
"name": {
"family": "Krivonos",
"given": "Roman"
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"orcid": "0000-0003-2737-5673"
},
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "Renee"
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mastroserio-Guglielmo",
"name": {
"family": "Mastroserio",
"given": "Guglielmo"
},
"orcid": "0000-0003-4216-7936"
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wik-Daniel",
"name": {
"family": "Wik",
"given": "Daniel"
},
"orcid": "0000-0001-9110-2245"
}
]
},
"title": "Extending the Baseline for SMC X-1's Spin and Orbital Behavior with NuSTAR Stray Light",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-ray binary stars; High mass x-ray binary stars; Pulsars; Neutron stars; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 November 12; revised 2022 January 6; accepted 2022 January 17; published 2022 February 24. \n\nThe authors thank the anonymous referee for their time in reading the manuscript and providing helpful comments. M.C.B. would like to thank J. Thorstensen for communication about calculating orbital ephemerides and acknowledges support from NASA funding award No. 80NSSC21K0263. R.K. acknowledges support from the Russian Science Foundation grant 19-12-00369. R.L. acknowledges the support of NASA through the Hubble Fellowship Program grant HST-HF2-51440.001. \n\nSoftware: HEAsoft (v6.29c; HEASARC 2014), NuSTARDAS, Stingray (Huppenkothen et al. 2019), HENDRICS (Bachetti 2018), MaLTPyNT (Bachetti 2015), nustar-gen-utils.\n\nPublished - Brumback_2022_ApJ_926_187.pdf
Accepted Version - 2202.11261.pdf
",
"abstract": "StrayCats, the catalog of NuSTAR stray light observations, contains data from bright X-ray sources that fall within crowded source regions. These observations offer unique additional data with which to monitor sources such as X-ray binaries that show variable timing behavior. In this work, we present a timing analysis of stray light data of the high-mass X-ray binary SMC X-1, the first scientific analysis of a single source from the StrayCats project. We describe the process of screening stray light data for scientific analysis, verify the orbital ephemeris, and create both time- and energy-resolved pulse profiles. We find that the orbital ephemeris of SMC X-1 is unchanged and confirm a long-term spin-up rate of \u03bd \u0307 = (2.52 \u00b1 0.03) \u00d7 10\u207b\u00b9\u00b9 Hz s\u207b\u00b9. We also note that the shape of SMC X-1's pulse profile, while remaining double peaked, varies significantly with time and only slightly with energy.",
"date": "2022-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "926",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 187",
"id_number": "CaltechAUTHORS:20220225-724712000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220225-724712000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC21K0263"
},
{
"agency": "Russian Science Foundation",
"grant_number": "19-12-00369"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA Einstein Fellowship"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ac4d24",
"primary_object": {
"basename": "2202.11261.pdf",
"url": "https://authors.library.caltech.edu/records/m4x3e-91c36/files/2202.11261.pdf"
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"basename": "Brumback_2022_ApJ_926_187.pdf",
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}
],
"pub_year": "2022",
"author_list": "Brumback, McKinley C.; Grefenstette, Brian W.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/z7eth-f1r13",
"eprint_id": 112879,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:56:05",
"lastmod": "2023-10-23 22:49:50",
"type": "article",
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"creators": {
"items": [
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Dauser-Thomas",
"name": {
"family": "Dauser",
"given": "Thomas"
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "Renee"
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Parker-Michael-L",
"name": {
"family": "Parker",
"given": "Michael"
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "Andrew"
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Wilms-J\u00f6rn",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Relativistic X-Ray Reflection Models for Accreting Neutron Stars",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; Relativistic disks; Atomic physics; Atomic spectroscopy; Neutron stars; X-ray astronomy; X-ray transient sources; Spectral line lists",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 March 11; revised 2021 November 17; accepted 2021 November 22; published 2022 February 8. \n\nWe thank the referee for thoughtful comments that greatly improved this paper. We also thank E. Kara, D. Barret, and E. Kammoun for clarifications regarding the simulations with XRISM and Athena instrumental responses. J.A.G. acknowledges support from NASA ATP grant 80NSSC20K0540 and from the Alexander von Humboldt Foundation. R.M.L. acknowledges the support of NASA through the Hubble Fellowship Program grant HST-HF2-51440.001. This work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacility: NuSTAR. - \n\nSoftware: xspec (v12.10.0c; Arnaud 1996), xillver (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), relxill (v1.5.0; Garc\u00eda et al. 2014; Dauser et al. 2014).\n\nPublished - Garc\u00eda_2022_ApJ_926_13.pdf
Accepted Version - 2111.12838.pdf
",
"abstract": "We present new reflection models specifically tailored to model the X-ray radiation reprocessed in accretion disks around neutron stars, in which the primary continuum is characterized by a single-temperature blackbody spectrum, emitted either at the surface of the star or at the boundary layer. These models differ significantly from those with a standard power-law continuum, typically observed in most accreting black holes. We show comparisons with earlier reflection models and test their performance in the NuSTAR observation of the neutron star 4U 1705\u221244. Simulations of upcoming missions such as XRISM-Resolve and Athena X-IFU are shown to highlight the diagnostic potential of these models for high-resolution X-ray reflection spectroscopy. These new reflection models xillverNS, and their relativistic counterpart relxillNS, are made publicly available to the community as an additional flavor in the relxill suite of reflection models.",
"date": "2022-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "926",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 13",
"id_number": "CaltechAUTHORS:20220113-182247899",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220113-182247899",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC20K0540"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Einstein Fellowship"
}
]
},
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"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/ac3cb7",
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"pub_year": "2022",
"author_list": "Garc\u00eda, Javier A.; Dauser, Thomas; et el."
},
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{
"id": "Satapathy-Kaushik",
"name": {
"family": "Satapathy",
"given": "Kaushik"
},
"orcid": "0000-0003-0433-3585"
},
{
"name": {
"family": "Psaltis",
"given": "Dimitrios"
},
"orcid": "0000-0003-4058-2837"
},
{
"name": {
"family": "\u00d6zel",
"given": "Feryal"
}
},
{
"name": {
"family": "Medeiros",
"given": "Lia"
},
"orcid": "0000-0003-2342-6728"
},
{
"name": {
"family": "Dougall",
"given": "Sean T."
},
"orcid": "0000-0002-3769-1314"
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{
"name": {
"family": "Chan",
"given": "Chi-Kwan"
},
"orcid": "0000-0001-6337-6126"
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{
"name": {
"family": "Wielgus",
"given": "Maciek"
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"orcid": "0000-0002-8635-4242"
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{
"name": {
"family": "Prather",
"given": "Ben S."
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"orcid": "0000-0002-0393-7734"
},
{
"name": {
"family": "Wong",
"given": "George N."
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{
"name": {
"family": "Gammie",
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{
"name": {
"family": "Akiyama",
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{
"name": {
"family": "Alberdi",
"given": "Antxon"
},
"orcid": "0000-0002-9371-1033"
},
{
"name": {
"family": "Alef",
"given": "Walter"
}
},
{
"name": {
"family": "Algaba",
"given": "Juan Carlos"
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"orcid": "0000-0001-6993-1696"
},
{
"name": {
"family": "Anantua",
"given": "Richard"
},
"orcid": "0000-0003-3457-7660"
},
{
"name": {
"family": "Asada",
"given": "Keiichi"
}
},
{
"name": {
"family": "Azulay",
"given": "Rebecca"
},
"orcid": "0000-0002-2200-5393"
},
{
"name": {
"family": "Baczko",
"given": "Anne-Kathrin"
},
"orcid": "0000-0003-3090-3975"
},
{
"name": {
"family": "Ball",
"given": "David"
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},
{
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
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"orcid": "0000-0003-0476-6647"
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{
"name": {
"family": "Barrett",
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{
"name": {
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"given": "Bradford A."
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"orcid": "0000-0002-5108-6823"
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"name": {
"family": "Bintley",
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{
"name": {
"family": "Blackburn",
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{
"name": {
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{
"name": {
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"name": {
"family": "Bower",
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"family": "Boyce",
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"title": "The Variability of the Black Hole Image in M87 at the Dynamical Timescale",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Black hole physics; High energy astrophysics; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 June 3; revised 2021 October 21; accepted 2021 October 24; published 2022 January 20. \n\nThis work was supported, in part, by the NSF PIRE award 1743747 and NASA ATP award 80NSSC20K0521. L.M. acknowledges support from an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award No. AST-1903847. M.W. acknowledges the support of the Black Hole Initiative at Harvard University, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation to Harvard University. All ray tracing calculations for Set A were performed with the El Gato GPU cluster at the University of Arizona that is funded by NSF award 1228509. All analyses for Set B were performed on CyVerse, supported by NSF grants DBI-0735191, DBI-1265383, and DBI-1743442. \n\nThe EHT Collaboration thanks the following organizations and programs: the Academy of Finland (projects 274477, 284495, 312496, and 315721); the Agencia Nacional de Investigaci\u00f3n y Desarrollo, Chile via NCN19\u2080\u2085\u2088 (TITANs) and Fondecyt 3190878; the Alexander von Humboldt Stiftung; an Alfred P. Sloan Research Fellowship; Allegro, the European ALMA Regional Centre node in the Netherlands, the NL astronomy research network NOVA, and the astronomy institutes of the University of Amsterdam, Leiden University, and Radboud University; the black hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation; the China Scholarship Council; Consejo Nacional de Ciencia y Tecnolog\u00eda (Mexico, projects U0004-246083, U0004-259839, F0003-272050, M0037-279006, F0003-281692, 104497, 275201, and 263356); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Direcci\u00f3n General de Asuntos del Personal Acad\u00e9mico-Universidad Nacional Aut\u00f3noma de M\u00e9xico (projects IN112417 and IN112820); the European Research Council Synergy Grant \"BlackHoleCam: Imaging the Event Horizon of Black Holes\" (grant 610058); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177 and GenT Program (project CIDEGENT/2018/021); MICINN Research Project PID2019-108995GB-C22; the Gordon and Betty Moore Foundation (grant GBMF-3561); the Istituto Nazionale di Fisica Nucleare sezione di Napoli, iniziative specifiche TEONGRAV; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; Joint Princeton/Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships; research at the Flatiron Institute is supported by the Simons Foundation; the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship (JP17J08829); the Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS; grants QYZDJ-SSW-SLH057, QYZDJSSW-SYS008, and ZDBS-LY-SLH011); the Leverhulme Trust Early Career Research Fellowship; the Max-Planck-Gesellschaft (MPG); the Max-Planck Partner Group of the MPG and the CAS; the MEXT/JSPS KAKENHI (grants 18KK0090, JP18K13594, JP18K03656, JP18H03721, 18K03709, 18H01245, and 25120007); the Malaysian Fundamental Research Grant Scheme (FRGS). FRGS/1/2019/STG02/UM/02/6; the MIT International Science and Technology Initiatives Funds; the Ministry of Science and Technology (MOST) of Taiwan (105-2112-M-001-025-MY3, 106-2112-M-001-011, 106-2119- M-001-027, 107-2119-M-001-017, 107-2119-M-001-020, 107-2119-M-110-005, 108-2112-M-001-048, and 109-2124-M-001-005); the National Aeronautics and Space Administration (NASA; Fermi Guest Investigator grant 80NSSC20K1567, NASA Astrophysics Theory Program grant 80NSSC20K0527, and NASA NuSTAR award 80NSSC20K0645); the National Institute of Natural Sciences of Japan; the National Key Research and Development Program of China (grants 2016YFA0400704 and 2016YFA0400702); the National Science Foundation (NSF; grants AST-0096454, AST-0352953, AST-0521233, AST-0705062, AST-0905844, AST-0922984, AST-1126433, AST-1140030, DGE-1144085, AST-1207704, AST-1207730, AST-1207752, MRI-1228509, OPP-1248097, AST-1310896, AST-1555365, AST-1615796, AST-1715061, AST-1716327, AST-1903847, and AST-2034306); the Natural Science Foundation of China (grants 11573051, 11633006, 11650110427, 10625314, 11721303, 11725312, 11933007, 11991052, and 11991053); a fellowship of China Postdoctoral Science Foundation (2020M671266); the Natural Sciences and Engineering Research Council of Canada (NSERC; including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral Program); the National Youth Thousand Talents Program of China; the National Research Foundation of Korea (the Global PhD Fellowship Grant: grants NRF-2015H1A2A1033752 and 2015- R1D1A1A01056807; the Korea Research Fellowship Program: NRF-2015H1D3A1066561 and Basic Research Support Grant 2019R1F1A1059721); the Netherlands Organization for Scientific Research VICI award (grant 639.043.513) and Spinoza Prize SPI 78-409; the New Scientific Frontiers with Precision Radio Interferometry Fellowship awarded by the South African Radio Astronomy Observatory, which is a facility of the National Research Foundation, an agency of the Department of Science and Technology of South Africa; the Onsala Space Observatory (OSO) national infrastructure, for the provisioning of its facilities/observational support (OSO receives funding through the Swedish Research Council under grant 2017\u201300648) the Perimeter Institute for Theoretical Physics (research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science, and Economic Development and by the Province of Ontario through the Ministry of Research, Innovation, and Science); the Spanish Ministerio de Econom\u00eda y Competitividad (grants PGC2018-098915-B-C21, AYA2016-80889-P, and PID2019-108995GB-C21); the State Agency for Research of the Spanish MCIU through the \"Center of Excellence Severo Ochoa\" award for the Instituto de Astrof\u00edsica de Andaluc\u00eda (SEV-2017\u20130709); the Toray Science Foundation; the Consejer\u00eda de Econom\u00eda, Conocimiento, Empresas y Universidad of the Junta de Andaluc\u00eda (grant P18-FR-1769), the Consejo Superior de Investigaciones Cient\u00edficas (grant 2019AEP112); the US Department of Energy (USDOE) through the Los Alamos National Laboratory (operated by Triad National Security, LLC), for the National Nuclear Security Administration of the USDOE (Contract 89233218CNA000001); the European Union's Horizon 2020 research and innovation program under grant agreement No. 730562 RadioNet; ALMA North America Development Fund; the Academia Sinica; Chandra DD7-18089X and TM6-17006X; the GenT Program (Generalitat Valenciana) Project CIDEGENT/2018/021. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), supported by NSF grant ACI-1548562, and CyVerse, supported by NSF grants DBI-0735191, DBI-1265383, and DBI-1743442. XSEDE Stampede2 resource at TACC was allocated through TG-AST170024 and TG-AST080026N. XSEDE JetStream resource at PTI and TACC was allocated through AST170028. The simulations were performed in part on the SuperMUC cluster at the LRZ in Garching, on the LOEWE cluster in CSC in Frankfurt, and on the HazelHen cluster at the HLRS in Stuttgart. This research was enabled, in part, by support provided by Compute Ontario (http://computeontario.ca), Calcul Quebec (http://www.calculquebec.ca), and Compute Canada (http://www.computecanada.ca). We thank the staff at the participating observatories, correlation centers, and institutions for their enthusiastic support. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.01154.V. ALMA is a partnership of the European Southern Observatory (ESO; Europe, representing its member states), NSF, and the National Institutes of Natural Sciences of Japan, together with National Research Council (Canada), MOST (Taiwan), the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA; Taiwan), and the Korea Astronomy and Space Science Institute (KASI; Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities, Inc. (AUI)/NRAO, and the National Astronomical Observatory of Japan (NAOJ). The NRAO is a facility of the NSF operated under cooperative agreement by AUI. APEX is a collaboration between the Max-Planck-Institut f\u00fcr Radioastronomie (Germany), ESO, and the OSO (Sweden). The SMA is a joint project between the SAO and ASIAA and is funded by the Smithsonian Institution and the Academia Sinica. The JCMT is operated by the East Asian Observatory on behalf of the NAOJ, ASIAA, and KASI, as well as the Ministry of Finance of China, CAS, and the National Key R&D Program (No. 2017YFA0402700) of China. Additional funding support for the JCMT is provided by the Science and Technologies Facility Council (UK) and participating universities in the UK and Canada. The LMT is a project operated by the Instituto Nacional de Astr\u00f3fisica, \u00d3ptica, y Electr\u00f3nica (Mexico) and the University of Massachusetts at Amherst (USA). The IRAM 30 m telescope in Pico Veleta, Spain is operated by IRAM and supported by CNRS (Centre National de la Recherche Scientifique, France), MPG (Max-Planck Gesellschaft, Germany), and IGN (Instituto Geogr\u00e1fico Nacional, Spain). The SMT is operated by the Arizona Radio Observatory, a part of the Steward Observatory of the University of Arizona, with financial support of operations from the State of Arizona and financial support for instrumentation development from the NSF. The SPT is supported by the NSF through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. The SPT hydrogen maser was provided on loan from the GLT, courtesy of ASIAA. The EHTC has received generous donations of FPGA chips from Xilinx Inc., under the Xilinx University Program. The EHTC has benefited from technology shared under an open-source license by the Collaboration for Astronomy Signal Processing and Electronics Research. The EHT project is grateful to T4Science and Microsemi for their assistance with hydrogen masers. This research has made use of NASA's Astrophysics Data System. We gratefully acknowledge the support provided by the extended staff of the ALMA, both from the inception of the ALMA Phasing Project through the observational campaigns of 2017 and 2018. We would like to thank A. Deller and W. Brisken for the EHT-specific support with the use of DiFX. We acknowledge the significance that Maunakea, where the SMA and JCMT-EHT stations are located, has for the indigenous Hawaiian people.\n\nPublished - Satapathy_2022_ApJ_925_13.pdf
Accepted Version - 2111.01317.pdf
",
"abstract": "The black hole images obtained with the Event Horizon Telescope (EHT) are expected to be variable at the dynamical timescale near their horizons. For the black hole at the center of the M87 galaxy, this timescale (5\u201361 days) is comparable to the 6 day extent of the 2017 EHT observations. Closure phases along baseline triangles are robust interferometric observables that are sensitive to the expected structural changes of the images but are free of station-based atmospheric and instrumental errors. We explored the day-to-day variability in closure-phase measurements on all six linearly independent nontrivial baseline triangles that can be formed from the 2017 observations. We showed that three triangles exhibit very low day-to-day variability, with a dispersion of \u223c3\u00b0\u20135\u00b0. The only triangles that exhibit substantially higher variability (\u223c90\u00b0\u2013180\u00b0) are the ones with baselines that cross the visibility amplitude minima on the u\u2013v plane, as expected from theoretical modeling. We used two sets of general relativistic magnetohydrodynamic simulations to explore the dependence of the predicted variability on various black hole and accretion-flow parameters. We found that changing the magnetic field configuration, electron temperature model, or black hole spin has a marginal effect on the model consistency with the observed level of variability. On the other hand, the most discriminating image characteristic of models is the fractional width of the bright ring of emission. Models that best reproduce the observed small level of variability are characterized by thin ring-like images with structures dominated by gravitational lensing effects and thus least affected by turbulence in the accreting plasmas.",
"date": "2022-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "925",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 13",
"id_number": "CaltechAUTHORS:20220125-723797779",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220125-723797779",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "Ministry of Science and Technology (Taipei)",
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{
"agency": "Ministerio de Ciencia, Innovaci\u00f3n y Universidades (MCIU)"
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"agency": "Severo Ochoa",
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{
"agency": "Toray Science Foundation"
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{
"agency": "Junta de Andaluc\u00eda",
"grant_number": "P18-FR-1769"
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"agency": "Department of Energy (DOE)",
"grant_number": "89233218CNA000001"
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{
"agency": "European Research Council (ERC)",
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"agency": "Academia Sinica"
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"agency": "NASA",
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"grant_number": "2017YFA0402700"
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{
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"grant_number": "GBMF 947"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "NuSTAR"
}
]
},
"corp_creators": {
"items": [
"Event Horizon Telescope Collaboration"
]
},
"doi": "10.3847/1538-4357/ac332e",
"primary_object": {
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"url": "https://authors.library.caltech.edu/records/pfdgb-c6k56/files/2111.01317.pdf"
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{
"basename": "Satapathy_2022_ApJ_925_13.pdf",
"url": "https://authors.library.caltech.edu/records/pfdgb-c6k56/files/Satapathy_2022_ApJ_925_13.pdf"
}
],
"pub_year": "2022",
"author_list": "Satapathy, Kaushik; Psaltis, Dimitrios; et el."
},
{
"id": "https://authors.library.caltech.edu/records/6h7g1-wq892",
"eprint_id": 113088,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:25:34",
"lastmod": "2023-10-23 22:55:10",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah"
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "F\u00fcrst-Felix",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
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},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "Marianne"
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Israel-Gian-Luca",
"name": {
"family": "Israel",
"given": "Gian Luca"
},
"orcid": "0000-0001-5480-6438"
},
{
"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "Sean"
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"orcid": "0000-0002-8403-0041"
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{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
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"orcid": "0000-0003-2686-9241"
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{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
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},
"title": "Evolution of the Spin, Spectrum and Superorbital Period of the Ultraluminous X-Ray Pulsar M51 ULX7",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "High mass x-ray binary stars; Ultraluminous x-ray sources; Pulsars; Neutron stars; Accretion; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 July 23; revised 2021 November 8; accepted 2021 November 8; published 2022 January 21. \n\nWe thank the referee for their thorough review of our paper which improved it. \n\nThis work was also supported under NASA Contract No. NNG08FD60C. NuSTAR is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nThis work was also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. \n\nWe wish to thank the Swift P.I., Brad Cenko, for approving the target of opportunity requests we made to observe M51, as well as the rest of the Swift team for carrying them out. We also acknowledge the use of public data from the Swift data archive. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. \n\nThis research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. \n\nG.L.I. acknowledges funding from the Italian MIUR PRIN grant No. 2017LJ39LM. The work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. D.J.W. acknowledges support from an STFC Ernest Rutherford Fellowship. \n\nFacilities: Swift(XRT) - Swift Gamma-Ray Burst Mission, NuSTAR - , XMM-Newton. - \n\nSoftware: NuSTARDAS, XMMSAS (Gabriel et al. 2004), XSPEC (Arnaud 1996), hendrics (Bachetti 2015).\n\nPublished - Brightman_2022_ApJ_925_18.pdf
Accepted Version - 2111.05342.pdf
",
"abstract": "M51 ULX7 is among a small group of known ultraluminous X-ray pulsars (ULXPs). The neutron star powering the source has a spin period of 2.8 s, orbits its companion star with a period of 2 days, and a superorbital period of 38 days is evident in its X-ray lightcurve. Here we present NuSTAR and XMM-Newton data on the source from 2019 obtained when the source was near its peak brightness. We detect the pulsations, having spun up at a rate of 3 \u00b1 0.5 \u00d7 10\u207b\u00b9\u2070 s s\u207b\u00b9 since they were previously detected in 2018. The data also provide the first high-quality broadband spectrum of the source. We find it to be very similar to that of other ULXPs, with two disk-like components, and a high-energy tail. When combined with XMM-Newton data obtained in 2018, we explore the evolution of the spectral components with superorbital phase, finding that the luminosity of the hotter component drives the superorbital flux modulation. The inclination the disk components appear to change with phase, which may support the idea that these superorbital periods are caused by disk precession. We also reexamine the superorbital period with 3 yr of Swift/XRT monitoring, finding that the period is variable, increasing from 38.2 \u00b1 0.5 days in 2018\u20132019 to 44.2 \u00b1 0.9 days in 2020\u20132021, which rules out alternative explanations for the superorbital period.",
"date": "2022-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "925",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 18",
"id_number": "CaltechAUTHORS:20220124-215321000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220124-215321000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)",
"grant_number": "2017LJ39LM"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ac3829",
"primary_object": {
"basename": "Brightman_2022_ApJ_925_18.pdf",
"url": "https://authors.library.caltech.edu/records/6h7g1-wq892/files/Brightman_2022_ApJ_925_18.pdf"
},
"related_objects": [
{
"basename": "2111.05342.pdf",
"url": "https://authors.library.caltech.edu/records/6h7g1-wq892/files/2111.05342.pdf"
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],
"pub_year": "2022",
"author_list": "Brightman, Murray; Bachetti, Matteo; et el."
},
{
"id": "https://authors.library.caltech.edu/records/9dcsw-at394",
"eprint_id": 112308,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:02:44",
"lastmod": "2023-10-23 21:01:20",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Feng-Ye",
"name": {
"family": "Feng",
"given": "Ye"
}
},
{
"id": "Zhao-Xueshan",
"name": {
"family": "Zhao",
"given": "XueShan"
}
},
{
"id": "Gou-Lijun",
"name": {
"family": "Gou",
"given": "LiJun"
}
},
{
"id": "Liu-Yufeng",
"name": {
"family": "Liu",
"given": "YuFeng"
},
"orcid": "0000-0002-1686-0545"
},
{
"id": "Steiner-James-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Wang-Yuan",
"name": {
"family": "Wang",
"given": "Yuan"
}
},
{
"id": "Jia-Nan",
"name": {
"family": "Jia",
"given": "Nan"
}
},
{
"id": "Liao-ZhenXuan",
"name": {
"family": "Liao",
"given": "ZhenXuan"
}
},
{
"id": "Li-Huixian",
"name": {
"family": "Li",
"given": "HuiXian"
}
}
]
},
"title": "Spectral analysis of new black hole candidate AT2019wey observed by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "NuSTAR, black hole physics, X-rays, binaries-stars, individual, AT2019we; General Physics and Astronomy",
"note": "c Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature 2021. \n\nReceived August 15, 2021; accepted September 16, 2021; published online November 24, 2021. \n\nYe Feng thanks the useful discussions with Prof. Mihoko Yukita on extracting NuSTAR spectrum. Ye Feng also thanks the useful discussions with Yunfeng Chen. The software used is provided by the High Energy Astrophysics Science Archive Research Centre (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC, Italy) and the California Institute of Technology (Caltech, USA). LiJun Gou is supported by the National Program on Key Research and Development Project (Grant No. 2016YFA0400804), the National Natural Science Foundation of China (Grant No. U1838114), and the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDB23040100).\n\nAccepted Version - 2109.07357.pdf
",
"abstract": "AT2019wey is a new galactic X-ray binary that was first discovered as an optical transient by the Australia Telescope Large Area Survey (ATLAS) on December 7, 2019. AT2019wey consists of a black hole candidate as well as a low-mass companion star (M_(star) \u2272 1.0 M_\u2299) and is likely to have a short orbital period (P_(orb) \u227216 h). Although AT2019wey began activation in the X-ray band during almost the entire outburst on March 8, 2020, it did not enter the soft state during the entire outburst. In this study, we present a detailed spectral analysis of AT2019wey in the low/hard state during its X-ray outburst on the basis of Nuclear Spectroscopic Telescope Array \\emph observations. We obtain tight constraints on several of its important physical parameters by applying the State-of-art \\texttt{relxill} relativistic reflection model family. In particular, we determine that the measured inner radius of the accretion disk is most likely to have extended to the innermost stable circular orbit (ISCO) radius, i.e., R_(in) = 1.38^(+0.23)_(\u22120.16) R_(ISCO). Hence, assuming R_(in) = R_(ISCO), we find the spin of AT2019wey to be a\u2217\u223c 0.97, which is close to the extreme and an inner disk inclination angle of ~i\u223c 22\u2218. Additionally, according to our adopted models, AT2019wey tends to have a relatively high iron abundance of A_(Fe)\u223c 5 A_(Fe,\u2299) and a high disk ionization state of log \u03be\u223c 3.4.",
"date": "2022-01",
"date_type": "published",
"publication": "Science China Physics, Mechanics and Astronomy",
"volume": "65",
"number": "1",
"publisher": "Springer Verlag",
"pagerange": "Art. No. 219512",
"id_number": "CaltechAUTHORS:20211208-951173000",
"issn": "1674-7348",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211208-951173000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "National Key Research and Development Program of China",
"grant_number": "2016YFA0400804"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "U1838114"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDB23040100"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1007/s11433-021-1790-7",
"primary_object": {
"basename": "2109.07357.pdf",
"url": "https://authors.library.caltech.edu/records/9dcsw-at394/files/2109.07357.pdf"
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"pub_year": "2022",
"author_list": "Feng, Ye; Zhao, XueShan; et el."
},
{
"id": "https://authors.library.caltech.edu/records/83erc-a5496",
"eprint_id": 113665,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:12:54",
"lastmod": "2023-10-23 17:47:26",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah P."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Forster-Karl",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Zoglauer-Andreas",
"name": {
"family": "Zoglauer",
"given": "Andreas"
},
"orcid": "0000-0001-9067-3150"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona"
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "Reconstruction of the NuSTAR point spread function using single-laser metrology",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "laser metrology; space telescopes; point spread functions; x-rays; Space and Planetary Science; Mechanical Engineering; Astronomy and Astrophysics; Instrumentation; Control and Systems Engineering; Electronic, Optical and Magnetic Materials",
"note": "\u00a9 2022 The Authors. Published by SPIE under a Creative Commons Attribution 4.0 International License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. \n\nPaper 21127 received Oct. 7, 2021; accepted for publication Feb. 8, 2022; published online Feb.\n22, 2022.\n\nWe thank our anonymous reviewers for helpful comments that improved this paper. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology.\n\nPublished - 014009_1.pdf
Accepted Version - 2202.04685.pdf
",
"abstract": "We describe a method by which the metrology system of the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray space observatory, which uses two lasers to characterize the relative motion of the optics and focal plane benches, can be approximated should one laser fail. The two benches are separated by a 10-m-long rigid mast that undergoes small amounts of thermal flexing that needs to be compensated for to produce a nonblurred image. We analyze the trends of mast motion by archival observation parameters to discover whether the mast motion in future observations can be predicted. We find that, using the solar aspect angle, observation date, and orbital phase, we can simulate the motion of one laser by translating the track produced by the other and applying modifications to the resulting mast aspect solution, allowing for the reconstruction of a minimally distorted point spread function in most cases. We will implement the generation of simulated mast files along with the usual NuSTAR data reduction pipeline for contingency purposes. This work has implications for reducing the risk of implementing laser metrology systems on future missions that use deployable masts to achieve the long focal lengths required in high-energy astronomy by mitigating the impact of a metrology laser failure in the extended phase of a mission.",
"date": "2022-01",
"date_type": "published",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"volume": "8",
"number": "1",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"pagerange": "Art. No. 014009",
"id_number": "CaltechAUTHORS:20220301-900015000",
"issn": "2329-4124",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220301-900015000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1117/1.jatis.8.1.014009",
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"pub_year": "2022",
"author_list": "Earnshaw, Hannah P.; Madsen, Kristin K.; et el."
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"id": "Gorgone-Nicholas-M",
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"given": "Nicholas M."
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"orcid": "0000-0002-1653-6411"
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{
"id": "Woudt-Patrick-A",
"name": {
"family": "Woudt",
"given": "Patrick A."
},
"orcid": "0000-0002-6896-1655"
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"id": "Buckley-David-A-H",
"name": {
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"given": "David"
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"orcid": "0000-0002-7004-9956"
},
{
"id": "Mukai-Koji",
"name": {
"family": "Mukai",
"given": "Koji"
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"orcid": "0000-0002-8286-8094"
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{
"id": "Kouveliotou-Chryssa",
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"family": "Kouveliotou",
"given": "Chryssa"
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{
"id": "Huppenkothen-Daniela",
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"family": "Huppenkothen",
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"orcid": "0000-0002-1169-7486"
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{
"id": "G\u00f6\u011f\u00fc\u015f-Ersin",
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"given": "Ersin"
},
"orcid": "0000-0002-5274-6790"
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{
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"name": {
"family": "Bellm",
"given": "Eric"
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"name": {
"family": "Linford",
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{
"id": "van-der-Horst-Alexander-J",
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"family": "van der Horst",
"given": "Alexander J."
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"id": "Baring-Matthew-G",
"name": {
"family": "Baring",
"given": "Matthew G."
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"id": "Hartmann-Dieter",
"name": {
"family": "Hartmann",
"given": "Dieter"
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"orcid": "0000-0002-8028-0991"
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"id": "Barrett-Paul",
"name": {
"family": "Barrett",
"given": "Paul"
},
"orcid": "0000-0002-8456-1424"
},
{
"id": "Cenko-S-Bradley",
"name": {
"family": "Cenko",
"given": "Bradley"
},
"orcid": "0000-0003-1673-970X"
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{
"id": "Graham-Melissa-Lynn",
"name": {
"family": "Graham",
"given": "Melissa"
},
"orcid": "0000-0002-9154-3136"
},
{
"id": "Granot-Jonathan",
"name": {
"family": "Granot",
"given": "Johnathan"
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"orcid": "0000-0001-8530-8941"
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona"
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"orcid": "0000-0003-2992-8024"
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{
"id": "Kennea-Jamie-A",
"name": {
"family": "Kennea",
"given": "Jamie"
},
"orcid": "0000-0002-6745-4790"
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{
"id": "O'Connor-Brendan-M",
"name": {
"family": "O'Connor",
"given": "Brendan M."
},
"orcid": "0000-0002-9700-0036"
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{
"id": "Potter-Stephen-B",
"name": {
"family": "Potter",
"given": "Stephen"
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{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
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"id": "Slane-Patrick",
"name": {
"family": "Slane",
"given": "Patrick"
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"id": "Wijers-Ralph",
"name": {
"family": "Wijers",
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},
"title": "Swift/XRT Deep Galactic Plane Survey Discovery of a New Intermediate Polar Cataclysmic Variable, Swift J183920.1-045350",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Cataclysmic variable stars; DQ Herculis stars; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 April 10; revised 2021 September 10; accepted 2021 September 14; published 2021 December 24. \n\nThe authors wish to thank Sylvia Rose Kowalski and Deena Mickelson for their roles in VLA data acquisition. They also thank Hannes Breytenbach for taking some of the SAAO data. P.A.W. acknowledges financial support from the University of Cape Town and the National Research Foundation. The SALT observations reported here were obtained through the SALT Large Science program 2018-2-LSP-001, with D.B. as PI, who also acknowledges support of the National Research Foundation. C.K. and N.G. acknowledge support under NASA grant 80NSSC19K0916 and Smithsonian Astrophysical Observatory grant GO9-20057X. B.O. is supported in part by the National Aeronautics and Space Administration through grants NNX16AB66G, NNX17AB18G, and 80NSSC20K0389. \n\nWe thank the NRAO for the generous allocation of VLA time for our observations. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nThis work has made use of data from the European Space Agency mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions participating in the Gaia Multilateral Agreement. \n\nFacilities: Swift - Swift Gamma-Ray Burst Mission, NuSTAR - , XMM-Newton - , Chandra - , SALT - , SAAO - , Gaia - , Pan-STARRS - , ZTF - , APO - , VLA - . \n\nSoftware: casa (McMullin et al. 2007), heasoft (v6.23; Nasa High Energy Astrophysics Science Archive Research Center (Heasarc), 2014), ds9 (Joye & Mandel 2003; Smithsonian Astrophysical Observatory 2000), sas (v1.2; Gabriel et al. 2004), pyspeckit (Ginsburg & Mirocha 2011), stingray (Huppenkothen et al. 2019, v0.1;), ciao (Fruscione et al. 2006, v4.9;), pydis (Davenport 2019), pysalt package (Crawford et al. 2010), python 3 (Van Rossum & Drake 2009), iraf (Tody 1986, 1993), vartools (Hartman & Bakos 2016)\n\nPublished - Gorgone_2021_ApJ_923_243.pdf
Submitted - 2103.14800.pdf
",
"abstract": "We report on the Swift/XRT Deep Galactic Plane Survey discovery and multiwavelength follow-up observations of a new intermediate polar (IP) cataclysmic variable, Swift J183920.1-045350. A 449.7 s spin period is found in XMM-Newton and NuSTAR data, accompanied by a 459.9 s optical period that is most likely the synodic, or beat period, produced from a 5.6 hr orbital period. The orbital period is seen with moderate significance in independent long-baseline optical photometry observations taken with the ZTF and SAAO telescopes. We find that the X-ray pulse fraction of the source decreases with increasing energy. The X-ray spectra are consistent with the presence of an Fe emission line complex with both local and interstellar absorption. In the optical spectra, strong H\u03b1, H i, He i, and He ii emission lines are observed, all common features in magnetic CVs. The source properties are thus typical of known IPs, with the exception of its estimated distance of 2.26_(\u22120.83)^(+1.93) kpc, which is larger than typical, extending the reach of the CV population in our Galaxy.",
"date": "2021-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "923",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 243",
"id_number": "CaltechAUTHORS:20220119-572561000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220119-572561000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Southern African Large Telescope (SALT)",
"grant_number": "2018-2-LSP-001"
},
{
"agency": "National Research Foundation (South Africa)"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K0916"
},
{
"agency": "Smithsonian Astrophysical Observatory",
"grant_number": "GO9-20057X"
},
{
"agency": "NASA",
"grant_number": "NNX16AB66G"
},
{
"agency": "NASA",
"grant_number": "NNX17AB18G"
},
{
"agency": "NASA",
"grant_number": "80NSSC20K0389"
},
{
"agency": "Gaia Multilateral Agreement"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/ac2738",
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}
],
"pub_year": "2021",
"author_list": "Gorgone, Nicholas M.; Woudt, Patrick A.; et el."
},
{
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"eprint_id": 112249,
"eprint_status": "archive",
"datestamp": "2023-08-22 12:46:23",
"lastmod": "2023-10-23 20:59:46",
"type": "article",
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"items": [
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta D."
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Deller-Adam-T",
"name": {
"family": "Deller",
"given": "Adam T."
},
"orcid": "0000-0001-9434-3837"
},
{
"id": "Gusinskaia-Nina",
"name": {
"family": "Gusinskaia",
"given": "Nina"
},
"orcid": "0000-0001-6128-3735"
},
{
"id": "Hessels-Jason-W-T",
"name": {
"family": "Hessels",
"given": "Jason W. T."
},
"orcid": "0000-0003-2317-1446"
},
{
"id": "Miller-Jones-James-C-A",
"name": {
"family": "Miller-Jones",
"given": "James C. A."
},
"orcid": "0000-0003-3124-2814"
},
{
"id": "Archibald-Anne-M",
"name": {
"family": "Archibald",
"given": "Anne M."
},
"orcid": "0000-0003-0638-3340"
},
{
"id": "Bogdanov-Slavko",
"name": {
"family": "Bogdanov",
"given": "Slavko"
},
"orcid": "0000-0002-9870-2742"
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{
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"name": {
"family": "Bassa",
"given": "Cees"
},
"orcid": "0000-0002-1429-9010"
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{
"id": "Wijnands-Rudy",
"name": {
"family": "Wijnands",
"given": "Rudy"
},
"orcid": "0000-0002-3516-2152"
},
{
"id": "Patruno-Alessandro",
"name": {
"family": "Patruno",
"given": "Alessandro"
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"orcid": "0000-0002-6459-0674"
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"family": "Sanidas",
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},
"title": "Quasi-simultaneous Radio/X-Ray Observations of the Candidate Transitional Millisecond Pulsar 3FGL J1544.6\u22121125 during its Low-luminosity Accretion-disk State",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Millisecond pulsars; Binary pulsars; Radio continuum emission; Accretion; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 December 23; revised 2021 August 20; accepted 2021 August 21; published 2021 December 7. \n\nWe thank Tom Russell for discussions about the radio analysis. A.J. and J.W.T.H. acknowledge funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement nr. 337062 (DRAGNET). A.J. also acknowledges support from the NuSTAR mission. A.P. acknowledges support from an NWO Vidi Fellowship. J.C.A.M.-J. is the recipient of an Australian Research Council Future Fellowship (FT 140101082). S.B. was supported in part by NASA Swift Guest Investigator Cycle 12 program grant NNX16AN79G awarded through Columbia University. \n\nWe thank B. Clark and the VLA schedulers for granting these DDT observations on short notice. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. \n\nThe data postprocessing and results preparation for this work relied heavily on Common Astronomy Software Applications (CASA 5.1) (McMullin et al. 2007). We would like to thank the staff at NRAO and externals involved in maintaining an extensive updated documentation and tutorials for CASA. This research also made use of Astropy, a community-developed core Python package for Astronomy (The Astropy Collaboration et al. 2013; Astropy Collaboration et al. 2018). Other important softwares used in this research are Matplotlib (Hunter 2007), Seaborn, and Scipy (Jones et al. 2001). Lastly, we have made extensive use of the NASA Astrophysics Data System (Eichhorn et al. 2000) and the arXiv e-print service (Ginsparg 2011).\n\nPublished - Jaodand_2021_ApJ_923_3.pdf
Accepted Version - 2110.10706.pdf
",
"abstract": "3FGL J1544.6\u22121125 is a candidate transitional millisecond pulsar (tMSP). Similar to the well-established tMSPs\u2014PSR J1023+0038, IGR J18245\u22122452, and XSS J12270\u22124859\u20143FGL J1544.6\u22121125 shows \u03b3-ray emission and discrete X-ray \"low\" and \"high\" modes during its low-luminosity accretion-disk state. Coordinated radio/X-ray observations of PSR J1023+0038 in its current low-luminosity accretion-disk state showed rapidly variable radio continuum emission\u2014possibly originating from a compact, self-absorbed jet, the \"propellering\" of accretion material, and/or pulsar moding. 3FGL J1544.6\u22121125 is currently the only other (candidate) tMSP system in this state, and can be studied to see whether tMSPs are typically radio-loud compared to other neutron star binaries. In this work, we present a quasi-simultaneous Very Large Array and Swift radio/X-ray campaign on 3FGL J1544.6\u22121125. We detect 10 GHz radio emission varying in flux density from 47.7 \u00b1 6.0 \u03bcJy down to \u227215 \u03bcJy (3\u03c3 upper limit) at four epochs spanning three weeks. At the brightest epoch, the radio luminosity is L_(5 GHz) = (2.17 \u00b1 0.17) \u00d7 10\u00b2\u2077 erg s\u207b\u00b9 for a quasi-simultaneous X-ray luminosity L_(2\u201310 keV) = (4.32 \u00b1 0.23) \u00d7 10\u00b3\u00b3 erg s\u207b\u00b9 (for an assumed distance of 3.8 kpc). These luminosities are close to those of PSR J1023+0038, and the results strengthen the case that 3FGL J1544.6\u22121125 is a tMSP showing similar phenomenology to PSR J1023+0038.",
"date": "2021-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "923",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 3",
"id_number": "CaltechAUTHORS:20211207-393224000",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211207-393224000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "337062"
},
{
"agency": "NuSTAR"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
},
{
"agency": "Australian Research Council",
"grant_number": "FT 140101082"
},
{
"agency": "NASA",
"grant_number": "NNX16AN79G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ac1ff7",
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"author_list": "Jaodand, Amruta D.; Deller, Adam T.; et el."
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"id": "Lazar-Hadar",
"name": {
"family": "Lazar",
"given": "Hadar"
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"orcid": "0000-0002-2752-9524"
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
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"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "Sean N."
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"orcid": "0000-0002-8403-0041"
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"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Hadar-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "Douglas J. K."
}
},
{
"id": "Connors-Riley-M-T",
"name": {
"family": "Connors",
"given": "Riley M. T."
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "F\u00fcrst-Felix",
"name": {
"family": "Fuerst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Hare-Jeremy",
"name": {
"family": "Hare",
"given": "Jeremy"
},
"orcid": "0000-0002-8548-482X"
},
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
},
"orcid": "0000-0002-9639-4352"
},
{
"id": "Shaw-Aarran-W",
"name": {
"family": "Shaw",
"given": "Aarran W."
},
"orcid": "0000-0002-8808-520X"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Spectral and Timing Analysis of NuSTAR and Swift/XRT Observations of the X-Ray Transient MAXI J0637\u2013430",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; Low-mass x-ray binary stars; Black hole physics; Space and Planetary Science; Astronomy and Astrophysics",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 June 17; revised 2021 July 28; accepted 2021 August 5; published 2021 November 10. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work also made use of data from the Neil Gehrels Swift Observatory. H.L. and J.A.T. acknowledge partial support under NASA NuSTAR Guest Investigator grant 80NSSC20K0644. J.H. acknowledges support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the Universities Space Research Association under contract with NASA. J.A.G. acknowledges support from NASA NuSTAR Guest Investigator grant 80NSSC20K1238, and from the Alexander von Humboldt Foundation. J.J. acknowledges support from the fellowship of China Postdoctoral Science Foundation (2021M691822), the Tsinghua Shuimu Scholar Program and the Tsinghua Astrophysics Outstanding Fellowship. Thank you to Dr. Thomas Dauser and Dr. Jack Steiner for the useful comments along the way. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift/XRT - . \n\nSoftware: XSPEC (v12.11.1c Arnaud 1996), HEAsoft (v6.27.2), relxill suite (Dauser et al. 2014; Garc\u00eda et al. 2014).\n\nPublished - Lazar_2021_ApJ_921_155.pdf
Accepted Version - 2108.03299.pdf
",
"abstract": "We present results for the first observed outburst from the transient X-ray binary source MAXI J0637\u2013430. This study is based on eight observations from the Nuclear Spectroscopic Telescope Array (NuSTAR) and six observations from the Neil Gehrels Swift Observatory X-Ray Telescope (Swift/XRT) collected from 2019 November 19 to 2020 April 26 as the 3\u201379 keV source flux declined from 8.2 \u00d7 10\u207b\u00b9\u2070 to 1.4 \u00d7 10\u207b\u00b9\u00b2 erg cm\u207b\u00b2 s\u207b\u00b9. We see the source transition from a soft state with a strong disk-blackbody component to a hard state dominated by a power-law or thermal Comptonization component. NuSTAR provides the first reported coverage of MAXI J0637\u2013430 above 10 keV, and these broadband spectra show that a two-component model does not provide an adequate description of the soft-state spectrum. As such, we test whether blackbody emission from the plunging region could explain the excess emission. As an alternative, we test a reflection model that includes a physical Comptonization continuum. Finally, we also test a spectral component based on reflection of a blackbody illumination spectrum, which can be interpreted as a simple approximation to the reflection produced by returning disk radiation due to the bending of light by the strong gravity of the black hole. We discuss the physical implications of each scenario and demonstrate the value of constraining the source distance.",
"date": "2021-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "921",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 155",
"id_number": "CaltechAUTHORS:20211123-234017978",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211123-234017978",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "NASA/JPL/Caltech"
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{
"agency": "NASA",
"grant_number": "80NSSC20K0644"
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"agency": "NASA Postdoctoral Program"
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{
"agency": "NASA",
"grant_number": "80NSSC20K1238"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "China Postdoctoral Science Foundation",
"grant_number": "2021M691822"
},
{
"agency": "Tsinghua University"
}
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"author_list": "Lazar, Hadar; Tomsick, John A.; et el."
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"title": "NuSTAR observations of a repeatedly microflaring active region",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: activity \u2013 Sun: corona \u2013 Sun: flares \u2013 Sun: magnetic fields \u2013 Sun: X-rays, gamma-rays",
"note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of The Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nAccepted 2021 August 3. Received 2021 July 29; in original form 2021 May 5. Published: 19 August 2021. \n\nThis paper made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, funded by the National Aeronautics and Space Administration. These observations were supported through the NuSTAR Guest Observer program (NASA grant 80NSSC18K1744). This research used version 2.0.6 (Mumford et al. 2021) of the SUNPY open source software package (SunPy Community et al. 2020), version 0.4.0 (Barnes et al. 2020a) of the\u2009AIAPY open source software package (Barnes et al. 2020b), and made use of ASTROPY,3 a community-developed core PYTHON package for Astronomy (The Astropy Collaboration 2018). Other PYTHON packages that were extensively used were MATPLOTLIB (Hunter 2007), NUMPY (Harris et al. 2020), and SCIPY (Virtanen et al. 2020). This research also made use of HEASOFT (a unified release of FTOOLS and XANADU software packages) and NuSTAR Data Analysis Software (NUSTARDAS). This paper also made use of the SolarSoft IDL distribution (SSW) from the IDL Astronomy Library. We would like to thank the anonymous reviewer for their helpful feedback. \n\nKC is supported by a Royal Society Research Fellows Enhancement Award (RGF\\EA\\180010) and IGH is supported by a Royal Society University Fellowship (URF\\R\\180010). \n\nData Availability: All data used are publicly available. SDO data can be obtained from the Joint Science Operations Center (JSOC)4 using SUNPY'SFido5 object while the NuSTAR data are available from the NuSTAR Master Catalog6 with the OBSIDs 80414201001, 80414202001, 80414203001, 80415201001, 80415202001, and 80415203001.\n\nPublished - stab2283.pdf
Accepted Version - 2109.00263.pdf
",
"abstract": "We investigate the spatial, temporal, and spectral properties of 10 microflares from AR12721 on 2018 September 9 and 10 observed in X-rays using the Nuclear Spectroscopic Telescope ARray and the Solar Dynamic Observatory's Atmospheric Imaging Assembly and Helioseismic and Magnetic Imager. We find GOES sub-A class equivalent microflare energies of 10\u00b2\u2076\u201310\u00b2\u2078 erg reaching temperatures up to 10 MK with consistent quiescent or hot active region (AR) core plasma temperatures of 3\u20134 MK. One microflare (SOL2018-09-09T10:33), with an equivalent GOES class of A0.1, has non-thermal hard X-ray emission during its impulsive phase (of non-thermal power \u223c7 \u00d7 10\u00b2\u2074 erg s\u207b\u00b9) making it one of the faintest X-ray microflares to have direct evidence for accelerated electrons. In 4 of the 10 microflares, we find that the X-ray time profile matches fainter and more transient sources in the extreme-ultraviolet, highlighting the need for observations sensitive to only the hottest material that reaches temperatures higher than those of the AR core (>5 MK). Evidence for corresponding photospheric magnetic flux cancellation/emergence present at the footpoints of eight microflares is also observed.",
"date": "2021-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "507",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3936-3951",
"id_number": "CaltechAUTHORS:20211116-184723183",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211116-184723183",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
{
"agency": "NASA/JPL/Caltech"
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{
"agency": "NASA",
"grant_number": "80NSSC18K1744"
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{
"agency": "Royal Society",
"grant_number": "RGF\\EA\\180010"
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{
"agency": "Royal Society",
"grant_number": "URF\\R\\180010"
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"doi": "10.1093/mnras/stab2283",
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"author_list": "Cooper, Kristopher; Hannah, Iain G.; et el."
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"title": "A Comprehensive X-Ray Report on AT2019wey",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; Black holes; Low-mass x-ray binary stars; X-ray transient sources; Transient sources; X-ray sources; X-ray binary stars",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 November 30; revised 2021 April 6; accepted 2021 April 14; published 2021 October 21. \n\nWe thank the anonymous reviewer for providing comments that have largely improved this manuscript. We thank Belinda Wilkes and Patrick Slane for allocating DD time on Chandra, and Fiona Harrison for allocating NuSTAR DD time. We thank Kumiko Morihana for providing the cleaned MAXI light curve of MAXI J1305\u2212704. Y.Y. thanks the Heising-Simons Foundation for support. R.M.L. acknowledges the support of NASA through the Hubble Fellowship Program grant HST-HF2-51440.001. J.A.G. acknowledges support from NASA grant 80NSSC17K0515 and from the Alexander von Humboldt Foundation. Z.W. acknowledges support from the NASA postdoctoral program. NICER research at NRL is supported by NASA. This work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (nustardas), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. \n\nFacilities: NICER - , NuSTAR - , CXO (ACIS-S) - , Swift (XRT - , BAT) - , MAXI. - \n\nSoftware: astropy (Astropy Collaboration et al. 2013), CIAO (Fruscione et al. 2006), HEASoft (v6.27; Heasarc 2014), HENDRICS (Bachetti 2015), isis (Houck & Denicola 2000), matplotlib (Hunter 2007), pandas (McKinney 2010), PRESTO (Ransom 2011); relxill (v1.3.10; Garc\u00eda et al. 2014; Dauser et al. 2014) Stingray (Huppenkothen et al. 2019), xspec (v12.11.0; Arnaud 1996).\n\nPublished - Yao_2021_ApJ_920_121.pdf
Submitted - 2012.00160.pdf
",
"abstract": "Here, we present MAXI, Swift, NICER, NuSTAR, and Chandra observations of the X-ray transient AT2019wey (SRGA J043520.9+552226, SRGE J043523.3+552234). From spectral and timing analyses we classify it as a Galactic low-mass X-ray binary (LMXB) with a black hole (BH) or neutron star (NS) accretor. AT2019wey stayed in the low/hard state (LHS) from 2019 December to 2020 August 21, and the hard-intermediate state (HIMS) from 2020 August 21 to 2020 November. For the first six months of the LHS, AT2019wey had a flux of \u223c1 mCrab, and displayed a power-law X-ray spectrum with photon index \u0393 = 1.8. From 2020 June to August, it brightened to \u223c20 mCrab. Spectral features characteristic of relativistic reflection became prominent. On 2020 August 21, the source left the \"hard line\" on the rms\u2013intensity diagram, and transitioned from LHS to HIMS. The thermal disk component became comparable to the power-law component. A low-frequency quasi-periodic oscillation (QPO) was observed. The QPO central frequency increased as the spectrum softened. No evidence of pulsation was detected. We are not able to decisively determine the nature of the accretor (BH or NS). However, the BH option is favored by the position of this source on the \u0393\u2013L_X, L_(radio)\u2013L_X, and L_(opt)\u2013L_X diagrams. We find the BH candidate XTE J1752\u2212223 to be an analog of AT2019wey. Both systems display outbursts with long plateau phases in the hard states. We conclude by noting the potential of SRG in finding new members of this emerging class of low luminosity and long-duration LMXB outbursts.",
"date": "2021-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "920",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 121",
"id_number": "CaltechAUTHORS:20210106-131324406",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210106-131324406",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "Heising-Simons Foundation"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA",
"grant_number": "80NSSC17K0515"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA Postdoctoral Program"
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{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Einstein Fellowship"
}
]
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"title": "A Month of Monitoring the New Magnetar Swift J1555.2\u22125402 during an X-Ray Outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Magnetars; Magnetic fields; Neutron stars; Pulsars; Soft gamma-ray repeaters; X-ray transient sources",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 August 5; revised 2021 September 8; accepted 2021 September 10; published 2021 October 5. \n\nThe authors are grateful to the NICER, NuSTAR, Swift, and DSN scheduling and operation teams. We thank Francesco Coti Zelati, Alice Borghese, Nanda Rea, Gian Luca Israel, and Paolo Esposito for helpful discussion about the initial observation and for preparing the GCN reports. We also acknowledge Alice Borghese for her request of the Swift observation at the earliest phase of the outburst. We thank Mareki Honma, Takaaki Jike, Aya Yamauchi, Toshio Terasawa, and Tomoya Hirota for useful comments on the VERA observation and all the staff of Mizusawa VLBI Observatory of NAOJ for operating the VERA array. T.E. and S.K. are supported by JSPS/MEXT KAKENHI grant Nos. 17K18776, 18H04584, 18H01246, 19K14712, and 21H01078. A.B.P. is a McGill Space Institute (MSI) Fellow and a Fonds de Recherche du Quebec\u2014Nature et Technologies (FRQNT) postdoctoral fellow. W.C.G.H. acknowledges support through grant 80NSSC20K0278 from NASA. NICER research at NRL is supported by NASA. W.A.M. is grateful to the DSN scheduling team and the Canberra Deep Space Communication Complex (CDSCC) staff for scheduling and carrying out the radio observations with the DSN. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a Research and Technology Development Grant through a contract with the National Aeronautics and Space Administration. U.S. government sponsorship is acknowledged. \n\nFacilities: NICER - , NuSTAR - , Swift - , DSN - , VERA. - \n\nSoftware: HEAsoft (v6.27.2; NASA High Energy Astrophysics Science Archive Research Center (HEASARC), 2014), astropy (Astropy Collaboration et al. 2013; Price-Whelan et al. 2018), PRESTO (Ransom et al. 2002), FETCH (Agarwal et al. 2020), PINT (v0.8.2; Luo et al. 2021), XSPEC (Arnaud 1996), NICERDAS (v2020-04-23_V007a).\n\nPublished - Enoto_2021_ApJL_920_L4.pdf
Submitted - 2108.02939.pdf
",
"abstract": "The soft gamma-ray repeater Swift J1555.2\u22125402 was discovered by means of a short burst detected with Swift BAT on 2021 June 3. Then, 1.6 hr after the burst, the Neutron star Interior Composition Explorer (NICER) started daily monitoring of this target for a month. The absorbed 2\u201310 keV flux stayed nearly constant at around 4 \u00d7 10\u207b\u00b9\u00b9 erg s\u207b\u00b9 cm\u207b\u00b2 during the monitoring, showing only a slight gradual decline. An absorbed blackbody with a temperature of 1.1 keV approximates the soft X-ray spectrum. A 3.86 s periodicity is detected, and the period derivative is measured to be 3.05(7) \u00d7 10\u207b\u00b9\u00b9 s s\u207b\u00b9. The soft X-ray pulse shows a single sinusoidal shape with an rms pulsed fraction that increases as a function of energy from 15% at 1.5 keV to 39% at 7 keV. The equatorial surface magnetic field, characteristic age, and spin-down luminosity are derived under the dipole field approximation to be 3.5 \u00d7 10\u00b9\u2074 G, 2.0 kyr, and 2.1 \u00d7 10\u00b3\u2074 erg s\u207b\u00b9, respectively. We detect 5 and 45 bursts with Swift/BAT and NICER, respectively. Based on these properties, this new source is classified as a magnetar. A hard X-ray power-law component that extends up to at least 40 keV is detected with the Nuclear Spectroscopic Telescope Array (NuSTAR). The 10\u201360 keV flux is \u223c9 \u00d7 10\u207b\u00b9\u00b2 erg s\u207b\u00b9 cm\u207b\u00b2 with a photon index of \u223c1.2. The pulsed fraction has a sharp cutoff at around 10 keV with an upper limit (\u227210%) in the hard-tail band. No radio pulsations are detected during the DSN or VERA observations. The 7\u03c3 upper limits of the flux density are 0.043 and 0.026 mJy at the S and X bands, respectively.",
"date": "2021-10-10",
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"publication": "Astrophysical Journal Letters",
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"number": "1",
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"title": "Constraining particle acceleration in Sgr A\u22c6 with simultaneous GRAVITY, Spitzer, NuSTAR, and Chandra observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center \u2013 accretion, accretion disks \u2013 black hole physics",
"note": "\u00a9 GRAVITY Collaboration 2021. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0),\nwhich permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived 1 April 2021; Accepted 1 July 2021; Published online 05 October 2021. \n\nGRAVITY is developed in a Collaboration by the Max Planck Institute for extraterrestrial Physics, LESIA of Observatoire de Paris/Universit\u00e9 PSL/CNRS/Sorbonne Universit\u00e9/Universit\u00e9 de Paris and IPAG of Universit\u00e9 Grenoble Alpes/CNRS, the Max Planck Institute for Astronomy, the University of Cologne, the CENTRA \u2013 Centro de Astrofisica e Gravita\u00e7\u00e3o, and the European Southern Observatory. \n\nSvF thanks Giulia Focchi for her contribution to the H-band acquisition camera pipeline. SvF, and FW acknowledge support by the Max Planck International Research School. GP is supported by the H2020 ERC Consolidator Grant Hot Milk under grant agreement Nr. 865637. A.A. and P.G. were supported by Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia, with grants reference UIDB/00099/2020 and SFRH/BSAB/142940/2018. This work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory. This work is based in part on observations made with NuSTAR, which is operated by NASA/JPL-Caltech. GGF, JLH, HAS, and SPW acknowledge support for this work from the NASA ADAP program under NASA grant 80NSSC18K0416.\n\nPublished - aa40981-21.pdf
Accepted Version - 2107.01096.pdf
",
"abstract": "We report the time-resolved spectral analysis of a bright near-infrared and moderate X-ray flare of Sgr A\u22c6. We obtained light curves in the M, K, and H bands in the mid- and near-infrared and in the 2 \u2212 8 keV and 2 \u2212 70 keV bands in the X-ray. The observed spectral slope in the near-infrared band is \u03bdL_\u03bd\u2004\u221d\u2004\u03bd^(0.5 \u00b1 0.2); the spectral slope observed in the X-ray band is \u03bdL_\u03bd\u2004\u221d\u2004\u03bd^(\u22120.7 \u00b1 0.5). Using a fast numerical implementation of a synchrotron sphere with a constant radius, magnetic field, and electron density (i.e., a one-zone model), we tested various synchrotron and synchrotron self-Compton scenarios. The observed near-infrared brightness and X-ray faintness, together with the observed spectral slopes, pose challenges for all models explored. We rule out a scenario in which the near-infrared emission is synchrotron emission and the X-ray emission is synchrotron self-Compton. Two realizations of the one-zone model can explain the observed flare and its temporal correlation: one-zone model in which the near-infrared and X-ray luminosity are produced by synchrotron self-Compton and a model in which the luminosity stems from a cooled synchrotron spectrum. Both models can describe the mean spectral energy distribution (SED) and temporal evolution similarly well. In order to describe the mean SED, both models require specific values of the maximum Lorentz factor \u03b3_(max), which differ by roughly two orders of magnitude. The synchrotron self-Compton model suggests that electrons are accelerated to \u03b3_(max)\u2004\u223c\u2004500, while cooled synchrotron model requires acceleration up to \u03b3_(max)\u2004\u223c\u20045 \u00d7 10\u2074. The synchrotron self-Compton scenario requires electron densities of 10\u00b9\u2070 cm\u207b\u00b3 that are much larger than typical ambient densities in the accretion flow. Furthermore, it requires a variation of the particle density that is inconsistent with the average mass-flow rate inferred from polarization measurements and can therefore only be realized in an extraordinary accretion event. In contrast, assuming a source size of 1\u2006R_S, the cooled synchrotron scenario can be realized with densities and magnetic fields comparable with the ambient accretion flow. For both models, the temporal evolution is regulated through the maximum acceleration factor \u03b3_(max), implying that sustained particle acceleration is required to explain at least a part of the temporal evolution of the flare.",
"date": "2021-10",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "654",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A22",
"id_number": "CaltechAUTHORS:20211011-220006826",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211011-220006826",
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"agency": "International Max Planck Research School (IMPRS) for Astronomy and Astrophysics"
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"agency": "European Research Council (ERC)",
"grant_number": "865637"
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"pub_year": "2021",
"author_list": "Abuter, R.; Amorim, A.; et el."
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{
"id": "Pike-Sean-N",
"name": {
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"given": "Sean N."
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"given": "Douglas J. K."
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"family": "Garc\u00eda",
"given": "Javier A."
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},
"title": "Photospheric Radius Expansion and a Double-peaked Type-I X-Ray Burst from GRS 1741.9\u20132853",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Neutron stars; Low-mass x-ray binary stars; X-ray bursts; X-ray sources",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 March 15; revised 2021 June 16; accepted 2021 June 24; published 2021 August 30. \n\nJ.J. acknowledges support by the Tsinghua Astrophysics Outstanding (TAO) Fellowship and the Tsinghua Shuimu Scholar Programme. R.M.L. acknowledges the support of NASA through Hubble Fellowship Program grant HST-HF2-51440.001. D.J.K.B. acknowledges support from the Royal Society. J.A.G. acknowledges support from NASA ATP grant 80NSSC20K0540 and from the Alexander von Humboldt Foundation. This work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would also like to acknowledge the insightful feedback provided by the reviewer, which significantly improved the quality of this work. \n\nSoftware: Astropy, DS9, Scipy, Stingray, XSpec.\n\nPublished - Pike_2021_ApJ_918_9.pdf
Accepted Version - 2106.13312.pdf
",
"abstract": "We present an analysis of two type-I X-ray bursts observed by NuSTAR originating from the very faint transient neutron star (NS) low-mass X-ray binary GRS 1741.9\u20132853 during a period of outburst in 2020 May. We show that the persistent emission can be modeled as an absorbed, Comptonized blackbody in addition to Fe K\u03b1 emission, which can be attributed to relativistic disk reflection. We measure a persistent bolometric, unabsorbed luminosity of L_(bol) = 7.03_(-0.05)^(+0.04) x 10\u00b3\u2076 erg s\u207b\u00b9, assuming a distance of 7 kpc, corresponding to an Eddington ratio of 4.5%. This persistent luminosity combined with light-curve analysis leads us to infer that the bursts were the result of pure He burning rather than mixed H/He burning. Time-resolved spectroscopy reveals that the bolometric flux of the first burst exhibits a double-peaked structure, placing the source within a small population of accreting NSs that exhibit multiple-peaked type-I X-ray bursts. We find that the second, brighter burst shows evidence for photospheric radius expansion (PRE) and that at its peak, this PRE event had an unabsorbed bolometric flux of F_(peak) = 2.94_(-0.26)^(+0.28) x 10\u207b\u2078 erg cm\u207b\u00b2 s\u207b\u00b9. This yields a new distance estimate of d = 9.0 \u00b1 0.5 kpc, assuming that this corresponds to the Eddington limit for pure He burning on the surface of a canonical NS. Additionally, we performed a detailed timing analysis that failed to find evidence for quasi-periodic oscillations or burst oscillations, and we place an upper limit of 16% on the rms variability around 589 Hz, the frequency at which oscillations have previously been reported.",
"date": "2021-09-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "918",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 9",
"id_number": "CaltechAUTHORS:20210914-225403760",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210914-225403760",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Tsinghua University"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "Royal Society"
},
{
"agency": "NASA",
"grant_number": "80NSSC20K0540"
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{
"agency": "Alexander von Humboldt Foundation"
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{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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"author_list": "Pike, Sean N.; Harrison, Fiona A.; et el."
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"id": "Gallo-Luigi-C-C",
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"title": "Extreme relativistic reflection in the active galaxy ESO\u2009033-G002",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 X-rays: individual: ESO 033-G002",
"note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2021 April 19; Received 2021 April 13; in original form 2021 March 10; Published: 19 July 2021. \n\nDJW acknowledges support from the Science and Technology Facilities Council (STFC) in the form of an Ernest Rutherford Fellowship (ST/N004027/1). MB acknowledges support from the YCAA Prize Postdoctoral Fellowship. CSR thanks the STFC for support under Consolidated Grant ST/S000623/1, as well as the European Research Council (ERC) for support under the European Union's Horizon 2020 research and innovation programme (grant 834203). CR acknowledges support from the FONDECYT Iniciacion grant 11190831. JAG acknowledges support from NASA grant 80NSSC19K1020 and from the Alexander von Humboldt Foundation. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by the NASA Jet Propulsion Laboratory (JPL), and has utilized the NUSTARDAS software package, jointly developed by the Space Science Data Centre (SSDC; Italy) and Caltech (USA). This research has also made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. This work has made use of the CORNER package (Foreman-Mackey 2016) for data visualization. \n\nData Availability: All of the data underlying this article will be available from June 2021 via ESA's XMM-Newton Science Archive (https://www.cosmos.esa.int/web/xmm-newton/xsa) and NASA's HEASARC archive (https://heasarc.gsfc.nasa.gov/).\n\nPublished - stab1290.pdf
Submitted - 2107.10278.pdf
",
"abstract": "We present the first high signal-to-noise broad-band X-ray spectrum of the radio-quiet type-2 Seyfert ESO\u2009033-G002, combining data from XMM\u2013Newton and NuSTAR. The nuclear X-ray spectrum is complex, showing evidence for both neutral and ionized absorption, as well as reflection from both the accretion disc and more distant material, but our broad-band coverage allows us to disentangle all of these different components. The total neutral column during this epoch is N_H \u223c (5\u22126) \u00d7 10\u00b2\u00b2\u2009cm\u207b\u00b2\u2060, consistent with the optical classification of ESO\u2009033-G002 as a type-2 Seyfert but not so large as to prevent us from robustly determining the properties of the innermost accretion flow. The ionized absorption \u2013 dominated by lines from Fe\u2009XXV and Fe\u2009XXVI \u2013 reveals a moderately rapid outflow (v_(out) \u223c 5400\u2009km s\u207b\u00b9) which has a column comparable to the neutral absorption. We find the disc reflection from the innermost regions to be extreme, with a reflection fraction of R_(frac) \u223c 5. This requires strong gravitational lightbending and, in turn, both an extremely compact corona (within \u223c2\u2009R_G of the black hole) and a rapidly rotating black hole (a* > 0.96). Despite this tight size constraint, with a temperature of kT_e = 40\u201370\u2009keV the X-ray corona in ESO\u2009033-G002 appears similar to other active galactic nucle in terms of its placement in the compactness\u2013temperature plane, consistent with sitting close to the limit determined by runaway pair production. Finally, combining X-ray spectroscopy, timing, and updated optical spectroscopy, we also estimate the mass of the black hole to be log[M_(BH)/M_\u2299] \u223c 7.0\u20137.5.",
"date": "2021-09",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "506",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1557-1572",
"id_number": "CaltechAUTHORS:20211011-221326133",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211011-221326133",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/N004027/1"
},
{
"agency": "Yale Center for Astronomy and Astrophysics"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/S000623/1"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "834203"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "11190831"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1020"
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{
"agency": "Alexander von Humboldt Foundation"
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{
"agency": "NASA/JPL/Caltech"
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{
"agency": "ESA Member States"
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"doi": "10.1093/mnras/stab1290",
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{
"id": "Walton-Dominic-J",
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"id": "Alston-William-N",
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{
"id": "Dauser-Thomas",
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{
"id": "Eikenberry-Stephen-S",
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"id": "Stern-Daniel",
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"given": "D."
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},
"title": "NuSTAR reveals the hidden nature of SS433",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013X-rays: binaries",
"note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2021 April 27. Received 2021 April 6; in original form 2020 May 29. Published: 06 May 2021. \n\nThe authors thank the anonymous referee for their valuable suggestions. MJM and DJW appreciate support via STFC Ernest Rutherford Fellowships. WNA is supported by an ESA research fellowship. This research was partially supported by the Australian Government through the Australian Research Council's Discovery Projects funding scheme (project DP200102471). The authors thank Keith Arnaud for useful suggestions. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). \n\nData Availability: The data underlying this article were accessed from the HEASARC NuSTAR data repository at https://heasarc.gsfc.nasa.gov/docs/archive.html. The derived data generated in this research will be shared on reasonable request to the corresponding author.\n\nPublished - stab1280.pdf
Submitted - 1810.10518.pdf
",
"abstract": "SS433 is the only Galactic binary system known to persistently accrete at highly super-critical (or hyper-critical) rates, similar to those in tidal disruption events, and likely needed to explain the rapid growth of those very high redshift quasars containing massive SMBHs. Probing the inner regions of SS433 in the X-rays is crucial to understanding this system, and super-critical accretion in general, but is highly challenging due to obscuration by the surrounding wind, driven from the accretion flow. NuSTAR observed SS433 in the hard X-ray band across multiple phases of its 162 d superorbital precession period. Spectral-timing tools allow us to infer that the hard X-ray emission from the inner regions is likely being scattered towards us by the walls of the wind-cone. By comparing to numerical models, we determine an intrinsic X-ray luminosity of \u2265 2 \u00d7 10\u00b3\u2077 erg s\u207b\u00b9 and that, if viewed face on, we would infer an apparent luminosity of >1 \u00d7 10\u00b3\u2079 erg s\u207b\u00b9, confirming SS433's long-suspected nature as an ultraluminous X-ray source (ULX). We present the discovery of a narrow, \u223c100 s lag due to atomic processes occurring in outflowing material travelling at least 0.14\u20130.29c, which matches absorption lines seen in ULXs and \u2013 in the future \u2013 will allow us to map a super-critical outflow for the first time.",
"date": "2021-09",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "506",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1045-1058",
"id_number": "CaltechAUTHORS:20190225-081654781",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190225-081654781",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "Australian Research Council",
"grant_number": "DP200102471"
},
{
"agency": "NASA/JPL/Caltech"
}
]
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"doi": "10.1093/mnras/stab1280",
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"basename": "stab1280.pdf",
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"pub_year": "2021",
"author_list": "Middleton, M. J.; Walton, D. J.; et el."
},
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"eprint_id": 109222,
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"datestamp": "2023-08-20 03:57:35",
"lastmod": "2023-10-23 17:44:24",
"type": "article",
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"creators": {
"items": [
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
},
"orcid": "0000-0002-9639-4352"
},
{
"id": "Balokovi\u0107-Mislav",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Liu-Honghui",
"name": {
"family": "Liu",
"given": "Honghui"
},
"orcid": "0000-0003-2845-1009"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Lansbury-George-B",
"name": {
"family": "Lansbury",
"given": "George B."
},
"orcid": "0000-0002-5328-9827"
}
]
},
"title": "A highly accreting low-mass black hole hidden in the dust: Suzaku and NuSTAR observations of the NLS1 Mrk 1239",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: nuclei \u2013 galaxies: Seyfert \u2013X-ray: galaxies",
"note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2021 May 4. Received 2021 April 26; in original form 2020 July 28. Published: 10 May 2021. \n\nThis paper was written during the worldwide COVID-19 pandemic in 2020\u20132021. We acknowledge the hard work of all the health care workers around the world. We could not have finished this paper without their protection. JJ acknowledges support from the Tsinghua Shui'Mu Scholar Program and the Tsinghua Astrophysics Outstanding Fellowship. MB acknowledges support from the YCAA Prize Postdoctoral Fellowship. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA, and data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology. \n\nData Availability: All the data can be downloaded from the HEASARC website at https://heasarc.gsfc.nasa.gov.\n\nPublished - stab1306.pdf
Accepted Version - 2105.02078.pdf
",
"abstract": "We present torus modelling for the X-ray spectra of a nearby narrow-line Seyfert 1 galaxy Mrk 1239 (z = 0.0199), based on archival Suzaku, NuSTAR, and Swift observations. Our model suggests very soft intrinsic power-law continuum emission of \u0393 \u2248 2.57 in 2019 and \u0393 \u2248 2.98 in 2007. By applying a correction factor to the unabsorbed X-ray luminosity, we find that Mrk 1239 is accreting near or around the Eddington limit. Our best-fitting spectral model also suggests a torus with a column density of log\u2009(N_(H,ave)/\u2009cm\u207b\u00b2) = 25.0 \u00b1 0.2 and a high covering factor of 0.90 in Mrk 1239, indicating that this source is most likely to be viewed almost face-on with i \u2248 26\u00b0. Our line of sight might cross the edge of the torus with N_(H,los) = 2\u20135 \u00d7 10\u00b2\u00b3\u2009cm\u207b\u00b2. The high Eddington ratio and the high line-of-sight column density makes Mrk 1239 one of the active galactic nuclei that are close to the limit where wind may form near the edge of the torus due to high radiation pressure.",
"date": "2021-07",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "505",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "702-712",
"id_number": "CaltechAUTHORS:20210520-150005274",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-150005274",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Tsinghua Univerisity"
},
{
"agency": "Yale Center for Astronomy and Astrophysics"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/stab1306",
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"basename": "2105.02078.pdf",
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"pub_year": "2021",
"author_list": "Jiang, Jiachen; Balokovi\u0107, Mislav; et el."
},
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"items": [
{
"id": "F\u00fcrst-Felix",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "M."
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Pinto-Ciro",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Middleton-Matthew-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "H. P."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Barret-Didier",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Kretschmar-Peter",
"name": {
"family": "Kretschmar",
"given": "P."
},
"orcid": "0000-0001-9840-2048"
},
{
"id": "Pottschmidt-Katja",
"name": {
"family": "Pottschmidt",
"given": "K."
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Ptak-Andrew",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Roberts-Timothy-P",
"name": {
"family": "Roberts",
"given": "T."
},
"orcid": "0000-0001-8252-6337"
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Webb-Natalie-A",
"name": {
"family": "Webb",
"given": "N."
}
},
{
"id": "Wilms-J\u00f6rn",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Long-term pulse period evolution of the ultra-luminous X-ray pulsar NGC 7793 P13",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 X-rays: binaries \u2013 stars: neutron \u2013 pulsars: individual: NGC7793 P13",
"note": "\u00a9 ESO 2021. Article published by EDP Sciences. \n\nReceived 22 February 2021; Accepted 28 April 2021; Published online 16 July 2021. \n\nWe would like the thank the referee for the very useful comments that helped to improve the manuscript. DJW and MJM acknowledge support from STFC Ernest Rutherford fellowships. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the nustardas software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and also made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). The material is based upon work supported by NASA under award number 80GSFC17M0002.\n\nPublished - aa40625-21.pdf
Accepted Version - 2105.04229.pdf
",
"abstract": "Ultra-luminous X-ray pulsars (ULXPs) provide a unique opportunity to study persistent super-Eddington accretion. Here we present the results of a long-term monitoring campaign of ULXP NGC 7793 P13, focusing on the pulse period evolution and the determination of the orbital ephemeris. Over our four year monitoring campaign with Swift, XMM-Newton, and NuSTAR, we measured a continuous spin-up with an average value of \u1e56 \u2248 \u22123.8 \u00d7 10\u207b\u00b9\u00b9 s s\u207b\u00b9. We find that the strength of the spin-up is independent of the observed X-ray flux, indicating that despite a drop in observed flux in 2019, accretion onto the source has continued at largely similar rates. The source entered an apparent off-state in early 2020, which might have resulted in a change in the accretion geometry as no pulsations were found in observations in July and August 2020. We used the long-term monitoring to update the orbital ephemeris, as well as the periodicities seen in both the observed optical and UV magnitudes and the X-ray fluxes. We find that the optical and UV period is very stable over the years, with P_(UV) = 63.75_(\u22120.12)^(+0.17) d. The best-fit orbital period determined from our X-ray timing results is 64.86 \u00b1 0.19 d, which is almost a day longer than previously implied, and the X-ray flux period is 65.21 \u00b1 0.15 d, which is slightly shorter than previously measured. The physical origin of these different flux periods is currently unknown. We study the hardness ratio of the XMM-Newton and NuSTAR data between 2013\u22122020 to search for indications of spectral changes. We find that the hardness ratios at high energies are very stable and not directly correlated with the observed flux. At lower energies we observe a small hardening with increased flux, which might indicate increased obscuration through outflows at higher luminosities. Comparing the changes in flux with the observed pulsed fraction, we find that the pulsed fraction is significantly higher at low fluxes. This seems to imply that the accretion geometry already changed before the source entered the deep off-state. We discuss possible scenarios to explain this behavior, which is likely driven by a precessing accretion disk.",
"date": "2021-07",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "651",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A75",
"id_number": "CaltechAUTHORS:20210520-150032176",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-150032176",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA",
"grant_number": "80GSFC17M0002"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1051/0004-6361/202140625",
"primary_object": {
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"pub_year": "2021",
"author_list": "F\u00fcrst, F.; Walton, D. J.; et el."
},
{
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"eprint_id": 109193,
"eprint_status": "archive",
"datestamp": "2023-08-20 03:18:23",
"lastmod": "2023-10-23 17:43:45",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Xu-Yerong",
"name": {
"family": "Xu",
"given": "Yerong"
},
"orcid": "0000-0002-2523-5485"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Connors-Riley-M-T",
"name": {
"family": "Connors",
"given": "Riley M. T."
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin"
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "The Nature of Soft Excess in ESO 362-G18 Revealed by XMM-Newton and NuSTAR Spectroscopy",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 August 10; revised 2021 March 24; accepted 2021 March 30; published 2021 May 19. \n\nWe thank the referee for their constructive comments. J.A.G. acknowledges support from NASA grant NNX17AJ65G and from the Alexander von Humboldt Foundation. He is also a member of Teams 458 and 486 at the International Space Science Institute (ISSI), Bern, Switzerland, and acknowledges support from ISSI during the meetings in Bern. R.M.T.C. has been supported by NASA grant 80NSSC177K0515. D.J.W. acknowledges support from STFC through an Ernest Rutherford fellowship. This work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR operations, software, and calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: NuSTAR (Harrison et al. 2013), XMM-Newton (Jansen et al. 2001), Athena (Nandra et al. 2013), eXTP (Zhang et al. 2017), HEX-P (Madsen et al. 2018). \n\nSoftware: xillver (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), relxillD/relxilllpD (Dauser et al. 2014; Garc\u00eda et al. 2014, 2016), borus12 (Balokovi\u0107 et al. 2019).\n\nPublished - Xu_2021_ApJ_913_13.pdf
Accepted Version - 2103.17002.pdf
",
"abstract": "We present a detailed spectral analysis of the joint XMM-Newton and NuSTAR observations of the active galactic nuclei (AGNs) in the Seyfert 1.5 Galaxy ESO 362-G18. The broadband (0.3\u201379 keV) spectrum shows the presence of a power-law continuum with a soft excess below 2 keV, iron K\u03b1 emission (~6.4 keV), and a Compton hump (peaking at ~20 keV). We find that the soft excess can be modeled by two different possible scenarios: a warm (kT_e ~ 0.2 keV) and optically thick (\u03c4 ~ 34) Comptonizing corona, or with a relativistically blurred reflection off a high-density (log [n_e/cm\u207b\u00b3 > 18.3) inner disk. These two models cannot be easily distinguished solely from their fit statistics. However, the low temperature (kT_e ~ 20 keV) and the thick optical depth (\u03c4 ~ 5) of the hot corona required by the warm corona scenario are uncommon for AGNs. We also fit a \"hybrid\" model, which includes both disk reflection and a warm corona. Unsurprisingly, as this is the most complex of the models considered, this provides the best fit, and more reasonable coronal parameters. In this case, the majority of the soft excess flux arises in the warm corona component. However, based on recent simulations of warm coronae, it is not clear whether such a structure can really exist at the low accretion rates relevant for ESO 362-G18 (\u1e41 ~ 0.015). This may therefore argue in favor of a scenario in which the soft excess is instead dominated by the relativistic reflection. Based on this model, we find that the data would require a compact hot corona (h ~ 3 R_(Horizon)) around a rapidly spinning (a_\u2605 > 0.927) black hole.",
"date": "2021-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "913",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 13",
"id_number": "CaltechAUTHORS:20210519-141321220",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210519-141321220",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX17AJ65G"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "International Space Science Institute (ISSI)"
},
{
"agency": "NASA",
"grant_number": "80NSSC177K0515"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/abf430",
"primary_object": {
"basename": "Xu_2021_ApJ_913_13.pdf",
"url": "https://authors.library.caltech.edu/records/hgbcm-bsv10/files/Xu_2021_ApJ_913_13.pdf"
},
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],
"pub_year": "2021",
"author_list": "Xu, Yerong; Garc\u00eda, Javier A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/a0pfa-9y081",
"eprint_id": 108894,
"eprint_status": "archive",
"datestamp": "2023-08-22 09:37:48",
"lastmod": "2023-10-23 17:24:12",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "A. D."
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Cackett-Edward-M",
"name": {
"family": "Cackett",
"given": "E. M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Fabian-Andrew-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Buisson-Douglas-J-K",
"name": {
"family": "Buisson",
"given": "D. J. K."
}
},
{
"id": "Shaw-Aarran-W",
"name": {
"family": "Shaw",
"given": "A. W."
},
"orcid": "0000-0002-8808-520X"
},
{
"id": "Chakrabarty-Deepto",
"name": {
"family": "Chakrabarty",
"given": "D."
},
"orcid": "0000-0001-8804-8946"
}
]
},
"title": "Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 1543\u2013624",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; Low-mass x-ray binary stars",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 December 7; revised 2021 March 8; accepted 2021 March 9; published 2021 April 26. \n\nSupport for this work was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51440.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Additional support was provided from NASA under the NICER Guest Observer grant 80NSSC21K0121. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). J.A.G. acknowledges support from NASA grant 80NSSC20K1238 and from the Alexander von Humboldt Foundation. E.M.C. gratefully acknowledges support through NSF CAREER award number AST-1351222. J.A.T. acknowledges partial support from NASA under NICER Guest Observer grant 80NSSC19K1445. D.J.K.B. acknowledges funding from the Royal Society. \n\nFacilities: ADS - , HEASARC - , NICER - , NuSTAR. - \n\nSoftware: HEAsoft (v6.27.2, HEASARC 2014), nustardas (v1.9.2), nicerdas (2020-04-23_V007a), xspec (v12.11.0, Arnaud 1996), Stingray (Huppenkothen et al. 2019).\n\nPublished - Ludlam_2021_ApJ_911_123.pdf
",
"abstract": "We present the first joint NuSTAR and NICER observations of the ultracompact X-ray binary (UCXB) 4U 1543\u2212624 obtained in 2020 April. The source was at a luminosity of L_(0.5\u221250 keV) = 4.9(D/7 kpc)\u00b2 \u00d7 1036 erg s\u207b\u00b9 and showed evidence of reflected emission in the form of an O viii line, Fe K line, and Compton hump within the spectrum. We used a full reflection model, known as xillverCO, that is tailored for the atypical abundances found in UCXBs, to account for the reflected emission. We tested the emission radii of the O and Fe line components and conclude that they originate from a common disk radius in the innermost region of the accretion disk (R_(in) \u2264 1.07 R_(ISCO)). Assuming that the compact accretor is a neutron star (NS) and the position of the inner disk is the Alfv\u00e9n radius, we placed an upper limit on the magnetic field strength to be B \u2264 0.7(D/7 kpc) \u00d7 10\u2078 G at the poles. Given the lack of pulsations detected and position of R_(in), it was likely that a boundary layer region had formed between the NS surface and inner edge of the accretion disk with an extent of 1.2 km. This implies a maximum radius of the neutron star accretor of R_(NS) \u2264 12.1 km when assuming a canonical NS mass of 1.4 M_\u2299.",
"date": "2021-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "911",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 123",
"id_number": "CaltechAUTHORS:20210429-144554967",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210429-144554967",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "NASA",
"grant_number": "80NSSC21K0121"
},
{
"agency": "NASA",
"grant_number": "80NSSC20K1238"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NSF",
"grant_number": "AST-1351222"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1445"
},
{
"agency": "Royal Society"
},
{
"agency": "NASA Einstein Fellowship"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/abedb0",
"primary_object": {
"basename": "Ludlam_2021_ApJ_911_123.pdf",
"url": "https://authors.library.caltech.edu/records/a0pfa-9y081/files/Ludlam_2021_ApJ_911_123.pdf"
},
"pub_year": "2021",
"author_list": "Ludlam, R. M.; Jaodand, A. D.; et el."
},
{
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"datestamp": "2023-08-20 02:36:17",
"lastmod": "2023-10-23 17:50:06",
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"items": [
{
"id": "Krivonos-Roman-A",
"name": {
"family": "Krivonos",
"given": "Roman"
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Wik-Daniel",
"name": {
"family": "Wik",
"given": "Daniel"
},
"orcid": "0000-0001-9110-2245"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian"
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin"
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Perez-Kerstin-M",
"name": {
"family": "Perez",
"given": "Kerstin"
},
"orcid": "0000-0002-6404-4737"
},
{
"id": "Rossland-Steven",
"name": {
"family": "Rossland",
"given": "Steven"
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},
{
"id": "Sazonov-Sergey",
"name": {
"family": "Sazonov",
"given": "Sergey"
}
},
{
"id": "Zoglauer-Andreas",
"name": {
"family": "Zoglauer",
"given": "Andreas"
},
"orcid": "0000-0001-9067-3150"
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]
},
"title": "NuSTAR measurement of the cosmic X-ray background in the 3\u201320\u00a0keV energy band",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "instrumentation: detectors \u2013 methods: data analysis \u2013 galaxies: active \u2013 cosmic background radiation \u2013 X-rays:\ngeneral",
"note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2021 January 21. Received 2021 January 11; in original form 2020 November 21. Published: 04 February 2021. \n\nThis work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. RK and SS acknowledge support for this research from the Russian Science Foundation (grant 19-12-00396). DW and SR acknowledge support for this work from the NASA Astrophysics Data Analysis Program 80NSSC18K0686. \n\nData Availability: This work is based on the NuSTAR data publicly available through the HEASARC Archive (https://heasarc.gsfc.nasa.gov).\n\nPublished - stab209.pdf
Accepted Version - 2011.11469.pdf
",
"abstract": "We present measurements of the intensity of the cosmic X-ray background (CXB) with the Nuclear Spectroscopic Telescope Array (NuSTAR) telescope in the 3\u201320 keV energy range. Our method uses spatial modulation of the CXB signal on the NuSTAR detectors through the telescope's side aperture. Based on the NuSTAR observations of selected extragalactic fields with a total exposure of 7 Ms, we have estimated the CXB 3\u201320 keV flux to be 2.8 \u00d7 10\u207b\u00b9\u00b9 erg s\u207b\u00b9 cm\u207b\u00b2 deg\u207b\u00b2, which is \u223c8 per cent higher than that measured with HEAO-1 and consistent with the INTEGRAL measurement. The inferred CXB spectral shape in the 3\u201320 keV energy band is consistent with the canonical model of Gruber et al. We demonstrate that the spatially modulated CXB signal measured by NuSTAR is not contaminated by systematic noise and is limited by photon statistics. The measured relative scatter of the CXB intensity between different sky directions is compatible with cosmic variance, which opens new possibilities for studying CXB anisotropy over the whole sky with NuSTAR.",
"date": "2021-04",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "502",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3966-3975",
"id_number": "CaltechAUTHORS:20210601-100040210",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210601-100040210",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Russian Science Foundation",
"grant_number": "19-12-00396"
},
{
"agency": "NASA",
"grant_number": "80NSSC18K0686"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1093/mnras/stab209",
"primary_object": {
"basename": "2011.11469.pdf",
"url": "https://authors.library.caltech.edu/records/6vsv2-ry133/files/2011.11469.pdf"
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"pub_year": "2021",
"author_list": "Krivonos, Roman; Wik, Daniel; et el."
},
{
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"eprint_status": "archive",
"datestamp": "2023-08-22 09:13:25",
"lastmod": "2023-10-23 15:09:32",
"type": "article",
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"creators": {
"items": [
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Ward-Charlotte-A",
"name": {
"family": "Ward",
"given": "Charlotte"
}
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Mooley-Kunal-Prakash",
"name": {
"family": "Mooley",
"given": "Kunal"
},
"orcid": "0000-0002-2557-5180"
},
{
"id": "De-Kishalay",
"name": {
"family": "De",
"given": "Kishalay"
},
"orcid": "0000-0002-8989-0542"
},
{
"id": "Gezari-Suvi",
"name": {
"family": "Gezari",
"given": "Suvi"
},
"orcid": "0000-0003-3703-5154"
},
{
"id": "van-Velzen-Sjoert",
"name": {
"family": "van Velzen",
"given": "Sjoert"
},
"orcid": "0000-0002-3859-8074"
},
{
"id": "Andreoni-Igor",
"name": {
"family": "Andreoni",
"given": "Igor"
},
"orcid": "0000-0002-8977-1498"
},
{
"id": "Graham-M-J",
"name": {
"family": "Graham",
"given": "Matthew"
},
"orcid": "0000-0002-3168-0139"
},
{
"id": "Masci-Frank-J",
"name": {
"family": "Masci",
"given": "Frank J."
},
"orcid": "0000-0002-8532-9395"
},
{
"id": "Riddle-Reed-L",
"name": {
"family": "Riddle",
"given": "Reed"
},
"orcid": "0000-0002-0387-370X"
},
{
"id": "Zolkower-Jeffry",
"name": {
"family": "Zolkower",
"given": "Jeffry"
}
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]
},
"title": "A Luminous X-Ray Transient in SDSS J143359.16+400636.0: A Likely Tidal Disruption Event",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Tidal disruption; X-ray transient sources; Transient sources; X-ray sources; Supermassive black holes",
"note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 October 23; revised 2021 January 8; accepted 2021 January 16; published 2021 March 10. \n\nThe majority of this research and manuscript preparation took place during the COVID-19 global pandemic. The authors would like to thank all those who risked their lives as essential workers in order for us to safely continue our work from home. \n\nWe wish to thank the Swift PI, Brad Cenko, for approving the target of opportunity requests we made to observe SDSS J143359.16+400636.0, as well as the rest of the Swift team for carrying the observations out. We also acknowledge the use of public data from the Swift data archive. \n\nWe also wish to thank the NuSTAR PI, Fiona Harrison, for approving the DDT request we made to observe SDSS J143359.16+400636.0, as well as the NuSTAR SOC for carrying out the observation. This work was also supported under NASA contract No. NNG08FD60C. NuSTAR is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThis paper is based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. SED Machine is based on work supported by the National Science Foundation under grant No. 1106171. \n\nThe ZTF forced-photometry service was funded under the Heising-Simons Foundation grant No. 12540303 (PI: Graham). \n\nFacilities: Swift (XRT - , UVOT) - , NuSTAR - , CXO - , Keck:I (LRIS) - , PO:1.2 m PO:1.5 m - , VLA. - \n\nSoftware: CASA (McMullin et al. 2007), CIAO (Fruscione et al. 2006), lpipe (Perley 2019), The Tractor (Lang et al. 2016), XSPEC (Arnaud 1996).\n\nPublished - Brightman_2021_ApJ_909_102.pdf
Submitted - 2010.12587.pdf
",
"abstract": "We present the discovery of a luminous X-ray transient, serendipitously detected by Swift's X-ray Telescope on 2020 February 5, located in the nucleus of the galaxy SDSS J143359.16+400636.0 at z = 0.099 (luminosity distance D_L = 456 Mpc). The transient was observed to reach a peak luminosity of ~10\u2074\u2074 erg s\u207b\u00b9 in the 0.3\u201310 keV X-ray band, which was ~20 times more than the peak optical/UV luminosity. Optical, UV, and X-ray light curves from the Zwicky Transient Facility and Swift show a decline in flux from the source consistent with t^(\u22125/3), and observations with NuSTAR and Chandra show a soft X-ray spectrum with photon index \u0393 = 2.9 \u00b1 0.1. The X-ray/UV properties are inconsistent with well-known active galactic nucleus properties and have more in common with known X-ray tidal disruption events (TDEs), leading us to conclude that it was likely a TDE. The broadband spectral energy distribution can be described well by a disk blackbody model with an inner disk temperature of 7.3^(+0.3)_(\u22120.8) \u00d7 10\u2075 K, with a large fraction (>40%) of the disk emission upscattered into the X-ray band. An optical spectrum taken with Keck/LRIS after the X-ray detection reveals LINER line ratios in the host galaxy, suggesting low-level accretion onto the supermassive black hole prior to the event, but no broad lines or other indications of a TDE were seen. The stellar velocity dispersion implies that the mass of the supermassive black hole powering the event is log(M_(BH)/M_\u2299) = 7.41 \u00b1 0.41, and we estimate that at peak the Eddington fraction of this event was ~50%. This likely TDE was not identified by wide-field optical surveys or optical spectroscopy, indicating that more events like this would be missed without wide-field UV or X-ray surveys.",
"date": "2021-03-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "909",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 102",
"id_number": "CaltechAUTHORS:20201203-151035641",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201203-151035641",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NSF",
"grant_number": "AST-1440341"
},
{
"agency": "ZTF partner institutions"
},
{
"agency": "NSF",
"grant_number": "AST-1106171"
},
{
"agency": "Heising-Simons Foundation",
"grant_number": "12540303"
}
]
},
"local_group": {
"items": [
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "Space-Radiation-Laboratory"
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{
"id": "Zwicky-Transient-Facility"
}
]
},
"doi": "10.3847/1538-4357/abde34",
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}
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"pub_year": "2021",
"author_list": "Brightman, Murray; Ward, Charlotte; et el."
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"items": [
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Ludlam-Renee-M",
"name": {
"family": "Ludlam",
"given": "Renee M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Thompson-Ellen-T",
"name": {
"family": "Thompson",
"given": "Ellen T."
},
"orcid": "0000-0002-3669-2294"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Hare-Jeremy",
"name": {
"family": "Hare",
"given": "Jeremy"
},
"orcid": "0000-0002-8548-482X"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta D."
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Krivonos-Roman-A",
"name": {
"family": "Krivonos",
"given": "Roman A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Madsen-Kristin-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mastroserio-Guglielmo",
"name": {
"family": "Mastroserio",
"given": "Guglielmo"
},
"orcid": "0000-0003-4216-7936"
},
{
"id": "Slaughter-Catherine-M",
"name": {
"family": "Slaughter",
"given": "Catherine M."
},
"orcid": "0000-0002-5752-3780"
},
{
"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wik-Daniel",
"name": {
"family": "Wik",
"given": "Daniel"
},
"orcid": "0000-0001-9110-2245"
},
{
"id": "Zoglauer-Andreas",
"name": {
"family": "Zoglauer",
"given": "Andreas"
},
"orcid": "0000-0001-9067-3150"
}
]
},
"title": "StrayCats: A Catalog of NuSTAR Stray Light Observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-ray surveys; Astrophysical black holes; Neutron stars; High mass x-ray binary stars; Low-mass x-ray binary stars; Pulsars",
"note": "\u00a9 2021 The American Astronomical Society. \n\nReceived 2020 November 13; revised 2021 January 18; accepted 2021 January 25; published 2021 March 3. \n\nThis work was supported by the National Aeronautics and Space Administration (NASA) under grant No. 80NSSC19K1023 issued through the NNH18ZDA001N Astrophysics Data Analysis Program (ADAP). R.M.L. acknowledges the support of NASA through Hubble Fellowship Program grant HST-HF2-51440.001. R.A.K. acknowledges support from the Russian Science Foundation (grant 19-12-00396). J.H. acknowledges support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the USRA through a contract with NASA. \n\nAdditionally, this work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - , MAXI - , HEASARC. - \n\nSoftware: astropy (Robitaille et al. 2013; Astropy Collaboration et al. 2018), astroquery (Ginsburg et al. 2019), HEASoft/FTOOLS, IDL, 19 matplotlib (Hunter 2007), numpy, 20 pandas (Pandas Development Team 2020), plotly, 21 scikit-image, 22 Veusz. 23\n\nPublished - Grefenstette_2021_ApJ_909_30.pdf
Accepted Version - 2102.01236.pdf
",
"abstract": "We present StrayCats, a catalog of NuSTAR stray light observations of X-ray sources. Stray light observations arise for sources 1\u00b0\u20134\u00b0 away from the telescope pointing direction. At this off-axis angle, X-rays pass through a gap between the optics and aperture stop and so do not interact with the X-ray optics; instead, they directly illuminate the NuSTAR focal plane. We have systematically identified and examined over 1400 potential observations resulting in a catalog of 436 telescope fields and 78 stray light sources that have been identified. The sources identified include historically known persistently bright X-ray sources, X-ray binaries in outburst, pulsars, and type I X-ray bursters. In this paper, we present an overview of the catalog, how we identified the StrayCats sources, and the analysis techniques required to produce high-level science products. Finally, we present a few brief examples of the science quality of these unique data.",
"date": "2021-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "909",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 30",
"id_number": "CaltechAUTHORS:20210305-073046158",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210305-073046158",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC19K1023"
},
{
"agency": "NASA",
"grant_number": "NNH18ZDA001N"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "Russian Science Foundation",
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"title": "Timing Calibration of the NuSTAR X-Ray Telescope",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Pulsar timing method; Cross-validation; X-ray detectors; X-ray astronomy; X-ray telescopes; Millisecond pulsars",
"note": "\u00a9 2021 The American Astronomical Society. \n\nReceived 2020 September 16; revised 2020 November 27; accepted 2020 December 7; published 2021 February 23. \n\nM.B. thanks the Fulbright Visiting Scholar Program for supporting a 9 month visit at Caltech. D.J.W. acknowledges financial support from STFC via an Ernest Rutherford fellowship. The authors wish to thank the NuSTAR X-ray Binaries WG, the Magnetars/RPP WG, and the Timing WG, for the hard work and fruitful discussions that led to, and improved, this work; Victoria Kaspi, Jill Burnham, Alessandro Riggio, Andrea Sanna, Paul Ray, Iulia Deneva, Franco Buffa and Alessio Trois for insightful discussions and suggestions. They also wish to thank the referee for their comments, that helped improving the quality of this paper. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, NICER - , HEASARC - . \n\nSoftware: Nustar Clock Utils,15 Stingray (Huppenkothen et al. 2016, 2019), HENDRICS (Bachetti 2018), astropy (Price-Whelan et al. 2018), PINT (Luo et al. 2019), HEASoft/FTOOLS (Blackburn 1995; Blackburn et al. 1999), ATNF pulsar catalog (Manchester et al. 2005), PRESTO (Ransom 2011), corner (Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), IDL.16 Veusz,17 Holoviews.18\n\nPublished - Bachetti_2021_ApJ_908_184.pdf
Accepted Version - 2009.10347.pdf
",
"abstract": "The Nuclear Spectroscopic Telescope Array (NuSTAR) mission is the first focusing X-ray telescope in the hard X-ray (3\u201379 keV) band. Among the phenomena that can be studied in this energy band, some require high time resolution and stability: rotation-powered and accreting millisecond pulsars, fast variability from black holes and neutron stars, X-ray bursts, and more. Moreover, a good alignment of the timestamps of X-ray photons to UTC is key for multi-instrument studies of fast astrophysical processes. In this paper, we describe the timing calibration of the NuSTAR mission. In particular, we present a method to correct the temperature-dependent frequency response of the on-board temperature-compensated crystal oscillator. Together with measurements of the spacecraft clock offsets obtained during downlinks passes, this allows a precise characterization of the behavior of the oscillator. The calibrated NuSTAR event timestamps for a typical observation are shown to be accurate to a precision of ~65 \u03bcs.",
"date": "2021-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "908",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 184",
"id_number": "CaltechAUTHORS:20210205-093236142",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210205-093236142",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Fulbright Foundation"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
}
]
},
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"doi": "10.3847/1538-4357/abd1d6",
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"pub_year": "2021",
"author_list": "Bachetti, Matteo; Markwardt, Craig B.; et el."
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"id": "Duncan-Jessie",
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{
"id": "Glesener-Lindsay",
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"title": "NuSTAR Observation of Energy Release in 11 Solar Microflares",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "The Sun; Solar flare spectra; Solar x-ray flares; Non-thermal radiation sources; Solar flares; Solar physics",
"note": "\u00a9 2021 The American Astronomical Society. \n\nReceived 2020 August 28; revised 2020 October 22; accepted 2020 November 11; published 2021 February 9. \n\nThis work was supported under an NSF Faculty Development Grant (AGS-1429512) to the University of Minnesota, the 2019 NASA Fellowship Program (80NSSC19k1687), an NSF CAREER award (NSF-AGS-1752268), the SolFER DRIVE center (80NSSC20K0627), and the NASA NuSTAR Guest Observer program (80NSSC18K1744). I.G.H is supported by a Royal Society University Fellowship. The authors also wish to thank Pascal Saint-Hilaire for help with eclipse predictions in planning the 2017 August 21 NuSTAR observation.\n\nPublished - Duncan_2021_ApJ_908_29.pdf
Accepted Version - 2011.06651.pdf
",
"abstract": "Solar flares are explosive releases of magnetic energy. Hard X-ray (HXR) flare emission originates from both hot (millions of Kelvin) plasma and nonthermal accelerated particles, giving insight into flare energy release. The Nuclear Spectroscopic Telescope ARray (NuSTAR) utilizes direct-focusing optics to attain much higher sensitivity in the HXR range than that of previous indirect imagers. This paper presents 11 NuSTAR microflares from two active regions (AR 12671 on 2017 August 21 and AR 12712 on 2018 May 29). The temporal, spatial, and energetic properties of each are discussed in context with previously published HXR brightenings. They are seen to display several \"large flare\" properties, such as impulsive time profiles and earlier peak times in higher-energy HXRs. For two events where the active region background could be removed, microflare emission did not display spatial complexity; differing NuSTAR energy ranges had equivalent emission centroids. Finally, spectral fitting showed a high-energy excess over a single thermal model in all events. This excess was consistent with additional higher-temperature plasma volumes in 10/11 microflares and only with an accelerated particle distribution in the last. Previous NuSTAR studies focused on one or a few microflares at a time, making this the first to collectively examine a sizable number of events. Additionally, this paper introduces an observed variation in the NuSTAR gain unique to the extremely low livetime (<1%) regime and establishes a correction method to be used in future NuSTAR solar spectral analysis.",
"date": "2021-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "908",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 29",
"id_number": "CaltechAUTHORS:20210205-093239844",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210205-093239844",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "NSF",
"grant_number": "AGS-1429512"
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{
"agency": "NASA Postdoctoral Program",
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{
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}
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"name": {
"family": "Salvaterra",
"given": "R."
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},
"title": "A new transient ultraluminous X-ray source in NGC\u20097090",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: black holes \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual (NGC 7090 ULX3)",
"note": "\u00a9 2020 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2020 November 18. Received 2020 November 17; in original form 2020 October 9. Published: 25 November 2020. \n\nThe authors would like to thank the reviewer for their positive feedback, which helped to improve the final version of the manuscript. DJW and MJM acknowledge support from the Science and Technology Facilities Council (STFC) in the form of Ernest Rutherford Fellowships. PAE acknowledges UK Space Agency (UKSA) support. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by the NASA Jet Propulsion Laboratory (JPL), and has utilized the NUSTARDAS software package, jointly developed by the Space Science Data Centre (SSDC; Italy) and Caltech (USA). This research has also made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, as well as public data from the Swift data archive. Finally, this work has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive, as well as data obtained from the 4XMM XMM-Newton serendipitous source catalogue, compiled by the 10 institutes of the XMM-Newton Survey Science Centre (SSC) selected by ESA. \n\nData Availability: All of the data underlying this article are either already publicly available from ESA's XMM\u2013Newton Science Archive (https://www.cosmos.esa.int/web/xmm-newton/xsa), NASA's HEASARC archive (https://heasarc.gsfc.nasa.gov/), and NASA's Chandra Data Archive (https://cxc.harvard.edu/cda/), or will be from 2021 May.\n\nPublished - staa3666.pdf
Accepted Version - 2011.08870.pdf
",
"abstract": "We report on the discovery of a new, transient ultraluminous X-ray source (ULX) in the galaxy NGC\u20097090. This new ULX, which we refer to as NGC\u20097090 ULX3, was discovered via monitoring with Swift during 2019\u20132020, and to date has exhibited a peak luminosity of L_X \u223c 6 \u00d7 10\u00b3\u2079 erg s\u207b\u00b9. Archival searches show that, prior to its recent transition into the ULX regime, ULX3 appeared to exhibit a fairly stable luminosity of L_X \u223c 10\u00b3\u2078 erg s\u207b\u00b9. Such strong long-time-scale variability may be reminiscent of the small population of known ULX pulsars, although deep follow-up observations with XMM\u2013Newton and NuSTAR do not reveal any robust X-ray pulsation signals. Pulsations similar to those seen from known ULX pulsars cannot be completely excluded, however, as the limit on the pulsed fraction of any signal that remains undetected in these data is \u227220 per cent. The broad-band spectrum from these observations is well modelled with a simple thin disc model, consistent with sub-Eddington accretion, which may instead imply a moderately large black hole accretor (M_(BH) \u223c 40\u2009M\u2299). Similarly, though, more complex models consistent with the super-Eddington spectra seen in other ULXs (and the known ULX pulsars) cannot be excluded given the limited signal-to-noise ratio of the available broad-band data. The nature of the accretor powering this new ULX therefore remains uncertain.",
"date": "2021-02",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "501",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1002-1012",
"id_number": "CaltechAUTHORS:20210201-140020702",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210201-140020702",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "United Kingdom Space Agency (UKSA)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.1093/mnras/staa3666",
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"title": "Constraints on Axionlike Particles from a Hard X-Ray Observation of Betelgeuse",
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"note": "\u00a9 2021 American Physical Society. \n\n(Received 14 October 2020; revised 28 November 2020; accepted 11 December 2020; published 21 January 2021) \n\nWe thank D.\u2009R. Wik and S. Rossland for helpful discussions on the NuSTAR instrument background; J.\u2009L. Han and S. Zhang for discussions concerning the Galactic magnetic field in the direction of Betelgeuse; Benjamin Safdi, Christopher Dessert, John Beacom, Shunsaku Horiuchi, and Kenny C.\u2009Y. Ng for helpful comments and discussions. The NuSTAR observations described in this work were awarded under NASA Grant No. 80NSSC20K0031. The computational aspects of this work made extensive use of the following packages: saoimage ds9 distributed by the Smithsonian Astrophysical Observatory; the scipy ecosystem, particularly matplotlib and numpy; and astropy, a community-developed core python package for Astronomy. This research has made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). M.\u2009X. and M.\u2009G. were supported by NASA Grant No. 80NSSC20K0031. O.\u2009S. has been supported by the Agenzia Spaziale Italiana (ASI) and the Instituto Nazionale di Astrofsica (INAF) under the Agreement No. 2017-14-H.0\u2014attivit\u00e0 di studio per la comunit\u00e0 scientifica di Astrofisica delle Alte Energie e Fisica Astroparticellare. A.\u2009M. is partially supported by the Italian Istituto Nazionale di Fisica Nucleare (INFN) through the \"Theoretical Astroparticle Physics\" project and by the research Grant No. 2017W4HA7S \"NAT-NET: Neutrino and Astroparticle Theory Network\" under the program PRIN 2017 funded by the Italian Ministero dell'Universit\u00e0 e della Ricerca (MUR). B.\u2009G. was supported under NASA Contract No. NNG08FD60C.\n\nPublished - PhysRevLett.126.031101.pdf
Accepted Version - 2009.09059.pdf
Supplemental Material - Betelgeuse_ALP_SM.pdf
",
"abstract": "We use the first observation of Betelgeuse in hard x rays to perform a novel search for axionlike particles (ALPs). Betelgeuse is not expected to be a standard source of x rays, but light ALPs produced in the stellar core could be converted back into photons in the Galactic magnetic field, producing a detectable flux that peaks in the hard x-ray band (E_\u03b3 > 10 keV). Using a 50 ks observation of Betelgeuse by the NuSTAR satellite telescope, we find no significant excess of events above the expected background. Using models of the regular Galactic magnetic field in the direction of Betelgeuse, we set a 95% C.L. upper limit on the ALP-photon coupling of g_(a\u03b3) < (0.5\u20131.8) \u00d7 10\u207b\u00b9\u00b9 GeV\u207b\u00b9 (depending on magnetic field model) for ALP masses m_a < (5.5\u20133.5) \u00d7 10 \u207b\u00b9\u00b9 eV.",
"date": "2021-01-22",
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"publication": "Physical Review Letters",
"volume": "126",
"number": "3",
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},
"title": "A Variable Ionized Disk Wind in the Black Hole Candidate EXO 1846\u2013031",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "High energy astrophysics; X-ray transient sources; Accretion",
"note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 July 30; revised 2020 October 25; accepted 2020 October 26; published 2020 December 29. \n\nWe are grateful to Timothy R. Kallman for help with xstar. We thank the anonymous referee for the helpful comments. This work made use of the data from the Insight-HXMT mission, a project funded by China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). The Insight-HXMT team gratefully acknowledges the support from the National Program on Key Research and Development Project (grant No. 2016YFA0400800) from the Minister of Science and Technology of China (MOST) and the Strategic Priority Research Program of the Chinese Academy of Sciences (grant No. XDB23040400). The authors thank the support from the National Natural Science Foundation of China under grant Nos. 11673023, 11733009, 11603037, 11973052, U1838201, U1838115, U1938103, and U1838202. Y.W. and L.Z. acknowledge support from the Royal Society Newton Funds. D.A. acknowledges support from the Royal Society. J.M. acknowledges the support from STFC (UK) through the University of Strathclyde UK APAP network grant ST/R000743/1. J.A.G. acknowledges support from NASA grant 80NSSC20K1238 and from the Alexander von Humboldt Foundation. Additionally, this work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nSoftware: XSPEC (v12.11.1; Arnaud 1996), NuSTARDAS (v2.0.0), HXMTDAS (v2.02; Zhang et al. 2020).\n\nPublished - Wang_2021_ApJ_906_11.pdf
Accepted Version - 2010.14662.pdf
",
"abstract": "After 34 yr, the black hole candidate EXO 1846\u2013031 went into outburst again in 2019. We investigate its spectral properties in the hard intermediate and the soft states with NuSTAR and Insight-HXMT. A reflection component has been detected in the two spectral states but possibly originating from different illumination spectra: in the intermediate state, the illuminating source is attributed to a hard coronal component, which has been commonly observed in other X-ray binaries, whereas in the soft state, the reflection is probably produced by disk self-irradiation. Both cases support EXO 1846\u2013031 as a low-inclination system of ~40\u00b0. An absorption line is clearly detected at ~7.2 keV in the hard intermediate state, corresponding to a highly ionized disk wind (log} \u03be > 6.1) with a velocity of up to 0.06c. Meanwhile, quasi-simultaneous radio emissions have been detected before and after the X-rays, implying the coexistence of disk winds and jets in this system. If only the high-flux segment of the NuSTAR observation is considered, the observed wind appears to be magnetically driven. The absorption line disappeared in the soft state and a narrow emission line appeared at ~6.7 keV on top of the reflection component, which may be evidence for disk winds, but data with higher spectral resolution are required to examine this.",
"date": "2021-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "906",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 11",
"id_number": "CaltechAUTHORS:20210112-151231714",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210112-151231714",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "China National Space Administration"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDB23040400"
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"agency": "National Key Research and Development Program of China",
"grant_number": "2016YFA0400800"
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"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Urry-C-Megan",
"name": {
"family": "Urry",
"given": "C. M."
},
"orcid": "0000-0002-0745-9792"
}
]
},
"title": "NuSTAR Survey of Obscured Swift/BAT-selected Active Galactic Nuclei. II. Median High-energy Cutoff in Seyfert II Hard X-Ray Spectra",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Active galactic nuclei; X-ray active galactic nuclei; Seyfert galaxies; High energy astrophysics; X-ray surveys",
"note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 April 19; revised 2020 August 7; accepted 2020 August 25; published 2020 December 11. \n\nThe authors appreciate helpful suggestions from the anonymous referee, which helped to improve the clarity of the paper. \n\nM.B. acknowledges support from the YCAA Prize Postdoctoal Fellowship, the National Aeronautics and Space Administration (NASA) under the NASA Earth and Space Science Fellowship program (grant NNX14AQ07H), and support from the Black Hole Initiative at Harvard University, which is funded in part by the Gordon and Betty Moore Foundation (grant GBMF8273) and in part by the John Templeton Foundation. A.C. and G.M. acknowledge support from the ASI/INAF grant I/037/12/0 and the Caltech Kingsley fellowship program. A.A. acknowledges financial support from Ministry of Education Malaysia Fundamental Research Grant Scheme grant code FRGS/1/2019/STG02/UKM/02/7. P.B. acknowledges financial support from the STFC and the Czech Science Foundation project No. 19-05599Y. P.G. acknowledges support from the STFC and a UGC/UKIERI Thematic Partnership. \n\nWe have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the Space Science Data Center (SSDC; ASI, Italy) and the California Institute of Technology (USA). Part of this work is based on archival data, software, or online services provided by the SSDC. This research has made use of the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center and NASA's Astrophysics Data System. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift. - \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018), ASURV (Feigelson et al. 2014), Matplotlib (Hunter 2007), Xspec (Arnaud 1996).\n\nPublished - Balokovic_2020_ApJ_905_41.pdf
Submitted - 2011-06583.pdf
",
"abstract": "Broadband X-ray spectroscopy of the X-ray emission produced in the coronae of active galactic nuclei (AGNs) can provide important insights into the physical conditions very close to their central supermassive black holes. The temperature of the Comptonizing plasma that forms the corona is manifested through a high-energy cutoff that has been difficult to directly constrain even in the brightest AGN because it requires high-quality data at energies above 10 keV. In this paper we present a large collection of coronal cutoff constraints for obscured AGNs based on a sample of 130 AGNs selected in the hard X-ray band with Swift/BAT and observed nearly simultaneously with NuSTAR and Swift/XRT. We find that under a reasonable set of assumptions regarding partial constraints the median cutoff is well constrained to 290 \u00b1 20 keV, where the uncertainty is statistical and given at the 68% confidence level. We investigate the sensitivity of this result to our assumptions and find that consideration of various known systematic uncertainties robustly places the median cutoff between 240 and 340 keV. The central 68% of the intrinsic cutoff distribution is found to be between about 140 and 500 keV, with estimated uncertainties of 20 and 100 keV, respectively. In comparison with the literature, we find no clear evidence that the cutoffs in obscured and unobscured AGNs are substantially different. Our analysis highlights the importance of carefully considering partial and potentially degenerate constraints on the coronal high-energy cutoff in AGNs.",
"date": "2020-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "905",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 41",
"id_number": "CaltechAUTHORS:20201215-141036856",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201215-141036856",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Yale Center for Astronomy and Astrophysics"
},
{
"agency": "Gordon and Betty Moore Foundation",
"grant_number": "GBMF8273"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Lewis A. Kingsley Fellowship"
},
{
"agency": "Ministry of Education (Malaysia)",
"grant_number": "FRGS/1/2019/STG02/UKM/02/7"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Czech Science Foundation",
"grant_number": "19-05599Y"
},
{
"agency": "UK India Education Research Initiative (UKIERI)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/abc342",
"primary_object": {
"basename": "2011-06583.pdf",
"url": "https://authors.library.caltech.edu/records/271rm-5s795/files/2011-06583.pdf"
},
"related_objects": [
{
"basename": "Balokovic_2020_ApJ_905_41.pdf",
"url": "https://authors.library.caltech.edu/records/271rm-5s795/files/Balokovic_2020_ApJ_905_41.pdf"
}
],
"pub_year": "2020",
"author_list": "Balokovi\u0107, M.; Harrison, F. A.; et el."
},
{
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"eprint_id": 106199,
"eprint_status": "archive",
"datestamp": "2023-08-19 23:39:13",
"lastmod": "2023-10-20 23:11:36",
"type": "article",
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"creators": {
"items": [
{
"id": "Staubert-R",
"name": {
"family": "Staubert",
"given": "R."
},
"orcid": "0000-0003-1498-1543"
},
{
"id": "Ducci-L",
"name": {
"family": "Ducci",
"given": "L."
}
},
{
"id": "Ji-L",
"name": {
"family": "Ji",
"given": "L."
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Rothschild-R-E",
"name": {
"family": "Rothschild",
"given": "R. E."
}
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "K."
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Brumback-M-C",
"name": {
"family": "Brumback",
"given": "M."
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "Cyclotron line energy in Hercules X-1: stable after the decay",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: magnetic field / radiation mechanisms: general / scattering / pulsars: individual: Her X-1 / stars: neutron / X-rays: stars",
"note": "\u00a9 ESO 2020. \n\nReceived: 6 July 2020. Accepted: 14 August 2020. \n\nWe would like to acknowledge the dedication of all the people who have contributed to the great success of all relevant missions, in particular NuSTAR. We especially thank the \"schedulers\", foremost Karl Forster, for his efforts with respect to the non-standard scheduling of the observations of Her X-1. We acknowledge the historical contributions to the subject at hand by Dmitry Klochkov. We thank the anonymous referee for valuable comments.\n\nPublished - aa38855-20.pdf
",
"abstract": "We summarize the results of a dedicated effort made between 2012 and 2019 to follow the evolution of the cyclotron line in Her X-1 through repeated NuSTAR observations. The previously observed nearly 20-year-long decay of the cyclotron line energy has ended in 2012: from then on, the pulse-phase-averaged flux-corrected cyclotron line energy has remained stable and constant at an average value of E_(cyc) = (37.44\u2005\u00b1\u20050.07) keV (normalized to a flux level of 6.8 RXTE/ASM-cts s\u207b\u00b9). The flux dependence of E_(cyc) discovered in 2007 is now measured with high precision, giving a slope of (0.675\u2005\u00b1\u20050.075) keV/(ASM-cts s\u207b\u00b9), corresponding to an increase of 6.5% of E_(cyc) for an increase in flux by a factor of two. We also find that all line parameters as well as the continuum parameters show a correlation with X-ray flux. While a correlation between E_(cyc) and X-ray flux (both positive and negative) is now known for several accreting binaries with various suggestions for the underlying physics, the phenomenon of a long-term decay has so far only been seen in Her X-1 and Vela X-1, with far less convincing explanations.",
"date": "2020-10",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "642",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A196",
"id_number": "CaltechAUTHORS:20201021-160147836",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201021-160147836",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/202038855",
"primary_object": {
"basename": "aa38855-20.pdf",
"url": "https://authors.library.caltech.edu/records/9n434-39v78/files/aa38855-20.pdf"
},
"pub_year": "2020",
"author_list": "Staubert, R.; Ducci, L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/rs3y8-xzy67",
"eprint_id": 105385,
"eprint_status": "archive",
"datestamp": "2023-08-19 23:11:09",
"lastmod": "2023-10-20 21:56:26",
"type": "article",
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"creators": {
"items": [
{
"id": "Ballhausen-R",
"name": {
"family": "Ballhausen",
"given": "Ralf"
},
"orcid": "0000-0002-1118-8470"
},
{
"id": "Lorenz-Maximilian",
"name": {
"family": "Lorenz",
"given": "Maximilian"
},
"orcid": "0000-0001-6553-9590"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Corrales-Lia",
"name": {
"family": "Corrales",
"given": "Lia"
},
"orcid": "0000-0002-5466-3817"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Bissinger-n\u00e9-K\u00fchnel-M",
"name": {
"family": "Bissinger n\u00e9 K\u00fchnel",
"given": "Matthias"
},
"orcid": "0000-0002-8709-8236"
},
{
"id": "Kretschmar-P",
"name": {
"family": "Kretschmar",
"given": "Peter"
},
"orcid": "0000-0001-9840-2048"
},
{
"id": "Kallman-Timothy-R",
"name": {
"family": "Kallman",
"given": "Timothy R."
},
"orcid": "0000-0002-5779-6906"
},
{
"id": "Grinberg-V",
"name": {
"family": "Grinberg",
"given": "Victoria"
},
"orcid": "0000-0003-2538-0188"
},
{
"id": "Hell-Natalie",
"name": {
"family": "Hell",
"given": "Natalie"
},
"orcid": "0000-0003-3057-1536"
},
{
"id": "Psadaraki-I",
"name": {
"family": "Psadaraki",
"given": "Ioanna"
}
},
{
"id": "Rogantini-Daniele",
"name": {
"family": "Rogantini",
"given": "Daniele"
},
"orcid": "0000-0002-5359-9497"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Dust and gas absorption in the high mass X-ray binary IGR J16318\u22124848",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries / dust, extinction / X-rays: individuals: IGR J16318-4848 / circumstellar matter",
"note": "\u00a9 ESO 2020. \n\nReceived 1 May 2020 / Accepted 2 July 2020. \n\nWe thank the anonymous referee for constructive comments that helped to improve the manuscript. We thank Jakob Stierhof, Daniel Stern, and Stefan Licklederer for extensive and fruitful discussions. R.B. acknowledges partial funding by the Bundesministerium f\u00fcr Wirtschaft under Deutsches Zentrum f\u00fcr Luft- und Raumfahrt contract 50 OR 1410. V.G. is supported through the Margarete von Wrangell fellowship by the ESF and the Ministry of Science, Research and the Arts Baden-W\u00fcrttemberg. Work at LLNL is conducted under the auspices of the US DOE under Contract DE-AC52-07NA27344. This research is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA and has made use of data obtained with NuSTAR, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We acknowledge the use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/).\n\nPublished - aa38317-20.pdf
",
"abstract": "Context. With an absorption column density on the order of 10\u00b2\u2074 cm\u207b\u00b2, IGR J16318\u22124848 is one of the most extreme cases of a highly obscured high mass X-ray binary. In addition to the overall continuum absorption, the source spectrum exhibits a strong iron and nickel fluorescence line complex at 6.4 keV. Previous empirical modeling of these features and comparison with radiative transfer simulations raised questions about the structure and covering fraction of the absorber and the profile of the fluorescence lines. \n\nAims. We aim at a self-consistent description of the continuum absorption, the absorption edges, and the fluorescence lines to constrain the properties of the absorbing material, such as ionization structure and geometry. We further investigate the effects of dust absorption on the observed spectra and the possibility of fluorescence emission from dust grains. \n\nMethods. We used XMM-Newton and NuSTAR spectra to first empirically constrain the incident continuum and fluorescence lines. Next we used XSTAR to construct a customized photoionization model where we vary the ionization parameter, column density, and covering fraction. In the third step we modeled the absorption and fluorescence in a dusty olivine absorber and employed both a simple analytical model for the fluorescence line emission and a Monte Carlo simulation of radiative transfer that generates line fluxes, which are very close to the observational data. \n\nResults. Our empirical spectral modeling is in agreement with previous works. Our second model, the single gas absorber does not describe the observational data. In particular, irrespective of the ionization state or column density of the absorber, a much higher covering fraction than previously estimated is needed to produce the strong fluorescence lines and the large continuum absorption. A dusty, spherical absorber (modeled as consisting of olivine dust, although the nature of dust cannot be constrained) is able to produce the observed continuum absorption and edges. \n\nConclusions. A dense, dusty absorber in the direct vicinity of the source consisting of dust offers a consistent description of both the strong continuum absorption and the strong emission features in the X-ray spectrum of IGR J16318\u22124848. In particular, for low optical depth of individual grains, which is the case for typical volume densities and grain size distribution models, the dust will contribute significantly to the fluorescence emission.",
"date": "2020-09",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "641",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A65",
"id_number": "CaltechAUTHORS:20200915-115017424",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200915-115017424",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "50 OR 1410"
},
{
"agency": "European Social Fund"
},
{
"agency": "Baden-W\u00fcrttemberg Ministry of Science, Research and the Arts"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-AC52-07NA27344"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/202038317",
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"pub_year": "2020",
"author_list": "Ballhausen, Ralf; Lorenz, Maximilian; et el."
},
{
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"eprint_id": 104379,
"eprint_status": "archive",
"datestamp": "2023-08-19 23:08:53",
"lastmod": "2023-10-20 19:21:57",
"type": "article",
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"items": [
{
"id": "Annuar-A",
"name": {
"family": "Annuar",
"given": "A."
},
"orcid": "0000-0003-0387-1429"
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "G. B."
},
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},
{
"id": "Asmus-D",
"name": {
"family": "Asmus",
"given": "D."
},
"orcid": "0000-0003-0220-2063"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "P. G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
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},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Chen-Chien-Ting-J",
"name": {
"family": "Chen",
"given": "C.-T. J."
},
"orcid": "0000-0002-4945-5079"
},
{
"id": "Del-Moro-A",
"name": {
"family": "Del Moro",
"given": "A."
}
},
{
"id": "Farrah-Duncan",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
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{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M. J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "L."
},
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{
"id": "Marchesi-S",
"name": {
"family": "Marchesi",
"given": "S."
},
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},
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
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{
"id": "Nardini-E",
"name": {
"family": "Nardini",
"given": "E."
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{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
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{
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"family": "Stern",
"given": "D."
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{
"id": "Zappacosta-L",
"name": {
"family": "Zappacosta",
"given": "L."
},
"orcid": "0000-0002-4205-6884"
}
]
},
"title": "NuSTAR Observations of Four Nearby X-ray Faint AGN: Low Luminosity or Heavy Obscuration?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 X-rays: individual: ESO 121-G6 \u2013X-rays: individual:NGC660 \u2013X-rays: individual:NGC3486 \u2013 X-rays: individual: NGC 5195",
"note": "\u00a9 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2020 June 15. Received 2020 June 8; in original form 2020 March 23. Published: 27 June 2020. \n\nWe acknowledge financial support from the Ministry of Higher Education Malaysia Fundamental Research Grant Scheme grant code FRGS/1/2019/STG02/UKM/02/7 (AA), the Science and Technology Facilities Council grant codes ST/P000541/1 and ST/T000244/1 (DMA), and ST/R000506/1 (PG). FEB acknowledges support from the CONICYT grant CATA-Basal AFB-170002, FONDECYT Regular 1190818 and 1200495, and Chile's Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. DA acknowledges funding through the European Union's Horizon 2020 and Innovation programme under the Marie Sklodowska-Curie grant agreement no. 793499 (DUSTDEVILS). MB acknowledges support from the Black Hole Initiative at Harvard University, which is funded in part by the Gordon and Betty Moore Foundation (grant GBMF8273) and in part by the John Templeton Foundation. CR acknowledges support from the CONICYT+PAI Convocatoria Nacional subvencion a instalacion en la academia convocatoria a\u00f1o 2017 PAI77170080, and Fondecyt Iniciacion grant 11190831. PB acknowledges financial support from the STFC and the Czech Science Foundation project no. 19-05599Y. EN acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.0 and partial support from the EU Horizon 2020 Marie Sk\u0142odowska-Curie grant agreement no. 664931. \n\nNuSTAR is a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). We thank the NuSTAR Operations, Software and Calibrations teams for support with these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory and data obtained from the Chandra Data Archive. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO. This work was also based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Besides these, we also used observations collected at the European Organisation for Astronomical Research in the Southern hemisphere under ESO programme 0101.B-0386(A). \n\nThis research made use of Astropy,12 a community-developed core Python package for Astronomy (Astropy Collaboration 2013; Astropy Collaboration 2018). We also used data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) Online Service, provided by the NASA/Goddard Space Flight Center, and the NASA/IPAC extragalactic Database (NED) operated by JPL, Caltech under contract with NASA. \n\nFacilities: Chandra, Gemini, NuSTAR, Swift, VLT, WISE, and XMM\u2013Newton. \n\nData availability: The data used in this paper are publicly available to access and download as follows:\ni.\tX-ray data\na.\tFrom NASA's High Energy Astrophysics Science Archive Research Center (https://heasarc.gsfc.nasa.gov/docs/archive.html). Details of the observations, including the observation identification numbers, are listed in Table 2.\nii.\tMid-IR data\na.\tESO121-G6: From the Gemini Observatory Archive (https://archive.gemini.edu/searchform); Program ID: GS-2010B-Q-3; PI: F. Bauer.\nb.\tNGC 660: From the European Southern Observatory Science Archive Facility (http://archive.eso.org/eso/eso_archive_main.html); Program ID: 0101.B-0386(A); PI: A. Annuar.\n\nPublished - staa1820.pdf
Accepted Version - 2006.13583.pdf
",
"abstract": "We present NuSTAR (Nuclear Spectroscopic Telescope Array) observations of four active galactic nuclei (AGNs) located within 15 Mpc. These AGNs, namely ESO 121-G6, NGC 660, NGC 3486, and NGC 5195, have observed X-ray luminosities of L_(2\u201310\u2009keV,obs) \u2272 10\u00b3\u2079 erg s\u207b\u00b9, classifying them as low-luminosity AGN (LLAGN). We perform broad-band X-ray spectral analysis for the AGN by combining our NuSTAR data with Chandra or XMM\u2013Newton observations to directly measure their column densities (N_H) and infer their intrinsic power. We complement our X-ray data with archival and new high-angular resolution mid-infrared (mid-IR) data for all objects, except NGC 5195. Based on our X-ray spectral analysis, we found that both ESO 121-G6 and NGC 660 are heavily obscured (N_H > 10\u00b2\u00b3 cm\u207b\u00b2; L_(2\u201310\u2009keV,int) \u223c 10\u2074\u00b9 erg s\u207b\u00b9), and NGC 660 may be Compton thick. We also note that the X-ray flux and spectral slope for ESO 121-G6 have significantly changed over the last decade, indicating significant changes in the obscuration and potentially accretion rate. On the other hand, NGC 3486 and NGC 5195 appear to be unobscured and just mildly obscured, respectively, with L_(2\u201310\u2009keV,int) < 10\u00b3\u2079 erg s\u207b\u00b9, i.e. genuine LLAGN. Both of the heavily obscured AGNs have L_(bol) > 10\u2074\u00b9 erg s\u207b\u00b9 and \u03bb_(Edd) \u2273 10\u207b\u00b3, and are detected in high-angular resolution mid-IR imaging, indicating the presence of obscuring dust on nuclear scale. NGC 3486, however, is undetected in high-resolution mid-IR imaging, and the current data do not provide stringent constraints on the presence or absence of obscuring nuclear dust in the AGN.",
"date": "2020-09",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "497",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "229-245",
"id_number": "CaltechAUTHORS:20200714-115518491",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200714-115518491",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Ministry of Education (Malaysia)",
"grant_number": "FRGS/1/2019/STG02/UKM/02/7"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/P000541/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/T000244/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/R000506/1"
},
{
"agency": "BASAL-CATA",
"grant_number": "AFB-170002"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1190818"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1200495"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
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},
{
"agency": "Marie Curie Fellowship",
"grant_number": "793499"
},
{
"agency": "Harvard University"
},
{
"agency": "Gordon and Betty Moore Foundation",
"grant_number": "GBMF8273"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "2017 PAI77170080"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "11190831"
},
{
"agency": "Czech Science Foundation",
"grant_number": "19-05599Y"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "2017-14-H.0"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "664931"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
}
]
},
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"doi": "10.1093/mnras/staa1820",
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"pub_year": "2020",
"author_list": "Annuar, A.; Alexander, D. M.; et el."
},
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"datestamp": "2023-08-22 06:01:47",
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"type": "article",
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"items": [
{
"id": "Wang-Jingyi",
"name": {
"family": "Wang",
"given": "Jingyi"
},
"orcid": "0000-0002-1742-2125"
},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "Erin"
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Homan-J",
"name": {
"family": "Homan",
"given": "Jeroen"
},
"orcid": "0000-0001-8371-2713"
},
{
"id": "Neilsen-J",
"name": {
"family": "Neilsen",
"given": "Joseph"
},
"orcid": "0000-0002-8247-786X"
},
{
"id": "Marcel-G",
"name": {
"family": "Marcel",
"given": "Gr\u00e9goire"
},
"orcid": "0000-0003-1780-5641"
},
{
"id": "Ludlam-R-M",
"name": {
"family": "Ludlam",
"given": "Renee M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Tombesi-F",
"name": {
"family": "Tombesi",
"given": "Francesco"
},
"orcid": "0000-0002-6562-8654"
},
{
"id": "Cackett-E-M",
"name": {
"family": "Cackett",
"given": "Edward M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Remillard-R-A",
"name": {
"family": "Remillard",
"given": "Ron A."
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},
"title": "Relativistic Reflection and Reverberation in GX 339\u20134 with NICER and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Black holes; High energy astrophysics; Astrophysical black holes; Stellar mass black holes; Low-mass X-ray binary stars; X-ray astronomy",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 October 2; revised 2020 June 17; accepted 2020 June 19; published 2020 August 11. \n\nJ.W., E.K., and J.A.G. acknowledges support from NASA grant 80NSSC17K0515 and thank the International Space Science Institute (ISSI) and participants of the ISSI Workshop \"Sombreros and Lampposts: The Geometry of Accretion onto Black Holes\" for fruitful discussions. J.A.G. is thankful for support from the Alexander von Humboldt Foundation. E.M.C. gratefully acknowledges support from the National Science Foundation, CAREER award No. AST-1351222. R.M.L. acknowledges the support of NASA through Hubble Fellowship Program grant HST-HF2-51440.001.\n\nPublished - Wang_2020_ApJ_899_44.pdf
Accepted Version - 1910.01245.pdf
",
"abstract": "We analyze seven Neutron Star Interior Composition Interior Explorer (NICER) and Nuclear Spectroscopic Telescope Array epochs of the black hole X-ray binary GX 339\u20134 in the hard state during its two most recent hard-only outbursts in 2017 and 2019. These observations cover the 1\u2013100 keV unabsorbed luminosities between 0.3% and 2.1% of the Eddington limit. With NICER's negligible pileup, high count rate, and unprecedented time resolution, we perform a spectral-timing analysis and spectral modeling using relativistic and distant reflection models. Our spectral fitting shows that as the inner disk radius moves inward, the thermal disk emission increases in flux and temperature, the disk becomes more highly ionized, and the reflection fraction increases. This coincides with the inner disk increasing its radiative efficiency around ~1% Eddington. We see a hint of the hysteresis effect at ~0.3% of Eddington; the inner radius is significantly truncated during the rise (>49R_g ), while only a mild truncation (~5R_g ) is found during the decay. At higher frequencies (2\u20137 Hz) in the highest-luminosity epoch, a soft lag is present whose energy dependence reveals a thermal reverberation lag with an amplitude similar to previous findings for this source. We also discuss the plausibility of the hysteresis effect and the debate of the disk truncation problem in the hard state.",
"date": "2020-08-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "899",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 44",
"id_number": "CaltechAUTHORS:20200811-131238093",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200811-131238093",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC17K0515"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NSF",
"grant_number": "AST-1351222"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
}
]
},
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{
"id": "Space-Radiation-Laboratory"
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"doi": "10.3847/1538-4357/ab9ec3",
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"pub_year": "2020",
"author_list": "Wang, Jingyi; Kara, Erin; et el."
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{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "D. J."
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},
{
"id": "Pinto-Ciro",
"name": {
"family": "Pinto",
"given": "C."
},
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},
{
"id": "Nowak-M-A",
"name": {
"family": "Nowak",
"given": "M."
},
"orcid": "0000-0001-6923-1315"
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{
"id": "Bachetti-Matteo",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Sathyaprakash-Rajath",
"name": {
"family": "Sathyaprakash",
"given": "R."
},
"orcid": "0000-0002-5254-3969"
},
{
"id": "Kara-Erin",
"name": {
"family": "Kara",
"given": "E."
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"given": "T. P."
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"id": "Soria-Roberto",
"name": {
"family": "Soria",
"given": "R."
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"name": {
"family": "Brightman",
"given": "M."
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"id": "Canizares-C-R",
"name": {
"family": "Canizares",
"given": "C. R."
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"given": "H. P."
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"family": "F\u00fcrst",
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"name": {
"family": "Heida",
"given": "M."
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"id": "Middleton-Matthew-J",
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"family": "Middleton",
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"family": "Stern",
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"family": "Barret",
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"family": "Fabian",
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},
"title": "The unusual broad-band X-ray spectral variability of NGC\u20091313 X-1 seen with XMM\u2013Newton, Chandra, and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries \u2013 X-rays: individual: NGC1313 X-1",
"note": "\u00a9 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2020 April 20. Received 2020 April 20; in original form 2019 November 20. Published: 26 April 2020. \n\nThe authors would like to thank the reviewer for their positive and thorough feedback, which helped to improve the final version of this manuscript. DJW and MJM acknowledge support from Science and Technology Facilities Council (STFC) Ernest Rutherford Fellowships. CP and FF acknowledge support from European Space Agency (ESA) Research Fellowships. HPE acknowledges support under National Aeronautics and Space Administration (NASA) contract NNG08FD60C. TPR was funded as part of the STFC consolidated grant ST/K000861/1. NW acknowledges support from Centre National d'Etudes Spatiales (CNES) for this work. CRC and MN acknowledge support from the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to the Massachusetts Institute of Technology (MIT), which is in turn supported by NASA under contract NAS8-03060 for the Chandra X-ray Center (CXC). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA Jet Propulsion Laboratory (JPL), and has utilized the NUSTARDAS software package, jointly developed by the Space Science Data Centre (SSDC; Italy) and Caltech (USA). This research has also made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States.\n\nPublished - staa1129.pdf
Submitted - 1911.09622.pdf
",
"abstract": "We present results from the major coordinated X-ray observing programme on the ULX NGC\u20091313 X-1 performed in 2017, combining XMM\u2013Newton, Chandra, and NuSTAR, focusing on the evolution of the broad-band (\u223c0.3\u201330.0\u2009keV) continuum emission. Clear and unusual spectral variability is observed, but this is markedly suppressed above \u223c10\u201315\u2009keV, qualitatively similar to the ULX Holmberg\u2009IX X-1. We model the multi-epoch data with two-component accretion disc models designed to approximate super-Eddington accretion, allowing for both a black hole and a neutron star accretor. With regards to the hotter disc component, the data trace out two distinct tracks in the luminosity\u2013temperature plane, with larger emitting radii and lower temperatures seen at higher observed fluxes. Despite this apparent anticorrelation, each of these tracks individually shows a positive luminosity\u2013temperature relation. Both are broadly consistent with L \u221d T\u2074, as expected for blackbody emission with a constant area, and also with L \u221d T\u00b2, as may be expected for an advection-dominated disc around a black hole. We consider a variety of possibilities for this unusual behaviour. Scenarios in which the innermost flow is suddenly blocked from view by outer regions of the super-Eddington disc/wind can explain the luminosity\u2013temperature behaviour, but are difficult to reconcile with the lack of strong variability at higher energies, assuming this emission arises from the most compact regions. Instead, we may be seeing evidence for further radial stratification of the accretion flow than is included in the simple models considered, with a combination of winds and advection resulting in the suppressed high-energy variability.",
"date": "2020-06",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "494",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "6012-6029",
"id_number": "CaltechAUTHORS:20200413-153610462",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200413-153610462",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K000861/1"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Smithsonian Astrophysical Observatory",
"grant_number": "SV3-73016"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"id": "Astronomy-Department"
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"doi": "10.1093/mnras/staa1129",
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"author_list": "Walton, D. J.; Pinto, C.; et el."
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"id": "Ludlam-R-M",
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"family": "Ludlam",
"given": "R. M."
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{
"id": "Cackett-E-M",
"name": {
"family": "Cackett",
"given": "E. M."
},
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{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Bult-P-M",
"name": {
"family": "Bult",
"given": "P. M."
}
},
{
"id": "Strohmayer-T-E",
"name": {
"family": "Strohmayer",
"given": "T. E."
},
"orcid": "0000-0001-7681-5845"
},
{
"id": "Guillot-S",
"name": {
"family": "Guillot",
"given": "S."
},
"orcid": "0000-0002-6449-106X"
},
{
"id": "Jaisawal-G-K",
"name": {
"family": "Jaisawal",
"given": "G. K."
},
"orcid": "0000-0002-6789-2723"
},
{
"id": "Malacaria-C",
"name": {
"family": "Malacaria",
"given": "C."
},
"orcid": "0000-0002-0380-0041"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Markwardt-C-B",
"name": {
"family": "Markwardt",
"given": "C. B."
},
"orcid": "0000-0001-9803-3879"
}
]
},
"title": "NICER\u2013NuSTAR Observations of the Neutron Star Low-mass X-Ray Binary 4U 1735\u201344",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; Neutron stars; Low-mass x-ray binary stars",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 February 21; revised 2020 April 4; accepted 2020 April 14; published 2020 May 22. \n\nSupport for this work was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51440.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.A.G. acknowledges support from NASA grant 80NSSC19K1020 and from the Alexander von Humboldt Foundation. E.M.C. gratefully acknowledges support through NSF CAREER award number AST-1351222. C.M. is supported by an appointment to the NASA Postdoctoral Program at the MSFC, administered by USRA. \n\nFacilities: ADS - , HEASARC - , NICER - , NuSTAR. - \n\nSoftware: heasoft (v6.26.1), nustardas (v1.8.0), nicerdas (2019-06-19_V006a), xspec (v12.10.1).\n\nPublished - Ludlam_2020_ApJ_895_45.pdf
Accepted Version - 2004.06723.pdf
",
"abstract": "We report on the first simultaneous Neutron Star Interior Composition Explore (NICER) and Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the neutron star (NS) low-mass X-ray binary 4U 1735\u221244, obtained in 2018 August. The source was at a luminosity of ~1.8 (D/5.6 kpc) \u00b2 \u00d7 10\u00b3\u2077 erg s\u207b\u00b9 in the 0.4\u201330 keV band. We account for the continuum emission with two different continuum descriptions that have been used to model the source previously. Despite the choice in continuum model, the combined passband reveals a broad Fe K line indicative of reflection in the spectrum. In order to account for the reflection spectrum we utilize a modified version of the reflection model RELXILL that is tailored for thermal emission from accreting NSs. Alternatively, we also use the reflection convolution model of RFXCONV to model the reflected emission that would arise from a Comptonized thermal component for comparison. We determine that the innermost region of the accretion disk extends close to the innermost stable circular orbit (R_(ISCO)) at the 90% confidence level regardless of reflection model. Moreover, the current flux calibration of NICER is within 5% of the NuSTAR/FPMA(B).",
"date": "2020-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "895",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 45",
"id_number": "CaltechAUTHORS:20200522-131436417",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200522-131436417",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1020"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NSF",
"grant_number": "AST-1351222"
},
{
"agency": "NASA Postdoctoral Program"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ab89a6",
"primary_object": {
"basename": "Ludlam_2020_ApJ_895_45.pdf",
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"basename": "2004.06723.pdf",
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"pub_year": "2020",
"author_list": "Ludlam, R. M.; Cackett, E. M.; et el."
},
{
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"eprint_status": "archive",
"datestamp": "2023-08-22 04:43:16",
"lastmod": "2023-10-20 00:25:56",
"type": "article",
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"creators": {
"items": [
{
"id": "Cooper-Kristopher",
"name": {
"family": "Cooper",
"given": "Kristopher"
},
"orcid": "0000-0001-8589-3378"
},
{
"id": "Hannah-Iain-G",
"name": {
"family": "Hannah",
"given": "Iain G."
},
"orcid": "0000-0003-1193-8603"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Glesener-Lindsay",
"name": {
"family": "Glesener",
"given": "Lindsay"
},
"orcid": "0000-0001-7092-2703"
},
{
"id": "Krucker-S\u00e4m",
"name": {
"family": "Krucker",
"given": "S\u00e4m"
},
"orcid": "0000-0002-2002-9180"
},
{
"id": "Hudson-Hugh-S",
"name": {
"family": "Hudson",
"given": "Hugh S."
},
"orcid": "0000-0001-5685-1283"
},
{
"id": "White-Stephen-M",
"name": {
"family": "White",
"given": "Stephen M."
},
"orcid": "0000-0002-8574-8629"
},
{
"id": "Smith-David-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
}
]
},
"title": "NuSTAR Observation of a Minuscule Microflare in a Solar Active Region",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Solar activity; Solar corona; Solar flares; Solar x-ray flares",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 March 17; revised 2020 April 4; accepted 2020 April 7; published 2020 April 22. \n\nThis Letter made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, funded by the National Aeronautics and Space Administration. These observations were supported through the NuSTAR Guest Observer program (NASA grant 80NSSC18K1744). This research has made use of SunPy v1.0.6, an open-source and free community-developed solar data analysis Python package (SunPy Community et al. 2015). This research also made use of HEASoft (a unified release of FTOOLS and XANADU software packages) and NuSTAR Data Analysis Software (NuSTARDAS). This Letter made use of the SolarSoft IDL distribution (SSW) from the IDL Astronomy Library. \n\nK.C. is supported by a Royal Society Research Fellows Enhancement Award and I.G.H is supported by a Royal Society University Fellowship.\n\nPublished - Cooper_2020_ApJL_893_L40.pdf
Accepted Version - 2004.11176.pdf
",
"abstract": "We present X-ray imaging spectroscopy of one of the weakest active region (AR) microflares ever studied. The microflare occurred at ~11:04 UT on 2018 September 9 and we studied it using the Nuclear Spectroscopic Telescope ARray (NuSTAR) and the Solar Dynamic Observatory's Atmospheric Imaging Assembly (SDO/AIA). The microflare is observed clearly in 2.5\u20137 keV with NuSTAR and in Fe XVIII emission derived from the hotter component of the 94 \u00c5 SDO/AIA channel. We estimate the event to be three orders of magnitude lower than a GOES A class microflare with an energy of 1.1 \u00d7 10\u00b2\u2076 erg. It reaches temperatures of 6.7 MK with an emission measure of 8.0 \u00d7 10\u2074\u00b3 cm\u207b\u00b3. Non-thermal emission is not detected but we instead determine upper limits to such emission. We present the lowest thermal energy estimate for an AR microflare in literature, which is at the lower limits of what is still considered an X-ray microflare.",
"date": "2020-04-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "893",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L40",
"id_number": "CaltechAUTHORS:20200422-095631058",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200422-095631058",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "80NSSC18K1744"
},
{
"agency": "Royal Society"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8213/ab873e",
"pmcid": "PMC8780508",
"primary_object": {
"basename": "2004.11176.pdf",
"url": "https://authors.library.caltech.edu/records/8wybd-rmk72/files/2004.11176.pdf"
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"basename": "Cooper_2020_ApJL_893_L40.pdf",
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}
],
"pub_year": "2020",
"author_list": "Cooper, Kristopher; Hannah, Iain G.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-22 04:41:55",
"lastmod": "2023-10-20 21:21:21",
"type": "article",
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"creators": {
"items": [
{
"id": "Lopez-L-A",
"name": {
"family": "Lopez",
"given": "Laura A."
},
"orcid": "0000-0002-1790-3148"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Auchettl-K",
"name": {
"family": "Auchettl",
"given": "Katie"
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Castro-D",
"name": {
"family": "Castro",
"given": "Daniel"
}
}
]
},
"title": "Evidence of Particle Acceleration in the Superbubble 30 Doradus C with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Shocks; X-ray astronomy; Interstellar medium; Superbubbles",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2018 November 30; revised 2020 March 19; accepted 2020 March 21; published 2020 April 24. \n\nWe thank Parviz Ghavamian, Maria Haupt, and Steve Reynolds for useful discussions and Annie Hughes for sharing the ATCA and Parkes survey data of the LMC. Additionally, we thank Daniel Wik for assistance with nuskybgd. We also acknowledge the continued work of the astronomical community contributing to AstroLib. Our work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Support for this work was provided by National Aeronautics and Space Administration through Chandra Award Number G08\u201319062X and through Smithsonian Astrophysical Observatory contract SV3\u201373016 to MIT issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8\u201303060. \n\nSoftware: CIAO (v4.7; Fruscione et al. 2006), XSPEC (v12.9.0; Arnaud 1996), ftools (Blackburn 1995), NuSTAR Data Analysis Software (v1.8.0), XMM-NewtonSAS (v15.0.0; Gabriel et al. 2004).\n\nPublished - Lopez_2020_ApJ_893_144.pdf
Submitted - 1811.12416.pdf
",
"abstract": "We present evidence of diffuse, non-thermal X-ray emission from the superbubble 30 Doradus C (30 Dor C) using hard X-ray images and spectra from NuSTAR observations. For this analysis, we utilize data from a 200 ks targeted observation of 30 Dor C as well as 2.8 Ms of serendipitous off-axis observations from the monitoring of nearby SN 1987A. The complete shell of 30 Dor C is detected up to 20 keV, and the young supernova remnant MCSNR J0536\u22126913 in the southeast of 30 Dor C is not detected above 8 keV. Additionally, six point sources identified in previous Chandra and XMM-Newton investigations have hard X-ray emission coincident with their locations. Joint spectral fits to the NuSTAR and XMM-Newton spectra across the 30 Dor C shell confirm the non-thermal nature of the diffuse emission. Given the best-fit rolloff frequencies of the X-ray spectra, we find maximum electron energies of \u224870\u2013110 TeV (assuming a B-field strength of 4 \u03bcG), suggesting 30 Dor C is accelerating particles. Particles are either accelerated via diffusive shock acceleration at locations where the shocks have not stalled behind the H\u03b1 shell, or cosmic-rays are accelerated through repeated acceleration of low-energy particles via turbulence and magnetohydrodynamic waves in the bubble's interior.",
"date": "2020-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "893",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 144",
"id_number": "CaltechAUTHORS:20190620-154339961",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190620-154339961",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "G08-19062X"
},
{
"agency": "Smithsonian Astrophysical Observatory",
"grant_number": "SV3-73016"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.48550/arXiv.1811.12416",
"primary_object": {
"basename": "1811.12416.pdf",
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}
],
"pub_year": "2020",
"author_list": "Lopez, Laura A.; Grefenstette, Brian W.; et el."
},
{
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"eprint_id": 102508,
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"datestamp": "2023-08-22 04:38:57",
"lastmod": "2023-10-20 00:16:10",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Hare-J",
"name": {
"family": "Hare",
"given": "Jeremy"
},
"orcid": "0000-0002-8548-482X"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "Michael L."
},
"orcid": "0000-0002-8466-7317"
}
]
},
"title": "Studying the Reflection Spectra of the New Black Hole X-Ray Binary Candidate MAXI J1631\u2212479 Observed by NuSTAR: A Variable Broad Iron Line Profile",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; black hole physics; X-ray binary stars; X-ray transient sources",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 August 26; revised 2020 March 5; accepted 2020 March 6; published 2020 April 13. \n\nWe thank the referee for the constructive comments that improved this paper. D.J.W. acknowledges support from an STFC Ernest Rutherford fellowship. J.A.G. acknowledges support from NASA grant NNX17AJ65G and from the Alexander von Humboldt Foundation. J.H. acknowledges support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the USRA through a contract with NASA. M.L.P. is supported by the European Space Agency (ESA) Research Fellowship. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has also made use of MAXI data provided by RIKEN, JAXA, and the MAXI team.\n\nPublished - Xu_2020_ApJ_893_30.pdf
Accepted Version - 2003.03465.pdf
",
"abstract": "We present results from the Nuclear Spectroscopic Telescope Array observations of the new black hole X-ray binary candidate MAXI J1631\u2013479 at two epochs during its 2018\u20132019 outburst, which caught the source in a disk dominant state and a power-law dominant state. Strong relativistic disk reflection features are clearly detected, displaying significant variations in the shape and strength of the broad iron emission line between the two states. Spectral modeling of the reflection spectra reveals that the inner radius of the optically thick accretion disk evolves from <1.9 r_g to 12 \u00b1 1 r_g (statistical errors at 90% confidence level) from the disk dominant to the power-law dominant state. Assuming in the former case that the inner disk radius is consistent with being at the innermost stable circular orbit, we estimate a black hole spin of a* > 0.94. Given that the bolometric luminosity is similar in the two states, our results indicate that the disk truncation observed in MAXI J1631\u2013479 in the power-law dominant state is unlikely to be driven by a global variation in the accretion rate. We propose that it may instead arise from local instabilities in the inner edge of the accretion disk at high accretion rates. In addition, we find an absorption feature in the spectra centered at 7.33 \u00b1 0.03 keV during the disk dominant state, which is evidence for the rare case that an extremely fast disk wind (v_(out) = 0.067^(+0.001)_(\u22120.004) c) is observed in a low-inclination black hole binary, with the viewing angle of 29\u00b0 \u00b1 1\u00b0 as determined by the reflection modeling.",
"date": "2020-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "893",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 30",
"id_number": "CaltechAUTHORS:20200413-123514628",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200413-123514628",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNX17AJ65G"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
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"id": "Space-Radiation-Laboratory"
},
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"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ab7dc0",
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}
],
"pub_year": "2020",
"author_list": "Xu, Yanjun; Harrison, Fiona A.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-19 20:55:56",
"lastmod": "2023-10-20 00:16:17",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Hare-J",
"name": {
"family": "Hare",
"given": "Jeremy"
},
"orcid": "0000-0002-8548-482X"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Evidence for Disk Truncation at Low Accretion States of the Black Hole Binary MAXI J1820+070 Observed by NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion, Black hole physics, X-ray binary stars, X-ray transient sources",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 January 26; revised 2020 March 2; accepted 2020 March 3; published 2020 April 14. \n\nWe thank the referee for helpful comments that improved the paper. We thank Norbert Schartel for approving the XMM-Newton DDT observation and the XMM-Newton SOC for prompt scheduling of the observation. J.H. acknowledges support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the USRA through a contract with NASA. D.J.W. acknowledge support from an STFC Ernest Rutherford Fellowship. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations.\n\nPublished - Xu_2020_ApJ_893_42.pdf
Submitted - 2003.01778.pdf
",
"abstract": "We present results from NuSTAR and XMM-Newton observations of the new black hole X-ray binary MAXI J1820+070 at low accretion rates (below 1% of the Eddington luminosity). We detect a narrow Fe K\u03b1 emission line, in contrast to the broad and asymmetric Fe K\u03b1 line profiles commonly present in black hole binaries at high accretion rates. The narrow line, with weak relativistic broadening, indicates that the Fe K\u03b1 line is produced at a large disk radius. Fitting with disk reflection models assuming standard disk emissivity finds a large disk truncation radius (a few tens to a few hundreds of gravitational radii, depending on the disk inclination). In addition, we detect a quasi-periodic oscillation (QPO) varying in frequency between 11.6 \u00b1 0.2 mHz and 2.8 \u00b1 0.1 mHz. The very low QPO frequencies suggest a large size for the optically thin Comptonization region according to the Lense\u2013Thirring precession model, supporting that the accretion disk recedes from the innermost stable circular orbit and is replaced by advection-dominated accretion flow at low accretion rates. We also discuss the possibility of an alternative accretion geometry that the narrow Fe K\u03b1 line is produced by a lamppost corona with a large height illuminating the disk.",
"date": "2020-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "893",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 42",
"id_number": "CaltechAUTHORS:20200413-152859389",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200413-152859389",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Astronomy-Department"
},
{
"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/ab7cdb",
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}
],
"pub_year": "2020",
"author_list": "Xu, Yanjun; Harrison, Fiona A.; et el."
},
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"eprint_id": 101925,
"eprint_status": "archive",
"datestamp": "2023-08-22 04:20:17",
"lastmod": "2023-10-19 23:39:07",
"type": "article",
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"creators": {
"items": [
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah P."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "Marianne"
},
"orcid": "0000-0002-1082-7496"
},
{
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"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "F\u00fcrst-Felix",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
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"orcid": "0000-0003-0388-0560"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Jaodand-Amruta-D",
"name": {
"family": "Jaodand",
"given": "Amruta"
},
"orcid": "0000-0002-3850-6651"
},
{
"id": "Middleton-Matthew-J",
"name": {
"family": "Middleton",
"given": "Matthew J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Roberts-Timothy-P",
"name": {
"family": "Roberts",
"given": "Timothy P."
},
"orcid": "0000-0001-8252-6337"
},
{
"id": "Sathyaprakash-Rajath",
"name": {
"family": "Sathyaprakash",
"given": "Rajath"
},
"orcid": "0000-0002-5254-3969"
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "The (Re)appearance of NGC 925 ULX-3, a New Transient ULX",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Accretion; Neutron stars; X-ray binary stars; Light curves; Black holes; X-ray transient sources",
"note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2019 November 20; revised 2020 January 31; accepted 2020 February 17; published 2020 March 16. \n\nWe thank our anonymous referee for useful comments on this paper. This work was supported under NASA contract NNG08FD60C. D.J.W. and M.J.M. acknowledge support from STFC in the form of Ernest Rutherford Fellowships. T.P.R. was funded as part of the STFC consolidated grant ST/K000861/1, and R.S. was funded by STFC studentship grant ST/N50404X/1. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory, as well as archival observations by XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, archival observations by the NuSTAR mission, a project led by the California Institute of Technology, managed by JPL, and funded by NASA, and observations from the Swift data archive. \n\nFacilities: XMM - Newton X-Ray Multimirror Mission satellite, CXO - , Swift(XRT) - , NuSTAR. - \n\nSoftware: astropy (Astropy Collaboration et al. 2013), CIAO (Fruscione et al. 2006), FTOOLS (Nasa High Energy Astrophysics Science Archive Research Center (Heasarc), 2014), XMM-Newton SAS.\n\nPublished - Earnshaw_2020_ApJ_891_153.pdf
Accepted Version - 2001.00642.pdf
",
"abstract": "We report the discovery of a third ULX in NGC 925 (ULX-3), detected in 2017 November by Chandra at a luminosity of L_X = (7.8 \u00b1 0.8) \u00d7 10\u00b3\u2079 erg s\u207b\u00b9. Examination of archival data for NGC 925 reveals that ULX-3 was detected by Swift at a similarly high luminosity in 2011, as well as by XMM-Newton in 2017 January at a much lower luminosity of L_X = (3.8 \u00b1 0.5) \u00d7 10\u00b3\u2078 erg s\u207b\u00b9. With an additional Chandra nondetection in 2005, this object demonstrates a high dynamic range of flux of factor \u227326. In its high-luminosity detections, ULX-3 exhibits a hard power-law spectrum with \u0393 = 1.6 \u00b1 0.1, whereas the XMM-Newton detection is slightly softer, with \u0393 = 1.8_(-0.1)^(+0.2), and is also well-fitted with a broadened disk model. The long-term light curve is sparsely covered and could be consistent either with the propeller effect or with a large-amplitude superorbital period, both of which are seen in ULXs, in particular those with neutron star accretors. Further systematic monitoring of ULX-3 will allow us to determine the mechanism by which ULX-3 undergoes its extreme variability and to better understand the accretion processes of ULXs.",
"date": "2020-03-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "891",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 153",
"id_number": "CaltechAUTHORS:20200316-150528314",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200316-150528314",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K000861/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/N50404X/1"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/ab77b8",
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}
],
"pub_year": "2020",
"author_list": "Earnshaw, Hannah P.; Heida, Marianne; et el."
},
{
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"eprint_id": 101248,
"eprint_status": "archive",
"datestamp": "2023-08-22 04:01:07",
"lastmod": "2023-10-19 22:34:14",
"type": "article",
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"items": [
{
"id": "Hare-J",
"name": {
"family": "Hare",
"given": "Jeremy"
},
"orcid": "0000-0002-8548-482X"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Buisson-D-J-K",
"name": {
"family": "Buisson",
"given": "Douglas J. K."
}
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "Ma\u00efca"
},
"orcid": "0000-0003-0724-2742"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
}
]
},
"title": "NuSTAR Observations of the Transient Galactic Black Hole Binary Candidate Swift J1858.6\u20130814: A New Sibling of V404 Cyg and V4641 Sgr?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Stellar mass black holes; X-ray transient sources; Lowmass X-ray binary stars",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 November 4; revised 2019 December 27; accepted 2020 January 8; published 2020 February 12. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J.H. and J.A.T. acknowledge partial support from NuSTAR Guest Observer grant 80NSSC19K0404. J.H. acknowledges support from an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the USRA through a contract with NASA. D.J.W. acknowledges support from STFC in the form of an Ernest Rutherford Fellowship. M.C. acknowledges support from the Centre National d'Etudes Spatiales (CNES). J.A.G. acknowledges support from NASA grant 80NSSC19K1020 and from the Alexander von Humboldt Foundation. We thank the anonymous referee for providing useful comments which have improved the quality of this paper. \n\nSoftware: XSPEC (v12.10.1; Arnaud 1996), NUSTARDAS (v1.8.0), NICERDAS (V005), Stingray (Huppenkothen et al. 2017), Xselect (v2.4e), Matplotlib (Hunter 2007), HEASOFT (v6.25), MWDust (Bovy et al. 2016), XILLVER (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), RELXILL (v1.2.0; Dauser et al. 2014; Garc\u00eda et al. 2014).\n\nPublished - Hare_2020_ApJ_890_57.pdf
Accepted Version - 2001.03214.pdf
",
"abstract": "Swift J1858.6\u22120814 was discovered by the Burst Alert Telescope on Swift on 2018 October 25. Here we report on the first follow-up Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the source, which shows variability spanning two orders of magnitude in count rate on timescales of ~10\u2013100 s. The power spectrum of the source does not show any quasi-periodic oscillations or periodicity, but has a large fractional rms amplitude of 147% \u00b1 3%, exhibiting a number of large flares throughout the observation. The hardness ratio (defined as R_(10\u201379keV)/R_(3\u201310keV)) of the flares tends to be soft, while the source spans a range of hardness ratios during nonflaring periods. The X-ray spectrum of the source shows strong reflection features, which become more narrow and peaked during the nonflaring intervals. We fit an absorbed relativistic reflection model to the source spectra to place physical constraints on the system. Most notably, we find that the source exhibits a large and varying intrinsic absorbing column density (N_H = (1.4\u20134.2) \u00d7 10\u00b2\u00b3 cm\u207b\u00b2). This large intrinsic absorption is further supported by the energy spectra extracted from two flares observed simultaneously by NuSTAR and the Neutron Star Interior Composition Explorer. We find that the inner accretion disk of the source has a low inclination, I < 29\u2218 (3\u03c3 upper limit), while the iron abundance in the disk is close to solar, A_(Fe) = 1.0 \u00b1 0.3. We set a 90% confidence upper limit on the inner radius of the accretion disk of r_(in) < 8r_(ISCO) and, by fixing r_(in) to be at r_(ISCO), a 90% confidence lower limit on the spin of the black hole of a\u2217 > 0.0. Finally, we compare the properties of Swift J1858.6\u22120814 to those of V404 Cygni and V4641 Sgr, which both show rapid flaring and a strong and variable absorption.",
"date": "2020-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "890",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 57",
"id_number": "CaltechAUTHORS:20200212-140525387",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200212-140525387",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K0404"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K1020"
},
{
"agency": "Alexander von Humboldt Foundation"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/ab6a12",
"primary_object": {
"basename": "2001.03214.pdf",
"url": "https://authors.library.caltech.edu/records/n30ph-h2c71/files/2001.03214.pdf"
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"basename": "Hare_2020_ApJ_890_57.pdf",
"url": "https://authors.library.caltech.edu/records/n30ph-h2c71/files/Hare_2020_ApJ_890_57.pdf"
}
],
"pub_year": "2020",
"author_list": "Hare, Jeremy; Tomsick, John A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/djp6e-qb369",
"eprint_id": 100924,
"eprint_status": "archive",
"datestamp": "2023-08-22 03:40:46",
"lastmod": "2023-10-19 22:15:05",
"type": "article",
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"creators": {
"items": [
{
"id": "Brightman-Murray",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah P."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Barret-Didier",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
}
]
},
"title": "Spectral Evolution of the Ultraluminous X-Ray Sources M82 X-1 and X-2",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Astrophysical black holes; Intermediate-mass black holes; Stellar mass black holes; X-ray point sources; X-ray sources; Pulsars; Neutron\nstars",
"note": "\u00a9 2020 The Author(s). Published by IOP Publishing Ltd on behalf of the American Astronomical Society. \n\nReceived 2019 September 18; revised 2019 December 5; accepted 2019 December 15; published 2020 January 27. \n\nThis research has made use of data obtained with NuSTAR, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO6-17080X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package ciao. We also acknowledge the use of public data from the Swift data archive. D.J.W. acknowledges support from an STFC Ernest Rutherford Fellowship. \n\nFacilities: Chandra (ACIS) - , NuSTAR - , Swift (XRT). -\n\nPublished - Brightman_2020_ApJ_889_71.pdf
Submitted - 2001.07285.pdf
",
"abstract": "M82 hosts two well-known ultraluminous X-ray sources (ULXs). X-1, an intermediate-mass black hole (IMBH) candidate, and X-2, an ultraluminous X-ray pulsar. Here, we present a broadband X-ray spectral analysis of both sources based on 10 simultaneous observations made with Chandra and NuSTAR. Chandra provides the high spatial resolution to resolve the crowded field in the 0.5\u20138 keV band, and NuSTAR provides the sensitive hard X-ray spectral data, extending the bandpass of our study above 10 keV. These observations, taken in 2015\u20132016, cover a period of flaring from X-1, allowing us to study the spectral evolution of this source with luminosity. During four of these observations, X-2 was found to be at a low flux level, allowing an unambiguous view of the emission from X-1. We find that the broadband X-ray emission from X-1 is consistent with that seen in other ULXs observed in detail with NuSTAR, with a spectrum that includes a broadened disk-like component and a high-energy tail. We find that the luminosity of the disk scales with inner disk temperature as L \u221d T^(\u22123/2), contrary to expectations of a standard accretion disk and previous results. These findings rule out a thermal state for sub-Eddington accretion, and therefore do not support M82 X-1 as an IMBH candidate. We also find evidence that the neutral column density of the material in the line of sight increases with L_X, perhaps due to an increased mass outflow with accretion rate. For X-2, we do not find any significant spectral evolution, but we find the spectral parameters of the phase-averaged broadband emission are consistent with the pulsed emission at the highest X-ray luminosities.",
"date": "2020-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "889",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 71",
"id_number": "CaltechAUTHORS:20200127-074253356",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200127-074253356",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "GO6-17080X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
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"doi": "10.3847/1538-4357/ab629a",
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"pub_year": "2020",
"author_list": "Brightman, Murray; Walton, Dominic J.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-22 03:40:10",
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"items": [
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Fryer-C-L",
"name": {
"family": "Fryer",
"given": "C. L."
},
"orcid": "0000-0003-2624-0056"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Lopez-L-A",
"name": {
"family": "Lopez",
"given": "L. A."
},
"orcid": "0000-0002-1790-3148"
},
{
"id": "Reynolds-S",
"name": {
"family": "Reynolds",
"given": "S."
},
"orcid": "0000-0002-5365-5444"
},
{
"id": "Zoglauer-A",
"name": {
"family": "Zoglauer",
"given": "A."
},
"orcid": "0000-0001-9067-3150"
}
]
},
"title": "NuSTAR Observations of G11.2\u20130.3",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Rotation powered pulsars; Supernova remnants; Single X-ray stars; X-ray stars",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 April 4; revised 2019 October 31; accepted 2019 November 4; published 2020 January 21. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would also like to thank Robert Archibald for his help with finding the timing solution. \n\nFacility: NuSTAR Chandra INTEGRAL - .\n\nPublished - Madsen_2020_ApJ_889_23.pdf
Accepted Version - 2002.12775.pdf
",
"abstract": "We present in this paper the hard X-ray view of the pulsar wind nebula in G11.2\u22120.3 and its central pulsar powered pulsar J1811\u22121925 as seen by NuSTAR. We complement the data with Chandra for a more complete picture and confirm the existence of a hard, power-law component in the shell with photon index \u0393 = 2.1 \u00b1 0.1, which we attribute to synchrotron emission. Our imaging observations of the shell show a slightly smaller radius at higher energies, consistent with Chandra results, and we find shrinkage as a function of increased energy along the jet direction, indicating that the electron outflow in the PWN may be simpler than that seen in other young PWNe. Combining NuSTAR with INTEGRAL, we find that the pulsar spectrum can be fit by a power law with \u0393 = 1.32 \u00b1 0.07 up to 300 keV without evidence of curvature.",
"date": "2020-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "889",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 23",
"id_number": "CaltechAUTHORS:20200122-085827125",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200122-085827125",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
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},
"doi": "10.3847/1538-4357/ab54ca",
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}
],
"pub_year": "2020",
"author_list": "Madsen, K. K.; Fryer, C. L.; et el."
},
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"items": [
{
"id": "Kamraj-N",
"name": {
"family": "Kamraj",
"given": "Nikita"
},
"orcid": "0000-0002-3233-2451"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
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"name": {
"family": "Brightman",
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},
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{
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"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
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"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Assef-R-J",
"name": {
"family": "Assef",
"given": "Roberto J."
},
"orcid": "0000-0002-9508-3667"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "Michael J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Oh-Kyuseok",
"name": {
"family": "Oh",
"given": "Kyuseok"
},
"orcid": "0000-0002-5037-951X"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "The Broadband X-Ray Spectrum of the X-Ray-obscured Type 1 AGN 2MASX J193013.80+341049.5",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Active galactic nuclei; Seyfert galaxies; X-ray astronomy",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 September 19; revised 2019 November 4; accepted 2019 November 13; published 2019 December 26. \n\nWe have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). M.B. acknowledges support from the Black Hole Initiative at Harvard University, through a grant from the John Templeton Foundation. M.K. acknowledges support from NASA through ADAP award NNH16CT03C. D.J.W. acknowledges support from STFC in the form of an Ernest Rutherford fellowship. R.J.A was supported by FONDECYT grant No. 1191124. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - , XMM-Newton - , Palomar DBSP. - \n\nSoftware: NuSTARDAS (v2.14.1), HEASOFT (v6.24), XMM SAS (v16.1.0), XSPEC (v12.8.2), Astropy, SciPy, NumPy, Matplotlib.\n\nPublished - Kamraj_2019_ApJ_887_255.pdf
Accepted Version - 1911.05820.pdf
",
"abstract": "We present results from modeling the broadband X-ray spectrum of the Type 1 active galactic nucleus (AGN) 2MASX J193013.80+341049.5 using NuSTAR, Swift, and archival XMM-Newton observations. We find this source to be highly X-ray obscured, with column densities exceeding 10\u00b2\u00b3 cm\u207b\u00b2 across all epochs of X-ray observations, spanning an 8 yr period. However, the source exhibits prominent broad optical emission lines, consistent with an unobscured Type 1 AGN classification. We fit the X-ray spectra with both phenomenological reflection models and physically motivated torus models to model the X-ray absorption. We examine the spectral energy distribution of this source and investigate some possible scenarios to explain the mismatch between X-ray and optical classifications. We compare the ratio of reddening to X-ray absorbing column density (E_(B\u2212V)/N_H) and find that 2MASX J193013.80+341049.5 likely has a much lower dust-to-gas ratio relative to the Galactic interstellar medium, suggesting that the broad line region itself could provide the source of extra X-ray obscuration, being composed of low-ionization, dust-free gas.",
"date": "2019-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "887",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 255",
"id_number": "CaltechAUTHORS:20200102-123811313",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200102-123811313",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Harvard University"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "NASA",
"grant_number": "NNH16CT03C"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1191124"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
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},
"doi": "10.3847/1538-4357/ab57fc",
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"basename": "Kamraj_2019_ApJ_887_255.pdf",
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}
],
"pub_year": "2019",
"author_list": "Kamraj, Nikita; Balokovi\u0107, Mislav; et el."
},
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"datestamp": "2023-08-22 03:16:25",
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"type": "article",
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"items": [
{
"id": "Fiocchi-M",
"name": {
"family": "Fiocchi",
"given": "M."
},
"orcid": "0000-0001-5697-6019"
},
{
"id": "Bazzano-A",
"name": {
"family": "Bazzano",
"given": "A."
},
"orcid": "0000-0002-2017-4396"
},
{
"id": "Bruni-G",
"name": {
"family": "Bruni",
"given": "G."
},
"orcid": "0000-0002-5182-6289"
},
{
"id": "Ludlam-R-M",
"name": {
"family": "Ludlam",
"given": "R."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "L."
},
"orcid": "0000-0002-6601-9543"
},
{
"id": "Onori-F",
"name": {
"family": "Onori",
"given": "F."
}
},
{
"id": "Ubertini-P",
"name": {
"family": "Ubertini",
"given": "P."
}
}
]
},
"title": "Quasi-simultaneous INTEGRAL, SWIFT, and NuSTAR Observations of the New X-Ray Clocked Burster 1RXS J180408.9-342058",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Binary stars; Low-mass X-ray binary stars; X-ray astronomy; Gamma-ray bursters; Gamma-ray astronomy",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2017 June 1; revised 2019 October 10; accepted 2019 October 11; published 2019 December. \n\nWe thank Dr. N. Degenaar and J. van den Eijnden for suggestions and discussion, that improved our work. \n\nWe acknowledge the ASI financial/programmatic support via contracts ASI-INAF agreement number 2013-025.R1 and ASI-INAF 2017-14-H.0. \n\nWe acknowledge the use of public data from the SWIFT and NuSTAR data archive. \n\nThis research has made use of data provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. \n\nR.L. gratefully acknowledges funding through a NASA Earth and Space Sciences Fellowship and the support of NASA through Hubble Fellowship Program grant HST-HF2-51440.001. \n\nF.O. acknowledges the support of the H2020 European HEMERA program, grant agreement No. 730970.\n\nPublished - Fiocchi_2019_ApJ_887_30.pdf
Accepted Version - 1910.09325.pdf
",
"abstract": "We report the quasi-simultaneous INTEGRAL, SWIFT, and NuSTAR observations showing spectral state transitions in the neutron star low-mass X-ray binary 1RXS J180408.9\u2212342058 during its 2015 outburst. We present results of the analysis of high-quality broad energy band (0.8\u2013200 keV) data in three different spectral states: high/soft, low/very-hard, and transitional state. The broadband spectra can be described in general as the sum of thermal Comptonization and reflection due to illumination of an optically thick accretion disk. During the high/soft state, blackbody emission is generated from the accretion disk and the surface of the neutron star. This emission, measured at a temperature of kT_(bb) ~ 1.2 keV, is then Comptonized by a thick corona with an electron temperature of ~2.5 keV. For the transitional and low/very-hard state, the spectra are successfully explained with emission from a double Comptonizing corona. The first component is described by thermal Comptonization of seed disk/neutron star photons (kT_(bb) ~ 1.2 keV) by a cold corona cloud with kT_e ~ 8\u201310 keV, while the second one originates from lower temperature blackbody photons (kT_(bb) \u2264 0.1 keV) Comptonized by a hot corona (kT_e ~ 35 keV). Finally, from NuSTAR observations, there is evidence that the source is a new clocked burster. The average time between two successive X-ray bursts corresponds to ~7.9 and ~4.0 ks when the persistent emission decreases by a factor of ~2, moving from a very hard to transitional state. The accretion rate (~4 x 10\u207b\u2079 M\u2299 yr \u207b\u00b9) and the decay time of the X-ray bursts longer than ~30 s suggest that the thermonuclear emission is due to mixed H/He burning triggered by thermally unstable He ignition.",
"date": "2019-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "887",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 30",
"id_number": "CaltechAUTHORS:20191209-081753551",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191209-081753551",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "2013-025.R1"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "2017-14-H.0"
},
{
"agency": "NASA Earth and Space Science Fellowship"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51440.001"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "730970"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ab4d59",
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"pub_year": "2019",
"author_list": "Fiocchi, M.; Bazzano, A.; et el."
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"items": [
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Mandel-S",
"name": {
"family": "Mandel",
"given": "Shifra"
}
},
{
"id": "Schutt-Y-E",
"name": {
"family": "Schutt",
"given": "Yve E."
}
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Coerver-A",
"name": {
"family": "Coerver",
"given": "Anna"
}
},
{
"id": "Baganoff-F-K",
"name": {
"family": "Baganoff",
"given": "Frederick K."
}
},
{
"id": "Dykaar-H",
"name": {
"family": "Dykaar",
"given": "Hannah"
}
},
{
"id": "Grindlay-J-E",
"name": {
"family": "Grindlay",
"given": "Jonathan E."
},
"orcid": "0000-0002-1323-5314"
},
{
"id": "Haggard-D",
"name": {
"family": "Haggard",
"given": "Daryl"
},
"orcid": "0000-0001-6803-2138"
},
{
"id": "Heuer-K",
"name": {
"family": "Heuer",
"given": "Keri"
}
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "Jaesub"
}
},
{
"id": "Hord-B-J",
"name": {
"family": "Hord",
"given": "Benjamin J."
}
},
{
"id": "Jin-Chichuan",
"name": {
"family": "Jin",
"given": "Chichuan"
},
"orcid": "0000-0002-2006-1615"
},
{
"id": "Nynka-M",
"name": {
"family": "Nynka",
"given": "Melania"
},
"orcid": "0000-0002-3310-1946"
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "Gabriele"
},
"orcid": "0000-0003-0293-3608"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
}
]
},
"title": "NuSTAR and Chandra Observations of New X-Ray Transients in the Central Parsec of the Galaxy",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galactic center; X-ray transient sources; low-mass X-ray\nbinary stars; X-ray telescopes",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 August 14; revised 2019 October 3; accepted 2019 October 3; published 2019 November 11. \n\nThis work used data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. We made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge the scheduling, data processing, and archive teams from the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration (NASA) under contract NAS8-03060. G.P. acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.0. C.J. acknowledges the National Natural Science Foundation of China through grant 11873054. D.H. acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant and the Canadian Institute for Advanced Research (CIFAR) Azrieli Global Scholars program. We would like to thank Daniela Huppenkothen for insightful discussions on NuSTAR timing analysis and Stingray software. We acknowledge help from Ninad Nirgudkar and Gabriel Lewis Bridges for generating the Swift/XRT light curve plots. \n\nSoftware: NuSTARDAS (v.1.7.1), HEAsoft (v6.21; HEASARC 2014), Stingray (Huppenkothen et al. 2019), XSPEC (v12.10.1; Arnaud 1996), SAOImage DS9 (Joye & Mandel 2003).\n\nPublished - Mori_2019_ApJ_885_142.pdf
Accepted Version - 1910.03459.pdf
",
"abstract": "We report NuSTAR and Chandra observations of two X-ray transients, SWIFT J174540.7\u2212290015 (T15) and SWIFT J174540.2\u2212290037 (T37), which were discovered by the Neil Gehrels Swift Observatory in 2016 within r ~ 1 pc of Sgr A*. NuSTAR detected bright X-ray outbursts from T15 and T37, likely in the soft and hard states, with 3\u201379 keV luminosities of 8 \u00d7 10\u00b3\u2076 and 3 \u00d7 10\u00b3\u2077 erg s\u207b\u00b9, respectively. No X-ray outbursts have previously been detected from the two transients and our Chandra ACIS analysis puts an upper limit of L_X \u227e 2 \u00d7 10\u00b3\u00b9 erg s\u207b\u00b9 on their quiescent 2\u20138 keV luminosities. No pulsations, significant quasi-periodic oscillations, or type I X-ray bursts were detected in the NuSTAR data. While T15 exhibited no significant red noise, the T37 power density spectra are well characterized by three Lorentzian components. The declining variability of T37 above \u03bd ~ 10 Hz is typical of black hole (BH) transients in the hard state. NuSTAR spectra of both transients exhibit a thermal disk blackbody, X-ray reflection with broadened Fe atomic features, and a continuum component well described by Comptonization models. Their X-ray reflection spectra are most consistent with high BH spin (a* \u2273 0.9) and large disk density (n_e ~ 10\u00b2\u00b9 cm\u207b\u00b3). Based on the best-fit ionization parameters and disk densities, we found that X-ray reflection occurred near the inner-disk radius, which was derived from the relativistic broadening and thermal disk component. These X-ray characteristics suggest the outbursting BH-low-mass X-ray binary scenario for both transients and yield the first BH spin measurements from X-ray transients in the central 100 pc region.",
"date": "2019-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "885",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 142",
"id_number": "CaltechAUTHORS:20191111-074450523",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191111-074450523",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "2017-14-H.0"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11873054"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
}
]
},
"local_group": {
"items": [
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},
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"id": "Space-Radiation-Laboratory"
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]
},
"doi": "10.3847/1538-4357/ab4b47",
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}
],
"pub_year": "2019",
"author_list": "Mori, Kaya; Hailey, Charles J.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-19 18:37:33",
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"items": [
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Sridhar-N",
"name": {
"family": "Sridhar",
"given": "Navin"
},
"orcid": "0000-0002-5519-9550"
},
{
"id": "Grinberg-V",
"name": {
"family": "Grinberg",
"given": "Victoria"
},
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{
"id": "Connors-R-M-T",
"name": {
"family": "Connors",
"given": "Riley M. T."
},
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{
"id": "Wang-Jingyi",
"name": {
"family": "Wang",
"given": "Jingyi"
},
"orcid": "0000-0002-1742-2125"
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{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
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{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "Thomas"
},
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"name": {
"family": "Walton",
"given": "Dominic J."
},
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{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
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{
"id": "Forster-K",
"name": {
"family": "Foster",
"given": "Karl"
},
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},
{
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"name": {
"family": "Grefenstette",
"given": "Brian"
},
"orcid": "0000-0002-1984-2932"
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{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin"
},
"orcid": "0000-0003-1252-4891"
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew"
},
"orcid": "0000-0002-9378-4072"
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]
},
"title": "The 2017 Failed Outburst of GX 339-4: Relativistic X-ray Reflection near the Black Hole Revealed by NuSTAR and Swift Spectroscopy",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 atomic processes \u2013 black hole physics \u2013 line: formation \u2013 X-rays: individual (GX 339-4)",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 May 4; revised 2019 August 1; accepted 2019 August 2; published 2019 October 29. \n\nWe thank the anonymous referee for the careful revision of this paper. We also thank Erin Kara and Didier Barret for enlightening discussions on the implications of the dual-lamppost model. J.A.G. acknowledges support from NASA grant NNX17AJ65G and from the Alexander von Humboldt Foundation. R.M.T.C. has been supported by NASA ADAP grant 80NSSC177K0515. V.G. is supported through the Margarete von Wrangell fellowship by the ESF and the Ministry of Science, Research and the Arts Baden-W\u00fcrttemberg. N.S. would like to acknowledge the support from DST-INSPIRE and Caltech SURF-2017 fellowships. This work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift. - \n\nSoftware: xspec (v12.10.0c; Arnaud 1996), xillver (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), relxill (v1.2.0; Dauser et al. 2014; Garc\u00eda et al. 2014), nustradas (v1.6.0).\n\nPublished - Garc\u00eda_2019_ApJ_885_48.pdf
Submitted - 1908.00965.pdf
",
"abstract": "We report on the spectroscopic analysis of the black hole binary GX 339\u22124 during its recent 2017\u20132018 outburst, observed simultaneously by the Swift and NuSTAR observatories. Although during this particular outburst the source failed to make state transitions, and despite Sun constraints during the peak luminosity, we were able to trigger four different observations sampling the evolution of the source in the hard state. We show that even for the lowest-luminosity observations the NuSTAR spectra show clear signatures of X-ray reprocessing (reflection) in an accretion disk. Detailed analysis of the highest signal-to-noise spectra with our family of relativistic reflection models RELXILL indicates the presence of both broad and narrow reflection components. We find that a dual-lamppost model provides a superior fit when compared to the standard single lamppost plus distant neutral reflection. In the dual-lamppost model two sources at different heights are placed on the rotational axis of the black hole, suggesting that the narrow component of the Fe K emission is likely to originate in regions far away in the disk, but still significantly affected by its rotational motions. Regardless of the geometry assumed, we find that the inner edge of the accretion disk reaches a few gravitational radii in all our fits, consistent with previous determinations at similar luminosity levels. This confirms a very low degree of disk truncation for this source at luminosities above ~1% Eddington. Our estimates of R_(in) reinforce the suggested behavior for an inner disk that approaches the innermost regions as the luminosity increases in the hard state.",
"date": "2019-11-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "885",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 48",
"id_number": "CaltechAUTHORS:20190809-154849136",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190809-154849136",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX17AJ65G"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA",
"grant_number": "80NSSC177K0515"
},
{
"agency": "European Social Fund"
},
{
"agency": "Baden-W\u00fcrttemberg Ministry of Science, Research and the Arts"
},
{
"agency": "Caltech Summer Undergraduate Research Fellowship (SURF)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
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]
},
"doi": "10.3847/1538-4357/ab384f",
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"basename": "Garc\u00eda_2019_ApJ_885_48.pdf",
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}
],
"pub_year": "2019",
"author_list": "Garc\u00eda, Javier A.; Tomsick, John A.; et el."
},
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"family": "F\u00fcrst",
"given": "F."
},
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},
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"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
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"family": "Kara",
"given": "E."
},
"orcid": "0000-0003-0172-0854"
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"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
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"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
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"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
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"name": {
"family": "Shaw",
"given": "A. W."
}
},
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"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
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"orcid": "0000-0001-5819-3552"
}
]
},
"title": "MAXI J1820+070 with NuSTAR I. An increase in variability frequency but a stable reflection spectrum: coronal properties and implications for the inner disc in black hole binaries",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs - black hole physics - X-rays: binaries",
"note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 September 20. Received 2019 September 19; in original form 2019 May 31. Published: 27 September 2019. \n\nWe thank Fiona Harrison for approval of these DDT observations and Karl Forster for their prompt scheduling. DJKB acknowledges financial support from the Science and Technology Facilities Council (STFC). ACF acknowledges support from the ERC Advanced Grant FEEDBACK 340442. AWS is supported by an NSERC Discovery Grant and a Discovery Accelerator Supplement. This work has used data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has used the NuSTARDAS jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - stz2681.pdf
Submitted - 1909.04688.pdf
",
"abstract": "MAXI J1820+070 (optical counterpart ASASSN-18ey) is a black hole candidate discovered through its recent very bright outburst. The low extinction column and long duration at high flux allow detailed measurements of the accretion process to be made. In this work, we compare the evolution of X-ray spectral and timing properties through the initial hard state of the outburst. We show that the inner accretion disc, as measured by relativistic reflection, remains steady throughout this period of the outburst. Nevertheless, subtle spectral variability is observed, which is well explained by a change in coronal geometry. However, characteristic features of the temporal variability \u2013 low-frequency roll-over and quasi-periodic oscillation frequency \u2013 increase drastically in frequency, as the outburst proceeds. This suggests that the variability time-scales are governed by coronal conditions rather than solely by the inner disc radius. We also find a strong correlation between X-ray luminosity and coronal temperature. This can be explained by electron pair production with a changing effective radius and a non-thermal electron fraction of \u223c20 per\u2009cent.",
"date": "2019-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "490",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1350-1362",
"id_number": "CaltechAUTHORS:20190917-134739032",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190917-134739032",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1093/mnras/stz2681",
"primary_object": {
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"pub_year": "2019",
"author_list": "Buisson, D. J. K.; Fabian, A. C.; et el."
},
{
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"eprint_id": 98668,
"eprint_status": "archive",
"datestamp": "2023-08-19 18:28:22",
"lastmod": "2023-10-18 17:33:01",
"type": "article",
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"creators": {
"items": [
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Longinotti-A-L",
"name": {
"family": "Longinotti",
"given": "A. L."
}
},
{
"id": "Schartel-N",
"name": {
"family": "Schartel",
"given": "N."
}
},
{
"id": "Grupe-D",
"name": {
"family": "Grupe",
"given": "D."
},
"orcid": "0000-0002-9961-3661"
},
{
"id": "Komossa-S",
"name": {
"family": "Komossa",
"given": "S."
}
},
{
"id": "Kriss-G-A",
"name": {
"family": "Kriss",
"given": "G."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Gallo-L-C",
"name": {
"family": "Gallo",
"given": "L."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Jiang-J",
"name": {
"family": "Jiang",
"given": "J."
}
},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Krongold-Y",
"name": {
"family": "Krongold",
"given": "Y."
}
},
{
"id": "Matzeu-G-A",
"name": {
"family": "Matzeu",
"given": "G. A."
}
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Santos-Lle\u00f3-M",
"name": {
"family": "Santos-Lle\u00f3",
"given": "M."
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]
},
"title": "The nuclear environment of the NLS1 Mrk 335: obscuration of the X-ray line emission by a variable outflow",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013 galaxies: active \u2013 X-rays: individual:\nMrk 335",
"note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 September 10. Received 2019 September 6; in original form 2019 July 30. Published: 13 September 2019. \n\nMLP, GAM, and CP are supported by European Space Agency (ESA) Research Fellowships. ACF acknowledges support from ERC Advanced Grant 340442. ALL is supported by CONACyT grant CB-2016-01-286316. JJ acknowledges support from the Cambridge Trust and the Chinese Scholarship Council joint scholarship (201604100032). DG acknowledges support by HST grant HST-GO-15439.002-A. Based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). We thank the anonymous referee for their constructive feedback, which has significantly improved this work.\n\nPublished - stz2566.pdf
Submitted - 1909.04924.pdf
",
"abstract": "We present XMM\u2013Newton, NuSTAR, Swift, and Hubble Space Telescope observations of the Narrow-line Seyfert 1 galaxy Mrk 335 in a protracted low state in 2018 and 2019. The X-ray flux is at the lowest level so far observed, and the extremely low continuum flux reveals a host of soft X-ray emission lines from photoionized gas. The simultaneous UV flux drop suggests that the variability is intrinsic to the source, and we confirm this with broad-band X-ray spectroscopy. The dominance of the soft X-ray lines at low energies and distant reflection at high energies, is therefore due to the respective emission regions being located far enough from the X-ray source that they have not yet seen the flux drop. Between the two XMM\u2013Newton spectra, taken 6 months apart, the emission line ratio in the O\u2009VII triplet changes drastically. We attribute this change to a drop in the ionization of intervening warm absorption, which means that the absorber must cover a large fraction of the line emitting region, and extend much further from the black hole than previously assumed. The HST spectrum, taken in 2018, shows that new absorption features have appeared on the blue wings of C\u2009III*, Ly\u2009\u03b1, N\u2009V, Si\u2009IV, and C\u2009IV, likely due to absorbing gas cooling in response to the low flux state.",
"date": "2019-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "490",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "683-697",
"id_number": "CaltechAUTHORS:20190916-161112944",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190916-161112944",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "CB-2016-01-286316"
},
{
"agency": "Cambridge Trust"
},
{
"agency": "Chinese Scholarship Council",
"grant_number": "201604100032"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-GO-15439.002-A"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Space Astronomy Centre"
}
]
},
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},
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"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/stz2566",
"primary_object": {
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"author_list": "Parker, M. L.; Longinotti, A. L.; et el."
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"datestamp": "2023-08-22 02:44:22",
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},
{
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"family": "Negoro",
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},
{
"name": {
"family": "Wijers",
"given": "Ralph A. M. J."
}
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{
"name": {
"family": "Bozzo",
"given": "Enrico"
}
},
{
"name": {
"family": "Guiriec",
"given": "Sylvain"
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{
"name": {
"family": "Bult",
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{
"name": {
"family": "Huppenkothen",
"given": "Daniela"
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"name": {
"family": "G\u00f6\u011f\u00fcs",
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"name": {
"family": "Linford",
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"name": {
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"name": {
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"name": {
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"id": "Harrison-F-A",
"name": {
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{
"name": {
"family": "Hartmann",
"given": "Dieter H."
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{
"name": {
"family": "Iwakiri",
"given": "Wataru"
}
},
{
"name": {
"family": "Kaper",
"given": "Lex"
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},
{
"name": {
"family": "Kara",
"given": "Erin"
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{
"name": {
"family": "Mazzola",
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"family": "Murata",
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"name": {
"family": "Stern",
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{
"name": {
"family": "Tomsick",
"given": "John A."
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{
"name": {
"family": "van der Horst",
"given": "Alexander J."
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"orcid": "0000-0001-9149-6707"
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{
"name": {
"family": "Younes",
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},
"title": "Discovery and Identification of MAXI J1621-501 as a Type I X-ray Burster with a Super-Orbital Period",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Low-mass X-ray binary stars; X-ray transient sources; X-ray bursters",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 June 27; revised 2019 August 15; accepted 2019 August 21; published 2019 October 22. \n\nWe thank the anonymous referee, whose comments improved the quality of this work. N.G., C.K., and P.B. acknowledge support from Chandra award number GO8-19061X and Swift award number NNH16ZDA001N-SWIFT. The IRSF project is supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (No. 10147207 and No. 10147214). H.N. acknowledges support from a Grant-in-Aid for Scientific Research (No. 16K05301). The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. Special thanks go to Nobuyuki Kawai, Christina Gilligan, and Jill Neeley for their indispensable roles in data acquisition for this project. D.H. acknowledges support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We thank all operations, software and calibration teams contributing to the facilities used in this study for support with the execution and analysis of these observations. \n\nFacilities: Swift - Swift Gamma-Ray Burst Mission, Chandra - , NuSTAR - , NICER - , MAXI - , INTEGRAL - , ATCA - , IRSF - , Gemini - , ADS - , HEASARC. - \n\nSoftware: MIRIAD (Sault et al. 1995), Stingray (Huppenkothen et al. 2016, 2019), emcee (Foreman-Mackey et al. 2013), CIAO (v4.9.3; Fruscione et al. 2006), HEAsoft (v624; HEASARC 2014), XSPEC (v12.10.0; Arnaud 1996).\n\nPublished - Gorgone_2019_ApJ_884_168.pdf
Submitted - 1908.03590.pdf
",
"abstract": "MAXI J1621-501 is the first Swift/XRT Deep Galactic Plane Survey transient that was followed up with a multitude of space missions (NuSTAR, Swift, Chandra, NICER, INTEGRAL, and MAXI) and ground-based observatories (Gemini, IRSF, and ATCA). The source was discovered with MAXI on 2017 October 19 as a new, unidentified transient. Further observations with NuSTAR revealed 2 Type I X-ray bursts, identifying MAXI J1621-501 as a Low Mass X-ray Binary (LMXB) with a neutron star primary. Overall, 24 Type I bursts were detected from the source during a 15 month period. At energies below 10 keV, the source spectrum was best fit with three components: an absorbed blackbody with kT = 2.3 keV, a cutoff power law with index \u0393 = 0.7, and an emission line centered on 6.3 keV. Timing analysis of the X-ray persistent emission and burst data has not revealed coherent pulsations from the source or an orbital period. We identified, however, a super-orbital period \u223c78 days in the source X-ray light curve. This period agrees very well with the theoretically predicted radiative precession period of \u223c82 days. Thus, MAXI J1621-501 joins a small group of sources characterized with super-orbital periods.",
"date": "2019-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "884",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 168",
"id_number": "CaltechAUTHORS:20190917-100259555",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190917-100259555",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "GO8-19061X"
},
{
"agency": "NASA",
"grant_number": "NNH16ZDA001N-SWIFT"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)",
"grant_number": "10147207"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)",
"grant_number": "10147214"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)",
"grant_number": "16K05301"
},
{
"agency": "Australian Government"
},
{
"agency": "Charles and Lisa Simonyi Fund for Arts and Sciences"
},
{
"agency": "Washington Research Foundation"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.3847/1538-4357/ab3e43",
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}
],
"pub_year": "2019",
"author_list": "Gorgone, Nicholas M.; Kouveliotou, Chryssa; et el."
},
{
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"eprint_id": 98660,
"eprint_status": "archive",
"datestamp": "2023-08-19 17:49:58",
"lastmod": "2023-10-18 17:32:31",
"type": "article",
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"creators": {
"items": [
{
"id": "Connors-R-M-T",
"name": {
"family": "Connors",
"given": "Riley M. T."
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Grinberg-V",
"name": {
"family": "Grinberg",
"given": "Victoria"
},
"orcid": "0000-0003-2538-0188"
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "Thomas"
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Sridhar-N",
"name": {
"family": "Sridhar",
"given": "Navin"
},
"orcid": "0000-0002-5519-9550"
},
{
"id": "Gatuzz-E",
"name": {
"family": "Gatuzz",
"given": "Efrain"
},
"orcid": "0000-0002-3252-9633"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John"
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Markoff-S-B",
"name": {
"family": "Markoff",
"given": "Sera B."
},
"orcid": "0000-0001-9564-0876"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona"
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "Conflicting Disk Inclination Estimates for the Black Hole X-Ray Binary XTE J1500\u2212564",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 atomic processes \u2013 black hole physics",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 May 31; revised 2019 July 19; accepted 2019 July 23; published 2019 September 16. \n\nWe thank Kristin Madsen, Brian Grefenstette, Hiromasa Miyasaka, Yoshihiro Ueda, and Ken Ebisawa for very valuable discussions regarding the details of the X-ray data used in our analysis. \n\nJ.A.G. acknowledges support from NASA grant NNX15AV31G and the Alexander von Humboldt Foundation. R.M.T.C. has been supported by NASA grant 80NSSC177K0515. V.G. is supported through the Margarete von Wrangell fellowship by the ESF and the Ministry of Science, Research and the Arts Baden-W\u00fcrttemberg. \n\nThis research has made use of data, software, and/or web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC, and the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. \n\nThis work has also been conducted within the NuSTAR working group, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We are thankful for the support of its members in producing this research. \n\nFacility: RXTE - Rossi X-ray Timing Explorer (PCA, Jahoda et al. 1996; HEXTE, Rothschild et al. 1998), ASCA (GIS; Makishima et al. 1996), HEASARC. \n\nSoftware: XSPEC v.12.10.0c (Arnaud 1996), EMCEE (Foreman-Mackey et al. 2013b), XILLVER (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), RELXILL (v1.2.0; Dauser et al. 2014; Garc\u00eda et al. 2014).\n\nPublished - Connors_2019_ApJ_882_179.pdf
Submitted - 1907.12114.pdf
",
"abstract": "The dynamical characteristics of XTE J1550\u2212564, a black hole X-ray binary, are well established, and the broadband spectral evolution of the source has been well studied. Its orbital inclination is known to be high, at ~75\u00b0, with the jet estimated to align well with the orbital axis. We explore simultaneous observations made with the Advanced Satellite for Cosmology and Astrophysics and Rossi X-ray Timing Explorer covering the 1\u2013200 keV band during the early stages of the first outburst of XTE J1550\u2212564 in its hard-intermediate state on 1998 September 23/24. We show that the most up-to-date reflection models applied to these data yield an inclination estimate much lower than that found in previous studies at ~40\u00b0, grossly disagreeing with the dynamically estimated orbital inclination. We discuss the possible explanations for this disagreement and its implications for reflection models, including possible physical scenarios in which either the inner disk is misaligned with both the binary orbit and the outer jet or the inner accretion flow, corona, and/or jet have vertical structure that leads to lower inferred disk inclination through various physical means.",
"date": "2019-09-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "882",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 179",
"id_number": "CaltechAUTHORS:20190916-143938315",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190916-143938315",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AV31G"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA",
"grant_number": "80NSSC177K0515"
},
{
"agency": "European Social Fund"
},
{
"agency": "Ministry of Science, Research and the Arts (Baden-W\u00fcrttemberg)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/ab35df",
"primary_object": {
"basename": "1907.12114.pdf",
"url": "https://authors.library.caltech.edu/records/0be4w-vzp04/files/1907.12114.pdf"
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"basename": "Connors_2019_ApJ_882_179.pdf",
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}
],
"pub_year": "2019",
"author_list": "Connors, Riley M. T.; Garc\u00eda, Javier A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/2tj66-ddk32",
"eprint_id": 97797,
"eprint_status": "archive",
"datestamp": "2023-08-19 17:49:15",
"lastmod": "2023-10-18 16:45:06",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "R. C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Civano-Francesca",
"name": {
"family": "Civano",
"given": "F."
},
"orcid": "0000-0002-2115-1137"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Brusa-Marcella",
"name": {
"family": "Brusa",
"given": "M."
},
"orcid": "0000-0002-5059-6848"
},
{
"id": "Lanzuisi-G",
"name": {
"family": "Lanzuisi",
"given": "G."
},
"orcid": "0000-0001-9094-0984"
}
]
},
"title": "Measuring the Obscuring Column of a Disk Megamaser AGN in a Nearby Merger",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 methods: observational \u2013 techniques: spectroscopic \u2013 X-rays: general",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 May 1; revised 2019 July 8; accepted 2019 July 11; published 2019 September 4. \n\nWe thank the anonymous referee for useful suggestions that improved the clarity of the paper, and M. Balokovi\u0107 for useful help and suggestions on Borus02 modeling. \n\nThis work was supported under NASA Contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has also made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC). A.M. and R.C.H. acknowledge support by the NSF through grant No. 1554584, and by NASA through grant No. NNX15AP24G and Chandra GO award GO7-18130X. M.K. acknowledges support from NASA through ADAP award NNH16CT03C. A.C., M.B., and G.L. acknowledge support from the ASI/INAF grant I/037/12/0-011/13. \n\nFacilities: Chandra - , NuSTAR. - \n\nSoftware: CIAO (Fruscione et al. 2006), NuSTARDAS, XSPEC (Arnaud 1996).\n\nPublished - Masini_2019_ApJ_882_83.pdf
Submitted - 1907.05426.pdf
",
"abstract": "Active galactic nuclei (AGNs) hosting disk water megamasers are well known to be obscured by large amounts of gas, likely due to the presence along the line of sight of an almost edge-on disky structure orbiting the supermassive black hole. Correcting for the high obscuration is crucial to infer parameters intrinsic to the source, like its luminosity. We present a broadband X-ray spectral analysis of a water megamaser AGN in an early merger (NGC 5765B), combining Chandra and NuSTAR data. NGC 5765B is highly Compton-thick and reflection-dominated, following the general trend among disk megamasers. Combining the exquisite black hole mass from masers with our X-ray spectroscopy, the Eddington ratio of the megamaser is estimated to be in the 2%\u201314% range, and its robustness is confirmed through SED fitting.",
"date": "2019-09-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "882",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 83",
"id_number": "CaltechAUTHORS:20190812-145519174",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190812-145519174",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NSF",
"grant_number": "AST-1554584"
},
{
"agency": "NASA",
"grant_number": "NNX15AP24G"
},
{
"agency": "NASA",
"grant_number": "GO7-18130X"
},
{
"agency": "NASA",
"grant_number": "NNH16CT03C"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/ab3214",
"primary_object": {
"basename": "1907.05426.pdf",
"url": "https://authors.library.caltech.edu/records/2tj66-ddk32/files/1907.05426.pdf"
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"basename": "Masini_2019_ApJ_882_83.pdf",
"url": "https://authors.library.caltech.edu/records/2tj66-ddk32/files/Masini_2019_ApJ_882_83.pdf"
}
],
"pub_year": "2019",
"author_list": "Masini, A.; Comastri, A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/81gjb-q9404",
"eprint_id": 98418,
"eprint_status": "archive",
"datestamp": "2023-08-22 02:25:47",
"lastmod": "2023-10-18 17:20:51",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Vievering-Juliana-T",
"name": {
"family": "Vievering",
"given": "Juliana T."
},
"orcid": "0000-0002-7407-6740"
},
{
"id": "Glesener-Lindsay",
"name": {
"family": "Glesener",
"given": "Lindsay"
},
"orcid": "0000-0001-7092-2703"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Smith-David-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
}
]
},
"title": "New Star Observations with NuSTAR: Flares from Young Stellar Objects in the \u03c1 Ophiuchi Cloud Complex in Hard X-Rays",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Star forming regions; Stellar flares; Stellar x-ray flares; Pre-main sequence stars; Young stellar objects; Stellar activity",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 October 25; revised 2019 June 7; accepted 2019 June 26; published 2019 September 4. \n\nThis work was supported by NSF grants AGS-1429512 and AGS-1752268 and by NASA Headquarters under the NASA Earth and Space Science Fellowship Program Grant 80NSSC17K0430. The authors would like to acknowledge and thank Eric Feigelson for encouraging the NuSTAR team early on to make these observations and for contributing to discussions of this analysis. \n\nSoftware: NuSTARDAS (v1.6.0), nuskybgd (Wik et al. 2014), XSPEC (Arnaud 1996).\n\nPublished - Vievering_2019_ApJ_882_72.pdf
",
"abstract": "We study the structure and dynamics of extreme flaring events on young stellar objects (YSOs) observed in hard X-rays by the Nuclear Spectroscopic Telescope Array (NuSTAR). During 2015 and 2016, NuSTAR made three observations of the star-forming region \u03c1 Ophiuchi, each with an exposure ~50 ks. NuSTAR offers unprecedented sensitivity above ~7 keV, making this data set the first of its kind. Through improved coverage of hard X-rays, it is finally possible to directly measure the high-energy thermal continuum for hot plasmas and to sensitively search for evidence of nonthermal emission from YSO flares. During these observations, multiple flares were observed, and spectral and timing analyses were performed on three of the brightest flares. By fitting an optically thin thermal plasma model to each of these events, we found flare plasma heated to high temperatures (~40\u221280 MK) and determined that these events are ~1000 times brighter than the brightest flares observed on the Sun. Two of the studied flares showed excess emission at 6.4 keV, and this excess may be attributable to iron fluorescence in the circumstellar disk. No clear evidence for a nonthermal component was observed, but upper limits on nonthermal emission allow for enough nonthermal energy to account for the estimated thermal energy in the flare on protostar IRS 43, which is consistent with the standard model for solar and stellar flares.",
"date": "2019-09-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "882",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 72",
"id_number": "CaltechAUTHORS:20190904-152822673",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190904-152822673",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NSF",
"grant_number": "AGS-1429512"
},
{
"agency": "NSF",
"grant_number": "AGS-1752268"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "80NSSC17K0430"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/ab2e0d",
"pmcid": "PMC8780732",
"primary_object": {
"basename": "Vievering_2019_ApJ_882_72.pdf",
"url": "https://authors.library.caltech.edu/records/81gjb-q9404/files/Vievering_2019_ApJ_882_72.pdf"
},
"pub_year": "2019",
"author_list": "Vievering, Juliana T.; Glesener, Lindsay; et el."
},
{
"id": "https://authors.library.caltech.edu/records/v3ayc-8xq09",
"eprint_id": 97866,
"eprint_status": "archive",
"datestamp": "2023-08-19 17:23:55",
"lastmod": "2023-10-18 16:49:51",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Hannah-I-G",
"name": {
"family": "Hannah",
"given": "Iain G."
},
"orcid": "0000-0003-1193-8603"
},
{
"id": "Kleint-L",
"name": {
"family": "Kleint",
"given": "Lucia"
}
},
{
"id": "Krucker-S",
"name": {
"family": "Krucker",
"given": "S\u00e4m"
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Glesener-L",
"name": {
"family": "Glesener",
"given": "Lindsay"
},
"orcid": "0000-0001-7092-2703"
},
{
"id": "Hudson-H-S",
"name": {
"family": "Hudson",
"given": "Hugh S."
},
"orcid": "0000-0001-5685-1283"
},
{
"id": "White-S-M",
"name": {
"family": "White",
"given": "Stephen M."
},
"orcid": "0000-0002-8574-8629"
},
{
"id": "Smith-D-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
}
]
},
"title": "Joint X-ray, EUV and UV Observations of a Small Microflare",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: activity \u2013 Sun: corona \u2013 Sun: transition region \u2013 Sun: UV radiation \u2013 Sun: X-rays, gamma rays",
"note": "\u00a9 2019 The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2018 December 21; revised 2019 June 20; accepted 2019 June 28; published 2019 August 20. \n\nThis paper made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy), and the California Institute of Technology (USA). \n\nIRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. \n\nI.G.H. is supported by a Royal Society University Fellowship. The authors thank the International Space Science Institute (ISSI) for support for P. Testa's team \"New Diagnostics of Particle Acceleration in Solar Coronal Nanoflares from Chromospheric Observations and Modeling,\" where this work benefited from productive discussions. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, IRIS - , SDO/AIA - , GOES. -\n\nPublished - Hannah_2019_ApJ_881_109.pdf
Accepted Version - 1812.09214.pdf
",
"abstract": "We present the first joint observation of a small microflare in X-rays with the Nuclear Spectroscopic Telescope ARray (NuSTAR), in UV with the Interface Region Imaging Spectrograph (IRIS), and in EUV with the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA). These combined observations allow us to study the hot coronal and cooler chromospheric/transition region emission from the microflare. This small microflare peaks from 2016 July 26 23:35 to 23:36 UT, in both NuSTAR, SDO/AIA, and IRIS. Spatially, this corresponds to a small loop visible in the SDO/AIA Fe XVIII emission, which matches a similar structure lower in the solar atmosphere seen by IRIS in SJI1330 and 1400 \u00c5. The NuSTAR emission in both 2.5\u20134 and 4\u20136 keV is located in a source at this loop location. The IRIS slit was over the microflaring loop, and fits show little change in Mg II but do show intensity increases, slight width enhancements, and redshifts in Si IV and O IV, indicating that this microflare had most significance in and above the upper chromosphere. The NuSTAR microflare spectrum is well fitted by a thermal component of 5.1 MK and 6.2 \u00d7 10^(44) cm^(\u22123), which corresponds to a thermal energy of 1.5 \u00d7 10^(26) erg, making it considerably smaller than previously studied active region microflares. No non-thermal emission was detected but this could be due to the limited effective exposure time of the observation. This observation shows that even ordinary features seen in UV can remarkably have a higher-energy component that is clear in X-rays.",
"date": "2019-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "881",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 109",
"id_number": "CaltechAUTHORS:20190814-073445942",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190814-073445942",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Royal Society"
}
]
},
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"doi": "10.3847/1538-4357/ab2dfa",
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"pub_year": "2019",
"author_list": "Hannah, Iain G.; Kleint, Lucia; et el."
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"family": "Grefenstette",
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"given": "Didier"
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"orcid": "0000-0002-0393-9190"
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"id": "F\u00fcrst-Felix",
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"given": "Felix"
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Heida-Marianne",
"name": {
"family": "Heida",
"given": "Marianne"
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Pike-Sean-N",
"name": {
"family": "Pike",
"given": "Sean N."
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Stern-Daniel",
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"family": "Stern",
"given": "Daniel"
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"orcid": "0000-0003-2686-9241"
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{
"id": "Webb-Natalie-A",
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"family": "Webb",
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]
},
"title": "A broadband look at the old and new ULXs of NGC 6946",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: black holes \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: general",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 April 5; revised 2019 May 7; accepted 2019 May 8; published 2019 August 9. \n\nWe thank our anonymous referee for useful comments on this paper. This work was supported under NASA contract NNG08FD60C. D.J.W. acknowledges financial support from STFC in the form of an Ernest Rutherford fellowship. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This work has also made use of observations by XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Results reported in this article are based in part on public data obtained from the Chandra and Swift data archives, and on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM - , CXO - , Swift(XRT) - , HST. - \n\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018), CIAO (Fruscione et al. 2006), HENDRICS (Bachetti 2015), HEASoft (NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), 2014), NuSTARDAS, XMM-Newton SAS.\n\nPublished - Earnshaw_2019_ApJ_881_38.pdf
Submitted - 1905.03383.pdf
",
"abstract": "Two recent observations of the nearby galaxy NGC 6946 with NuSTAR, one simultaneous with an XMM-Newton observation, provide an opportunity to examine its population of bright accreting sources from a broadband perspective. We study the three known ultraluminous X-ray sources (ULXs) in the galaxy, and find that ULX-1 and ULX-2 have very steep power-law spectra with \u0393=3.6^(+0.4)_(\u22120.3) in both cases. Their properties are consistent with being super-Eddington accreting sources with the majority of their hard emission obscured and down-scattered. ULX-3 (NGC 6946 X-1) is significantly detected by both XMM-Newton and NuSTAR at L_X = (6.5 \u00b1 0.1) \u00d7 10^(39) erg s^(\u22121), and has a power-law spectrum with \u0393 = 2.51 \u00b1 0.05. We are unable to identify a high-energy break in its spectrum like that found in other ULXs, but the soft spectrum likely hinders our ability to detect one. We also characterize the new source, ULX-4, which is only detected in the joint XMM-Newton and NuSTAR observation, at L X = (2.27 \u00b1 0.07) \u00d7 10^(39) erg s^(\u22121), and is absent in a Chandra observation 10 days later. It has a very hard cutoff power-law spectrum with \u0393 = 0.7 \u00b1 0.1 and E_(cut)=11^(+9)_(\u22124) keV. We do not detect pulsations from ULX-4, but its transient nature can be explained either as a neutron star ULX briefly leaving the propeller regime or as a micro-tidal disruption event induced by a stellar-mass compact object.",
"date": "2019-08-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "881",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 38",
"id_number": "CaltechAUTHORS:20190618-153955252",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190618-153955252",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA",
"grant_number": "NAS 5-26555"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
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},
"doi": "10.3847/1538-4357/ab20cd",
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],
"pub_year": "2019",
"author_list": "Earnshaw, Hannah P.; Grefenstette, Brian W.; et el."
},
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"datestamp": "2023-08-19 17:06:11",
"lastmod": "2023-10-18 16:53:49",
"type": "article",
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"creators": {
"items": [
{
"id": "Bharali-P",
"name": {
"family": "Bharali",
"given": "Priya"
}
},
{
"id": "Chandra-S",
"name": {
"family": "Chandra",
"given": "Sunil"
},
"orcid": "0000-0002-8776-1835"
},
{
"id": "Chauhan-J",
"name": {
"family": "Chauhan",
"given": "Jaiverdhan"
},
"orcid": "0000-0003-0330-1901"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Roy-J",
"name": {
"family": "Roy",
"given": "Jayashree"
},
"orcid": "0000-0002-2329-5863"
},
{
"id": "Boettcher-M",
"name": {
"family": "Boettcher",
"given": "Markus"
}
},
{
"id": "Boruah-K",
"name": {
"family": "Boruah",
"given": "Kalyanee"
}
}
]
},
"title": "Re-awakening of GRS 1716\u2013249 after 23\u00a0yr, observed by Swift/XRT and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013X-rays: binaries \u2013 X-rays: individual: GRS 1716\u2013249",
"note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 May 28. Received 2019 May 28; in original form 2017 July 18. Published: 04 June 2019. \n\nThis research has made use of the software and/or data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) online service, provided by the NASA/Goddard Space Flight Center and the SWIFT data center. We thank NuSTAR team for making NuSTAR data public. MAXI data are obtained from MAXI team, RIKEN, JAXA. The authors gratefully acknowledge the anonymous referee for constructive comments that improved the paper. The authors are also thankful to PI's for proposing these observations. JC and SC are also grateful to Prof. H. M. Antia, Prof. A. R. Rao, and Prof. S. Bhattacharyya for constructive discussions about diagnostics and interpretations. The work by MB is supported by the Department of Science and Technology and National Research Foundation (NRF) of South Africa through the South African Research Chairs Initiative (SARChI), grant no. 64789. SC acknowledges the supports by CSR-NWU and NRF.\n\nPublished - stz1492.pdf
Accepted Version - 1905.12657.pdf
",
"abstract": "In this work, we present a spectral and temporal analysis of Swift/XRT and NuSTAR observations of GRS 1716\u2013249 during its recent 2016\u20132017 outburst. This low-mass X-ray binary underwent an extraordinary outburst after a long quiescence of 23 yr, since its last major outburst in 1993. The source was observed over two different epochs during 2017 April 7 and 10. The best-fitting joint spectral fitting in the energy range 0.5\u201379.0 keV indicates that the spectrum is best described by relatively cold, weak disc blackbody emission, dominant thermal Comptonization emission, and a relativistically broadened fluorescent iron K \u03b1 emission line. We observed a clear indication of a Compton hump around 30 keV. We also detected an excess feature of 1.3 keV. Assuming a lamp-post geometry of the corona, we constrained the inner disc radius for both observations to 11.92^(+8.62)_(\u221211.92) R_(ISCO) (i.e. an upper limit) and 10.39^(+9.51)_(\u22123.02) R_(ISCO)(where R_(ISCO) \u2261 radius of the innermost stable circular orbit) for the first epoch (E1) and second epoch (E2), respectively. A significant (5\u03c3) type C quasi-periodic oscillation (QPO) at 1.20 \u00b1 0.04 Hz is detected for the first time for GRS 1716\u2013249, which drifts to 1.55 \u00b1 0.04 Hz (6\u03c3) at the end of the second observation. The derived spectral and temporal properties show a positive correlation between the QPO frequency and the photon index.",
"date": "2019-08",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "487",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3150-3161",
"id_number": "CaltechAUTHORS:20190816-075233072",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190816-075233072",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Department of Science and Technology (South Africa)"
},
{
"agency": "National Research Foundation (South Africa)"
},
{
"agency": "South African Research Chairs Initiative (SARChI)",
"grant_number": "64789"
},
{
"agency": "North-West University Potchefstroom"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1093/mnras/stz1492",
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"pub_year": "2019",
"author_list": "Bharali, Priya; Chandra, Sunil; et el."
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"items": [
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Uttley-P",
"name": {
"family": "Uttley",
"given": "Phil"
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Broadband X-ray Spectral and Timing Analyses of the Black Hole Binary Candidate Swift J1658.2-4242: Rapid Flux Variation and the Turn-on of a Transient QPO",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 X-rays: binaries \u2013 X-rays: individual (Swift J1658.2-4242)",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 February 27; revised 2019 May 1; accepted 2019 May 23; published 2019 July 10. \n\nWe thank the anonymous referee for the helpful comments that improved the paper. We thank Tom Russell and James Miller-Jones for providing information about ATCA radio observations. D.J.W. acknowledges support from the STFC Ernest Rutherford Fellowship. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software, and calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, and Swift, a NASA mission with participation of the Italian Space Agency (ASI) and the Particle Physics and Astronomy Research Council in the United Kingdom.\n\nPublished - Xu_2019_ApJ_879_93.pdf
Submitted - 1905.10909.pdf
",
"abstract": "We report results from joint Nuclear Spectroscopic Telescope Array, Swift, and XMM-Newton observations of the newly discovered black hole X-ray binary candidate Swift J1658.2\u20134242 in the intermediate state. We observe a peculiar event in this source, with its X-ray flux rapidly decreasing by ~45% in ~40 s, accompanied by only subtle changes in the shape of the broadband X-ray spectrum. In addition, we find a sudden turn-on of a transient quasi-periodic oscillation (QPO) with a frequency of 6\u20137 Hz around the time of the flux change, and the total fractional rms amplitude of the power spectrum increases from ~2% to ~10%. The X-ray spectral and timing analyses indicate that the flux decrease is driven by intrinsic changes in the accretion flow around the black hole, rather than intervening material along the line of sight. In addition, we do not significantly detect any relativistic disk reflection component, indicating it is much weaker than previously observed while the source was in the bright hard state. We propose accretion disk instabilities triggered at a large disk radius as the origin of the fast transition in spectral and timing properties, and discuss possible causes of the unusual properties observed in Swift J1658.2\u20134242. The prompt flux variation detected along with the emergence of a QPO makes the event an interesting case for investigating QPO mechanisms in black hole X-ray binaries.",
"date": "2019-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "879",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 93",
"id_number": "CaltechAUTHORS:20190619-085644567",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-085644567",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"id": "NuSTAR"
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"id": "Space-Radiation-Laboratory"
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"doi": "10.3847/1538-4357/ab24bf",
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"pub_year": "2019",
"author_list": "Xu, Yanjun; Harrison, Fiona A.; et el."
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"items": [
{
"id": "Iwakiri-Wataru-B",
"name": {
"family": "Iwakiri",
"given": "Wataru B."
},
"orcid": "0000-0002-0207-9010"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Falkner-S",
"name": {
"family": "Falkner",
"given": "Sebastian"
},
"orcid": "0000-0001-5209-991X"
},
{
"id": "Hemphill-P-B",
"name": {
"family": "Hemphill",
"given": "Paul B."
},
"orcid": "0000-0002-1676-6954"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Nishimura-Osamu",
"name": {
"family": "Nishimura",
"given": "Osamu"
}
},
{
"id": "Schwarm-F-W",
"name": {
"family": "Schwarm",
"given": "Fritz-Walter"
}
},
{
"id": "Wolff-M-T",
"name": {
"family": "Wolff",
"given": "Michael T."
},
"orcid": "0000-0002-4013-5650"
},
{
"id": "Marcu-Cheatham-D-M",
"name": {
"family": "Marcu-Cheatham",
"given": "Diana M."
},
"orcid": "0000-0001-8061-611X"
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{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "Deepto"
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wilson-Hodge-C-A",
"name": {
"family": "Wilson-Hodge",
"given": "Colleen A."
},
"orcid": "0000-0002-8585-0084"
},
{
"id": "Bissinger-K\u00fchnel-M",
"name": {
"family": "Bissinger K\u00fchnel",
"given": "Matthias"
},
"orcid": "0000-0002-8709-8236"
},
{
"id": "Terada-Yukikatsu",
"name": {
"family": "Terada",
"given": "Yukikatsu"
},
"orcid": "0000-0002-2359-1857"
},
{
"id": "Enoto-Teruaki",
"name": {
"family": "Enoto",
"given": "Teruaki"
},
"orcid": "0000-0003-1244-3100"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Spectral and Timing Analysis of the Accretion-powered Pulsar 4U 1626\u201367 Observed with Suzaku and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "magnetic fields; pulsars: individual (4U 1626\u201367); X-rays: binaries",
"note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2017 November 1; revised 2019 April 29; accepted 2019 May 5; published 2019 June 20. \n\nThe authors appreciate very much the many constructive comments from the anonymous referee. This work is based on data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We also thank the Suzaku, Fermi/GBM and MAXI team members for their dedicated support in satellite operations and calibration. This work has been partially funded by the Deutsche Forschungsgemeinschaft under the DFG grant No. WI 1860/11-1. It uses ISIS functions (ISISscripts) provided by the ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). The figures in this work have been produced with the S-Lang module slxfig. K.P. acknowledges support by NASA's NuSTAR Cycle 1 Guest Observer grant No. NNX15AV17G. M.T.W. is supported by the Chief of Naval Research. W.I. is supported by the Special Postdoctoral Researchers Program in RIKEN and JSPS KAKENHI grant No. 16K17717.\n\nPublished - Iwakiri_2019_ApJ_878_121.pdf
Accepted Version - 1905.05356.pdf
",
"abstract": "We present an analysis of the spectral shape and pulse profile of the accretion-powered pulsar 4U 1626\u221267 observed with Suzaku and Nuclear Spectroscopic Telescope Array (NuSTAR) during a spin-up state. The pulsar, which experienced a torque reversal to spin-up in 2008, has a spin period of ~7.7 s. Comparing the phase-averaged spectra obtained with Suzaku in 2010 and with NuSTAR in 2015, we find that the spectral shape changed between the two observations: the 3\u201310 keV flux increased by ~5%, while the 30\u201360 keV flux decreased significantly by ~35%. Phase-averaged and phase-resolved spectral analysis shows that the continuum spectrum observed by NuSTAR is well described by an empirical negative and positive power law times exponential continuum with an added broad Gaussian emission component around the spectral peak at ~20 keV. Taken together with the observed \u1e56 value obtained from the Fermi/gamma-ray burst monitor data, we conclude that the spectral change between the Suzaku and NuSTAR observations was likely caused by an increase in the accretion rate. We also report the possible detection of asymmetry in the profile of the fundamental cyclotron line. Furthermore, we present a study of the energy-resolved pulse profiles using a new relativistic ray tracing code, where we perform a simultaneous fit to the pulse profiles assuming a two-column geometry with a mixed pencil- and fan-beam emission pattern. The resulting pulse profile decompositions enable us to obtain geometrical parameters of accretion columns (inclination, azimuthal and polar angles) and a fiducial set of beam patterns. This information is important to validate the theoretical predictions from radiation transfer in a strong magnetic field.",
"date": "2019-06-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "878",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 121",
"id_number": "CaltechAUTHORS:20190620-093003303",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190620-093003303",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "WI 1860/11-1"
},
{
"agency": "NASA",
"grant_number": "NNX15AV17G"
},
{
"agency": "Chief of Naval Research"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "16K17717"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/ab1f87",
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}
],
"pub_year": "2019",
"author_list": "Iwakiri, Wataru B.; Pottschmidt, Katja; et el."
},
{
"id": "https://authors.library.caltech.edu/records/z3kwe-azj32",
"eprint_id": 96270,
"eprint_status": "archive",
"datestamp": "2023-08-19 16:19:04",
"lastmod": "2023-10-20 21:02:14",
"type": "article",
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"creators": {
"items": [
{
"id": "Liu-Honghui",
"name": {
"family": "Liu",
"given": "Honghui"
}
},
{
"id": "Abdikamalov-A-B",
"name": {
"family": "Abdikamalov",
"given": "Askar B."
}
},
{
"id": "Ayzenberg-D",
"name": {
"family": "Ayzenberg",
"given": "Dimitry"
}
},
{
"id": "Bambi-C",
"name": {
"family": "Bambi",
"given": "Cosimo"
},
"orcid": "0000-0002-3180-9502"
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "Thomas"
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Nampalliwar-S",
"name": {
"family": "Nampalliwar",
"given": "Sourabh"
}
}
]
},
"title": "Testing the Kerr hypothesis using x-ray reflection spectroscopy with NuSTAR data of Cygnus X-1 in the soft state",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2019 American Physical Society. \n\nReceived 19 April 2019; published 11 June 2019. \n\nWe thank Dominic Walton for providing us his xstar table. This work was supported by the Innovation Program of the Shanghai Municipal Education Commission, Grant No. 2019-01-07-00-07-E00035, and Fudan University, Grant No. IDH1512060. A.\u2009B.\u2009A. also acknowledges the support from the Shanghai Government Scholarship (SGS). J.\u2009A.\u2009G. and S.\u2009N. acknowledge support from the Alexander von Humboldt Foundation. S.\u2009N. also acknowledges support from the Excellence Initiative at Eberhard-Karls Universit\u00e4t T\u00fcbingen.\n\nPublished - PhysRevD.99.123007.pdf
Submitted - 1904.08027.pdf
",
"abstract": "We continue exploring the constraining capabilities of x-ray reflection spectroscopy to test the Kerr-nature of astrophysical black holes, and we present the results of our analysis of two NuSTAR observations of Cygnus X-1 in the soft state. We find that the final measurement can strongly depend on the assumption of the intensity profile. We conclude that Cygnus X-1 is not suitable for tests of general relativity using x-ray reflection spectroscopy, and we discuss the desired properties of a source to be a good candidate for our studies.",
"date": "2019-06-15",
"date_type": "published",
"publication": "Physical Review D",
"volume": "99",
"number": "12",
"publisher": "American Physical Society",
"pagerange": "Art. No. 123007",
"id_number": "CaltechAUTHORS:20190611-092516240",
"issn": "2470-0010",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190611-092516240",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Shanghai Municipal Education Commission",
"grant_number": "2019-01-07-00-07-E00035"
},
{
"agency": "Fudan University",
"grant_number": "IDH1512060"
},
{
"agency": "Shanghai Government Scholarship"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "Eberhard-Karls Universit\u00e4t T\u00fcbingen"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1103/PhysRevD.99.123007",
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"basename": "PhysRevD.99.123007.pdf",
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}
],
"pub_year": "2019",
"author_list": "Liu, Honghui; Abdikamalov, Askar B.; et el."
},
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"eprint_id": 97411,
"eprint_status": "archive",
"datestamp": "2023-08-19 16:06:06",
"lastmod": "2023-10-20 22:19:27",
"type": "article",
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"items": [
{
"id": "Grupe-D",
"name": {
"family": "Grupe",
"given": "Dirk"
},
"orcid": "0000-0002-9961-3661"
},
{
"id": "Komossa-S",
"name": {
"family": "Komossa",
"given": "S."
}
},
{
"id": "Gallo-L-C",
"name": {
"family": "Gallo",
"given": "Luigi"
}
},
{
"id": "Schartel-N",
"name": {
"family": "Schartel",
"given": "Norbert"
}
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "Michael"
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Santos-Lleo-M",
"name": {
"family": "Santos-Lleo",
"given": "Maria"
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona"
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Miniutti-G",
"name": {
"family": "Miniutti",
"given": "Giovanni"
}
}
]
},
"title": "Swift, NuStar and XMM-Newton observations of the NLS1 galaxy RX\u00a0J2317.8-4422 in an extreme X-ray low flux state",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: nuclei, quasars: individual: RX J2317.8\u20134422, galaxies: Seyfert",
"note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) \n\nAccepted 2019 March 18. Received 2019 March 16; in original form 2019 January 17. \n\nWe thank our referee, Chris Done, for useful comments and suggestions that improved this paper. We would like to thank Neil Gehrels and Brad Cenko for approving our Target of Opportunity (ToO) requests and the Swift team for performing the ToO observations of RX J2317\u20134422. We also want to thank our Morehead State University students Mason Bush, Chelsea Pruett, Sonny Ernst, and Taylor Barber for looking through the Swift data to find AGNs in low X-ray flux states. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with the National Aeronautics and Space Administration. Based on observations obtained with XMM-Newton, an European Space Agency (ESA) science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. ACF acknowledges European Research Council Advanced Grant 340442.\n\nPublished - stz819.pdf
Accepted Version - 1903.07689.pdf
",
"abstract": "We report the discovery of RX J2317.8\u20134422 in an extremely low X-ray flux state by the Neil Gehrels Swift observatory in 2014 April/May. In total, the low-energy X-ray emission dropped by a factor of 100. We have carried out multiwavelength follow-up observations of this narrow-line Seyfert 1 galaxy. Here we present observations with Swift, XMM\u2013Newton, and NuSTAR in 2014 October and November and further monitoring observations by Swift from 2015 to 2018. Compared with the beginning of the Swift observations in 2005, in the November 2014 XMM\u2013Newton and NuSTAR observations RX J2317\u20134422.8 dropped by a factor of about 80 in the 0.3\u201310\u2009keV band. While the high-state Swift observations can be interpreted by a partial covering absorption model with a moderate absorption column density of N_H = 5.4 \u00d7 10^(22)\u2009cm^(\u22122) or blurred reflection, due to the dominating background at energies above 2\u2009keV the low-state XMM\u2013Newton data cannot distinguish between different multicomponent models and were adequately fitted with a single power-law model. We discuss various scenarios like a long-term change of the accretion rate or absorption as the cause for the strong variability seen in RX J2317.8\u20134422.",
"date": "2019-06",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "486",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "227-235",
"id_number": "CaltechAUTHORS:20190725-125943820",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190725-125943820",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/stz819",
"primary_object": {
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"author_list": "Grupe, Dirk; Komossa, S.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-19 15:28:15",
"lastmod": "2023-10-20 18:26:02",
"type": "article",
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"items": [
{
"id": "Pike-S-N",
"name": {
"family": "Pike",
"given": "Sean N."
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Brumback-M-C",
"name": {
"family": "Brumback",
"given": "McKinley C."
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix S."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Observing the Transient Pulsations of SMC X-1 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual (SMC X-1)",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 October 8; revised 2019 March 10; accepted 2019 March 11; published 2019 April 24. \n\nThis work was supported under NASA grant No. NNG08FD60C, and made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). We would also like to thank the anonymous referee for providing helpful comments that helped to improve the quality of this paper. \n\nSoftware: Stingray (Huppenkothen et al. 2016), HENDRICS (Bachetti 2015), NUSTARDAS, MaLTPyNT (Bachetti 2015), DS9 (Joye & Mandel 2003).\n\nPublished - Pike_2019_ApJ_875_144.pdf
Accepted Version - 1903.06306.pdf
",
"abstract": "We report on Nuclear Spectroscopic Telescope Array observations of transient pulsations in the neutron star X-ray binary SMC X-1. The transition from nonpulsing to pulsing states was not accompanied by a large change in flux. Instead, both pulsing and nonpulsing states were observed in a single observation during the low-flux super-orbital state. During the high state, we measure a pulse period of P = 0.70117(9) s at T_(ref) = 56145 MJD. Spectral analysis during nonpulsing and pulsing states reveals that the observations can be consistently modeled by an absorbed power law with a phenomenological cutoff resembling a Fermi\u2013Dirac distribution, or by a partially obscured cutoff power law. The shapes of the underlying continua show little variability between epochs, while the covering fraction and column density vary between super-orbital states. The strength of pulsations also varies, leading us to infer that the absence and reemergence of pulsations are related to changing obscuration, such as by a warped accretion disk. SMC X-1 is accreting near or above its Eddington limit, reaching an unabsorbed X-ray luminosity of L_X(2\u201310 keV) \u2248 5 \u00d7 10^(38) erg s^(\u22121). This suggests that SMC X-1 may be a useful local analog to ultraluminous X-ray pulsars (ULXPs), which likewise exhibit strong variability in their pulsed fractions, as well as flux variability on similar timescales. In particular, the gradual pulse turn-on, which has been observed in M82 X-2, is similar to the behavior we observe in SMC X-1. Thus we propose that pulse fraction variability of ULXPs may also be due to variable obscuration.",
"date": "2019-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "875",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 144",
"id_number": "CaltechAUTHORS:20190424-160205673",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190424-160205673",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"doi": "10.3847/1538-4357/ab0f2b",
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"pub_year": "2019",
"author_list": "Pike, Sean N.; Harrison, Fiona A.; et el."
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{
"id": "Walton-D-J",
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"family": "Walton",
"given": "D. J."
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},
{
"id": "Nardini-E",
"name": {
"family": "Nardini",
"given": "E."
},
"orcid": "0000-0001-9226-8992"
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{
"id": "Gallo-L-C",
"name": {
"family": "Gallo",
"given": "L. C."
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},
{
"id": "Reynolds-M-T",
"name": {
"family": "Reynolds",
"given": "M. T."
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"id": "Ricci-C",
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{
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"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
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},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Harrison-F-A",
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"family": "Harrison",
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{
"id": "Risaliti-G",
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{
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},
"title": "A low-flux state in IRAS\u200900521\u22127054 seen with NuSTAR and XMM\u2013Newton: relativistic reflection and an ultrafast outflow",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 X-rays: individual: (IRAS 00521\u22127054)",
"note": "\u00a9 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 January 1. Received 2018 December 19; in original form 2018 November 8. Published: 16 January 2019. \n\nThe authors would like to thank the reviewer for their feedback, which helped improve the clarity of the final version of the manuscript, and C. Done for useful discussion. DJW acknowledges support from an STFC Ernest Rutherford Fellowship; EN acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sk\u0142odowska-Curie grant agreement no. 664931; CR acknowledges the CONICYT + PAI Convocatoria Nacional subvencion a instalacion en la academia convocatoria a\u00f1o 2017 PAI77170080; ACF acknowledges support from ERC Advanced Grant 340442; JAG acknowledges support from NASA grant NNX17AJ65G and from the Alexander von Humboldt Foundation. \n\nThis research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States.\n\nPublished - stz115.pdf
Accepted Version - 1901.05016.pdf
",
"abstract": "We present results from a deep, coordinated XMM\u2013Newton + NuSTARobservation of the Seyfert 2 galaxy IRAS\u200900521\u22127054. The NuSTAR data provide the first detection of this source in high-energy X-rays (E > 10\u2009keV), and the broad-band data show this to be a highly complex source which exhibits relativistic reflection from the inner accretion disc, further reprocessing by more distant material, neutral absorption, and evidence for ionized absorption in an extreme, ultrafast outflow (\u2060v_(out) \u223c 0.4c). Based on lamppost disc reflection models, we find evidence that the central supermassive black hole is rapidly rotating (a > 0.77), consistent with previous estimates from the profile of the relativistic iron line, and that the accretion disc is viewed at a fairly high inclination (i \u223c 59\u00b0). Based on extensive simulations, we find the ultrafast outflow is detected at \u223c4\u03c3 significance (or greater). We also estimate that the extreme outflow should be sufficient to power galaxy-scale feedback, and may even dominate the energetics of the total output from the system.",
"date": "2019-04-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "484",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2544-2555",
"id_number": "CaltechAUTHORS:20190222-073613522",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190222-073613522",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "664931"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "PAI77170080"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "NASA",
"grant_number": "NNX17AJ65G"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.1093/mnras/stz115",
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"author_list": "Walton, D. J.; Nardini, E.; et el."
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{
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"family": "Halpern",
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"family": "Alford",
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"id": "Negoro-H",
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"id": "Kawai-Nobuyuki",
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"family": "Kawai",
"given": "N."
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{
"id": "Dai-Y-Sophia",
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"family": "Dai",
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"family": "Johnston",
"given": "S."
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"name": {
"family": "Bailes",
"given": "M."
},
"orcid": "0000-0003-3294-3081"
},
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"id": "Os\u0142owski-S",
"name": {
"family": "Os\u0142owski",
"given": "S."
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"id": "Camilo-F",
"name": {
"family": "Camilo",
"given": "F."
},
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},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "H."
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},
"title": "2018 X-Ray and Radio Outburst of Magnetar XTE J1810\u2013197",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: general \u2013 pulsars: individual (XTE J1810\u2013197) \u2013 stars: neutron \u2013 X-rays: stars",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 February 21; revised 2019 March 14; accepted 2019 March 15; published 2019 April 2. \n\nThe NuSTAR mission is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Director for timely approval of this observation of XTE J1810\u2212197, and the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of the observation. We thank the UTMOST team and the University of Sydney for maintaining the Molonglo Observatory. E.V.G. acknowledges NASA ADAP Grant NNX16AF30G. M.B. acknowledges ARC grant LF150100148. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research also made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. We also acknowledge use of the Astronomer's Telegram (ATel) and the NASA Astrophysics Data Service (ADS).\n\nPublished - Gotthelf_2019_ApJL_874_L25.pdf
Submitted - 1902.08358.pdf
",
"abstract": "We present the earliest X-ray observations of the 2018 outburst of XTE J1810\u2212197, the first outburst since its 2003 discovery as the prototypical transient and radio-emitting anomalous X-ray pulsar (AXP). The Monitor of All-sky X-ray Image (MAXI) detected XTE J1810\u2212197 immediately after a November 20\u201326 visibility gap, contemporaneous with its reactivation as a radio pulsar, first observed on December 8. On December 13 the Nuclear Spectroscopic Telescope Array (NuSTAR) detected X-ray emission up to at least 30 keV, with a spectrum well-characterized by a blackbody plus power-law model with temperature kT = 0.74 \u00b1 0.02 keV and photon index \u0393 = 4.4 \u00b1 0.2 or by a two-blackbody model with kT = 0.59 \u00b1 0.04 keV and kT = 1.0 \u00b1 0.1 keV, both including an additional power-law component to account for emission above 10 keV, with \u0393_h = \u22120.2 \u00b1 1.5 and \u0393_h = 1.5 \u00b1 0.5, respectively. The latter index is consistent with hard X-ray flux reported for the nontransient magnetars. In the 2\u201310 keV bandpass, the absorbed flux is 2 \u00d7 10^(\u221210) erg s^(\u22121) cm^(\u22122), a factor of 2 greater than the maximum flux extrapolated for the 2003 outburst. The peak of the sinusoidal X-ray pulse lags the radio pulse by \u22480.13 cycles, consistent with their phase relationship during the 2003 outburst. This suggests a stable geometry in which radio emission originates on magnetic field lines containing currents that heat a spot on the neutron star surface. However, a measured energy-dependent phase shift of the pulsed X-rays suggests that all X-ray emitting regions are not precisely coaligned.",
"date": "2019-04-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "874",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L25",
"id_number": "CaltechAUTHORS:20190402-112157216",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190402-112157216",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX16AF30G"
},
{
"agency": "Australian Research Council",
"grant_number": "LF150100148"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
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]
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"doi": "10.3847/2041-8213/ab101a",
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"pub_year": "2019",
"author_list": "Gotthelf, E. V.; Halpern, J. P.; et el."
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"items": [
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
},
"orcid": "0000-0002-9639-4352"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Wang-Jingyi",
"name": {
"family": "Wang",
"given": "Jingyi"
},
"orcid": "0000-0002-1742-2125"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "Michael L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
}
]
},
"title": "High-density reflection spectroscopy: I. A case study of GX\u00a0339-4",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013X-rays: binaries \u2013 X-rays: individual (GX 339-4)",
"note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2019 January 6. Received 2019 January 6; in original form 2018 November 26. Published: 10 January 2019. \n\nJJ acknowledges support by the Cambridge Trust and the Chinese Scholarship Council Joint Scholarship Programme (201604100032). DJW acknowledges support from an STFC Ernest Rutherford Fellowship. ACF acknowledges support by the ERC Advanced Grant 340442. MLP is supported by European Space Agency (ESA) Research Fellowships. JFS has been supported by NASA Einstein Fellowship grant No. PF5-160144. JAG acknowledges support from the Alexander von Humboldt Foundation. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We acknowledge support from European Space Astronomy Center (ESAC).\n\nPublished - stz095.pdf
Accepted Version - 1901.01739.pdf
",
"abstract": "We present a broad-band spectral analysis of the black hole binary GX 339-4 with NuSTAR and Swift using high-density reflection model. The observations were taken when the source was in low-flux (LF) hard states during the outbursts in 2013 and 2015, and in a very high-flux (HF) soft state in 2015. The high-density reflection model can explain its LF spectra with no requirement for an additional low temperature thermal component. This model enables us to constrain the density in the disc surface of GX 339-4 in different flux states. The disc density in the LF state is log\u2009(ne/\u2009cm^(\u22123)) \u2248 21, 100 times higher than the density in the HF state (log\u2009(n_e/\u2009cm^(\u22123)) = 18.93^(+0.12)_(\u22120.16). A close-to-solar iron abundance is obtained by modelling the LF and HF broad-band spectra with variable density reflection model (\u2060Z_(Fe) = 1.50^(+0.12)_(\u22120.04)Z\u2299 and Z_(Fe) = 1.05^(+0.17)_(\u22120.15)Z\u2299, respectively).",
"date": "2019-04",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "484",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1972-1982",
"id_number": "CaltechAUTHORS:20190416-083122873",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190416-083122873",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Cambridge Trust"
},
{
"agency": "Chinese Scholarship Council",
"grant_number": "201604100032"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF5-160144"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.1093/mnras/stz095",
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"pub_year": "2019",
"author_list": "Jiang, Jiachen; Fabian, Andrew C.; et el."
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"datestamp": "2023-08-19 14:41:53",
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"items": [
{
"id": "Ludlam-R-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Cackett-E-M",
"name": {
"family": "Cackett",
"given": "E. M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Coughenour-B-M",
"name": {
"family": "Coughenour",
"given": "B. M."
}
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Paerels-F",
"name": {
"family": "Paerels",
"given": "F."
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},
"title": "NuSTAR Observations of the Accreting Atolls GX 3+1, 4U 1702-429, 4U 0614+091, and 4U 1746-371",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: neutron \u2013 stars: individual (GX 3+1, 4U 1746-371, 4U 1702-429, 4U\n0614+091) \u2013 X-rays: binaries",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 July 12; revised 2019 January 30; accepted 2019 January 31; published 2019 March 7. \n\nWe thank the referee for their comments that have improved this work. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). R.M.L. is funded through a NASA Earth and Space Science Fellowship. E.M.C. gratefully acknowledges NSF CAREER award AST-1351222. We thank J. van den Eijnden for verifying the unabsorbed flux of IGR J17062\u22126143.\n\nPublished - Ludlam_2019_ApJ_873_99.pdf
Submitted - 1902.00520.pdf
",
"abstract": "Atoll sources are accreting neutron star (NS) low-mass X-ray binaries. We present a spectral analysis of four persistent atoll sources (GX 3+1, 4U 1702\u2212429, 4U 0614+091, and 4U 1746\u2212371) observed for ~20 ks each with NuSTAR to determine the extent of the inner accretion disk. These sources range from an apparent luminosity of 0.006\u20130.11 of the Eddington limit (assuming the empirical limit of 3.8 \u00d7 10^(38) erg s^(\u22121)). Broad Fe emission features shaped by Doppler and relativistic effects close to the NS were firmly detected in three of these sources. The position of the disk appears to be close to the innermost stable circular orbit (ISCO) in each case. For GX 3+1, we determine R_(in) = 1.8^(+0.2)_(\u22120.6) R_(ISCO) (90% confidence level) and an inclination of 27\u00b0\u201331\u00b0. For 4U 1702\u2212429, we find a R_(in) = 1.5^(+1.6)_(\u22120.4) R_(ISCO) and inclination of 53\u00b0\u201364\u00b0. For 4U 0614+091, the disk has a position of R_(in) = 1.3^(+5.4)_(\u22120.2) R_(ISCO) and inclination of 50\u00b0\u201362\u00b0. If the disk does not extend to the innermost stable circular orbit, we can place conservative limits on the magnetic field strength in these systems in the event that the disk is truncated at the Alfv\u00e9n radius. This provides the limit at the poles of B \u2264 6.7 \u00d7 10^8 G, 3.3 \u00d7 10^8 G, and 14.5 \u00d7 10^8 G for GX 3+1, 4U 1702\u2212429, and 4U 0614+091, respectively. For 4U 1746\u2212371, we argue that the most plausible explanation for the lack of reflection features is a combination of source geometry and strong Comptonization. We place these sources among the larger sample of NSs that have been observed with NuSTAR.",
"date": "2019-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "873",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 99",
"id_number": "CaltechAUTHORS:20190225-075539902",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190225-075539902",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Earth and Space Science Fellowship"
},
{
"agency": "NSF",
"grant_number": "AST-1351222"
}
]
},
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"items": [
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"id": "NuSTAR"
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"id": "Space-Radiation-Laboratory"
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"doi": "10.3847/1538-4357/ab0414",
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}
],
"pub_year": "2019",
"author_list": "Ludlam, R. M.; Miller, J. M.; et el."
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"items": [
{
"id": "Trakhtenbrot-B",
"name": {
"family": "Trakhtenbrot",
"given": "Benny"
},
"orcid": "0000-0002-3683-7297"
},
{
"id": "Arcavi-I",
"name": {
"family": "Arcavi",
"given": "Iair"
},
"orcid": "0000-0001-7090-4898"
},
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"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Tacchella-S",
"name": {
"family": "Tacchella",
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"title": "A new class of flares from accreting supermassive black holes",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 The Author(s), under exclusive licence to Springer Nature Limited 2019. \n\nReceived: 23 November 2017; Accepted: 21 November 2018; Published online: 14 January 2019. \n\nB.T. is a Zwicky Fellow. I.A. is an Einstein Fellow. E.K. is a Hubble Fellow. We thank N. Caplar, J. Guillochon, Z. Haiman, E. Lusso, and K. Schawinski for useful discussions. We thank C. Tadhunter for providing the spectrum of the F01004-2237 transient and his helpful comments. Part of this work was inspired by discussions within International Team #371, 'Using Tidal Disruption Events to Study Super-Massive Black Holes', hosted at the International Space Science Institute in Bern, Switzerland. We thank all the participants of the team meeting for their beneficial comments. Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. C.R. acknowledges support from the CONICYT\u2009+\u2009PAI Convocatoria Nacional subvencion a instalacion en la academia convocatoria a no 2017 PAI77170080. P.G.J. acknowledges support from European Research Council Consolidator Grant 647208. A. Horesh acknowledges support by the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation. G.H., D.A.H. and C.M. acknowledge support from NSF grant AST-1313484. M.B. acknowledges support from the Black Hole Initiative at Harvard University, which is funded by a grant from the John Templeton Foundation. G.L. acknowledges support from a Herchel Smith Research Fellowship of the University of Cambridge. \u0141.W., M.G. and A. Hamanowicz acknowledge Polish National Science Centre grant OPUS no 2015/17/B/ST9/03167 to \u0141.W. Research by D.J.S. is supported by NSF grants AST-1412504 and AST-1517649. E.Y.H. acknowledges the support provided by the National Science Foundation under Grant No. AST-1613472 and by the Florida Space Grant Consortium. This work makes use of observations from the Las Cumbres Observatory network. This publication also makes use of data products from the Wide-field Infrared Survey Explorer. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software and calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nWe thank the Swift, NuSTAR and NICER teams for scheduling and performing the target-of-opportunity observations presented here on short notice. The LRIS spectrum presented herein was obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nThese results made use of the Discovery Channel Telescope (DCT) at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale. \n\nThe FLAMINGOS-2 spectrum was obtained at the Gemini Observatory under program GS-2017A-Q-33 (PI: Sand), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (USA), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina) and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil). \n\nAuthor Contributions: B.T. and I.A. led the data collection, analysis and interpretation, as well as the manuscript preparation. C.R. performed the analysis and modelling of archival and new X-ray data. S.T. performed the morphological and SED modelling of the host galaxy. D.S., M.B., M.H., N.K. and G.B.L. took part in obtaining and calibrating the Palomar and Keck spectra. H.N. contributed to the identification and interpretation of the Bowen fluorescence spectral features. P.G.J. and A. Horesh contributed to the interpretation of multi-wavelength data and to pursuing follow-up observations. J.E.M.-R. contributed to the analysis of optical spectra. G.H., V.H. and C.M. contributed to collecting, calibrating and analysing the Las Cumbres Observatory and Swift/UVOT data. D.A.H. helped schedule and monitor the data from the Las Cumbres Observatory. \u0141.W., M.G. and A. Hamanowicz contributed to NIR line identification and provided the optical spectrum of OGLE17aaj. S.B.C. provided the the DCT spectrum. D.J.S. provided the the Gemini-South/FLAMINGOS-2 NIR spectrum. E.Y.H., M.M.P. and T.R.D. provided the Magellan/FIRE NIR spectrum. E.K. contributed to the X-ray data analysis and interpretation. K.C.G., Z.A. and R.R. contributed to the NICER data acquisition and calibration. \n\nData availability: The data that support the findings of this study are available from the corresponding author upon reasonable request. All of our spectra are publicly available on the Weizmann Interactive Supernova data REPository (WISeREP). The data used to prepare Supplementary Fig. 1 are available from the ASAS-SN Light Curve Server (https://asas-sn.osu.edu/). \n\nThe authors declare no competing interests.\n\nAccepted Version - 1901.03731.pdf
Supplemental Material - 41550_2018_661_MOESM1_ESM.pdf
",
"abstract": "Accreting supermassive black holes (SMBHs) can exhibit variable emission across the electromagnetic spectrum and over a broad range of timescales. The variability of active galactic nuclei (AGNs) in the ultraviolet and optical is usually at the few tens of per cent level over timescales of hours to weeks. Recently, rare, more dramatic changes to the emission from accreting SMBHs have been observed, including tidal disruption events, 'changing look' AGNs and other extreme variability objects. The physics behind the 're-ignition', enhancement and 'shut-down' of accretion onto SMBHs is not entirely understood. Here we present a rapid increase in ultraviolet\u2013optical emission in the centre of a nearby galaxy, marking the onset of sudden increased accretion onto a SMBH. The optical spectrum of this flare, dubbed AT 2017bgt, exhibits a mix of emission features. Some are typical of luminous, unobscured AGNs, but others are likely driven by Bowen fluorescence\u2014robustly linked here with high-velocity gas in the vicinity of the accreting SMBH. The spectral features and increased ultraviolet flux show little evolution over a period of at least 14 months. This disfavours the tidal disruption of a star as their origin, and instead suggests a longer-term event of intensified accretion. Together with two other recently reported events with similar properties, we define a new class of SMBH-related flares. This has important implications for the classification of different types of enhanced accretion onto SMBHs.",
"date": "2019-03",
"date_type": "published",
"publication": "Nature Astronomy",
"volume": "3",
"number": "3",
"publisher": "Nature Publishing Group",
"pagerange": "242-250",
"id_number": "CaltechAUTHORS:20190614-111557235",
"issn": "2397-3366",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190614-111557235",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "ETH Zurich"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF6-170148"
},
{
"agency": "NASA Hubble Fellowship"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "2017 PAI77170080"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "647208"
},
{
"agency": "I-CORE Program of the Planning and Budgeting Committee"
},
{
"agency": "Israel Science Foundation"
},
{
"agency": "NSF",
"grant_number": "AST-1313484"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "University of Cambridge"
},
{
"agency": "OPUS Program",
"grant_number": "2015/17/B/ST9/03167"
},
{
"agency": "NSF",
"grant_number": "AST-1412504"
},
{
"agency": "NSF",
"grant_number": "AST-1517649"
},
{
"agency": "NSF",
"grant_number": "AST-1613472"
},
{
"agency": "Florida Space Grant Consortium"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "W. M. Keck Foundation"
},
{
"agency": "John and Ginger Giovale"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1038/s41550-018-0661-3",
"primary_object": {
"basename": "1901.03731.pdf",
"url": "https://authors.library.caltech.edu/records/vwdy6-1ah10/files/1901.03731.pdf"
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}
],
"pub_year": "2019",
"author_list": "Trakhtenbrot, Benny; Arcavi, Iair; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ck00f-k8j82",
"eprint_id": 94728,
"eprint_status": "archive",
"datestamp": "2023-08-19 14:36:07",
"lastmod": "2023-10-20 18:12:42",
"type": "article",
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"creators": {
"items": [
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Buisson-D-J-K",
"name": {
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"given": "D. J. K."
}
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{
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"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
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"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
}
]
},
"title": "XRB continuum fitting with sensitive high-energy X-ray detectors",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013X-rays: binaries",
"note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 December 29. Received 2018 November 22; in original form 2018 April 18. Published: 07 January 2019. \n\nMLP and FF are supported by European Space Agency (ESA) Research Fellowships. ACF acknowledges support from ERC Advanced Grant Feedback 340442. DJW acknowledges support from an STFC Ernest Rutherford fellowship. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - stz045.pdf
Accepted Version - 1901.00683.pdf
",
"abstract": "The launch of the Nuclear Spectroscopic Telescope Array (NuSTAR) heralded a new era of sensitive high-energy X-ray spectroscopy for X-ray binaries (XRBs). In this paper we show how multiple physical parameters can be measured from the accretion disc spectrum when the high-energy side of the disc spectrum can be measured precisely using NuSTAR. This immediately makes two exciting developments possible. If the mass and distance of the source are known, the continuum fitting method can be used to calculate the spin and inner disc inclination independently of the iron line fitting method. If the mass and distance are unknown, the two methods can be combined to constrain these values to a narrow region of parameter space. In this paper we perform extensive simulations to establish the reliability of these techniques. We find that with high-quality spectra, spin and inclination can indeed be simultaneously measured using the disc spectrum. These measurements are much more precise at higher spin values, where the relativistic effects are stronger. The inclusion of a soft X-ray snapshot observation alongside the NuSTAR data significantly improves the reliability, particularly for lower temperature discs, as it gives a greatly improved measurement of the disc peak. High signal-to-noise data are not necessary for this, as measuring the peak temperature is relatively easy. We discuss the impact of systematic effects on this technique, and the implications of our results such as robust measurements of accretion disc warps and XRB mass surveys.",
"date": "2019-03",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "484",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1202-1212",
"id_number": "CaltechAUTHORS:20190416-082517519",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190416-082517519",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
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},
"doi": "10.1093/mnras/stz045",
"primary_object": {
"basename": "1901.00683.pdf",
"url": "https://authors.library.caltech.edu/records/ck00f-k8j82/files/1901.00683.pdf"
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"pub_year": "2019",
"author_list": "Parker, M. L.; Buisson, D. J. K.; et el."
},
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"datestamp": "2023-08-19 14:16:18",
"lastmod": "2023-10-19 14:37:55",
"type": "article",
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"creators": {
"items": [
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"id": "Margutti-R",
"name": {
"family": "Margutti",
"given": "R."
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"orcid": "0000-0003-4768-7586"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
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]
},
"title": "An Embedded X-Ray Source Shines through the Aspherical AT 2018cow: Revealing the Inner Workings of the Most Luminous Fast-evolving Optical Transients",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: black holes \u2013 supernovae: individual (AT 2018cow) \u2013 X-rays: general",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 October 25; revised 2018 December 19; accepted 2018 December 19; published 2019 February 6. \n\nWe are very grateful to the entire NuSTAR, INTEGRAL, Swift, XMM-Newton, VLA, and VLBA teams for making this observing campaign possible. We thank R. Lunnan, A. Suzuki for their feedback on the first version of the paper that appeared on the archive. \n\nSome of the observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution under programs (2018A-UAO-G15, 2018B-SAO-21, 2018B-UAO-G16; PIs Fong, Patnaude, Terreran). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration under program NW254 (PI Miller). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The Keck and MMT observations were supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). This paper includes data acquired with UKIRT under program (U/18A/UA01, PI Fong). UKIRT is owned by the University of Hawaii (UH) and operated by the UH Institute for Astronomy; operations are enabled through the cooperation of the East Asian Observatory. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO Prop. 2018A-0343, 2018B-0210; PI: G. Terreran), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist\u00e9rio da Ci\u00eancia, Tecnologia, Inova\u00e7\u00e3os e Comunica\u00e7\u00e3oes (MCTIC) do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. Support for this work was provided to MRD by NASA through Hubble Fellowship grant NSG-HF2-51373 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. \n\nPartly based on observations with INTEGRAL, an ESA project with instruments and science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain) and with the participation of Russia and the USA. Partly based on observations obtained with XMM-Newton (IDs: 0822580401, 0822580501, AO-17, program #82258; PI Margutti), an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. R.M. acknowledges partial support from NASA XMM-Newton Guest Investigator program grant 80NSSC19K0384. We acknowledge the use of public data from the Swift data archive. This work made use of data from the NuSTAR mission (IDs 90401327002, 90401327004, 90401327006, 90401327008), a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Observations taken with the VLA (program 18A-123; PI Coppejans) were used in this research. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nB.D.M. acknowledges support from NSF grant AST-1615084, NASA Fermi Guest Investigator Program grants NNX16AR73G and 80NSSC17K0501, and through the Hubble Space Telescope Guest Investigator Program grant HST-AR-15041.001-A. P.U. and S.M. acknowledge financial support from ASI under contracts ASI/INAF 2013-025-R0. D.G. acknowledges the financial support of the UnivEarthS Labex program at Sorbonne Paris Cit\u00e9 (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). K.D.A. acknowledges support provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51403.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. I.C. acknowledges support by the Telescope Data Center, Smithsonian Astrophysical Observatory and the Russian Science Foundation grant 17-72-20119. D.J.P. acknowledges support through NASA Contract NAS8-03060. L.D. acknowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie and the Deutsches Zentrum f\u00fcr Luft und Raumfahrt through the grant FKZ 50 OG 1602. N.R. acknowledges the support from the University of Maryland through the Joint Space Science Institute Prize Postdoctoral Fellowship as well support from the Center for Research and Exploration in Space Science and Technology II. M.R.D. acknowledges support from the Dunlap Institute at the University of Toronto. D.D.F. and A.V.K. gratefully acknowledge support from RFBR grant 18-02-00062. \n\nFacilities: Swift - Swift Gamma-Ray Burst Mission, XMM - , NuSTAR - , INTEGRAL - , Odyssey - , WIND (Konus) - , Fermi - Fermi Gamma-Ray Space Telescope (formerly GLAST), Magellan:Baade (LDSS2 imaging spectrograph, Boller & Chivens spectrograph), Magellan:Clay (LDSS2 imaging spectrograph) - , SOAR - , Keck:I - , Keck:II - , WIYN - , CTIO:0.9m - , UKIRT - , MMT - , VLA - , VLBA - . \n\nSoftware: BOXFIT (Version 2; van Eerten et al. 2010, 2012), CASA (McMullin et al. 2007), CIAO (Fruscione et al. 2006), HEAsoft (Version 6.24), HOTPANTS (Becker 2015), INTEGRAL Off-line Scientific Analysis (OSA), IRAF (Tody 1986, 1993), pwkit (Williams et al. 2017), SNOoPY (http://sngroup.oapd.inaf.it/snoopy.html), XMM-Newton SAS (Version 17.0), XSPEC (Arnaud 1996).\n\nPublished - Margutti_2019_ApJ_872_18.pdf
Submitted - 1810.10720.pdf
",
"abstract": "We present the first extensive radio to \u03b3-ray observations of a fast-rising blue optical transient, AT 2018cow, over its first ~100 days. AT 2018cow rose over a few days to a peak luminosity L_(pk) ~ 4 \u00d7 10^(44) erg s^(\u22121), exceeding that of superluminous supernovae (SNe), before declining as L \u221d t^(\u22122). Initial spectra at \u03b4t \u227e 15 days were mostly featureless and indicated large expansion velocities v ~ 0.1c and temperatures reaching T ~ 3 \u00d7 10^4 K. Later spectra revealed a persistent optically thick photosphere and the emergence of H and He emission features with v ~ 4000 km s^(\u22121) with no evidence for ejecta cooling. Our broadband monitoring revealed a hard X-ray spectral component at E \u2265 10 keV, in addition to luminous and highly variable soft X-rays, with properties unprecedented among astronomical transients. An abrupt change in the X-ray decay rate and variability appears to accompany the change in optical spectral properties. AT 2018cow showed bright radio emission consistent with the interaction of a blast wave with v_(sh) ~ 0.1c with a dense environment (M ~ 10^(-3) \u2013 10^(-4) M\u2299\n Yr^(-1) for v w = 1000 km s\u22121). While these properties exclude ^(56)Ni-powered transients, our multiwavelength analysis instead indicates that AT 2018cow harbored a \"central engine,\" either a compact object (magnetar or black hole) or an embedded internal shock produced by interaction with a compact, dense circumstellar medium. The engine released ~10^(50)\u201310^(51.5) erg over ~10^3\u201310^5 s and resides within low-mass fast-moving material with equatorial\u2013polar density asymmetry (M_(ej,fast) \u227e 0.3 M \u2609). Successful SNe from low-mass H-rich stars (like electron-capture SNe) or failed explosions from blue supergiants satisfy these constraints. Intermediate-mass black holes are disfavored by the large environmental density probed by the radio observations.",
"date": "2019-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "872",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 18",
"id_number": "CaltechAUTHORS:20181102-101636582",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181102-101636582",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "W. M. Keck Foundation"
},
{
"agency": "Northwestern University"
},
{
"agency": "Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)"
},
{
"agency": "Smithsonian Astrophysical Observatory"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "NSG-HF2-51373"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA",
"grant_number": "80NSSC19K0384"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NSF",
"grant_number": "AST-1615084"
},
{
"agency": "NASA",
"grant_number": "NNX16AR73G"
},
{
"agency": "NASA",
"grant_number": "80NSSC17K0501"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-AR-15041.001-A"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "INAF 2013-025-R0"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-10-LABX-0023"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-11-IDEX-0005-02"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51403.001"
},
{
"agency": "Telescope Data Center"
},
{
"agency": "Russian Science Foundation",
"grant_number": "17-72-20119"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft und Raumfahrt (DLR)",
"grant_number": "FKZ 50 OG 1602"
},
{
"agency": "University of Maryland"
},
{
"agency": "Dunlap Institute"
},
{
"agency": "Russian Foundation for Basic Research",
"grant_number": "18-02-00062"
}
]
},
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"id": "NuSTAR"
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"doi": "10.3847/1538-4357/aafa01",
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"pub_year": "2019",
"author_list": "Margutti, R. and Grefenstette, B. W."
},
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"lastmod": "2023-10-20 16:20:56",
"type": "article",
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"items": [
{
"id": "Marchesi-S",
"name": {
"family": "Marchesi",
"given": "S."
},
"orcid": "0000-0001-5544-0749"
},
{
"id": "Ajello-M",
"name": {
"family": "Ajello",
"given": "M."
},
"orcid": "0000-0002-6584-1703"
},
{
"id": "Zhao-X",
"name": {
"family": "Zhao",
"given": "X."
}
},
{
"id": "Marcotulli-L",
"name": {
"family": "Marcotulli",
"given": "L."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Cusumano-G",
"name": {
"family": "Cusumano",
"given": "G."
}
},
{
"id": "Lanzuisi-G",
"name": {
"family": "Lanzuisi",
"given": "G."
},
"orcid": "0000-0001-9094-0984"
},
{
"id": "La-Parola-V",
"name": {
"family": "La Parola",
"given": "V."
},
"orcid": "0000-0002-8087-6488"
},
{
"id": "Segreto-A",
"name": {
"family": "Segreto",
"given": "A."
}
},
{
"id": "Vignali-C",
"name": {
"family": "Vignali",
"given": "C."
},
"orcid": "0000-0002-8853-9611"
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]
},
"title": "Compton-thick AGNs in the NuSTAR Era. III. A Systematic Study of the Torus Covering Factor",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 X-rays: galaxies",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 July 15; revised 2018 November 23; accepted 2018 December 20; published 2019 February 6. \n\nWe thank an anonymous referee for the useful comments, which helped in improving the paper. \n\nS.M., M.A., and X.Z. acknowledge funding under NASA contract 80NSSC17K0635. Mi.Ba. acknowledges support from the Black Hole Initiative at Harvard University, which is funded by a grant from the John Templeton Foundation. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, as well as of the TOPCAT software (Taylor 2005) for the analysis of data tables.\n\nPublished - Marchesi_2019_ApJ_872_8.pdf
Accepted Version - 1812.09217.pdf
",
"abstract": "We present the analysis of a sample of 35 candidate Compton-thick active galactic nuclei (AGNs) selected in the nearby universe (average redshift \u3008z\u3009 ~ 0.03) with the Swift-BAT 100-month survey. All sources have available NuSTAR data, thus allowing us to constrain with unprecedented quality important spectral parameters such as the obscuring torus line-of-sight column density (N_(H,z)), the average torus column density (N H,tor), and the torus covering factor (f_c ). We compare the best-fit results obtained with the widely used MYTorus (Murphy & Yaqoob 2009) model with those of the recently published borus02 model (Balokovi\u0107 et al. 2018) used in the same geometrical configuration of MYTorus (i.e., with f_c = 0.5). We find a remarkable agreement between the two, although with increasing dispersion in N_(H,z) moving toward higher column densities. We then use borus02 to measure f_c . High-f c sources have, on average, smaller offset between N_(H,z) and N_(H,tor) than low-f_c ones. Therefore, low f c values can be linked to a \"patchy torus\" scenario, where the AGN is seen through an overdense region in the torus, while high-f c objects are more likely to be obscured by a more uniform gas distribution. Finally, we find potential evidence of an inverse trend between f c and the AGN 2\u201310 keV luminosity, i.e., sources with higher f c values have on average lower luminosities.",
"date": "2019-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "872",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 8",
"id_number": "CaltechAUTHORS:20190206-100219625",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190206-100219625",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "80NSSC17K0635"
},
{
"agency": "Harvard University"
},
{
"agency": "John Templeton Foundation"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/aafbeb",
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"basename": "1812.09217.pdf",
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"basename": "Marchesi_2019_ApJ_872_8.pdf",
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}
],
"pub_year": "2019",
"author_list": "Marchesi, S.; Ajello, M.; et el."
},
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"datestamp": "2023-08-19 14:10:23",
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"type": "article",
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"creators": {
"items": [
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Schartel-N",
"name": {
"family": "Schartel",
"given": "N."
}
},
{
"id": "Grupe-D",
"name": {
"family": "Grupe",
"given": "D."
},
"orcid": "0000-0002-9961-3661"
},
{
"id": "Komossa-S",
"name": {
"family": "Komossa",
"given": "S."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kollatschny-W",
"name": {
"family": "Kollatschny",
"given": "W."
}
},
{
"id": "Mikula-R",
"name": {
"family": "Mikula",
"given": "R."
}
},
{
"id": "Santos-Lle\u00f3-M",
"name": {
"family": "Santos-Lle\u00f3",
"given": "M."
}
},
{
"id": "Tom\u00e1s-L",
"name": {
"family": "Tom\u00e1s",
"given": "L."
}
}
]
},
"title": "X-ray spectra reveal the reawakening of the repeat changing-look AGN NGC 1566",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs, galaxies: active, galaxies: individual: NGC 1566, galaxies: Seyfert",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 November 23. Received 2018 November 13; in original form 2018 October 19. Published: 27 November 2018. \n\nMLP is supported by an ESA Research Fellowship. We thank the anonymous referee for detailed and constructive feedback. We thank J. Lewis for editing the manuscript. Based on observations obtained with XMM\u2013Newton, an ESA science mission funded by ESA Member States and NASA, and the NuSTAR mission, a project led by Caltech, managed by JPL, and funded by NASA. This work has been supported by the Deutsche Forschungsgemeinschaft (DFG) grant Ko 857/33-1. We thank the Swift team for carrying out our ToO requests.\n\nPublished - sly224.pdf
Accepted Version - 1811.10289.pdf
",
"abstract": "We present simultaneous XMM\u2013Newton and NuSTAR observations of the repeat changing-look AGN NGC 1566, which dramatically increased in brightness in the IR to X-ray bands in 2018. The broad-band X-ray spectrum was taken at the peak of the outburst and is typical of Seyfert 1 AGN. The spectrum shows a soft excess, Compton hump, warm absorption and reflection, ruling out tidal disruption as the cause of the outburst and demonstrating that a 'standard' accretion disk can develop very rapidly. The high-resolution grating spectrum reveals that the outburst has launched a \u223c500\u2009km s^(\u22121) outflow, and shows photoionized emission lines from rest-frame gas. We discuss possible mechanisms for the outburst, and conclude that it is most likely caused by a disk instability.",
"date": "2019-02",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "483",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L88-L92",
"id_number": "CaltechAUTHORS:20190905-110449716",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190905-110449716",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "857/33-1"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnrasl/sly224",
"primary_object": {
"basename": "1811.10289.pdf",
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"basename": "sly224.pdf",
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"pub_year": "2019",
"author_list": "Parker, M. L.; Schartel, N.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/hxn77-asd24",
"eprint_id": 90366,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:57:59",
"lastmod": "2023-10-18 23:24:01",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Bhargava-Y",
"name": {
"family": "Bhargava",
"given": "Yash"
},
"orcid": "0000-0002-5967-8399"
},
{
"id": "Bhalerao-V-B",
"name": {
"family": "Bhalerao",
"given": "Varun"
},
"orcid": "0000-0002-6112-7609"
},
{
"id": "Ballhausen-R",
"name": {
"family": "Ballhausen",
"given": "Ralf"
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "Joern"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Explaining the asymmetric line profile in Cepheus X-4 with spectral variation across pulse phase",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual (Cep X-4)",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 October 16. Received 2018 October 16; in original form 2018 April 5. Published: 22 October 2018. \n\nThis work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). RB acknowledges support by DLR grant 50 OR 1410.\n\nAccepted Version - 1810.07724.pdf
",
"abstract": "The high mass X-ray binary Cepheus X-4, during its 2014 outburst, showed evidence for an asymmetric cyclotron line in its hard X-ray spectrum. The 2014 spectrum provides one of the clearest cases of an asymmetric line profile among all studied sources with Cyclotron Resonance Scattering Features (CRSF). We present a phase-resolved analysis of NuSTAR and Suzaku data taken at the peak and during the decline phases of this outburst. We find that the pulse-phased resolved spectra are well-fit by a single, symmetric cyclotron feature. The fit parameters vary strongly with pulse phase: most notably the central energy and depth of the cyclotron feature, the slope of the power-law component, and the absorbing column density. We synthesise a 'phase averaged' spectrum using the best-fitting parameters for these individual pulse phases, and find that this combined model spectrum has a similar asymmetry in the cyclotron features as discovered in phase-averaged data. We conclude that the pulse phase resolved analysis with simple symmetric line profiles when combined can explain the asymmetry detected in the phase-averaged data.",
"date": "2019-01-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "482",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2902-2912",
"id_number": "CaltechAUTHORS:20181023-115819195",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181023-115819195",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty2823",
"primary_object": {
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"pub_year": "2019",
"author_list": "Bhargava, Yash; Bhalerao, Varun; et el."
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{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
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},
"orcid": "0000-0003-3828-2448"
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{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "Erin"
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"orcid": "0000-0003-0172-0854"
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{
"id": "Walton-D-J",
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"family": "Walton",
"given": "Dominic"
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"orcid": "0000-0001-5819-3552"
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{
"id": "Beuchert-T",
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"family": "Beuchert",
"given": "Tobias"
}
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{
"id": "Dauser-T",
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"orcid": "0000-0003-4583-9048"
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{
"id": "Gatuzz-E",
"name": {
"family": "Gatuzz",
"given": "Efrain"
},
"orcid": "0000-0002-3252-9633"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Tombesi-F",
"name": {
"family": "Tombesi",
"given": "Francesco"
},
"orcid": "0000-0002-6562-8654"
},
{
"id": "Connors-R-M-T",
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"family": "Connors",
"given": "Riley M. T."
},
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},
{
"id": "Kallman-Timothy-R",
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{
"id": "Harrison-F-A",
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"family": "Harrison",
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},
{
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"family": "Fabian",
"given": "Andrew"
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
},
{
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"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "Lauranne"
},
"orcid": "0000-0002-3249-8224"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "David R."
},
"orcid": "0000-0001-8128-6976"
}
]
},
"title": "Implications of the Warm Corona and Relativistic Reflection Models for the Soft Excess in Mrk 509",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: active \u2013 galaxies: individual (Mrk 509) \u2013 galaxies: nuclei",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 September 24; revised 2018 November 26; accepted 2018 December 7; published 2019 January 24. \n\nWe thank P.O. Petrucci, J. Malzac, B. Czerny, A. R\u00f3\u017ca\u0144ska, C. Done, and the members of the FERO collaboration for insightful discussions that promoted many aspects of this paper. We also thank F. Ursini for comments that improved the manuscript. \n\nJ.A.G. acknowledges support from NASA grant NNX15AV31G and the Alexander von Humboldt Foundation. R.M.T.C. has been supported by NASA grant 80NSSC177K0515. M.B. acknowledges support from the black hole initiative at Harvard University, which is funded by a grant from the John Templeton Foundation. J.F.S. has been supported by NASA Einstein Fellowship grant PF5-160144. F.T. acknowledges support by the Programma per Giovani Ricercatori\u2014anno 2014 \"Rita Levi Montalcini.\" L.L. acknowledges support from NASA through grant No. NNX15AP24G C.R. acknowledges support from the CONICYT+PAI Convocatoria Nacional subvenci\u00f3n a instalaci\u00f3n en la academia convocatoria a\u00f1o 2017 PAI77170080. \n\nThis work was partially supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Suzaku (XIS) - . \n\nSoftware: xspec (v12.9.0d; Arnaud 1996), MYtorus (Murphy & Yaqoob 2009), borus02 (Balokovi\u0107 et al. 2018), xillver (Garc\u00eda & Kallman 2010; Garc\u00eda et al. 2013), relxill (v1.2.0; Garc\u00eda et al. 2014; Dauser et al. 2014), xstar (v2.41; Kallman & Bautista 2001), nustardas (v1.6.0).\n\nPublished - Garc\u00eda_2019_ApJ_871_88.pdf
Accepted Version - 1812.03194.pdf
",
"abstract": "We present the analysis of the first Nuclear Spectroscopic Telescope Array observations (~220 ks), simultaneous with the last Suzaku observations (~50 ks), of the active galactic nucleus of the bright Seyfert 1 galaxy Mrk 509. The time-averaged spectrum in the 1\u201379 keV X-ray band is dominated by a power-law continuum (\u0393 ~ 1.8\u20131.9), a strong soft excess around 1 keV, and signatures of X-ray reflection in the form of Fe K emission (~6.4 keV), an Fe K absorption edge (~7.1 keV), and a Compton hump due to electron scattering (~20\u201330 keV). We show that these data can be described by two very different prescriptions for the soft excess: a warm (kT ~ 0.5\u20131 keV) and optically thick (\u03c4 ~ 10\u201320) Comptonizing corona or a relativistically blurred ionized reflection spectrum from the inner regions of the accretion disk. While these two scenarios cannot be distinguished based on their fit statistics, we argue that the parameters required by the warm corona model are physically incompatible with the conditions of standard coronae. Detailed photoionization calculations show that even in the most favorable conditions, the warm corona should produce strong absorption in the observed spectrum. On the other hand, while the relativistic reflection model provides a satisfactory description of the data, it also requires extreme parameters, such as maximum black hole spin, a very low and compact hot corona, and a very high density for the inner accretion disk. Deeper observations of this source are thus necessary to confirm the presence of relativistic reflection and further understand the nature of its soft excess.",
"date": "2019-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "871",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 88",
"id_number": "CaltechAUTHORS:20190124-112047031",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190124-112047031",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AV31G"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA",
"grant_number": "80NSSC177K0515"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF5-160144"
},
{
"agency": "Programma per Giovani Ricercatori",
"grant_number": "anno 2014"
},
{
"agency": "NASA",
"grant_number": "NNX15AP24G"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "PAI77170080"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aaf739",
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"basename": "1812.03194.pdf",
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"pub_year": "2019",
"author_list": "Garc\u00eda, Javier A.; Kara, Erin; et el."
},
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"id": "Yan-Wei",
"name": {
"family": "Yan",
"given": "Wei"
},
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},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "Ryan C."
},
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},
{
"id": "Hainline-K-N",
"name": {
"family": "Hainline",
"given": "Kevin N."
},
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},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "George"
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "David M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Hviding-R-E",
"name": {
"family": "Hviding",
"given": "Raphael E."
},
"orcid": "0000-0002-4684-9005"
},
{
"id": "Assef-R-J",
"name": {
"family": "Assef",
"given": "Roberto J."
},
"orcid": "0000-0002-9508-3667"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "David R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "DiPompeo-M-A",
"name": {
"family": "DiPompeo",
"given": "Michael A."
},
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},
{
"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "Lauranne"
},
"orcid": "0000-0002-3249-8224"
},
{
"id": "Carroll-C-M",
"name": {
"family": "Carroll",
"given": "Christopher M."
},
"orcid": "0000-0003-3574-2963"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "Michael"
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Lamperti-I",
"name": {
"family": "Lamperti",
"given": "Isabella"
},
"orcid": "0000-0003-3336-5498"
},
{
"id": "Civano-Francesca",
"name": {
"family": "Civano",
"given": "Francesca"
},
"orcid": "0000-0002-2115-1137"
},
{
"id": "Del-Moro-A",
"name": {
"family": "Del Moro",
"given": "Agnese"
}
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Myers-A-D",
"name": {
"family": "Myers",
"given": "Adam D."
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}
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},
"title": "NuSTAR and Keck Observations of Heavily Obscured Quasars Selected by WISE",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 X-rays: galaxies",
"note": "\u00a9 2019 The American Astronomical Society.\n\nReceived 2018 March 7; revised 2018 October 30; accepted 2018 November 2; published 2019 January 2.\n\nThis research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT). R.C.H. acknowledges support from NASA grant NNX15AP24G and National Science Foundation CAREER Award number 1554584. R.J.A. was supported by FONDECYT grant number 1151408.\n\nAccepted Version - 1811.02585.pdf
",
"abstract": "A primary aim of the Nuclear Spectroscopic Telescope Array (NuSTAR) mission is to find and characterize heavily obscured Active Galactic Nuclei (AGNs). Based on mid-infrared photometry from the Wide-Field Infrared Survey Explorer (WISE) and optical photometry from the Sloan Digital Sky Surveys, we have selected a large population of luminous obscured AGNs (i.e., \"obscured quasars\"). Here we report NuSTAR observations of four WISE-selected heavily obscured quasars for which we have optical spectroscopy from the Southern African Large Telescope and W. M. Keck Observatory. Optical diagnostics confirm that all four targets are AGNs. With NuSTAR hard X-ray observations, three of the four objects are undetected, while the fourth has a marginal detection. We confirm that these objects have observed hard X-ray (10\u201340 keV) luminosities at or below ~10^(43) erg s^(\u22121). We compare X-ray and IR luminosities to obtain estimates of the hydrogen column densities (N_H) based on the suppression of the hard X-ray emission. We estimate N_H of these quasars to be at or larger than 10^(25) cm^(\u22122), confirming that WISE and optical selection can identify very heavily obscured quasars that may be missed in X-ray surveys, and they do not contribute significantly to the cosmic X-ray background. From the optical Balmer decrements, we found that our three extreme obscured targets lie in highly reddened host environments. This galactic extinction cannot adequately explain the more obscured AGNs, but it may imply a different scale of obscuration in the galaxy.",
"date": "2019-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "870",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 33",
"id_number": "CaltechAUTHORS:20181108-091200724",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181108-091200724",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aaeed4",
"primary_object": {
"basename": "1811.02585.pdf",
"url": "https://authors.library.caltech.edu/records/f3r74-7jr21/files/1811.02585.pdf"
},
"pub_year": "2019",
"author_list": "Yan, Wei; Hickox, Ryan C.; et el."
},
{
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"items": [
{
"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "Lauranne"
},
"orcid": "0000-0002-3249-8224"
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "Ryan C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Shimizu-Taro",
"name": {
"family": "Shimizu",
"given": "Taro"
},
"orcid": "0000-0002-2125-4670"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Goulding-A-D",
"name": {
"family": "Goulding",
"given": "Andy D."
}
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "David R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "Franz E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Chen-Chien-Ting-J",
"name": {
"family": "Chen",
"given": "Chien-Ting J."
},
"orcid": "0000-0002-4945-5079"
},
{
"id": "Del-Moro-A",
"name": {
"family": "Del Moro",
"given": "Agnese"
}
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "Duncan"
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "Michael J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "LaMassa-S",
"name": {
"family": "LaMassa",
"given": "Stephanie"
},
"orcid": "0000-0002-5907-3330"
},
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "Alberto"
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Zappacosta-L",
"name": {
"family": "Zappacosta",
"given": "Luca"
},
"orcid": "0000-0002-4205-6884"
}
]
},
"title": "Investigating the Covering Fraction Distribution of Swift/BAT AGNs with X-Ray and Infrared Observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 galaxies: Seyfert \u2013 X-rays: galaxies \u2013 infrared: galaxies",
"note": "\u00a9 2018 The American Astronomical Society.\n\nReceived 2017 December 22; revised 2018 October 25; accepted 2018 November 2; published 2018 December 31.\n\nWe thank the referee for useful comments, which particularly strengthened the statistical analysis. L.L. and R.C.H. acknowledge support from NASA through grant No. NNX15AP24G. L.L. acknowledges support from NASA through grant No. NNX17AB58G. R.C.H acknowledges support from the National Science Foundation through CAREER grant No. 1554584. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant No. NNX14AQ07H, and support from the black hole Initiative, which is funded by a grant from the John Templeton Foundation. C.R. acknowledges the CONICYT+PAI (Convocatoria Nacional subvencion a instalacion en la academia convocatoria a\u00f1o 2017 PAI77170080) and financial support from FONDECYT 1141218, Basal-CATA PFB-06/2007, and the China-CONICYT fund. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT Regular 1141218), the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant No. IC120009, awarded to The Millennium Institute of Astrophysics, MAS. M.K. acknowledges support from NASA through ADAP award No. NNH16CT03C. A.M. acknowledges support from the ASI/INAF through grant No. I/037/12/0-011/13. L.Z. acknowledges financial support under ASI/INAF contract No. I/037/12/0. This work made use of ASURV Rev. 1.2 (Lavalley et al. 1992), which implements the methods presented in Isobe et al. (1986).\n\nFacilities: Herschel - European Space Agency's Herschel space observatory, NuSTAR - , Swift - , WISE - .\n\nPublished - Lanz_2019_ApJ_870_26.pdf
Accepted Version - 1811.02570.pdf
",
"abstract": "We present an analysis of a sample of 69 local obscured Swift/Burst Alert Telescope active galactic nuclei (AGNs) with X-ray spectra from NuSTAR and infrared (IR) spectral energy distributions from Herschel and WISE. We combine this X-ray and IR phenomenological modeling and find a significant correlation between reflected hard X-ray emission and IR AGN emission, with suggestive indications that this correlation may be stronger than the one between intrinsic hard X-ray and IR emissions. This relation between the IR and reflected X-ray emission suggests that both are the result of the processing of intrinsic emission from the corona and accretion disk by the same structure. We explore the resulting implications on the underlying distribution of covering fraction for all AGNs, by generating mock observables for the reflection parameter and IR luminosity ratio using empirical relations found for the covering fraction with each quantity. We find that the observed distributions of the reflection parameter and IR-to-X-ray ratio are reproduced with broad distributions centered around covering fractions of at least ~40%\u201350%, whereas narrower distributions match our observations only when centered around covering fractions of ~70%\u201380%. Our results are consistent with both independent estimates of the covering fractions of individual objects and the typical covering fraction obtained on the basis of obscured fractions for samples of AGNs. These results suggest that the level of reprocessing in AGNs, including X-ray reflection, is related in a relatively straightforward way to the geometry of the obscuring material.",
"date": "2019-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "870",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 26",
"id_number": "CaltechAUTHORS:20181108-091558649",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181108-091558649",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aaee6c",
"primary_object": {
"basename": "1811.02570.pdf",
"url": "https://authors.library.caltech.edu/records/s5vf0-qbv16/files/1811.02570.pdf"
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"basename": "Lanz_2019_ApJ_870_26.pdf",
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}
],
"pub_year": "2019",
"author_list": "Lanz, Lauranne; Hickox, Ryan C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ctjzy-ykc33",
"eprint_id": 90242,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:43:50",
"lastmod": "2023-10-18 23:18:31",
"type": "article",
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"creators": {
"items": [
{
"id": "Mereminskiy-I-A",
"name": {
"family": "Mereminskiy",
"given": "Ilya A."
},
"orcid": "0000-0001-8931-1320"
},
{
"id": "Semena-A-N",
"name": {
"family": "Semena",
"given": "Andrey N."
}
},
{
"id": "Bykov-S-D",
"name": {
"family": "Bykov",
"given": "Sergey D."
}
},
{
"id": "Filippova-E-V",
"name": {
"family": "Filippova",
"given": "Ekaterina V."
}
},
{
"id": "Lutovinov-A-A",
"name": {
"family": "Lutovinov",
"given": "Alexander A."
}
},
{
"id": "Poutanen-J",
"name": {
"family": "Poutanen",
"given": "Juri"
},
"orcid": "0000-0002-0983-0049"
}
]
},
"title": "Studying temporal variability of GRS1739-278 during the 2014 outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs, X-rays: binaries, X-rays: individual: GRS\u20091739-278",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 October 9. Received 2018 September 4; in original form 2018 June 27. Published: 12 October 2018. \n\nThis work was supported by the Russian Science Foundation grant no. 14-12-01287. We thank E. M. Churazov for fruitful discussions and useful suggestions. We are grateful for T. Dauser and J. Gracia for their help with RELXILL model. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center, as well as of data supplied by the UK Swift Science Data Centre at the University of Leicester.\n\nAccepted Version - 1810.04451.pdf
",
"abstract": "We report a discovery of low-frequency quasi-periodic oscillation at 0.3\u20130.7 Hz in the power spectra of the accreting black hole GRS\u20091739\u2013278 in the hard-intermediate state during its 2014 outburst based on the NuSTAR and Swift/XRT data. The QPO frequency strongly evolved with the source flux during the NuSTAR observation. The source spectrum became softer with rising QPO frequency and simultaneous increasing of the power-law index and decreasing of the cut-off energy. In the power spectrum, a prominent harmonic is clearly seen together with the main QPO peak. The fluxes in the soft and the hard X-ray bands are coherent, however, the coherence drops for the energy bands separated by larger gaps. The phase lags are generally positive (hard) in the 0.1\u20133 Hz frequency range, and negative below 0.1 Hz. The accretion disc inner radius estimated with the relativistic reflection spectral model appears to be R_(in) < 7.3R_g. In the framework of the relativistic precession model, in order to satisfy the constraints from the observed QPO frequency and the accretion disc truncation radius, a massive black hole with M_(BH) \u2248 100\u2009M\u2299 is required.",
"date": "2019-01-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "482",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1392-1405",
"id_number": "CaltechAUTHORS:20181011-090326652",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181011-090326652",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01287"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty2752",
"primary_object": {
"basename": "1810.04451.pdf",
"url": "https://authors.library.caltech.edu/records/ctjzy-ykc33/files/1810.04451.pdf"
},
"pub_year": "2019",
"author_list": "Mereminskiy, Ilya A.; Semena, Andrey N.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/m3tx7-0q593",
"eprint_id": 90462,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:44:02",
"lastmod": "2023-10-18 23:28:13",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Makishima-Kazuo",
"name": {
"family": "Makishima",
"given": "Kazuo"
}
},
{
"id": "Murakami-Hiroaki",
"name": {
"family": "Murakami",
"given": "Hiroaki"
}
},
{
"id": "Enoto-Teruaki",
"name": {
"family": "Enoto",
"given": "Teruaki"
},
"orcid": "0000-0003-1244-3100"
},
{
"id": "Nakazawa-Kazuhiro",
"name": {
"family": "Nakazawa",
"given": "Kazuhiro"
}
}
]
},
"title": "A NuSTAR study of the 55 ks hard X-ray pulse-phase modulation in the magnetar 4U 0142+61",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron stars: magnetars stars: individual stars: magnetic fields",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Astronomical Society of Japan. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nReceived 2018 July 28; Accepted 2018 October 22. Published: 28 November 2018. \n\nThe authors thank Toshio Nakano and Yoshihiro Furuta for their help in data analysis and participation in discussion. This work was supported partially by the Ministry of Education, Culture, Sports, Science and Technology Grant-in-Aid for Scientific Research (C), Grant No. 18K03694.\n\nAccepted Version - 1810.11147.pdf
",
"abstract": "Archival NuSTAR data of the magnetar 4U\u20090142+61, acquired in 2014 March for a total time span of 258\u2009ks, were analyzed. This is to reconfirm the 55 ks modulation in the hard X-ray pulse phases of this source, found with a Suzaku observation in 2009 (Makishima et al., 2014, Phys. Rev. Lett., 112, 171102). Indeed, the 10\u201370\u2009keV X-ray pulsation, detected with NuSTAR at 8.68917\u2009s, was found to be also phase-modulated (at >98% confidence) at the same \u223c55 ks period, or half that value. Furthermore, a brief analysis of another Suzaku data set of 4U\u20090142+61, acquired in 2013, reconfirmed the same 55 ks phase modulation in the 15\u201340\u2009keV pulses. Thus, the hard X-ray pulse-phase modulation was detected with Suzaku (in 2009 and 2013) and NuSTAR (in 2014) at a consistent period. However, the modulation amplitude varied significantly; A \u223c 0.7\u2009s with Suzaku (in 2009), A \u223c 1.2\u2009s with Suzaku (in 2013), and A \u223c 0.17\u2009s with NuSTAR. In addition, the phase modulation properties detected with NuSTAR differed considerably between the first 1/3 and the latter 2/3 of the observation. In energies below 10\u2009keV, the pulse-phase modulation was not detected with either Suzaku or NuSTAR. These results reinforce the view of Makishima et al. (2014, Phys. Rev. Lett., 112, 171102); the neutron star in 4U\u20090142+61 keeps free precession, under a slight axial deformation due probably to ultra-high toroidal magnetic fields of \u223c10^(16)\u2009G. The wobbling angle of precession should remain constant, but the pulse-phase modulation amplitude varies on time scales of months to years, presumably as asymmetry of the hard X-ray emission pattern around the star's axis changes.",
"date": "2019-01-01",
"date_type": "published",
"publication": "Publications of the Astronomical Society of Japan",
"volume": "71",
"number": "1",
"publisher": "Astronomical Society of Japan",
"pagerange": "Art. No. 15",
"id_number": "CaltechAUTHORS:20181029-101613379",
"issn": "0004-6264",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181029-101613379",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/pasj/psy129",
"primary_object": {
"basename": "1810.11147.pdf",
"url": "https://authors.library.caltech.edu/records/m3tx7-0q593/files/1810.11147.pdf"
},
"pub_year": "2019",
"author_list": "Makishima, Kazuo; Murakami, Hiroaki; et el."
},
{
"id": "https://authors.library.caltech.edu/records/kxjs6-yyr15",
"eprint_id": 89558,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:32:58",
"lastmod": "2023-10-18 22:49:45",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Georgantopoulos-I",
"name": {
"family": "Georgantopoulos",
"given": "I."
}
},
{
"id": "Akylas-A",
"name": {
"family": "Akylas",
"given": "A."
}
}
]
},
"title": "NuSTAR observations of heavily obscured Swift/BAT AGN: constraints on the Compton-thick AGN fraction",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: general \u2013 galaxies: active \u2013 catalogs \u2013 quasars: supermassive black holes",
"note": "\u00a9 2018 ESO. Article published by EDP Sciences.\n\n\nReceived 16 March 2018; Accepted 31 August 2018; Published online 03 January 2019.\n\nWe would like to thank the anonymous referee for comments and suggestions that helped to improve the paper. We acknowledge the use of MYTORUS spectral models by Yaqoob & Murphy (2011). We would also like to thank Tahir Yaqoob for his help and suggestions in the application of the above models. The research leading to these results has received funding from the European Union's Horizon 2020 Programme under the AHEAD project (grant agreement n. 654215).\n\nAccepted Version - 1809.03747.pdf
",
"abstract": "The evolution of the accretion history of the Universe has been studied in unprecedented detail owing to recent X-ray surveys performed by Chandra and XMM-Newton. A focus on the most heavily obscured or Compton-thick active galactic nuclei (AGNs) is missing in these studies. These AGNs evade detection even in X-ray surveys owing to their extreme hydrogen column densities, which exceed 10^(24)\u2006cm^(\u22122). Recently, the all-sky hard X-ray survey performed by Swift/BAT brought a breakthrough, allowing the detection of many of these AGNs. This is because of the very high energy bandpass (14\u2013195 keV) of this instrument, which helps to minimise attenuation effects. In our previous work, we identified more than 50 candidate Compton-thick AGNs in the local Universe, corresponding to an observed fraction of about 7% of the total AGNs population. This number can only be converted to the intrinsic Compton-thick AGNs number density if we know their exact selection function. This function sensitively depends on the form of the Compton-thick AGN spectrum, that is the energy of their absorption turnover, photon-index and its cut-off energy at high energies, and the strength of the reflection component on the matter surrounding the nucleus. For example, the reflection component at hard energies 20\u201340 keV antagonises the number density of missing Compton-thick AGNs in the sense that the stronger the reflection the easier these sources are detected in the BAT band. In order to constrain their number density, we analysed the spectra of 19 Compton-thick AGNs that have been detected with Swift/BAT and have been subsequently observed with NuSTAR in the 3\u201380 keV band. We analysed their X-ray spectra using the MYTORUS models which properly take into account the Compton scattering effects. These were combined with physically motivated Comptonisation models, which accurately describe the primary coronal X-ray emission. We derived absorbing column densities that are consistent with those derived by the previous Swift/BAT analyses. We estimate the coronal temperatures to be roughly between 25 and 80 keV corresponding to high energy cut-offs roughly between 75 and 250 keV. Furthermore, we find that the majority of our AGNs lack a strong reflection component in the 20\u201340 keV band placing tighter constraints on the intrinsic fraction of Compton-thick AGNs. Combining these results with our X-ray background synthesis models, we estimate a percentage of Compton-thick AGNs in the local Universe of \u224820 \u00b1 3 % relative to the type-II AGNs population.",
"date": "2019-01",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "621",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A28",
"id_number": "CaltechAUTHORS:20180912-092926899",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180912-092926899",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201833038",
"primary_object": {
"basename": "1809.03747.pdf",
"url": "https://authors.library.caltech.edu/records/kxjs6-yyr15/files/1809.03747.pdf"
},
"pub_year": "2019",
"author_list": "Georgantopoulos, I. and Akylas, A."
},
{
"id": "https://authors.library.caltech.edu/records/pbj4c-nd619",
"eprint_id": 89172,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:07:30",
"lastmod": "2023-10-18 22:34:37",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Sanna-A",
"name": {
"family": "Sanna",
"given": "A."
}
},
{
"id": "Pintore-F",
"name": {
"family": "Pintore",
"given": "F."
}
},
{
"id": "Riggio-A",
"name": {
"family": "Riggio",
"given": "A."
}
},
{
"id": "Mazzola-S-M",
"name": {
"family": "Mazzola",
"given": "S. M."
}
},
{
"id": "Bozzo-E",
"name": {
"family": "Bozzo",
"given": "E."
}
},
{
"id": "Di-Salvo-T",
"name": {
"family": "Di Salvo",
"given": "T."
}
},
{
"id": "Ferrigno-C",
"name": {
"family": "Ferrigno",
"given": "C."
}
},
{
"id": "Gambino-A-F",
"name": {
"family": "Gambino",
"given": "A. F."
}
},
{
"id": "Papitto-A",
"name": {
"family": "Papitto",
"given": "A."
}
},
{
"id": "Iaria-R",
"name": {
"family": "Iaria",
"given": "R."
}
},
{
"id": "Burderi-L",
"name": {
"family": "Burderi",
"given": "L."
}
}
]
},
"title": "SWIFT J1756.9\u22122508: spectral and timing properties of its 2018 outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disc \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 August 18. Received 2018 August 18; in original form 2018 June 17. Published: 27 August 2018. \n\nWe thank N. Schartel for providing us with the possibility to perform the ToO observation in the Director Discretionary Time, and the XMM\u2013Newton team for the technical support. We also use Director Discretionary Time on NuSTAR, for which we thank Fiona Harrison for approving and the NuSTAR team for the technical support. We acknowledge financial contribution from the agreements ASI-INAF I/037/12/0 and ASI-INAF 2017-14-H.O. This work was partially supported by the Regione Autonoma della Sardegna through POR-FSE Sardegna 2007-2013, L.R. 7/2007, Progetti di Ricerca di Base e Orientata, Project N. CRP-60529. AP acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sk\u0142odowska-Curie grant agreement 660657-TMSP-H2020-MSCA-IF-2014, as well as the International Space Science Institute (ISSIBern) which funded and hosted the international team 'The disc magnetosphere interaction around transitional millisecond pulsar'.\n\nAccepted Version - 1808.06796.pdf
",
"abstract": "We discuss the spectral and timing properties of the accreting millisecond X-ray pulsar SWIFT J1756.9\u22122508 observed by XMM\u2013Newton, NICER, and NuSTARduring the X-ray outburst occurred in April 2018. The spectral properties of the source are consistent with a hard state dominated at high energies by a non-thermal power-law component with a cut-off at \u223c70 keV. No evidence of iron emission lines or reflection humps has been found. From the coherent timing analysis of the pulse profiles, we derived an updated set of orbital ephemerides. Combining the parameters measured from the three outbursts shown by the source in the last \u223c11 yr, we investigated the secular evolution of the spin frequency and the orbital period. We estimated a neutron magnetic field of \n3.1 \u00d7 10^8 < B_(PC) < 4.5 \u00d7 10^8 G and measured an orbital period derivative of \u22124.1 \u00d7 10^(\u221212) < P\u02d9_(orb) < 7.1 \u00d7 10^(\u221212) s s^(\u22121). We also studied the energy dependence of the pulse profile by characterizing the behaviour of the pulse fractional amplitude in the energy range 0.3\u201380 keV. These results are compared with those obtained from the previous outbursts of SWIFT J1756.9\u22122508 and other previously known accreting millisecond X-ray pulsars.",
"date": "2018-12-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "481",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1658-1666",
"id_number": "CaltechAUTHORS:20180827-122554035",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180827-122554035",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty2316",
"primary_object": {
"basename": "1808.06796.pdf",
"url": "https://authors.library.caltech.edu/records/pbj4c-nd619/files/1808.06796.pdf"
},
"pub_year": "2018",
"author_list": "Sanna, A.; Pintore, F.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/zgs75-9q530",
"eprint_id": 89435,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:07:41",
"lastmod": "2023-10-18 22:45:05",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Turner-T-J",
"name": {
"family": "Turner",
"given": "T. J."
},
"orcid": "0000-0003-2971-1722"
},
{
"id": "Reeves-J-N",
"name": {
"family": "Reeves",
"given": "J. N."
}
},
{
"id": "Braito-V",
"name": {
"family": "Braito",
"given": "V."
},
"orcid": "0000-0002-2629-4989"
},
{
"id": "Lobban-A-P",
"name": {
"family": "Lobban",
"given": "A."
},
"orcid": "0000-0002-6433-1357"
},
{
"id": "Kraemer-S-B",
"name": {
"family": "Kraemer",
"given": "S."
}
},
{
"id": "Miller-L",
"name": {
"family": "Miller",
"given": "L."
}
}
]
},
"title": "A rapid occultation event in NGC 3227",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual: NGC 3227 \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.\nThis article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model).\n\nAccepted 2018 September 3. Received 2018 August 31; in original form 2018 July 23. Published: 06 September 2018.\n\nTJT acknowledges National Aeronautics and Space Administration (NASA) grant NNX17AD91G. Valentina Braito acknowledges financial support through NASA grant NNX17AC40G and through the CSST Visiting Scientist Initiative. APL acknowledges support from Science and Technology Facilities Council (STFC) consolidated grant ST/M001040/1. We are grateful to the XMM and NuSTAR operations teams for performing this campaign and providing software and calibration for the data analysis.\n\nAccepted Version - 1809.01172.pdf
",
"abstract": "NGC 3227 exhibits rapid flux and spectral variability in the X-ray band. To understand this behaviour, we conducted a coordinated observing campaign using 320 ks of XMM\u2013Newton exposures together with 160 ks of overlapping NuSTAR observations, spanning a month. Here, we present a rapid variability event that occurs toward the end of the campaign. The spectral hardening event is accompanied by a change in the depth of an unresolved transition array (UTA), whose time-dependent behaviour is resolved using the RGS data. This UTA fingerprint allows us to identify this as a transit event, where a clump of gas having N_H\u223c5\u00d710^(22) atoms cm^(\u22122 ), log \u03be \u223c 2 occults \u223c60 per cent of the continuum photons over the course of approximately a day. This occulting gas is likely associated with clouds in the inner broad-line region. An additional zone of gas with lower column and higher ionization, matches the outflow velocity of the variable zone, and may represent transmission through the cloud limb.",
"date": "2018-12-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "481",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2470-2478",
"id_number": "CaltechAUTHORS:20180906-154725591",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180906-154725591",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty2447",
"primary_object": {
"basename": "1809.01172.pdf",
"url": "https://authors.library.caltech.edu/records/zgs75-9q530/files/1809.01172.pdf"
},
"pub_year": "2018",
"author_list": "Turner, T. J.; Reeves, J. N.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ehwb0-9t616",
"eprint_id": 92017,
"eprint_status": "archive",
"datestamp": "2023-08-19 13:02:27",
"lastmod": "2023-10-19 23:54:20",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Falkner-S",
"name": {
"family": "Falkner",
"given": "S."
},
"orcid": "0000-0001-5209-991X"
},
{
"id": "Marcu-Cheatham-D-M",
"name": {
"family": "Marcu-Cheatham",
"given": "D."
},
"orcid": "0000-0001-8061-611X"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "J."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "K."
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "L."
},
"orcid": "0000-0002-6601-9543"
},
{
"id": "Kretschmar-P",
"name": {
"family": "Kretschmar",
"given": "P."
},
"orcid": "0000-0001-9840-2048"
}
]
},
"title": "Multiple cyclotron line-forming regions in GX 301\u22122",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks / magnetic fields / X-rays: binaries / stars: neutron / pulsars: individual: GX 301-2",
"note": "\u00a9 ESO 2018. \n\nReceived 19 October 2017 / Accepted 13 September 2018. \n\nWe thank the referee for their helpful comments. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. The Swift/BAT transient monitor results were provided by the Swift/BAT team. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). L.N. acknowledges support by ASI/INAF grant I/037/12/0 and PRIN-INAF 2014 grant \"Towards a unified picture of accretion in High Mass X-Ray Binaries\".\n\nPublished - aa32132-17.pdf
Accepted Version - 1809.05691.pdf
",
"abstract": "We present two observations of the high-mass X-ray binary GX 301\u22122 with NuSTAR, taken at different orbital phases and different luminosities. We find that the continuum is well described by typical phenomenological models, like a very strongly absorbed NPEX model. However, for a statistically acceptable description of the hard X-ray spectrum we require two cyclotron resonant scattering features (CRSF), one at \u223c35 keV and the other at \u223c50 keV. Even though both features strongly overlap, the good resolution and sensitivity of NuSTAR allows us to disentangle them at \u226599.9% significance. This is the first time that two CRSFs have been seen in GX 301\u22122. We find that the CRSFs are very likely independently formed, as their energies are not harmonically related and, if the observed feature were due to a single line, the deviation from a Gaussian shape would be very large. We compare our results to archival Suzaku data and find that our model also provides a good fit to those data. We study the behavior of the continuum as well as the CRSF parameters as function of pulse phase in seven phase bins. We find that the energy of the 35 keV CRSF varies smoothly as a function of phase, between 30 and 38 keV. To explain this variation, we apply a simple model of the accretion column, taking into account the altitude of the line-forming region, the velocity of the in-falling material, and the resulting relativistic effects. We find that in this model the observed energy variation can be explained as being simply due to a variation of the projected velocity and beaming factor of the line-forming region towards us.",
"date": "2018-12",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "620",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A153",
"id_number": "CaltechAUTHORS:20190102-155139776",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190102-155139776",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN-INAF 2014"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1051/0004-6361/201732132",
"primary_object": {
"basename": "1809.05691.pdf",
"url": "https://authors.library.caltech.edu/records/ehwb0-9t616/files/1809.05691.pdf"
},
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{
"basename": "aa32132-17.pdf",
"url": "https://authors.library.caltech.edu/records/ehwb0-9t616/files/aa32132-17.pdf"
}
],
"pub_year": "2018",
"author_list": "F\u00fcrst, F.; Falkner, S.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/x1f4c-dck53",
"eprint_id": 89197,
"eprint_status": "archive",
"datestamp": "2023-08-19 12:46:58",
"lastmod": "2023-10-18 22:35:39",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Jiang-Jiachen",
"name": {
"family": "Jiang",
"given": "Jiachen"
},
"orcid": "0000-0002-9639-4352"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "Michael L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
}
]
},
"title": "The ultrafast outflow of WKK 4438: Suzaku and NuSTAR X-ray spectral analysis",
"ispublished": "pub",
"full_text_status": "restricted",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 August 23. Received 2018 August 22; in original form 2018 May 3. Published: 28 August 2018. \n\nJ.J. acknowledges support by the Cambridge Trust and the Chinese Scholarship Council Joint Scholarship Programme (201604100032). D.J.W. acknowledges support from an Science and Technology Facilities Council Ernest Rutherford fellowship. M.L.P. is supported by a European Space Agency (ESA) research fellowship. A.C.F. acknowledges support by the European Research Council Advanced Grant 340442. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA, and data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology.",
"abstract": "Previous X-ray spectral analysis has revealed an increasing number of active galactic nuclei (AGNs) with high accretion rates where an outflow with a mildly relativistic velocity originates from the inner accretion disc. Here we report the detection of a new ultrafast outflow (UFO) with a velocity of v_(out) = 0.319^(+0.005)_(\u22120.008)c in addition to a relativistic disc reflection component in a poorly studied NLS1 WKK 4438, based on archival NuSTAR and Suzaku observations. The spectra of both Suzaku and NuSTAR observations show an Fe\u2009XXVI absorption feature and the Suzaku data also show evidence for an Ar\u2009XVIII with the same blueshift. A supersolar argon abundance (Z\u2032_(Ar) > 6Z\u2299) and a slight iron overabundance (Z\u2032_(Fe) = 2.6^(+1.9)_(\u22122.0) Z\u2299) are found in our spectral modelling. Based on Monte Carlo simulations, the detection of the UFO is estimated to be at around 3\u03c3 significance. The fast wind most likely arises from a radius of \u226520rg away from the central black hole. The disc is accreting at a high Eddington ratio (L_(bol) = 0.4\u22120.7L_(Edd)). The mass outflow rate of the UFO is comparable with the disc mass inflow rate (M_(out) > 30% M_(in)), assuming a maximum covering factor. The kinetic power of the wind might not be high enough to have an influence on AGN feedback (E_(wind)/L_(bol) \u2248 3\u22125 per cent) due to a relatively small column density (12^(+9)_(\u22124) \u00d7 10^(22) cm^(\u22122)). However, note that both the inferred velocity and the column density could be lower limits owing to the low viewing angle (i=23^(+3)_(\u22122)\u2218).",
"date": "2018-11-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "481",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "639-644",
"id_number": "CaltechAUTHORS:20180828-093504739",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-093504739",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
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}
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"doi": "10.1093/mnras/sty2344",
"pub_year": "2018",
"author_list": "Jiang, Jiachen; Walton, Dominic J.; et el."
},
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{
"id": "Balokovi\u0107-Mislav",
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{
"id": "Koss-Michael-J",
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"family": "Koss",
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},
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"family": "Annuar",
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"name": {
"family": "Hornschemeier",
"given": "A. E."
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"family": "Lehmer",
"given": "B."
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"name": {
"family": "Powell",
"given": "M. C."
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"name": {
"family": "Ptak",
"given": "A."
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"name": {
"family": "Rangelov",
"given": "B."
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"id": "Roberts-Timothy-P",
"name": {
"family": "Roberts",
"given": "T. P."
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"id": "Stern-Daniel",
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"family": "Stern",
"given": "D."
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"name": {
"family": "Zezas",
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"title": "A Long Hard-X-Ray Look at the Dual Active Galactic Nuclei of M51 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual (M51) \u2013 galaxies: nuclei \u2013 X-rays: binaries \u2013 X-rays: galaxies",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 May 29; revised 2018 September 6; accepted 2018 September 12; published 2018 November 5. \n\nThe authors thank the anonymous referee for the thorough and detailed review of our manuscript, which improved it. M. Balokovi\u0107 acknowledges support from the Black Hole Initiative at Harvard University, through the grant from the John Templeton Foundation. M.K. acknowledges support from NASA through ADAP award NNH16CT03C. D.M.A. acknowledges the Science and Technology Facilities Council (STFC) through grant ST/P000541/1. The work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. A.Z. acknowledges funding from the European Research Council under the European Unions Seventh Framework Programme (FP/2007\u20132013)/ERC Grant Agreement n. 617001. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO7-18105X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This work was also supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: Chandra (ACIS) - , NuSTAR - , Hale (DBSP) - .\n\nPublished - Brightman_2018_ApJ_867_110.pdf
Accepted Version - 1805.12140.pdf
",
"abstract": "We present a broadband X-ray spectral analysis of the M51 system, including the dual active galactic nuclei (AGNs) and several off-nuclear point sources. Using a deep observation by NuSTAR, new high-resolution coverage of M51b by Chandra, and the latest X-ray torus models, we measure the intrinsic X-ray luminosities of the AGNs in these galaxies. The AGN of M51a is found to be Compton-thick, and both AGNs have very low accretion rates (\u03bb_Edd) < 10^(-4)). The latter is surprising considering that the galaxies of M51 are in the process of merging, which is generally predicted to enhance nuclear activity. We find that the covering factor of the obscuring material in M51a is 0.26 \u00b1 0.03, consistent with the local AGN obscured fraction at L_X ~10^(40) erg s^(\u22121). The substantial obscuring column does not support theories that the torus, presumed responsible for the obscuration, disappears at these low accretion luminosities. However, the obscuration may have resulted from the gas infall driven by the merger rather than the accretion process. We report on several extranuclear sources with L_X > 10^(-39) erg s^(\u22121) and find that a spectral turnover is present below 10 keV in most such sources, in line with recent results on ultraluminous X-ray sources.",
"date": "2018-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "867",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 110",
"id_number": "CaltechAUTHORS:20181106-105511630",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181106-105511630",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Harvard University"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "NASA",
"grant_number": "NNH16CT03C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/P000541/1"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "617001"
},
{
"agency": "NASA",
"grant_number": "GO7-18105X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
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"pub_year": "2018",
"author_list": "Brightman, M.; Balokovi\u0107, M.; et el."
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"id": "Masini-A",
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"family": "Stern",
"given": "D."
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"title": "The NuSTAR Extragalactic Surveys: Unveiling Rare, Buried AGNs and Detecting the Contributors to the Peak of the Cosmic X-Ray Background",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: Seyfert",
"note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2018 July 20; revised 2018 August 31; accepted 2018 September 27; published 2018 November 12. \n\nWe thank the anonymous referee, whose comments helped improve the quality and clarity of the paper. This work was supported under NASA Contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has also made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC). Figure 4 is partially based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The DEIMOS spectrum presented herein was obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013; The Astropy Collaboration et al. 2018), and XSPEC (Arnaud 1996). \n\nA.M. and A.C. acknowledge support from the ASI/INAF grant I/037/12/0011/13. R.C.H. acknowledges support from the National Science Foundation through CAREER award 1554584, and from NASA through grant number NNX15AP24G. W.N.B. acknowledges support from Caltech NuSTAR subcontract 44A-1092750. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Chandra - . \n\nSoftware: NuSTARDAS, FTOOLS.\n\nPublished - Masini_2018_ApJ_867_162.pdf
Accepted Version - 1810.00010
",
"abstract": "We report on the results of active galactic nuclei (AGNs) detection by NuSTAR performed in three extragalactic survey fields (COSMic Evolutionary Survey field (COSMOS), Ultra Deep Survey (UDS), and Extended Chandra Deep Field-South (ECDFS)) in three hard bands, namely H1 (8\u201316 keV), H2 (16\u201324 keV), and VH (35\u201355 keV). The aggregated area of the surveys is ~2.7 deg^2. While a large number of sources is detected in the H1 band (72 at the 97% level of reliability), the H2 band directly probing close to the peak of the Cosmic X-ray Background (CXB) returns four significant detections, and two tentative (although not significant) detections are found in the VH-band. All of the sources detected above 16 keV are also detected at lower energies. We compute the integral number counts for sources in such bands, which show broad consistency with population-synthesis models of the CXB. We furthermore identify two Compton-thick AGNs, one in the COSMOS field, associated with a hard and faint Chandra source, and one in the UDS field, never detected in the X-ray band before. Both sources are at the same redshift z ~ 1.25, which shifts their Compton-hump into the H1 band, and were previously missed in the usually employed NuSTAR bands, confirming the potential for using the H1 band to discover obscured AGNs at z > 1 in deep surveys.",
"date": "2018-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "867",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 162",
"id_number": "CaltechAUTHORS:20181113-112609358",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181113-112609358",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "W. M. Keck Foundation"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "NSF",
"grant_number": "AST-1554584"
},
{
"agency": "NASA",
"grant_number": "NNX15AP24G"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
}
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},
"title": "NuSTAR observations of Mrk 766: distinguishing reflection from absorption",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs, black hole physics, galaxies: individual: Mrk 766, galaxies: Seyfert",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) \n\nAccepted 2018 July 30. Received 2018 July 27; in original form 2017 May 23. \n\nDJKB, MLP, and RVV acknowledge financial support from the Science and Technology Facilities Council (STFC). ACF, AML, CP, and MLP acknowledge support from the ERC Advanced Grant FEEDBACK 340442. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This work has made use of observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC).\n\nPublished - sty2081.pdf
Accepted Version - 1808.00014
",
"abstract": "We present two new NuSTAR observations of the narrow-line Seyfert 1 (NLS1) galaxy Mrk 766 and give constraints on the two scenarios previously proposed to explain its spectrum and that of other NLS1s: relativistic reflection and partial covering. The NuSTAR spectra show a strong hard (>15 \u2009keV) X-ray excess, while simultaneous soft X-ray coverage of one of the observations provided by XMM\u2013Newton constrains the ionized absorption in the source. The pure reflection model requires a black hole of high spin (a > 0.92) viewed at a moderate inclination (\u2060i=46^(+1)_(\u22124)\u2218\u2060). The pure partial covering model requires extreme parameters: the cut-off of the primary continuum is very low (\u206022^(+7)_(\u22125)\u2009keV) in one observation and the intrinsic X-ray emission must provide a large fraction (75 per cent) of the bolometric luminosity. Allowing a hybrid model with both partial covering and reflection provides more reasonable absorption parameters and relaxes the constraints on reflection parameters. The fractional variability reduces around the iron K band and at high energies including the Compton hump, suggesting that the reflected emission is less variable than the continuum.",
"date": "2018-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "480",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3689-3701",
"id_number": "CaltechAUTHORS:20181128-153100321",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181128-153100321",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Space Astronomy Centre"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/sty2081",
"primary_object": {
"basename": "1808.00014",
"url": "https://authors.library.caltech.edu/records/sz2gq-etx80/files/1808.00014"
},
"related_objects": [
{
"basename": "sty2081.pdf",
"url": "https://authors.library.caltech.edu/records/sz2gq-etx80/files/sty2081.pdf"
}
],
"pub_year": "2018",
"author_list": "Buisson, D. J. K.; Parker, M. L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/mmyh5-7dv48",
"eprint_id": 86358,
"eprint_status": "archive",
"datestamp": "2023-09-22 22:45:58",
"lastmod": "2023-10-23 23:28:39",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kaastra-J-S",
"name": {
"family": "Kaastra",
"given": "J. S."
},
"orcid": "0000-0001-5540-2822"
},
{
"id": "Mehdipour-M",
"name": {
"family": "Mehdipour",
"given": "M."
}
},
{
"id": "Behar-E",
"name": {
"family": "Behar",
"given": "E."
}
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Branduardi-Raymont-G",
"name": {
"family": "Branduardi-Raymont",
"given": "G."
}
},
{
"id": "Brenneman-L-W",
"name": {
"family": "Brenneman",
"given": "L."
}
},
{
"id": "Cappi-M",
"name": {
"family": "Cappi",
"given": "M."
}
},
{
"id": "Costantini-E",
"name": {
"family": "Costantini",
"given": "E."
}
},
{
"id": "De-Marco-B",
"name": {
"family": "De Marco",
"given": "B."
}
},
{
"id": "di-Gesu-L",
"name": {
"family": "di Gesu",
"given": "L."
}
},
{
"id": "Ebrero-J",
"name": {
"family": "Ebrero",
"given": "J."
},
"orcid": "0000-0001-5924-8818"
},
{
"id": "Kriss-G-A",
"name": {
"family": "Kriss",
"given": "G. A."
}
},
{
"id": "Mao-Junjie",
"name": {
"family": "Mao",
"given": "J."
},
"orcid": "0000-0001-7557-9713"
},
{
"id": "Peretz-U",
"name": {
"family": "Peretz",
"given": "U."
}
},
{
"id": "Petrucci-P-O",
"name": {
"family": "Petrucci",
"given": "P.-O."
}
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "G."
},
"orcid": "0000-0003-0293-3608"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Recurring obscuration in NGC 3783",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: galaxies \u2013 galaxies: active \u2013 galaxies: Seyfert \u2013 galaxies: individual: NGC3783 \u2013 techniques: spectroscopic",
"note": "\u00a9 2018 ESO. Article published by EDP Sciences. \n\nReceived 12 January 2018; Accepted 25 August 2018; Published online 13 November 2018.\n\nSRON is financially supported by NWO, The Netherlands Organization for Scientific Research. The research at the Technion is supported by the I-CORE program of the Planning and Budgeting Committee (grant number 1937/12). EB acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement no. 655324. SB and MC acknowledge financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0, and under the agreement ASI-INAF n.2017-14-H.O. BDM acknowledges support from Polish National Science Centre grant Polonez 2016/21/P/ST9/04025. POP aknowledges support from the CNES and French PNHE. GP acknowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luftund Raumfahrt (BMWI/DLR, FKZ 50 OR 1604) and the Max Planck Society.\n\nSubmitted - 1805.03538.pdf
",
"abstract": "Context. Obscuration of the continuum emission from active galactic nuclei by streams of gas with relatively high velocity (>1000 km s^(\u22121)) and column density (>3 \u00d7 10^(25) m^(\u22122)) has been seen in a few Seyfert galaxies. This obscuration has a transient nature. In December 2016 we witnessed such an event in NGC 3783.\nAims. The frequency and duration of these obscuration events is poorly known. Here we study archival data of NGC 3783 in order to constrain this duty cycle.\nMethods. We use archival Chandra/NuSTAR spectra taken in August 2016. We also study the hardness ratio of all Swift XRT spectra taken between 2008 and 2017.\nResults. In August 2016, NGC 3783 also showed evidence of obscuration. While the column density of the obscuring material is ten times lower than in December 2016, the opacity is still sufficient to block a significant fraction of the ionising X-ray and extreme ultraviolet photons. From the Swift hardness ratio behaviour we find several other epochs with obscuration. Obscuration with columns >10^(26) m^(\u22122) may take place about half of the time. Also, in archival X-ray data taken by the Advanced Satellite for Cosmology and Astrophysics (ASCA) in 1993 and 1996 we find evidence of obscuration.\nConclusions. Obscuration of the ionising photons in NGC 3783 occurs more frequently than previously thought. This may not always have been recognised due to low-spectral-resolution observations, overly limited spectral bandwidth or confusion with underlying continuum variations.",
"date": "2018-11",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "619",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A112",
"id_number": "CaltechAUTHORS:20180510-154544556",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180510-154544556",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201832629",
"primary_object": {
"basename": "1805.03538.pdf",
"url": "https://authors.library.caltech.edu/records/mmyh5-7dv48/files/1805.03538.pdf"
},
"pub_year": "2018",
"author_list": "Kaastra, J. S.; Mehdipour, M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/jr44y-7pg86",
"eprint_id": 90350,
"eprint_status": "archive",
"datestamp": "2023-08-19 12:02:44",
"lastmod": "2023-10-18 23:23:20",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kamraj-N",
"name": {
"family": "Kamraj",
"given": "N."
},
"orcid": "0000-0002-3233-2451"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A."
}
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
}
]
},
"title": "Coronal Properties of Swift/BAT-selected Seyfert 1 AGNs Observed with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 X-rays: galaxies",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 April 20; revised 2018 August 23; accepted 2018 August 24; published 2018 October 19. \n\nWe would like to thank the referee for comments that helped improve the final version of the manuscript. We have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program (grant NNX14AQ07H) and support from the black hole Initiative at Harvard University, through the grant from the John Templeton Foundation. \n\nFacility: NuSTAR. -\n\nPublished - Kamraj_2018_ApJ_866_124.pdf
Accepted Version - 1809.01757.pdf
",
"abstract": "The NuSTAR observatory, with its high sensitivity in hard X-rays, has enabled detailed broadband modeling of the X-ray spectra of active galactic nuclei (AGNs), thereby allowing constraints to be placed on the high-energy cutoff of the X-ray coronal continuum. We investigate the spectral properties of a sample of 46 NuSTAR-observed Seyfert 1 AGNs selected from the Swift/Burst Alert Telescope 70 month hard X-ray survey. Our measurements of the high-energy cutoff of the continuum from modeling the NuSTAR X-ray spectra are used to map out the temperature\u2013compactness (\u03b8\u2013l) plane for AGN coronae. We find that most of the coronae lie clustered near the boundary for runaway pair production, suggesting that annihilation and pair production act to regulate the temperature of the corona. We discuss the implications of coronae whose high-energy cutoff may indicate a low coronal temperature on the heating and thermalization mechanisms in the corona.",
"date": "2018-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "866",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 124",
"id_number": "CaltechAUTHORS:20181023-091921294",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181023-091921294",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Harvard University"
},
{
"agency": "John Templeton Foundation"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aadd0d",
"primary_object": {
"basename": "1809.01757.pdf",
"url": "https://authors.library.caltech.edu/records/jr44y-7pg86/files/1809.01757.pdf"
},
"related_objects": [
{
"basename": "Kamraj_2018_ApJ_866_124.pdf",
"url": "https://authors.library.caltech.edu/records/jr44y-7pg86/files/Kamraj_2018_ApJ_866_124.pdf"
}
],
"pub_year": "2018",
"author_list": "Kamraj, N.; Harrison, F. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/82gby-7zg46",
"eprint_id": 90056,
"eprint_status": "archive",
"datestamp": "2023-08-19 11:55:47",
"lastmod": "2023-10-18 23:10:20",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Rani-B",
"name": {
"family": "Rani",
"given": "B."
}
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G. M."
}
},
{
"id": "Mushotzky-R-F",
"name": {
"family": "Mushotzky",
"given": "R. F."
},
"orcid": "0000-0002-7962-5446"
},
{
"id": "Reynolds-C",
"name": {
"family": "Reynolds",
"given": "C."
},
"orcid": "0000-0002-1510-4860"
},
{
"id": "Hodgson-J-A",
"name": {
"family": "Hodgson",
"given": "J. A."
}
}
]
},
"title": "NuSTAR view of the central region of the Perseus cluster",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: clusters: individual (Perseus cluster) \u2013 galaxies: individual (3C 84) \u2013 quasars: individual (3C 84) \u2013 X-rays: galaxies",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 July 19; revised 2018 September 14; accepted 2018 September 26; published 2018 October 11. \n\nThis research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Universities Space Research Association through a contract with NASA. B.R. thanks Erin Kara, Mihoko Yukita, Dave Thompson, Stefan Walker, Amy Lien, Hans Krimm, and Chris Shrader, for interesting discussions about AGN disks and coronas.\n\nAccepted Version - 1809.10163.pdf
",
"abstract": "Located at the center of the Perseus cluster, 3C 84 is an extremely bright and nearby radio galaxy. Because of the strong diffuse thermal emission from the cluster in X-rays, the detailed properties and the origin of a power-law component from the central active galactic nucleus (AGN) remains unclear in the source. We report here the first NuSTAR observations of 3C 84. The source was observed for 24.2 and 32 ks on 2018 February 1 and 4, respectively. NuSTAR observations spectrally decompose the power-law AGN component above 10 keV. The power-law component dominates the spectrum above 20 keV with a photon index ~1.9 and an energy flux F_(20\u201330 keV) = 1.0 \u00d7 10^(\u221211) erg cm^(\u22122) s^(\u22121), corresponding to an isotropic luminosity, L_(20\u201330 keV) = 7.4 \u00d7 10^(42) erg s^(\u22121). We discuss possible emitting sites for the power-law component. The expected thermal emission from the accretion disk is not hot enough to account for the hard X-rays detected from the source. Similar X-ray and \u03b3-ray photon indices and long-term flux variations, the absence of cutoff energy in the hard X-ray spectrum of the source, correlated hard X-ray flux and hardness ratio variations, and the similarity of optical-X-ray slope to blazar rather than Seyfert galaxies supports the hard X-ray power-law component originating from the jet.",
"date": "2018-10-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "866",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L13",
"id_number": "CaltechAUTHORS:20181001-104903603",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181001-104903603",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8213/aae48f",
"primary_object": {
"basename": "1809.10163.pdf",
"url": "https://authors.library.caltech.edu/records/82gby-7zg46/files/1809.10163.pdf"
},
"pub_year": "2018",
"author_list": "Rani, B.; Madejski, G. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ej798-6wr14",
"eprint_id": 89560,
"eprint_status": "archive",
"datestamp": "2023-08-19 11:41:30",
"lastmod": "2023-10-18 22:49:52",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Nikolaeva-S-M",
"name": {
"family": "Nikolaeva",
"given": "S. M."
}
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "R. A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Sazonov-S-Yu",
"name": {
"family": "Sazonov",
"given": "S. Yu."
}
}
]
},
"title": "Broadband Spectrum of the X-ray Binary M33 X-6 from NuSTAR and Swift-XRT Data: An Extragalactic Z-Source?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "mass accretion, X-ray binaries, nearby galaxies, galaxy M33",
"note": "\u00a9 2018 Pleiades Publishing, Inc. Original Russian Text \u00a9 S.M. Nikolaeva, R.A. Krivonos, S.Yu. Sazonov, 2018, published in Pis'ma v Astronomicheskii Zhurnal, 2018, Vol. 44, No. 10, pp. 648\u2013658. \n\nFirst Online: 18 October 2018. \n\nThe results presented in this paper were obtained with the Neil Gehrels (Swift) and NuSTAR orbital observatories. This work was supported by the Russian Science Foundation (project no. 14-12-01315).\n\nAccepted Version - 1809.02871.pdf
",
"abstract": "We present the results of our study of the X-ray spectrum for the source X-6 in the nearby galaxy M33 obtained for the first time at energies above 10 keV from the data of the NuSTAR orbital telescope. The archival Swift\u2013XRT data for energy coverage below 3 keV have been used, which has allowed the spectrum of M33 X-6 to be constructed in the wide energy range 0.3\u201320 keV. The spectrum of the source is well described by the model of an optically and geometrically thick accretion disk with a maximum temperature of ~2 keV and an inner radius of ~5 cos^(\u22121/2)\u03b8 km (where >\u03b8 is the unknown disk inclination angle with respect to the observer). There is also evidence for the presence of an additional hard component in the spectrum. The X-ray luminosity of M33 X-6 measured for the first time in the wide energy range 0.3\u201320 keV is ~2 \u00d7 10^(38) erg s^(\u22121), with the luminosity in the hard 10\u201320 keV X-ray band being ~10% of the source's total luminosity. The results obtained suggest that X-6 may be a Z-source, i.e., an X-ray binary with subcritical accretion onto a weakly magnetized neutron star.",
"date": "2018-10",
"date_type": "published",
"publication": "Astronomy Letters",
"volume": "44",
"number": "10",
"publisher": "Springer",
"pagerange": "593-602",
"id_number": "CaltechAUTHORS:20180912-093210194",
"issn": "1063-7737",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180912-093210194",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01315"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1134/S1063773718100055",
"primary_object": {
"basename": "1809.02871.pdf",
"url": "https://authors.library.caltech.edu/records/ej798-6wr14/files/1809.02871.pdf"
},
"pub_year": "2018",
"author_list": "Nikolaeva, S. M.; Krivonos, R. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/qm82v-7xj61",
"eprint_id": 85195,
"eprint_status": "archive",
"datestamp": "2023-08-19 11:32:31",
"lastmod": "2023-10-18 17:57:14",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kosec-P",
"name": {
"family": "Kosec",
"given": "P."
}
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
}
]
},
"title": "Evidence for a Variable Ultrafast Outflow in the Newly Discovered Ultraluminous Pulsar NGC 300 ULX-1",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices). \n\nAccepted 2018 June 12. Received 2018 June 12; in original form 2018 March 5. Published: 20 June 2018. \n\nWe are grateful to the anonymous referee for useful comments that improved the clarity and quality of the paper. PK acknowledges support from the Science and Technology Facilities Council (STFC). CP and ACF acknowledge support from the European Research Council Advanced Grant Feedback 340442. DJW acknowledges support from STFC Ernest Rutherford fellowships. This work is based on observations obtained with XMM\u2013Newton, an ESA science mission funded by ESA Member States and USA (NASA). This research has used the NASA/IPAC Extragalactic Database (NED) that is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has used the SIMBAD database, operated at CDS, Strasbourg, France.\n\nPublished - sty1626.pdf
Submitted - 1803.02367v1.pdf
",
"abstract": "Ultraluminous pulsars are a definite proof that persistent super-Eddington accretion occurs in nature. They support the scenario according to which most Ultraluminous X-ray Sources (ULXs) are super-Eddington accretors of stellar mass rather than sub-Eddington intermediate mass black holes. An important prediction of theories of supercritical accretion is the existence of powerful outflows of moderately ionized gas at mildly relativistic speeds. In practice, the spectral resolution of X-ray gratings such as RGS onboard XMM\u2013Newton is required to resolve their observational signatures in ULXs. Using RGS, outflows have been discovered in the spectra of three ULXs (none of which are currently known to be pulsars). Most recently, the fourth ultraluminous pulsar was discovered in NGC 300. Here we report detection of an ultrafast outflow (UFO) in the X-ray spectrum of the object, with a significance of more than 3\u03c3, during one of the two simultaneous observations of the source by XMM\u2013Newton and NuSTAR in December 2016. The outflow has a projected velocity of\u200965 000\u2009km\u2009s^(\u22121)(0.22c) and a high ionization factor with a log value of 3.9. This is the first direct evidence for a UFO in a neutron star ULX and also the first time that this evidence in a ULX spectrum is seen in both soft and hard X-ray data simultaneously. We find no evidence of the UFO during the other observation of the object, which could be explained by either clumpy nature of the absorber or a slight change in our viewing angle of the accretion flow.",
"date": "2018-09-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "479",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3978-3986",
"id_number": "CaltechAUTHORS:20180308-083847600",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180308-083847600",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technologies Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Space Agency (ESA)"
}
]
},
"local_group": {
"items": [
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"doi": "10.1093/mnras/sty1626",
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"pub_year": "2018",
"author_list": "Kosec, P.; Pinto, C.; et el."
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"items": [
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
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},
{
"id": "Harrison-F-A",
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"family": "Harrison",
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{
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"name": {
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"given": "Jamie A."
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{
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"family": "Walton",
"given": "Dominic J."
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{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
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{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
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"name": {
"family": "Fabian",
"given": "Andrew C."
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"family": "Forster",
"given": "Karl"
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"family": "F\u00fcrst",
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"name": {
"family": "Gandhi",
"given": "Poshak"
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"orcid": "0000-0003-3105-2615"
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{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
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},
"title": "The Hard State of the Highly Absorbed High Inclination Black Hole Binary Candidate Swift J1658.2\u20134242 Observed by NuSTAR and Swift",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 X-rays: binaries \u2013 X-rays: individual (Swift J1658.2-4242)",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 May 18; revised 2018 July 30; accepted 2018 August 9; published 2018 September 18. \n\nWe thank the referee for helpful comments that improved this work. D.J.W. acknowledges support from STFC Ernest Rutherford Fellowship. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Xu_2018_ApJ_865_18.pdf
Accepted Version - 1805.07705.pdf
",
"abstract": "We present a spectral and timing analysis of the newly reported Galactic X-ray transient Swift J1658.2\u20134242 observed by Nuclear Spectroscopic Telescope Array (NuSTAR) and Swift. The broadband X-ray continuum is typical of a black hole binary in the bright hard state, with a photon index of \u0393 = 1.63 \u00b1 0.02 and a low coronal temperature of kT_e = 22 \u00b1 1 keV, corresponding to a low spectral cutoff well constrained by NuSTAR. Spectral modeling of the relativistic disk reflection features, consisting of a broad Fe K\u03b1 line and the Compton reflection hump, reveals that the black hole is rapidly spinning with the spin parameter of a* > 0.96, and the inner accretion disk is viewed at a high inclination angle of I = 64^(2 o)_(-3) (statistical errors, 90% confidence). The high inclination is independently confirmed by dips in the light curves, which can be explained by absorbing material located near the disk plane temporarily obscuring the central region. In addition, we detect an absorption line in the NuSTAR spectra centered at 7.03^(+0.04)_(-0.03) keV. If associated with ionized Fe K absorption lines, this provides evidence for the presence of outflowing material in the low/hard state of a black hole binary candidate. A timing analysis shows the presence of a type-C quasi-periodic oscillation in the power spectrum, with the frequency increasing from ~0.14 to ~0.21 Hz during the single NuSTAR exposure. Our analysis reveals that Swift J1658.2\u20134242 displays characteristics typical for a black hole binary that is viewed at a high inclination angle, making it a good system for studying the accretion geometry in black hole binaries.",
"date": "2018-09-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "865",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 18",
"id_number": "CaltechAUTHORS:20180918-091012752",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180918-091012752",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
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"id": "Space-Radiation-Laboratory"
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{
"id": "Astronomy-Department"
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"doi": "10.3847/1538-4357/aada03",
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}
],
"pub_year": "2018",
"author_list": "Xu, Yanjun; Harrison, Fiona A.; et el."
},
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"eprint_id": 89202,
"eprint_status": "archive",
"datestamp": "2023-08-19 11:25:57",
"lastmod": "2023-10-18 22:35:51",
"type": "article",
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"creators": {
"items": [
{
"id": "Fukumura-Keigo",
"name": {
"family": "Fukumura",
"given": "Keigo"
},
"orcid": "0000-0001-5709-7606"
},
{
"id": "Kazanas-D",
"name": {
"family": "Kazanas",
"given": "Demosthenes"
},
"orcid": "0000-0002-7435-7809"
},
{
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"name": {
"family": "Shrader",
"given": "Chris"
}
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"id": "Behar-E",
"name": {
"family": "Behar",
"given": "Ehud"
}
},
{
"id": "Tombesi-F",
"name": {
"family": "Tombesi",
"given": "Francesco"
},
"orcid": "0000-0002-6562-8654"
},
{
"id": "Contopoulos-I",
"name": {
"family": "Contopoulos",
"given": "Ioannis"
},
"orcid": "0000-0001-6890-4143"
}
]
},
"title": "Variable Nature of Magnetically-Driven Ultra-Fast Outflows",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 galaxies: individual (PDS 456) \u2013 magnetohydrodynamics (MHD) \u2013 methods: numerical \u2013 quasars: absorption lines",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 June 6; revised 2018 July 26; accepted 2018 August 27; published 2018 September 6. \n\nWe are grateful to the anonymous referee for helpful comments on the original manuscript and James Reeves for providing us with the XMM-Newton/NuSTAR spectrum. K.F. thanks Alex Sanner for his assistance on wind visualization calculations. This work is supported in part by NASA/ADAP (NNH15ZDA001N-ADAP) and Chandra Cycle 17 archive proposal (17700504).\n\nSubmitted - 1808.08935.pdf
",
"abstract": "Among a number of active galactic nuclei that drive ionized outflows in X-rays, a low-redshift (z = 0.184) quasar, PDS 456, is long known to exhibit one of the exemplary ultra-fast outflows (UFOs). However, the physical process of acceleration mechanisms is yet to be definitively constrained. In this work, we model the variations of the Fe K UFO properties in PDS 456 over many epochs in X-ray observations in the context of magnetohydrodynamic (MHD) accretion disk winds employed in our earlier studies of similar X-ray absorbers. We applied the model to the 2013/2014 XMM-Newton/NuSTAR spectra to determine the UFO's condition; namely, velocity, ionization parameter, column density, and equivalent width (EW). Under some provisions on the dependence of X-ray luminosity on the accretion rate applicable to near-Eddington state, our photoionization calculations, coupled to a 2.5-dimensional MHD-driven wind model, can further reproduce the observed correlations of the UFO velocity and the anticorrelation of its EW with the X-ray strength of PDS 456. This work demonstrates that UFOs, even without radiative pressure, can be driven as an extreme case purely by magnetic interaction while also producing the observed spectrum and correlations.",
"date": "2018-09-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "864",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L27",
"id_number": "CaltechAUTHORS:20180828-095719590",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-095719590",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8213/aadd10",
"primary_object": {
"basename": "1808.08935.pdf",
"url": "https://authors.library.caltech.edu/records/rjfmf-qy802/files/1808.08935.pdf"
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"pub_year": "2018",
"author_list": "Fukumura, Keigo; Kazanas, Demosthenes; et el."
},
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"datestamp": "2023-08-19 10:54:49",
"lastmod": "2023-10-25 16:07:32",
"type": "article",
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"creators": {
"items": [
{
"id": "Sun-Shangyu",
"name": {
"family": "Sun",
"given": "Shangyu"
}
},
{
"id": "Guainazzi-M",
"name": {
"family": "Guainazzi",
"given": "Matteo"
}
},
{
"id": "Ni-Qingling",
"name": {
"family": "Ni",
"given": "Qingling"
}
},
{
"id": "Wang-Jingchun",
"name": {
"family": "Wang",
"given": "Jingchun"
}
},
{
"id": "Qian-Chenyang",
"name": {
"family": "Qian",
"given": "Chenyang"
}
},
{
"id": "Shi-Fangzheng",
"name": {
"family": "Shi",
"given": "Fangzheng"
}
},
{
"id": "Wang-Yu",
"name": {
"family": "Wang",
"given": "Yu"
},
"orcid": "0000-0003-3589-9274"
},
{
"id": "Bambi-C",
"name": {
"family": "Bambi",
"given": "Cosimo"
},
"orcid": "0000-0002-3180-9502"
}
]
},
"title": "Multi-epoch analysis of the X-ray spectrum of the active galactic nucleus in NGC 5506",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 galaxies: active \u2013 galaxies: individual: NGC 5506",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices). \n\nAccepted 2018 May 9. Received 2018 May 9; in original form 2017 April 13. Published: 11 May 2018. \n\nWe thank the referee's useful comments for improving this article. This work was supported by the NSFC (Grant Nos. U1531117 and 11305038), Fudan University (Grant No. IDH1512060), and the Thousand Young Talents Program. SS also acknowledges support from the AHEAD program for his visit to INAF-Bologna in June 2016. CB also acknowledges support from the Alexander von Humboldt Foundation. In this work, the authors used the data supplied by NASA's High Energy Astrophysics Science Archive Research Center in the US. The authors also used the data products from the XMM\u2013Newton, Suzaku, NuSTAR, and Chandra, funded by the ESA, JAXA, and NASA.\n\nSubmitted - 1704.03716.pdf
",
"abstract": "We present a multi-epoch X-ray spectroscopy analysis of the nearby narrow-line Seyfert\u2009I galaxy NGC\u20095506. For the first time, spectra taken by Chandra, XMM\u2013Newton, Suzaku, and NuSTAR\u2013 covering the 2000\u20132014 time span \u2013 are analysed simultaneously, using state-of-the-art models to describe reprocessing of the primary continuum by optical thick matter in the active galactic nucleus environment. The main goal of our study is determining the spin of the supermassive black hole (SMBH). The nuclear X-ray spectrum is photoelectrically absorbed by matter with column density \u2243 3 \u00d7 1022\u2009cm\u22122. A soft excess is present at energies lower than the photoelectric cut-off. Both photoionized and collisionally ionized components are required to fit it. This component is constant over the time-scales probed by our data. The spectrum at energies higher than 2\u2009keV is variable. We propose that its evolution could be driven by flux-dependent changes in the geometry of the innermost regions of the accretion disc. The black hole spin in NGC 5506 is constrained to be 0.93\n\u00b1^(0.04)_(0.04) at 90\u2009per\u2009cent confidence level for one interesting parameter.",
"date": "2018-08-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "478",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1900-1910",
"id_number": "CaltechAUTHORS:20170414-100328272",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170414-100328272",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
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"id": "NuSTAR"
}
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},
"doi": "10.1093/mnras/sty1233",
"primary_object": {
"basename": "1704.03716.pdf",
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"pub_year": "2018",
"author_list": "Sun, Shangyu; Guainazzi, Matteo; et el."
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{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
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"name": {
"family": "Petrucci",
"given": "P.-O."
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{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Cappi-M",
"name": {
"family": "Cappi",
"given": "M."
}
},
{
"id": "Dadina-M",
"name": {
"family": "Dadina",
"given": "M."
}
},
{
"id": "Grandi-P",
"name": {
"family": "Grandi",
"given": "P."
}
},
{
"id": "Torresi-E",
"name": {
"family": "Torresi",
"given": "E."
}
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"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "De-Marco-B",
"name": {
"family": "De Marco",
"given": "B."
}
},
{
"id": "De-Rosa-A",
"name": {
"family": "De Rosa",
"given": "A."
},
"orcid": "0000-0001-5668-6863"
},
{
"id": "Giroletti-M",
"name": {
"family": "Giroletti",
"given": "M."
}
},
{
"id": "Malzac-J",
"name": {
"family": "Malzac",
"given": "J."
}
},
{
"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "A."
}
},
{
"id": "Middei-R",
"name": {
"family": "Middei",
"given": "R."
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"orcid": "0000-0001-9815-9092"
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{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "G."
},
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{
"id": "Tortosa-A",
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"family": "Tortosa",
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},
"title": "Radio/X-ray monitoring of the broad-line radio galaxy 3C 382. High-energy view with XMM\u2013Newton and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active, X-rays: galaxies, X-rays: individuals (3C 382)",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. \nThis article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices).\n\nAccepted 2018 May 11. Received 2018 May 11; in original form 2018 February 13. Published: 15 May 2018. \n\nWe are grateful to the referee for helpful comments that improved the manuscript. This work is based on observations obtained with: the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA; XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of data, software\nand/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. The research leading to these results has received funding from the European Union's Horizon 2020 Programme under the AHEAD project (grant agreement n. 654215). FU acknowledges financial support from the Italian Space Agency (ASI) under contract ASI/INAF 2013-025-R01. SB and MC acknowledge financial\nsupport from ASI under grant ASI-INAF I/037/12/0, while\nGM, AM and AT from ASI/INAF I/037/12/0-011/13. SB, GM,\nAM, RM and AT acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. FU, GM, SB, MC, MD, PG, ET, ADR, MG, AM, RM and AT acknowledge financial contribution from the agreement ASI-INAF n. 2017-14-H.O. BDM acknowledges support from the Polish National Science Center grant Polonez 2016/21/P/ST9/04025. GP ackowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society.\n\nSubmitted - 1805.06229.pdf
",
"abstract": "We present the analysis of five joint XMM\u2013Newton/NuSTARobservations, 20 ks each and separated by 12 days, of the broad-line radio galaxy 3C 382. The data were obtained as part of a campaign performed in September-October 2016 simultaneously with VLBA. The radio data and their relation with the X-ray ones will be discussed in a following paper. The source exhibits a moderate flux variability in the UV/X-ray bands, and a limited spectral variability especially in the soft X-ray band. In agreement with past observations, we find the presence of a warm absorber, an iron K\u03b1 line with no associated Compton reflection hump, and a variable soft excess well described by a thermal Comptonization component. The data are consistent with a \"two-corona\" scenario, in which the UV emission and soft excess are produced by a warm (kT \u2243 0.6 keV), optically thick (\u03c4 \u2243 20) corona consistent with being a slab fully covering a nearly passive accretion disc, while the hard X-ray emission is due to a hot corona intercepting roughly 10% of the soft emission. These results are remarkably similar to those generally found in radio-quiet Seyferts, thus suggesting a common accretion mechanism.",
"date": "2018-08-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "478",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2663-2675",
"id_number": "CaltechAUTHORS:20180517-185733548",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180517-185733548",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty1258",
"primary_object": {
"basename": "1805.06229.pdf",
"url": "https://authors.library.caltech.edu/records/hq7ke-vzk64/files/1805.06229.pdf"
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"pub_year": "2018",
"author_list": "Ursini, F.; Petrucci, P.-O.; et el."
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"id": "Walton-D-J",
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"given": "M. J."
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"family": "Pinto",
"given": "C."
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"name": {
"family": "Rana",
"given": "V."
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"orcid": "0000-0003-1703-8796"
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"name": {
"family": "Tramper",
"given": "F."
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"family": "Webb",
"given": "N."
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"family": "Kretschmar",
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"title": "A tale of two periods: determination of the orbital ephemeris of the super-Eddington pulsar NGC 7793 P13",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron / X-rays: binaries / techniques: radial velocities / accretion / accretion disks / pulsars: individual: NGC 7793 P13",
"note": "\u00a9 ESO 2018. \n\nReceived 24 April 2018 / Accepted 17 May 2018. \n\nWe would like to thank the referee for the very helpful comments that helped to improve the manuscript. We thank M. K\u00fchnel and M. Nowak for the useful discussions. DJW and MJM acknowledge support from STFC Ernest Rutherford fellowships. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the nustardas software package, jointly developed by ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. This work has made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and also of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/).\n\nPublished - aa33292-18.pdf
Accepted Version - 1805.05336.pdf
",
"abstract": "We present a timing analysis of multiple XMM-Newton and NuSTAR observations of the ultra-luminous pulsar NGC 7793 P13 spread over its 65 d variability period. We use the measured pulse periods to determine the orbital ephemeris, confirm a long orbital period with P_(orb) = 63.9^(+0.5)_(\u22120.6) d, and find an eccentricity of e \u2264 0.15. The orbital signature is imprinted on top of a secular spin-up, which seems to get faster as the source becomes brighter. We also analyze data from dense monitoring of the source with Swift and find an optical photometric period of 63.9 \u00b1 0.5 d and an X-ray flux period of 66.8 \u00b1 0.4 d. The optical period is consistent with the orbital period, while the X-ray flux period is significantly longer. We discuss possible reasons for this discrepancy, which could be due to a super-orbital period caused by a precessing accretion disk or an orbital resonance. We put the orbital period of P13 into context with the orbital periods implied for two other ultra-luminous pulsars, M82 X-2 and NGC 5907 ULX, and discuss possible implications for the system parameters.",
"date": "2018-08",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "616",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A186",
"id_number": "CaltechAUTHORS:20180517-190441870",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180517-190441870",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
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"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
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{
"id": "Astronomy-Department"
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]
},
"doi": "10.1051/0004-6361/201833292",
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"pub_year": "2018",
"author_list": "F\u00fcrst, F.; Walton, D. J.; et el."
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"items": [
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"id": "Troja-E",
"name": {
"family": "Troja",
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{
"id": "Piro-L",
"name": {
"family": "Piro",
"given": "L."
}
},
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"id": "Ryan-G",
"name": {
"family": "Ryan",
"given": "G."
}
},
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"id": "van-Eerten-H",
"name": {
"family": "van Eerten",
"given": "H."
}
},
{
"id": "Ricci-R",
"name": {
"family": "Ricci",
"given": "R."
}
},
{
"id": "Wieringa-M",
"name": {
"family": "Wieringa",
"given": "M."
}
},
{
"id": "Lotti-S",
"name": {
"family": "Lotti",
"given": "S."
},
"orcid": "0000-0002-3088-1561"
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{
"id": "Sakamoto-Takeshi",
"name": {
"family": "Sakamoto",
"given": "T."
}
},
{
"id": "Cenko-S-B",
"name": {
"family": "Cenko",
"given": "S. B."
},
"orcid": "0000-0003-1673-970X"
}
]
},
"title": "The outflow structure of GW170817 from late-time broad-band observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "gravitational waves \u2013 gamma-ray burst: general \u2013 gamma-ray burst.",
"note": "\u00a9 The Author(s) 2018. Published by Oxford University Press on behalf of The Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nAccepted 2018 April 4. Received 2018 March 19; in original form 2018 January 18. Published: 13 April 2018. \n\nFor their support to these observations we thank B. Wilkes and the Chandra staff, J. Stevens and the CSIRO staff. Support for this work was partially provided by the National Aeronautics and Space Administration through grants issued by the Chandra X-ray Observatory Center and by the Space Telescope Science Insitute. This work was partially supported by the European Union Horizon 2020 Programme under the AHEAD project.\n\nPublished - sly061.pdf
Submitted - 1801.06516.pdf
Supplemental Material - sly061_supp.zip
",
"abstract": "We present our broad-band study of GW170817 from radio to hard X-rays, including NuSTAR and Chandra observations up to 165\u2009 d after the merger, and a multimessenger analysis including LIGO constraints. The data are compared with predictions from a wide range of models, providing the first detailed comparison between non-trivial cocoon and jet models. Homogeneous and power-law shaped jets, as well as simple cocoon models are ruled out by the data, while both a Gaussian shaped jet and a cocoon with energy injection can describe the current data set for a reasonable range of physical parameters, consistent with the typical values derived from short GRB afterglows. We propose that these models can be unambiguously discriminated by future observations measuring the post-peak behaviour, with F_\u03bd \u221d t^(\u223c\u22121.0) for the cocoon and F_\u03bd\u221d t^(\u223c\u22122.5) for the jet model.",
"date": "2018-07-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "478",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L18-L23",
"id_number": "CaltechAUTHORS:20180123-131751240",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180123-131751240",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/sly061",
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"pub_year": "2018",
"author_list": "Troja, E.; Piro, L.; et el."
},
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"datestamp": "2023-08-19 10:32:29",
"lastmod": "2023-10-18 19:12:11",
"type": "article",
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"creators": {
"items": [
{
"id": "Jaisawal-G-K",
"name": {
"family": "Jaisawal",
"given": "Gaurava K."
},
"orcid": "0000-0002-6789-2723"
},
{
"id": "Naik-S",
"name": {
"family": "Naik",
"given": "Sachindra"
},
"orcid": "0000-0003-2865-4666"
},
{
"id": "Gupta-Shivangi",
"name": {
"family": "Gupta",
"given": "Shivangi"
}
},
{
"id": "Chnevez-J",
"name": {
"family": "Chenevez",
"given": "J\u00e9r\u00f4me"
}
},
{
"id": "Epili-P",
"name": {
"family": "Epili",
"given": "Prahlad"
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},
"title": "A curious case of the accretion-powered X-ray pulsar GX 1+4",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron, pulsars: individual: GX 1+4, X-rays: stars",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2018 April 24. Received 2018 April 24; in original form 2017 November 2. Published: 26 April 2018. \n\nWe sincerely thank the referee for suggestions on the paper. GKJ thanks C. Ferrigno and M. Wolff for discussions on the physical models. The research work at Physical Research Laboratory is funded by the Department of Space, Government of India. The research leading to these results has received funding from the European Union's Seventh Framework Programme and Horizon 2020 Research and Innovation Programme under the Marie Sk\u0142odowska-Curie Actions grant no. 609405 (FP7) and 713683 (H2020; COFUNDPostdocDTU). This research has made use of data obtained through HEASARC Online Service, provided by the NASA/GSFC, in support of NASA High Energy Astrophysics Programs.\n\nSubmitted - 1804.08989.pdf
",
"abstract": "We present detailed spectral and timing studies using a NuSTAR observation of GX 1+4 in 2015 October during an intermediate-intensity state. The measured spin period of 176.778 s is found to be one of the highest values since its discovery. In contrast to a broad sinusoidal-like pulse profile, a peculiar sharp peak is observed in profiles below \u223c25 keV. The profiles at higher energies are found to be significantly phase shifted compared to the soft X-ray profiles. Broad-band energy spectra of GX 1+4, obtained from NuSTAR and Swiftobservations, are described with various continuum models. Among these, a two-component model consisting of a bremsstrahlung and a blackbody component is found to best fit the phase-averaged and phase-resolved spectra. Physical models are also used to investigate the emission mechanism in the pulsar, which allows us to estimate the magnetic field strength to be in \u223c(5\u201310) \u00d7 10^(12) G range. Phase-resolved spectroscopy of NuSTAR observation shows a strong blackbody emission component in a narrow pulse phase range. This component is interpreted as the origin of the peculiar peak in the pulse profiles below \u226425 keV. The size of emitting region is calculated to be \u223c400 m. The bremsstrahlung component is found to dominate in hard X-rays and explains the nature of simple profiles at high energies.",
"date": "2018-07-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "478",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "448-459",
"id_number": "CaltechAUTHORS:20180425-093642490",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180425-093642490",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
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"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty1049",
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"pub_year": "2018",
"author_list": "Jaisawal, Gaurava K.; Naik, Sachindra; et el."
},
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{
"id": "Lazzarini-M",
"name": {
"family": "Lazzarini",
"given": "M."
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},
{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "A. E."
},
"orcid": "0000-0001-8667-2681"
},
{
"id": "Williams-B-F",
"name": {
"family": "Williams",
"given": "B. F."
},
"orcid": "0000-0002-7502-0597"
},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "D."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Vulic-N",
"name": {
"family": "Vulic",
"given": "N."
},
"orcid": "0000-0001-7855-8336"
},
{
"id": "Yukita-Mihoko",
"name": {
"family": "Yukita",
"given": "M."
},
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},
{
"id": "Zezas-A",
"name": {
"family": "Zezas",
"given": "A."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Lewis-A-R",
"name": {
"family": "Lewis",
"given": "A. R."
},
"orcid": "0000-0002-5238-0282"
},
{
"id": "Durbin-M",
"name": {
"family": "Durbin",
"given": "M."
}
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Bodaghee-A",
"name": {
"family": "Bodaghee",
"given": "A."
},
"orcid": "0000-0002-7315-3732"
},
{
"id": "Lehmer-B-D",
"name": {
"family": "Lehmer",
"given": "B. D."
},
"orcid": "0000-0003-2192-3296"
},
{
"id": "Antoniou-V",
"name": {
"family": "Antoniou",
"given": "V."
},
"orcid": "0000-0001-7539-1593"
},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T."
},
"orcid": "0000-0003-0976-4755"
}
]
},
"title": "Young Accreting Compact Objects in M31: The Combined Power of NuSTAR, Chandra, and Hubble",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: individual (M31) \u2013 pulsars: general \u2013 stars: black holes \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: galaxies",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 March 19; revised 2018 May 31; accepted 2018 June 5; published 2018 July 19. \n\nWe thank Antara Basu-Zych for useful discussions that led to an improvement of the paper. We acknowledge funding through Chandra program award GO5-17077Z (PI Hornschemeier). Support for this work was provided in part by Chandra Award Number GO5-16085X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060.\n\nSubmitted - 1806.03305.pdf
",
"abstract": "We present 15 high-mass X-ray binary (HMXB) candidates in the disk of M31 for which we are able to infer compact object type, spectral type of the donor star, and age using multiwavelength observations from NuSTAR, Chandra, and the Hubble Space Telescope. The hard X-ray colors and luminosities from NuSTAR permit the tentative classification of accreting X-ray binary systems by compact object type, distinguishing black hole from neutron star systems. We find hard-state black holes, pulsars, and non-magnetized neutron stars associated with optical point-source counterparts with similar frequency. We also find nine non-magnetized neutron stars coincident with globular clusters and an equal number of pulsars with and without point-source optical counterparts. We perform spectral energy distribution (SED) fitting for the most likely optical counterparts to the HMXB candidates, finding seven likely high-mass stars and one possible red helium-burning star. The remaining seven HMXB optical counterparts have poor SED fits, so their companion stars remain unclassified. Using published star formation histories, we find that the majority of HMXB candidates\u2014X-ray sources with UV-bright point-source optical counterpart candidates\u2014are found in regions with star formation bursts less than 50 Myr ago, and three are associated with young stellar ages (<10 Myr). This is consistent with similar studies of HMXB populations in the Magellanic Clouds, M33, NGC 300, and NGC 2403.",
"date": "2018-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "862",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 28",
"id_number": "CaltechAUTHORS:20180613-100106697",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180613-100106697",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aacb2a",
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"pub_year": "2018",
"author_list": "Lazzarini, M.; Hornschemeier, A. E.; et el."
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{
"id": "Jiang-Junle",
"name": {
"family": "Jiang",
"given": "J."
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{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
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"orcid": "0000-0002-8466-7317"
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
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{
"id": "Alston-W-N",
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{
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"given": "D. J. K."
}
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{
"id": "Cackett-E-M",
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"family": "Cackett",
"given": "E. M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Chiang-Chia-Ying",
"name": {
"family": "Chiang",
"given": "C.-Y."
},
"orcid": "0000-0002-9630-4003"
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Gallo-L-C",
"name": {
"family": "Gallo",
"given": "L. C."
}
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
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"given": "J. A."
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"id": "Harrison-F-A",
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"family": "Harrison",
"given": "F. A."
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"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
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"family": "De Marco",
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"id": "Miller-J-M",
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"id": "Miniutti-G",
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{
"id": "Pinto-C",
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"family": "Pinto",
"given": "C."
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},
"title": "The 1.5\u2009Ms observing campaign on IRAS 13224\u22123809 \u2013 I. X-ray spectral analysis",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs\u2009\u2013\u2009black hole physics, galaxies: Seyfert, X-rays: galaxies",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices) \n\nAccepted 2018 March 28. Received 2018 March 1; in original form 2017 September 11. \n\nJ.J. acknowledges support by the Cambridge Trust and the Chinese Scholarship Council Joint Scholarship Programme (201604100032). A.C.F., M.L.P., and C.P. acknowledge support by the ERC Advanced Grant 340442. B.D.M. acknowledges support by the Polish National Science Center grant Polonez 2016/21/P/ST9/04025. W.N.A. acknowledges support from the European Union Seventh Framework Program (FP7/2013\u20132017) under grant agreement no. 312789, StrongGravity. G.M. acknowledges support from the European Union Seventh Framework Program (FP7/2007\u20132013) under grant agreement no. 312789, StrongGravity and the Spanish grant ESP2015-65597-C4-1-R. D.J.K.B. is supported by the Science and Technology Facilities Council (STFC). J.A.G. acknowledges the support from the Alexander von Humboldt Foundation. D.R.W. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF6-170160, awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. D.J.W. acknowledges support from an STFC Ernest Rutherford fellowship. Based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This project has made use of the Science Analysis Software (SAS), an extensive suite to process the data collected by the XMM\u2013Newton observatory. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology.\n\nPublished - sty836.pdf
Accepted Version - 1804.00349
",
"abstract": "We present a detailed spectral analysis of the recent 1.5\u2009Ms XMM\u2013Newton observing campaign on the narrow-line Seyfert 1 galaxy IRAS 13224\u22123809, taken simultaneously with 500\u2009ks of NuSTAR data. The X-ray light curve shows three flux peaks, registering at about 100 times the minimum flux seen during the campaign, and rapid variability with a time-scale of kiloseconds. The spectra are well fit with a primary power-law continuum, two relativistic-blurred reflection components from the inner accretion disc with very high iron abundance, and a simple blackbody-shaped model for the remaining soft excess. The spectral variability is dominated by the power-law continuum from a corona region within a few gravitational radii from the black hole. Additionally, blueshifted Ne\u2009X, Mg\u2009XII, Si\u2009XIV, and S\u2009XVI absorption lines are identified in the stacked low-flux spectrum, confirming the presence of a highly ionized outflow with velocity up to v = 0.267 and 0.225\u2009c. We fit the absorption features with xstar models and find a relatively constant velocity outflow through the whole observation. Finally, we replace the bbody and supersolar abundance reflection models by fitting the soft excess successfully with the extended reflection model relxillD, which allows for higher densities than the standard relxill model. This returns a disc electron density n_e > 10^(18.7)\u2009cm^(\u22123) and lowers the iron abundance from Z_(Fe) = 24^(+3)_(\u22124)Z_\u2299 with n-e = 10^(15) cm^(-3) to Z_(Fe) = 6.6^(+0.8)_(-2.1)Z_\u2299.",
"date": "2018-07-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "477",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3711-3726",
"id_number": "CaltechAUTHORS:20180620-154958509",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180620-154958509",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Cambridge Overseas Trust"
},
{
"agency": "Chinese Scholarship Council",
"grant_number": "201604100032"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "National Science Centre (Poland)",
"grant_number": "2016/21/P/ST9/04025"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)",
"grant_number": "ESP2015-65597-C4-1-R"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF6-170160"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/sty836",
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"pub_year": "2018",
"author_list": "Jiang, J.; Parker, M. L.; et el."
},
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"items": [
{
"id": "Brumback-M-C",
"name": {
"family": "Brumback",
"given": "McKinley C."
},
"orcid": "0000-0002-4024-6967"
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "Ryan C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Ballhausen-R",
"name": {
"family": "Ballhausen",
"given": "Ralf"
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix S."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Pike-S-N",
"name": {
"family": "Pike",
"given": "Sean"
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Discovery of Pulsation Dropout and Turn-on during the High State of the Accreting X-Ray Pulsar LMC X-4",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (LMC X-4) \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 April 26; revised 2018 June 11; accepted 2018 June 16; published 2018 June 28. \n\nWe would like to thank the anonymous referee for comments that substantially improved this Letter. We would also like to thank the NuSTAR Galactic Binaries Science Team for comments and contributions. M.C.B. acknowledges support from NASA grant Nos. NNX15AV32G and NNX15AH79H. This research made use of NuSTARDAS, developed by ASDC (Italy) and Caltech (USA) and of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/).\n\nPublished - Brumback_2018_ApJL_861_L7.pdf
Accepted Version - 1806.09630.pdf
",
"abstract": "Two Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the luminous X-ray pulsar LMC X-4 in 2015 October and November captured several bright accretion flares from this source, which has a long history of stable pulse and superorbital behavior. We present a timing analysis of these data in which we detect a rapid pulse \"turn-on\" in association with the accretion flares, during which the source reaches super-Eddington luminosities. Pulsations, which are normally seen from this source, are found to only occur for approximately one hour before and during the bright flares. Beyond one hour before and after the flares, we find pulsations to be weak or nonexistent, with fractional rms amplitudes of less than 0.05. At the onset of the flare, the pulse profiles exhibit a phase shift of 0.25 cycles that could be associated with a change in the emission geometry. This increase in pulse strength occurring well before the flare cannot be explained by the propeller effect, and potentially offers a connection between the magnetic properties of pulsars that accrete close to their Eddington limits and ultra-luminous X-ray pulsars.",
"date": "2018-07-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "861",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L7",
"id_number": "CaltechAUTHORS:20180627-093050466",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180627-093050466",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AV32G"
},
{
"agency": "NASA",
"grant_number": "NNX15AH79H"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8213/aacd13",
"primary_object": {
"basename": "1806.09630.pdf",
"url": "https://authors.library.caltech.edu/records/9rynd-vk473/files/1806.09630.pdf"
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"basename": "Brumback_2018_ApJL_861_L7.pdf",
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}
],
"pub_year": "2018",
"author_list": "Brumback, McKinley C.; Hickox, Ryan C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/5888w-52f34",
"eprint_id": 87283,
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"datestamp": "2023-08-19 10:09:54",
"lastmod": "2023-10-18 21:00:49",
"type": "article",
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"creators": {
"items": [
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "Peter G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona"
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
}
]
},
"title": "An Iwasawa-Taniguchi Effect for Compton-thick Active Galactic Nuclei",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 infrared: galaxies \u2013X-rays: galaxies",
"note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices) \n\nAccepted 2018 March 29. Received 2018 March 29; in original form 2017 September 28. \n\nWe thank the anonymous referee for invaluable comments on the paper. \n\nP. B. and P. G. (grant reference ST/J003697/2) thank the STFC for support. In addition, the authors thank R. Gilli and C. Circosta for providing the 4 and \u20097 Msspectra of LESS J0033229.4-275619 used in Fig. 2. \n\nThis work was supported in part by the Black Hole Initiative at Harvard University, which is funded by a grant from the John Templeton Foundation. \n\nM. B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. \n\nWe acknowledge financial support from FONDECYT 1141218 (C. R.), Basal-CATA PFB\u201306/2007 (C. R.), the China-CONICYT fund (C. R.). This work is partly sponsored by the Chinese Academy of Sciences (CAS), through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile. \n\nThe scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. \n\nThis research has made use of data, software and/or web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. \n\nThis research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nThis work is based [in part] on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. \n\nThis publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work made use of the NUMPY (Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), SCIPY(Jones et al. 2001), PANDAS (McKinney2010), ASTROPY (Astropy Collaboration 2013) and ADJUSTTEXT12 Python packages. \n\nP. B. would also like to thank S. H\u00f6nig, C. Knigge, J. Matthews, M. Middleton, M. Smith, A. Beri, A. Hill, J. Buchner and others for vital scientific discussions into the data analysis and interpretations of the Compton-thick Iwasawa-Taniguchi effect.\n\nPublished - sty861.pdf
Accepted Version - 1804.01100
Supplemental Material - sty861_supp.pdf
",
"abstract": "We present the first study of an Iwasawa\u2013Taniguchi/'X-ray Baldwin' effect for Compton-thick active galactic nuclei (AGN). We report a statistically significant anticorrelation between the rest-frame equivalent width (EW) of the narrow core of the neutral Fe\u2009K\u03b1 fluorescence emission line, ubiquitously observed in the reflection spectra of obscured AGN, and the mid-infrared 12\u03bcm continuum luminosity (taken as a proxy for the bolometric AGN luminosity). Our sample consists of 72 Compton-thick AGN selected from pointed and deep-field observations covering a redshift range of z \u223c 0.0014\u22123.7. We employ a Monte Carlo-based fitting method, which returns a Spearman's Rank correlation coefficient of \u03c1\u2009= \u2009\u2212 0.28 \u00b1 0.12, significant to 98.7\u2009per\u2009cent confidence. The best-fitting found is \nlog(EW_(FeK\u03b1)) \u221d \u22120.08 \u00b1 0.04log(L_(12\u03bcm)), which is consistent with multiple studies of the X-ray Baldwin effect for unobscured and mildly obscured AGN. This is an unexpected result, as the Fe\u2009K\u03b1 line is conventionally thought to originate from the same region as the underlying reflection continuum, which together constitute the reflection spectrum. We discuss the implications this could have if confirmed on larger samples, including a systematic underestimation of the line-of-sight X-ray obscuring column density and hence the intrinsic luminosities and growth rates for the most luminous AGN.",
"date": "2018-07-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "477",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3775-3790",
"id_number": "CaltechAUTHORS:20180620-160311395",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180620-160311395",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "John Templeton Foundation"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB\u201306/2007"
},
{
"agency": "China-CONICYT fund"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)"
},
{
"agency": "Chinese Academy of Sciences"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
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"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/sty861",
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"pub_year": "2018",
"author_list": "Boorman, Peter G.; Gandhi, Poshak; et el."
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"datestamp": "2023-08-19 09:57:10",
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"items": [
{
"id": "Middei-R",
"name": {
"family": "Middei",
"given": "R."
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{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Cappi-M",
"name": {
"family": "Cappi",
"given": "M."
}
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{
"id": "Petrucci-P-O",
"name": {
"family": "Petrucci",
"given": "P.-O."
}
},
{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
}
},
{
"id": "Arav-N",
"name": {
"family": "Arav",
"given": "N."
}
},
{
"id": "Behar-E",
"name": {
"family": "Behar",
"given": "E."
}
},
{
"id": "Branduardi-Raymont-G",
"name": {
"family": "Branduardi-Raymont",
"given": "G."
}
},
{
"id": "Costantini-E",
"name": {
"family": "Costantini",
"given": "E."
}
},
{
"id": "De-Marco-B",
"name": {
"family": "De Marco",
"given": "B."
}
},
{
"id": "Di-Gesu-L",
"name": {
"family": "Di Gesu",
"given": "L."
}
},
{
"id": "Ebrero-J",
"name": {
"family": "Ebrero",
"given": "J."
},
"orcid": "0000-0001-5924-8818"
},
{
"id": "Kaastra-J-S",
"name": {
"family": "Kaastra",
"given": "J."
},
"orcid": "0000-0001-5540-2822"
},
{
"id": "Kaspi-S",
"name": {
"family": "Kaspi",
"given": "S."
}
},
{
"id": "Kriss-G-A",
"name": {
"family": "Kriss",
"given": "G. A."
}
},
{
"id": "Mao-Jiajing",
"name": {
"family": "Mao",
"given": "J."
}
},
{
"id": "Mehdipour-M",
"name": {
"family": "Mehdipour",
"given": "M."
}
},
{
"id": "Paltani-S",
"name": {
"family": "Paltani",
"given": "S."
},
"orcid": "0000-0002-8108-9179"
},
{
"id": "Peretz-U",
"name": {
"family": "Peretz",
"given": "U."
}
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "G."
},
"orcid": "0000-0003-0293-3608"
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]
},
"title": "Multi-wavelength campaign on NGC 7469. IV. The broad-band X-ray spectrum",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 quasars: general \u2013 X-rays: galaxies",
"note": "\u00a9 2018 ESO. Article published by EDP Sciences. \n\nReceived: 29 January 2018; Accepted: 19 March 2018. Published online 01 August 2018. \n\nWe thank the referee for helping us improve the quality of this paper. This work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the nustardas jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work is also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). RM and SB acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. SB acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0. POP acknowledges financial support from the CNES french agency and the CNRS PNHE. GP acknowledges support by the Bundesministerium f\u00fc r Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luftund Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research.BDM acknowledges support from the Polish National Science Center grant Polonez 2016/21/P/ST9/04025. The research at the Technion is supported by the I-CORE programme of the Planning and Budgeting Committee (grant number 1937/12). EB acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska\u2013Curie grant agreement no. 655324. M.C. acknowledges financial contribution from the agreement ASI-INAF n.2017-14-H.O.\n\nSubmitted - 1803.07334.pdf
",
"abstract": "We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe K\u03b1emission line in all the spectra and weaker contributions from Fe K\u03b2, neutral Ni K\u03b1, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (\u0393 = 1.78 \u00b1 0.02) together with a high energy cut-off E_(cut) = 170_(\u221240)^(+60) keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45_(\u221212)^(+15) keV and, assuming a spherical geometry, an optical depth \u03c4 = 2.6 \u00b1 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3\u22120.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 \u00b1 0.03 keV and a corresponding optical depth \u03c4 = 9.2 \u00b1 0.2.",
"date": "2018-07",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "615",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A163",
"id_number": "CaltechAUTHORS:20180325-184643880",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180325-184643880",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201832726",
"primary_object": {
"basename": "1803.07334.pdf",
"url": "https://authors.library.caltech.edu/records/jydhn-jz108/files/1803.07334.pdf"
},
"pub_year": "2018",
"author_list": "Middei, R.; Bianchi, S.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/zm7zw-k4y77",
"eprint_id": 85555,
"eprint_status": "archive",
"datestamp": "2023-08-19 09:11:05",
"lastmod": "2023-10-18 18:19:25",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Yamada-Satoshi",
"name": {
"family": "Yamada",
"given": "Satoshi"
}
},
{
"id": "Ueda-Yoshihiro",
"name": {
"family": "Ueda",
"given": "Yoshihiro"
},
"orcid": "0000-0001-7821-6715"
},
{
"id": "Oda-Saeko",
"name": {
"family": "Oda",
"given": "Saeko"
}
},
{
"id": "Tanimoto-Atsushi",
"name": {
"family": "Tanimoto",
"given": "Atsushi"
},
"orcid": "0000-0002-0114-5581"
},
{
"id": "Imanishi-Masatoshi",
"name": {
"family": "Imanishi",
"given": "Masatoshi"
},
"orcid": "0000-0001-6186-8792"
},
{
"id": "Terashima-Yuichi",
"name": {
"family": "Terashima",
"given": "Yuichi"
},
"orcid": "0000-0003-1780-5481"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
}
]
},
"title": "Broadband X-ray Spectral Analysis of the Double-Nucleus Luminous Infrared Galaxy Mrk 463",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 galaxies: individual (Mrk 463) \u2013 infrared: galaxies \u2013 X-rays:\ngalaxies",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 January 23; revised 2018 March 19; accepted 2018 March 27; published 2018 May 11. \n\nPart of this work was financially supported by the Grant-in-Aid for Scientific Research 17K05384 (Y.U.), 15K05030 (M.I.), 15H02070, 16K05296 (Y.T.), and for JSPS Fellows for young researchers (A.T.). C.R. acknowledges financial support from the China-CONICYT fellowship, FONDECYT 1141218, and Basal-CATA PFB-06/2007. Support for this work was provided by the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. This research also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and with Chandra, supported by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA.\n\nSubmitted - 1803.11223.pdf
",
"abstract": "We present a broadband (0.4\u201370 keV) X-ray spectral analysis of the luminous infrared galaxy (LIRG) system Mrk 463 observed with Nuclear Spectroscopic Telescope Array (NuSTAR), Chandra, and XMM-Newton, which contains double active galactic nuclei (AGNs; Mrk 463E and Mrk 463W) with a separation of ~3.8 kpc. Detecting their transmitted hard X-ray >10 keV continua with NuSTAR, we confirm that Mrk 463E and Mrk 463W have AGNs with intrinsic luminosities of (1.6\u20132.2) \u00d7 10^(43) and (0.5\u20130.6) \u00d7 10^(43) erg s^(\u22121) (2\u201310 keV) obscured by hydrogen column densities of 8 \u00d7 10^(23) and 3 \u00d7 10^(23) cm^(\u22122), respectively. Both nuclei show strong reflection components from cold matter. The luminosity ratio between X-ray (2\u201310 keV) and [O IV] 25.89 \u03bcm of Mrk 463E is ~5 times smaller than those of normal Seyfert galaxies, suggesting that the intrinsic SED is X-ray weak relative to the UV luminosity. In fact, the bolometric AGN luminosity of Mrk 463E estimated from L'-band (3.8 \u03bcm), [O IV] 25.89 \u03bcm, and [Ne V] 14.32 \u03bcm lines indicate a large bolometric-to-X-ray luminosity ratio, \u03ba_(2\u201310 keV) \u2248 110\u2013410, and a high Eddington ratio, \u03bb_(Edd) ~ 0.4\u20130.8. We suggest that the merger triggered a rapid growth of the black hole in Mrk 463E, which is not yet deeply \"buried\" by circumnuclear dust. By contrast, the L'-band luminosity of Mrk 463W is unusually small relative to the X-ray luminosity, suggesting that the Eddington ratio is low (<10^(\u22123)) and it might be still in an early phase of merger-driven AGN activity.",
"date": "2018-05-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "858",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 106",
"id_number": "CaltechAUTHORS:20180402-090755050",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180402-090755050",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aabacb",
"primary_object": {
"basename": "1803.11223.pdf",
"url": "https://authors.library.caltech.edu/records/zm7zw-k4y77/files/1803.11223.pdf"
},
"pub_year": "2018",
"author_list": "Yamada, Satoshi; Ueda, Yoshihiro; et el."
},
{
"id": "https://authors.library.caltech.edu/records/m4d41-pfx84",
"eprint_id": 85210,
"eprint_status": "archive",
"datestamp": "2023-08-19 09:05:39",
"lastmod": "2023-10-18 17:58:19",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Carpano-S",
"name": {
"family": "Carpano",
"given": "S."
}
},
{
"id": "Haberl-F",
"name": {
"family": "Haberl",
"given": "F."
}
},
{
"id": "Maitra-C",
"name": {
"family": "Maitra",
"given": "C."
}
},
{
"id": "Vasilopoulos-G",
"name": {
"family": "Vasilopoulos",
"given": "G."
}
}
]
},
"title": "Discovery of pulsations from NGC\u2009300\u2009ULX1 and its fast period evolution",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron, pulsars: individual: NGC\u2009300\u2009ULX1\u2013 galaxies: individual: NGC 300, X-rays: binaries",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2018 February 23. Received 2018 February 16; in original form 2018 January 31. Published: 27 February 2018. \n\nThis research has made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and data obtained from the NuSTAR Data Archive. The XMM\u2013Newton project is supported by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ\u200950OG1601) and the Max Planck Society.\n\nSubmitted - 1802.10341.pdf
",
"abstract": "The supernova impostor SN 2010da located in the nearby galaxy NGC 300, later identified as a likely supergiant B[e] high-mass X-ray binary, was simultaneously observed by NuSTAR and XMM\u2013Newton between 2016 December 16 and 20, over a total time span of \u223c310\u2009ks. We report the discovery of a strong periodic modulation in the X-ray flux with a pulse period of 31.6\u2009s and a very rapid spin-up, and confirm therefore that the compact object is a neutron star. We find that the spin period is changing from 31.71\u2009s to 31.54\u2009s over that period, with a spin-up rate of \u22125.56 \u00d7 10^(\u22127)\u2009s\u2009s^(\u22121), likely the largest ever observed from an accreting neutron star. The spectrum is described by a power-law and a disc blackbody model, leading to a 0.3\u201330\u2009keV unabsorbed luminosity of 4.7 \u00d7 10^(39)\u2009erg\u2009s^(\u22121). Applying our best-fitting model successfully to the spectra of an XMM\u2013Newton observation from 2010, suggests that the lower fluxes of NGC\u2009300\u2009ULX1 reported from observations around that time are caused by a large amount of absorption, while the intrinsic luminosity was similar as seen in 2016. A more constant luminosity level is also consistent with the long-term pulse period evolution approaching an equilibrium value asymptotically. We conclude that the source is another candidate for the new class of ultraluminous X-ray pulsars.",
"date": "2018-05-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "476",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L45-L49",
"id_number": "CaltechAUTHORS:20180308-140547917",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180308-140547917",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/sly030",
"primary_object": {
"basename": "1802.10341.pdf",
"url": "https://authors.library.caltech.edu/records/m4d41-pfx84/files/1802.10341.pdf"
},
"pub_year": "2018",
"author_list": "Carpano, S.; Haberl, F.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/hntsh-s9v29",
"eprint_id": 84710,
"eprint_status": "archive",
"datestamp": "2023-08-19 09:05:16",
"lastmod": "2023-10-18 16:38:07",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Turner-T-J",
"name": {
"family": "Turner",
"given": "T. J."
},
"orcid": "0000-0003-2971-1722"
},
{
"id": "Reeves-J-N",
"name": {
"family": "Reeves",
"given": "J. N."
}
},
{
"id": "Braito-V",
"name": {
"family": "Braito",
"given": "V."
},
"orcid": "0000-0002-2629-4989"
},
{
"id": "Costa-M",
"name": {
"family": "Costa",
"given": "M."
}
}
]
},
"title": "On the Nature of the High-Energy Rollover in 1H 0419-577",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 quasars: individual: 1H 0419-577 \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2018 February 2. Received 2018 February 1; in original form 2017 September 15. Published: 09 February 2018. \n\nTJT acknowledges NASA grant NNH13CH63C. JNR acknowledges NASA grant NNX15AV18G. We are grateful to the NuSTAR operations team for performing this observation and providing software and calibration for the data analysis. We thank the anonymous referee for comments which improved this manuscript. This research has also made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center and from the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.\n\nAccepted Version - 1802.00795.pdf
",
"abstract": "A NuSTAR/Swift observation of the luminous Seyfert 1 galaxy 1H 0419-577 taken during 2015 reveals one of the most extreme high-energy cut-offs observed to date from an AGN \u2013 an origin due to thermal Comptonization would imply a remarkably low coronal temperature kT \u223c 15\u2009keV. The low-energy peak of the spectrum in the hard X-ray NuSTAR band, which peaks before the expected onset of a Compton hump, rules out strong reflection as the origin of the hard excess in this AGN. We show the origin of the high-energy rollover is likely due to a combination of both thermal Comptonization and an intrinsically steeper continuum, which is modified by absorption at lower energies. Furthermore, modelling the broad-band XUV continuum shape as a colour-corrected accretion disc, requires the presence of a variable warm absorber to explain all flux and spectral states of the source, consistent with the previous work on this AGN. While absorber variations produce marked spectral variability in this AGN, consideration of all flux states allows us to isolate a colourless component of variability that may arise from changes in the inner accretion flow, typically at around 10\u2009r_g.",
"date": "2018-05-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "476",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "1258-1270",
"id_number": "CaltechAUTHORS:20180207-091935800",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-091935800",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/sty318",
"primary_object": {
"basename": "1802.00795.pdf",
"url": "https://authors.library.caltech.edu/records/hntsh-s9v29/files/1802.00795.pdf"
},
"pub_year": "2018",
"author_list": "Turner, T. J.; Reeves, J. N.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/n0xy6-hxk04",
"eprint_id": 81958,
"eprint_status": "archive",
"datestamp": "2023-08-19 08:55:57",
"lastmod": "2023-10-17 21:57:25",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Huppenkothen-D",
"name": {
"family": "Huppenkothen",
"given": "D."
},
"orcid": "0000-0002-1169-7486"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
}
]
},
"title": "On the Statistical Properties of Cospectra",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "methods: data analysis \u2013 methods: statistical \u2013 X-rays: general",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 September 27; revised 2018 January 16; accepted 2018 January 16; published 2018 May 11. \n\nThe authors thank the anonymous referee for their helpful comments. The authors also thank Thomas Laetsch for helpful suggestions regarding the mathematical derivations, and Peter Bult for spotting a mathematical error. D.H. is supported by the James Arthur Postdoctoral Fellowship and the Moore-Sloan Data Science Environment at New York University. D.H. acknowledges support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. M.B. is supported in part by the Italian Space Agency through agreement ASI-INAF n.2017-12-H.0 and ASI-INFN agreement n.2017-13-H.0.\n\nSubmitted - 1709.09666.pdf
",
"abstract": "In recent years, the cross-spectrum has received considerable attention as a means of characterizing the variability of astronomical sources as a function of wavelength. The cospectrum has only recently been understood as a means of mitigating instrumental effects dependent on temporal frequency in astronomical detectors, as well as a method of characterizing the coherent variability in two wavelength ranges on different timescales. In this paper, we lay out the statistical foundations of the cospectrum, starting with the simplest case of detecting a periodic signal in the presence of white noise, under the assumption that the same source is observed simultaneously in independent detectors in the same energy range. This case is especially relevant for detecting faint X-ray pulsars in detectors heavily affected by instrumental effects, including NuSTAR, Astrosat, and IXPE, which allow for even sampling and where the cospectrum can act as an effective way to mitigate dead time. We show that the statistical distributions of both single and averaged cospectra differ considerably from those for standard periodograms. While a single cospectrum follows a Laplace distribution exactly, averaged cospectra are approximated by a Gaussian distribution only for more than ~30 averaged segments, dependent on the number of trials. We provide an instructive example of a quasi-periodic oscillation in NuSTAR and show that applying standard periodogram statistics leads to underestimated tail probabilities for period detection. We also demonstrate the application of these distributions to a NuSTAR observation of the X-ray pulsar Hercules X-1.",
"date": "2018-05",
"date_type": "published",
"publication": "Astrophysical Journal Supplement Series",
"volume": "236",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 13",
"id_number": "CaltechAUTHORS:20171002-134855167",
"issn": "1538-4365",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171002-134855167",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4365/aabe38",
"primary_object": {
"basename": "1709.09666.pdf",
"url": "https://authors.library.caltech.edu/records/n0xy6-hxk04/files/1709.09666.pdf"
},
"pub_year": "2018",
"author_list": "Huppenkothen, D. and Bachetti, M."
},
{
"id": "https://authors.library.caltech.edu/records/av3yr-mdj98",
"eprint_id": 85431,
"eprint_status": "archive",
"datestamp": "2023-08-21 23:09:16",
"lastmod": "2023-10-18 18:13:24",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Heida-M",
"name": {
"family": "Heida",
"given": "M."
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Kennea-J-A",
"name": {
"family": "Kennea",
"given": "J."
},
"orcid": "0000-0002-6745-4790"
},
{
"id": "Kosec-P",
"name": {
"family": "Kosec",
"given": "P."
}
},
{
"id": "Lau-Ryan-M",
"name": {
"family": "Lau",
"given": "R. M."
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "J. F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Webb-N-A",
"name": {
"family": "Webb",
"given": "N."
}
}
]
},
"title": "A Potential Cyclotron Resonant Scattering Feature in the Ultraluminous X-Ray Source Pulsar NGC 300 ULX1 Seen by NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron; X-rays: binaries; X-rays: individual (NGC 300 ULX1)",
"note": "\u00a9 2018. The American Astronomical Society. Received 2018 March 20; revised 2018 March 27; accepted 2018 March 29; published 2018 April 9. The authors would like to thank the reviewer for timely and positive feedback. D.J.W. and M.J.M. acknowledge support from STFC Ernest Rutherford fellowships. A.C.F. acknowledges ERC Advanced Grant 340442, P.K. acknowledges support from the STFC, and D.B. acknowledges support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This work has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. Facilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM - Newton X-Ray Multimirror Mission satellite.\n\nPublished - Walton_2018_ApJL_857_L3.pdf
Submitted - 1803.07571.pdf
",
"abstract": "Based on phase-resolved broadband spectroscopy using XMM-Newton and NuSTAR, we report on a potential cyclotron resonant scattering feature (CRSF) at E ~ 13 keV in the pulsed spectrum of the recently discovered ultraluminous X-ray source (ULX) pulsar NGC 300 ULX1. If this interpretation is correct, the implied magnetic field of the central neutron star is B ~ 1012 G (assuming scattering by electrons), similar to that estimated from the observed spin-up of the star, and also similar to known Galactic X-ray pulsars. We discuss the implications of this result for the connection between NGC 300 ULX1 and the other known ULX pulsars, particularly in light of the recent discovery of a likely proton cyclotron line in another ULX, M51 ULX-8.",
"date": "2018-04-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "857",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L3",
"id_number": "CaltechAUTHORS:20180325-185226577",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180325-185226577",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
}
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"doi": "10.3847/2041-8213/aabadc",
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"pub_year": "2018",
"author_list": "Walton, D. J.; Bachetti, M.; et el."
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"id": "Walton-D-J",
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"family": "Walton",
"given": "D. J."
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"family": "F\u00fcrst",
"given": "F."
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{
"id": "Heida-M",
"name": {
"family": "Heida",
"given": "M."
},
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{
"id": "Harrison-F-A",
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"family": "Harrison",
"given": "F. A."
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"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
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{
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"family": "Stern",
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{
"id": "Bachetti-M",
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"family": "Bachetti",
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"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
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{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
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},
"title": "Evidence for Pulsar-like Emission Components in the Broadband ULX Sample",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual (NGC 5907 ULX)",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 February 1; revised 2018 March 2; accepted 2018 March 8; published 2018 April 2. \n\nThe authors would like to thank the reviewer for positive feedback which helped to improve the final manuscript. D.J.W. and M.J.M. acknowledge support from STFC Ernest Rutherford fellowships, A.C.F. acknowledges support from ERC Advanced Grant 340442, and D.B. acknowledges financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This work has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, and with Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM - Newton X-Ray Multimirror Mission satellite, Suzaku - Suzaku (ASTRO-EII).\n\nPublished - Walton_2018_ApJ_856_128.pdf
Submitted - 1803.04424.pdf
",
"abstract": "We present broadband X-ray analyses of a sample of bright ultraluminous X-ray sources (ULX) with the goal of investigating the spectral similarity of this population to the known ULX pulsars, M82 X-2, NGC 7793 P13, and NGC 5907 ULX. We perform a phase-resolved analysis of the broadband XMM-Newton+NuSTAR data set of NGC 5907 ULX, finding that the pulsed emission from the accretion column in this source exhibits a similar spectral shape to that seen in both M82 X-2 and NGC 7793 P13, and that this is responsible for the excess emission observed at the highest energies when the spectra are fit with accretion disk models. We then demonstrate that similar \"hard\" excesses are seen in all ULXs in the broadband sample. Finally, for ULXs where the nature of the accretor is currently unknown, we test whether the hard excesses are all consistent with being produced by an accretion column similar to those present in M82 X-2, NGC 7793 P13, and NGC 5907 ULX. Based on the average shape of the pulsed emission, we find that in all cases a similar accretion column can successfully reproduce the observed data, consistent with the hypothesis that this ULX sample may be dominated by neutron star accretors. Compared to the known pulsar ULXs, our spectral fits for the remaining ULXs suggest that the non-pulsed emission from the accretion flow beyond the magnetosphere makes a stronger relative contribution than the component associated with the accretion column. If these sources do also contain neutron star accretors, this may help to explain the lack of detected pulsations.",
"date": "2018-04-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "856",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 128",
"id_number": "CaltechAUTHORS:20180315-091957565",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180315-091957565",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
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"id": "NuSTAR"
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"doi": "10.3847/1538-4357/aab610",
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"pub_year": "2018",
"author_list": "Walton, D. J.; F\u00fcrst, F.; et el."
},
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"items": [
{
"id": "Kuhar-M",
"name": {
"family": "Kuhar",
"given": "Matej"
},
"orcid": "0000-0002-7210-180X"
},
{
"id": "Krucker-S",
"name": {
"family": "Krucker",
"given": "S\u00e4m"
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{
"id": "Glesener-L",
"name": {
"family": "Glesener",
"given": "Lindsay"
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"orcid": "0000-0001-7092-2703"
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{
"id": "Hannah-I-G",
"name": {
"family": "Hannah",
"given": "Iain G."
},
"orcid": "0000-0003-1193-8603"
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{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Smith-D-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
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{
"id": "Hudson-H-S",
"name": {
"family": "Hudson",
"given": "Hugh S."
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"orcid": "0000-0001-5685-1283"
},
{
"id": "White-S-M",
"name": {
"family": "White",
"given": "Stephen M."
},
"orcid": "0000-0002-8574-8629"
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},
"title": "NuSTAR Detection of X-Ray Heating Events in the Quiet Sun",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: flares \u2013 Sun: particle emission \u2013 Sun: X-rays, gamma rays",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 December 18; revised 2018 March 20; accepted 2018 March 21; published 2018 March 30. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. M.K. and S.K. acknowledge funding from the Swiss National Science Foundation (200021-140308). I.G.H. is supported by a Royal Society University Research Fellowship. L.G. was supported by an NSF Faculty Development Grant (AGS-1429512). We thank the referee for the thorough reading of the manuscript and the helpful comments that substantially improved the paper.\n\nPublished - Kuhar_2018_ApJL_856_L32.pdf
Accepted Version - 1803.08365.pdf
",
"abstract": "The explanation of the coronal heating problem potentially lies in the existence of nanoflares, numerous small-scale heating events occurring across the whole solar disk. In this Letter, we present the first imaging spectroscopy X-ray observations of three quiet Sun flares during the Nuclear Spectroscopic Telescope ARray (NuSTAR) solar campaigns on 2016 July 26 and 2017 March 21, concurrent with the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) observations. Two of the three events showed time lags of a few minutes between peak X-ray and extreme ultraviolet emissions. Isothermal fits with rather low temperatures in the range 3.2\u20134.1 MK and emission measures of (0.6\u201315) \u00d7 10^(44) cm^(\u22123) describe their spectra well, resulting in thermal energies in the range (2\u20136) \u00d7 10^(26) erg. NuSTAR spectra did not show any signs of a nonthermal or higher temperature component. However, as the estimated upper limits of (hidden) nonthermal energy are comparable to the thermal energy estimates, the lack of a nonthermal component in the observed spectra is not a constraining result. The estimated Geostationary Operational Environmental Satellite (GOES) classes from the fitted values of temperature and emission measure fall between 1/1000 and 1/100 A class level, making them eight orders of magnitude fainter in soft X-ray flux than the largest solar flares.",
"date": "2018-04-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "856",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L32",
"id_number": "CaltechAUTHORS:20180330-111231496",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180330-111231496",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "200021-140308"
},
{
"agency": "Royal Society"
},
{
"agency": "NSF",
"grant_number": "AGS-1429512"
}
]
},
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"id": "NuSTAR"
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"doi": "10.3847/2041-8213/aab889",
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"pub_year": "2018",
"author_list": "Kuhar, Matej; Krucker, S\u00e4m; et el."
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"datestamp": "2023-08-19 08:28:48",
"lastmod": "2023-10-17 22:04:21",
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"items": [
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"id": "R\u00f3\u017ca\u0144ska-A",
"name": {
"family": "R\u00f3\u017ca\u0144ska",
"given": "A."
},
"orcid": "0000-0002-5275-4096"
},
{
"id": "Bresler-K",
"name": {
"family": "Bresler",
"given": "K."
}
},
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"id": "Beldycki-B",
"name": {
"family": "Beldycki",
"given": "B."
}
},
{
"id": "Madej-J",
"name": {
"family": "Madej",
"given": "J."
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},
"title": "Ultraluminous X-ray sources: new distance indicators?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: neutron \u2013 X-rays: general",
"note": "\u00a9 2018 ESO. Article published by EDP Sciences. \n\nReceived 20 February 2018; Accepted 16 April 2018; Published online 10 May 2018. \n\nThis research was supported by Polish National Science Center grants No. 2015/17/B/ST9/03422, 2015/18/M/ST9/00541, and 2016/21/N/ST9/03311. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA, and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by ASDC (Italy) and Caltech (USA). This work has also made use of data obtained with XMM-Newton directly funded by ESA Member States.\n\nSubmitted - 1710.02024.pdf
",
"abstract": "Aims. In this paper we fit the NuSTAR and XMM-Newton data of three sources: NGC 7793 P13, NGC5907 ULX1, and Circinus ULX5. \n\nMethods. Our single model contains emission from a non-spherical system: a neutron star plus an accretion disk directed towards the observer. \n\nResults. We obtained a very good fit with the reduced \u03c72 per degree of freedom equal to 1.08 for P13, 1.01 for ULX1, and 1.14 for ULX5. The normalization of our model constrains the distance to the source. The resulting distances are D = 3.41_(\u22120.10)^(+0.11), 6.55_(\u22120.81)^(+0.69), and 2.60_(\u22120.03)^(+0.05) Mpc for P13, ULX1, and ULX5 respectively. The distances to P13 and ULX5 are in perfect agreement with previous distance measurements to their host galaxies. \n\nConclusions. Our results confirm that P13, ULX1, and ULX5 may contain central hot neutron stars. When the outgoing emission is computed by integration over the emitting surface and successfully fitted to the data, then the resulting model normalization is the direct distance indicator.",
"date": "2018-04",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "612",
"publisher": "EDP Sciences",
"pagerange": "Art. No. L12",
"id_number": "CaltechAUTHORS:20171006-100014623",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171006-100014623",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"doi": "10.1051/0004-6361/201832864",
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"author_list": "R\u00f3\u017ca\u0144ska, A.; Bresler, K.; et el."
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"items": [
{
"id": "Wang-Ji-Jingyi",
"name": {
"family": "Wang-Ji",
"given": "Jingyi"
}
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Bambi-C",
"name": {
"family": "Bambi",
"given": "Cosimo"
},
"orcid": "0000-0002-3180-9502"
},
{
"id": "Petrucci-Pierre-Olivier",
"name": {
"family": "Petrucci",
"given": "Pierre-Olivier"
}
},
{
"id": "Ferreira-J",
"name": {
"family": "Ferreira",
"given": "Jonathan"
}
},
{
"id": "Chakravorty-S",
"name": {
"family": "Chakravorty",
"given": "Susmita"
}
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "Ma\u00efca"
},
"orcid": "0000-0003-0724-2742"
}
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},
"title": "The Evolution of GX 339-4 in the Low-hard State as Seen by NuSTAR and Swift",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 line: formation \u2013 X-rays: individual (GX 339\u20134)",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 November 15; revised 2018 January 9; accepted 2018 January 19; published 2018 March 8. \n\nPart of this work was carried out by JW during attendance to the Summer Undergraduate Research Fellowship (SURF) at California Institute of Technology in 2017. Warm hospitality and tutelage are kindly acknowledged, in particular from the members of the NuSTAR Science Operations Team (K. Foster, B. Grenfestette, K. Madsen, M. Heida, M. Brightman, and D. Stern). We would like to thank the referee for useful comments toward the improvement of this paper. We also thank B. de Marco and G. Ponti for useful discussions. J.A.G. acknowledges support from NASA grants NNX17AJ65G and 80NSSC177K0515, and from the Alexander von Humboldt Foundation. J.F.S. has been supported by NASA Hubble Fellowship grant HST-HF-51315.01. S.C. is supported by the SERB National Postdoctoral Fellowship (No. PDF/2017/000841). We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations.\n\nPublished - Wang-Ji_2018_ApJ_855_61.pdf
Accepted Version - 1712.02571.pdf
",
"abstract": "We analyze 11 Nuclear Spectroscopic Telescope Array and Swift observations of the black hole X-ray binary GX 339\u20134 in the hard state, 6 of which were taken during the end of the 2015 outburst and 5 during a failed outburst in 2013. These observations cover luminosities from 0.5% to 5% of the Eddington luminosity. Implementing the most recent version of the reflection model relxillCp, we perform simultaneous spectral fits on both data sets to track the evolution of the properties in the accretion disk, including the inner edge radius, the ionization, and the temperature of the thermal emission. We also constrain the photon index and electron temperature of the primary source (the \"corona\"). We observe a maximum truncation radius of 37 R_g in the preferred fit for the 2013 data set, and a marginal correlation between the level of truncation and luminosity. We also explore a self-consistent model under the framework of coronal Comptonization, and find consistent results regarding the disk truncation in the 2015 data, providing a more physical preferred fit for the 2013 observations.",
"date": "2018-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "855",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 61",
"id_number": "CaltechAUTHORS:20180308-105914434",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180308-105914434",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Caltech Summer Undergraduate Research Fellowship (SURF)"
},
{
"agency": "NASA",
"grant_number": "NNX17AJ65G"
},
{
"agency": "NASA",
"grant_number": "80NSSC177K0515"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF-51315.01"
},
{
"agency": "Science and Engineering Research Board (SERB)",
"grant_number": "PDF/2017/000841"
}
]
},
"local_group": {
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"id": "NuSTAR"
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"id": "Space-Radiation-Laboratory"
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},
"doi": "10.3847/1538-4357/aaa974",
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],
"pub_year": "2018",
"author_list": "Wang-Ji, Jingyi; Garc\u00eda, Javier A.; et el."
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"id": "Tomsick-J-A",
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"family": "Tomsick",
"given": "John A."
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{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "Michael L."
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"orcid": "0000-0002-8466-7317"
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{
"id": "Garc\u00eda-Javier-A",
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"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Yamaoka-Kazutaka",
"name": {
"family": "Yamaoka",
"given": "Kazutaka"
}
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Chiu-Jeng-Lun",
"name": {
"family": "Chiu",
"given": "Jeng-Lun"
}
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "Ma\u00efca"
},
"orcid": "0000-0003-0724-2742"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew"
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Grinberg-V",
"name": {
"family": "Grinberg",
"given": "Victoria"
},
"orcid": "0000-0003-2538-0188"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Alternative Explanations for Extreme Supersolar Iron Abundances Inferred from the Energy Spectrum of Cygnus X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics; stars: individual (Cygnus X-1); X-rays: general; X-rays: stars",
"note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 December 1. Accepted 2018 January 22. Published 2018 February 27. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). J.A.T. acknowledges partial support from NuSTAR Guest Observer grant NNX15AV23G. A.C.F. acknowledges support from ERC Advanced Grant 340442. D.J.W. acknowledges support from STFC in the form of an Ernest Rutherford fellowship. J.A.T. thanks K. Hamaguchi for help with the XIS data reduction and T. Dauser, K. Koljonen, and A. Zoghbi for useful discussions. This research has made use of the MAXI data provided by RIKEN, JAXA, and the MAXI team.\n\nPublished - Tomsick_2018_ApJ_855_3.pdf
Submitted - 1801.07267.pdf
",
"abstract": "Here we study a 1\u2013200 keV energy spectrum of the black hole binary Cygnus X-1 taken with NuSTAR and Suzaku. This is the first report of a NuSTAR observation of Cyg X-1 in the intermediate state, and the observation was taken during the part of the binary orbit where absorption due to the companion's stellar wind is minimal. The spectrum includes a multi-temperature thermal disk component, a cutoff power-law component, and relativistic and nonrelativistic reflection components. Our initial fits with publicly available constant density reflection models (relxill and reflionx) lead to extremely high iron abundances (>9.96 and 10.6_(-0.9)^(+1.6) times solar, respectively). Although supersolar iron abundances have been reported previously for Cyg X-1, our measurements are much higher and such variability is almost certainly unphysical. Using a new version of reflionx that we modified to make the electron density a free parameter, we obtain better fits to the spectrum even with solar iron abundances. We report on how the higher density (n_e = (3.98)_(-0.25)^(+0.12)) x 10^(20) cm^(\u22123)) impacts other parameters such as the inner radius and inclination of the disk.",
"date": "2018-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "855",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 3",
"id_number": "CaltechAUTHORS:20180227-133907106",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180227-133907106",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX15AV23G"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/1538-4357/aaaab1",
"primary_object": {
"basename": "1801.07267.pdf",
"url": "https://authors.library.caltech.edu/records/5kgmy-rfa06/files/1801.07267.pdf"
},
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{
"basename": "Tomsick_2018_ApJ_855_3.pdf",
"url": "https://authors.library.caltech.edu/records/5kgmy-rfa06/files/Tomsick_2018_ApJ_855_3.pdf"
}
],
"pub_year": "2018",
"author_list": "Tomsick, John A.; Parker, Michael L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/3q2ca-b0j09",
"eprint_id": 85206,
"eprint_status": "archive",
"datestamp": "2023-08-21 22:52:09",
"lastmod": "2023-10-18 17:58:03",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Civano-Francesca",
"name": {
"family": "Civano",
"given": "F."
},
"orcid": "0000-0002-2115-1137"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Fornasini-F",
"name": {
"family": "Fornasini",
"given": "F."
},
"orcid": "0000-0002-9286-9963"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "G. B."
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Treister-E",
"name": {
"family": "Treister",
"given": "E."
},
"orcid": "0000-0001-7568-6412"
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "P. G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "R. C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Kocevski-D-D",
"name": {
"family": "Kocevski",
"given": "D. D."
}
},
{
"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "L."
},
"orcid": "0000-0002-3249-8224"
},
{
"id": "Marchesi-S",
"name": {
"family": "Marchesi",
"given": "S."
},
"orcid": "0000-0001-5544-0749"
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Saez-C",
"name": {
"family": "Saez",
"given": "C."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zappacosta-L",
"name": {
"family": "Zappacosta",
"given": "L."
},
"orcid": "0000-0002-4205-6884"
}
]
},
"title": "The NuSTAR Extragalactic Surveys: Source Catalog and the Compton-thick Fraction in the UDS Field",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: evolution; X-rays: general",
"note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 September 13. Accepted 2018 January 4. Published 2018 March 8. \n\nWe thank the anonymous referee for providing helpful comments, which significantly improved the clarity and robustness of the paper. \n\nThis work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nThis research has also made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, software provided by the Chandra X-ray Center (CXC), and observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, together with data obtained from the 3XMM XMM-Newton serendipitous source catalog compiled by the 10 institutes of the XMM-Newton Survey Science Centre selected by ESA. \n\nA.M. and A.C. acknowledge support from the ASI/INAF grant I/037/12/0011/13. W.N.B. acknowledges Caltech NuSTAR subcontract 44A-1092750. L.Z. acknowledges financial support under ASI/INAF contract I/037/12/0. G.B.L. acknowledges support from a Herchel Smith Fellowship of the University of Cambridge. E.T. acknowledges support from CONICYT-Chile grants Basal-CATA PFB-06/2007 and FONDECYT Regular 1160999. R.C.H. acknowledges support from NASA through grant no. NNX15AP24G. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Chandra - , XMM-Newton. -\n\nPublished - Masini_2018_ApJS_235_17.pdf
Submitted - 1801.01881.pdf
",
"abstract": "We present the results and the source catalog of the NuSTAR survey in the UKIDSS Ultra Deep Survey (UDS) field, bridging the gap in depth and area between NuSTAR's ECDFS and COSMOS surveys. The survey covers a ~0.6 deg2 area of the field for a total observing time of ~1.75 Ms, to a half-area depth of ~155 ks corrected for vignetting at 3\u201324 keV, and reaching sensitivity limits at half-area in the full (3\u201324 keV), soft (3\u20138 keV), and hard (8\u201324 keV) bands of 2.2 \u00d7 10\u221214 erg cm\u22122 s\u22121, 1.0 \u00d7 10\u221214 erg cm\u22122 s\u22121, and 2.7 \u00d7 10\u221214 erg cm\u22122 s\u22121, respectively. A total of 67 sources are detected in at least one of the three bands, 56 of which have a robust optical redshift with a median of $\\langle z\\rangle \\sim 1.1$. Through a broadband (0.5\u201324 keV) spectral analysis of the whole sample combined with the NuSTAR hardness ratios, we compute the observed Compton-thick (CT; N H > 1024 cm\u22122) fraction. Taking into account the uncertainties on each N H measurement, the final number of CT sources is 6.8 \u00b1 1.2. This corresponds to an observed CT fraction of 11.5% \u00b1 2.0%, providing a robust lower limit to the intrinsic fraction of CT active galactic nuclei and placing constraints on cosmic X-ray background synthesis models.",
"date": "2018-03",
"date_type": "published",
"publication": "Astrophysical Journal Supplement Series",
"volume": "235",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 17",
"id_number": "CaltechAUTHORS:20180308-120302328",
"issn": "1538-4365",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180308-120302328",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Herchel Smith Foundation"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Basal-CATA PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1160999"
},
{
"agency": "NASA",
"grant_number": "NNX15AP24G"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4365/aaa83d",
"primary_object": {
"basename": "1801.01881.pdf",
"url": "https://authors.library.caltech.edu/records/3q2ca-b0j09/files/1801.01881.pdf"
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{
"basename": "Masini_2018_ApJS_235_17.pdf",
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}
],
"pub_year": "2018",
"author_list": "Masini, A.; Civano, F.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/swp2a-ted79",
"eprint_id": 84230,
"eprint_status": "archive",
"datestamp": "2023-08-19 08:29:36",
"lastmod": "2023-10-18 16:00:43",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Heida-M",
"name": {
"family": "Heida",
"given": "M."
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
}
]
},
"title": "Magnetic field strength of a neutron-star-powered ultraluminous X-ray source",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2018 Macmillan Publishers. \n\nReceived: 05 December 2017. Accepted: 16 January 2018. Published online: 26 February 2018. \n\nM.J.M. and D.J.W. appreciate support from Ernest Rutherford Science and Technology Facilities Council fellowships. The work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nAuthor Contributions: M. Brightman reduced and analysed the Chandra and XMM-Newton data. F.F. performed timing analysis of the Chandra and XMM-Newton data. M.H. analysed the ULX multiwavelength counterpart. M. Brightman, F.A.H., F.F., M.J.M., D.J.W., A.C.F., D.B. and M. Bachetti interpreted the results. M. Brightman, F.A.H., D.J.W. and D.S. prepared the manuscript. \n\nThe authors declare no competing interests.\n\nAccepted Version - 1803.02376
",
"abstract": "Ultraluminous X-ray sources (ULXs) are bright X-ray sources in nearby galaxies not associated with the central supermassive black hole. Their luminosities imply they are powered by either an extreme accretion rate onto a compact stellar remnant, or an intermediate mass (~100\u201310^5M_\u2299) black hole. Recently detected coherent pulsations coming from three bright ULXs demonstrate that some of these sources are powered by accretion onto a neutron star, implying accretion rates significantly in excess of the Eddington limit, a high degree of geometric beaming, or both. The physical challenges associated with the high implied accretion rates can be mitigated if the neutron star surface field is very high (10^(14)\u2009G), since this suppresses the electron scattering cross-section, reducing the radiation pressure that chokes off accretion for high luminosities. Surface magnetic field strengths can be determined through cyclotron resonance scattering features produced by the transition of charged particles between quantized Landau levels. Here, we present the detection at a significance of 3.8\u03c3 of an absorption line at 4.5\u2009keV in the Chandra spectrum of a ULX in M51. This feature is likely to be a cyclotron resonance scattering feature produced by the strong magnetic field of a neutron star. Assuming scattering off electrons, the magnetic field strength is implied to be ~10^(11)\u2009G, while protons would imply a magnetic field of B\u2009~\u200910^(15)\u2009G.",
"date": "2018-02-26",
"date_type": "published",
"publication": "Nature Astronomy",
"volume": "2",
"number": "4",
"publisher": "Nature Publishing Group",
"pagerange": "312-316",
"id_number": "CaltechAUTHORS:20180110-105628140",
"issn": "2397-3366",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180110-105628140",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1038/s41550-018-0391-6",
"primary_object": {
"basename": "1803.02376",
"url": "https://authors.library.caltech.edu/records/swp2a-ted79/files/1803.02376"
},
"pub_year": "2018",
"author_list": "Brightman, Murray; Harrison, Fiona A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ds1ze-07b73",
"eprint_id": 84774,
"eprint_status": "archive",
"datestamp": "2023-08-21 22:46:22",
"lastmod": "2023-10-18 16:41:04",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Bucher-J",
"name": {
"family": "Buchner",
"given": "J."
},
"orcid": "0000-0003-0426-6634"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
}
]
},
"title": "New Spectral Model for Constraining Torus Covering Factors from Broadband X-Ray Spectra of Active Galactic Nuclei",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: individual (3C 390.3, NGC 2110, IC 5063, NGC 7582); methods: data analysis; techniques: spectroscopic; X-rays: galaxies",
"note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 April 22. Accepted 2018 January 13. Published 2018 February 9. \n\nThe authors thank the anonymous referee for careful reading and constructive suggestions that improved the paper. The authors gratefully acknowledge financial support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.), the ASI/INAF grant I/037/12/0\u2013011/13 (A.C.), the Caltech Kingsley visitor program (A.C.), FONDECYT 1141218 (C.R.), Basal-CATA PFB\u201306/2007 (C.R.), and the China-CONICYT fund (C.R.). \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. Furthermore, this research made use of the following resources: the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center; NASA's Astrophysics Data System; matplotlib, a Python library for publication quality graphics (Hunter 2007). \n\nFacility: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission.\n\nPublished - Balokovi\u0107_2018_ApJ_854_42.pdf
Submitted - 1801.04938.pdf
",
"abstract": "The basic unified model of active galactic nuclei (AGNs) invokes an anisotropic obscuring structure, usually referred to as a torus, to explain AGN obscuration as an angle-dependent effect. We present a new grid of X-ray spectral templates based on radiative transfer calculations in neutral gas in an approximately toroidal geometry, appropriate for CCD-resolution X-ray spectra (FWHM \u2265 130 eV). Fitting the templates to broadband X-ray spectra of AGNs provides constraints on two important geometrical parameters of the gas distribution around the supermassive black hole: the average column density and the covering factor. Compared to the currently available spectral templates, our model is more flexible, and capable of providing constraints on the main torus parameters in a wider range of AGNs. We demonstrate the application of this model using hard X-ray spectra from NuSTAR (3\u201379 keV) for four AGNs covering a variety of classifications: 3C 390.3, NGC 2110, IC 5063, and NGC 7582. This small set of examples was chosen to illustrate the range of possible torus configurations, from disk-like to sphere-like geometries with column densities below, as well as above, the Compton-thick threshold. This diversity of torus properties challenges the simple assumption of a standard geometrically and optically thick toroidal structure commonly invoked in the basic form of the unified model of AGNs. Finding broad consistency between our constraints and those from infrared modeling, we discuss how the approach from the X-ray band complements similar measurements of AGN structures at other wavelengths.",
"date": "2018-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "854",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 42",
"id_number": "CaltechAUTHORS:20180212-071654657",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180212-071654657",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0\u2013011/13"
},
{
"agency": "Caltech Kingsley visitor program"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB\u201306/2007"
},
{
"agency": "China-CONICYT fund"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
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},
"doi": "10.3847/1538-4357/aaa7eb",
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"url": "https://authors.library.caltech.edu/records/ds1ze-07b73/files/Balokovi\u0107_2018_ApJ_854_42.pdf"
}
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"pub_year": "2018",
"author_list": "Balokovi\u0107, M.; Brightman, M.; et el."
},
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"items": [
{
"id": "Zappacosta-L",
"name": {
"family": "Zappacosta",
"given": "L."
},
"orcid": "0000-0002-4205-6884"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
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}
]
},
"title": "The NuSTAR Extragalactic Surveys: X-Ray Spectroscopic Analysis of the Bright Hard-band Selected Sample",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; surveys; X-rays: galaxies",
"note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 May 24. Accepted 2017 December 29. Published 2018 February 8. \n\nWe thank the anonymous referee for useful comments that helped improve our analysis and the presentation of our results. We thank Johannes Buchner and Yoshihiro Ueda for providing machine-readable results on the absorbed fractions. L.Z. thanks R. Gilli, F. Nicastro, E. Piconcelli, R. Valiante, F. Vito, and D. Burlon for useful discussions. L.Z., A.C., F.F., G.L., and A.M. acknowledge financial support under ASI/INAF contract I/037/12/0. A.C. acknowledges the Caltech Kingsley fellowship program. G.L. acknowledges financial support from the CIG grant eEASY No. 321913. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT Regular 1141218), the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. This work was supported under NASA Contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Zappacosta_2018_ApJ_854_33.pdf
",
"abstract": "We discuss the spectral analysis of a sample of 63 active galactic nuclei (AGN) detected above a limiting flux of S(8-24 keV) = 7 x 10^(-14) erg s^(-1) cm^(-2 in the multi-tiered NuSTAR extragalactic survey program. The sources span a redshift range z = 0-2.1 (median (z) = 0.58). The spectral analysis is performed over the broad 0.5\u201324 keV energy range, combining NuSTAR with Chandra and/or XMM-Newton data and employing empirical and physically motivated models. This constitutes the largest sample of AGN selected at \u3009 10 keV to be homogeneously spectrally analyzed at these flux levels. We study the distribution of spectral parameters such as photon index, column density (N_H), reflection parameter (R), and 10\u201340 keV luminosity (L_X). Heavily obscured (log[N_H/cm^(-2] \u2265 23) and Compton-thick (CT; log[N_H/cm^(-2)] \u2265 24) AGN constitute ~25% (15\u201317 sources) and ~2\u20133% (1\u20132 sources) of the sample, respectively. The observed N_H distribution agrees fairly well with predictions of cosmic X-ray background population-synthesis models (CXBPSM). We estimate the intrinsic fraction of AGN as a function of N_H, accounting for the bias against obscured AGN in a flux-selected sample. The fraction of CT AGN relative to log[N_H/cm^(-2] = 20-24 AGN is poorly constrained, formally in the range 2\u201356% (90% upper limit of 66%). We derived a fraction (f_(abs)) of obscured AGN (log[N_H/cm^(-2]= 22-24) as a function of L_X in agreement with CXBPSM and previous z \u3008 1 X-ray determinations. Furthermore, f_(abs) at z = 0.1-0.5 and log(L_x/erg s^(-1) \u2248 43.6-44.3 agrees with observational measurements/trends obtained over larger redshift intervals. We report a significant anti-correlation of R with L_X (confirmed by our companion paper on stacked spectra) with considerable scatter around the median R values.",
"date": "2018-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "854",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 33",
"id_number": "CaltechAUTHORS:20180208-112709097",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180208-112709097",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Caltech Kingsley fellowship"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "321913 eEasy"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Basal-CATA PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Ministry of Economy, Development and Tourism's Millennium Science Initiative",
"grant_number": "IC120009"
},
{
"agency": "Millennium Institute of Astrophysics (MAS)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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"doi": "10.3847/1538-4357/aaa550",
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"pub_year": "2018",
"author_list": "Zappacosta, L. and Harrison, F. A."
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"id": "Walton-D-J",
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},
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"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Tao-Lian",
"name": {
"family": "Tao",
"given": "L."
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},
"title": "Super-Eddington accretion on to the neutron star NGC 7793 P13: Broad-band X-ray spectroscopy and ultraluminous X-ray sources",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual: NGC7793 P13",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 October 9. Received 2017 October 9; in original form 2017 May 29. Published: 11 October 2017.\n\nThe authors would like to thank the reviewer for the feedback provided, which helped to improve the final version of the manuscript. DJW and MJM acknowledge support from an STFC Ernest Rutherford fellowship, ACF acknowledges support from ERC Advanced Grant 340442 and DB acknowledges financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This work has also made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States.\n\nPublished - stx2650.pdf
Accepted Version - 1705.10297.pdf
",
"abstract": "We present a detailed, broad-band X-ray spectral analysis of the ultraluminous X-ray source (ULX) pulsar NGC\u20097793 P13, a known super-Eddington source, utilizing data from the XMM\u2013Newton, NuSTAR and Chandra observatories. The broad-band XMM\u2013Newton+NuSTAR spectrum of P13 is qualitatively similar to the rest of the ULX sample with broad-band coverage, suggesting that additional ULXs in the known population may host neutron star accretors. Through time-averaged, phase-resolved and multi-epoch studies, we find that two non-pulsed thermal blackbody components with temperatures \u223c0.5 and 1.5\u2009keV are required to fit the data below 10\u2009keV, in addition to a third continuum component which extends to higher energies and is associated with the pulsed emission from the accretion column. The characteristic radii of the thermal components appear to be comparable, and are too large to be associated with the neutron star itself, so the need for two components likely indicates the accretion flow outside the magnetosphere is complex. We suggest a scenario in which the thick inner disc expected for super-Eddington accretion begins to form, but is terminated by the neutron star's magnetic field soon after its onset, implying a limit of B \u2272 6 \u00d7 10^(12)\u2009G for the dipolar component of the central neutron star's magnetic field. Evidence of similar termination of the disc in other sources may offer a further means of identifying additional neutron star ULXs. Finally, we examine the spectrum exhibited by P13 during one of its unusual 'off' states. These data require both a hard power-law component, suggesting residual accretion on to the neutron star, and emission from a thermal plasma, which we argue is likely associated with the P13 system.",
"date": "2018-02-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "473",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4360-4376",
"id_number": "CaltechAUTHORS:20180221-134250534",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180221-134250534",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"id": "Space-Radiation-Laboratory"
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"id": "NuSTAR"
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},
"doi": "10.1093/mnras/stx2650",
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"author_list": "Walton, D. J.; F\u00fcrst, F.; et el."
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"id": "Walton-D-J",
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"family": "Brightman",
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},
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"id": "Risaliti-G",
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"family": "Risaliti",
"given": "G."
}
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{
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"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
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{
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"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
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"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A."
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"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Miniutti-G",
"name": {
"family": "Miniutti",
"given": "G."
}
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
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},
"title": "Disentangling the Complex Broadband X-ray Spectrum of IRAS 13197-1627 with NuSTAR, XMM-Newton and Suzaku",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 X-rays: individual: IRAS 13197\u22121627",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 October 9. Received 2017 October 9; in original form 2017 June 7. Published: 12 October 2017. \n\nThe authors would like to thank the reviewer for their helpful feedback, which helped to improve the final version of the manuscript. DJW acknowledges support from an STFC Ernest Rutherford Fellowship, and ACF acknowledges support from ERC Advanced Grant 340442. GM thanks the European Union Seventh Framework Program (FP7/2007\u20132013) for funding under grant 312789 (StrongGravity). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, and with Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA).\n\nPublished - stx2659.pdf
Accepted Version - 1706.02088.pdf
",
"abstract": "We present results from a coordinated XMM\u2013Newton+NuSTAR observation of the type 1.8 Seyfert galaxy IRAS\u200913197\u22121627. This is a highly complex source, with strong contributions from relativistic reflection from the inner accretion disc, neutral absorption and further reprocessing by more distant material, and ionized absorption from an outflow. We undertake a detailed spectral analysis combining the broad-band coverage provided by XMM\u2013Newton+NuSTAR with a multi-epoch approach incorporating archival observations performed by XMM\u2013Newton and Suzaku. Our focus is on characterizing the reflection from the inner accretion disc, which previous works have suggested may dominate the AGN emission, and constraining the black hole spin. Using lamppost disc reflection models, we find that the results for the inner disc are largely insensitive to assumptions regarding the geometry of the distant reprocessor and the precise form of the illuminating X-ray continuum. However, these results do depend on the treatment of the iron abundance of the distant absorber/reprocessor. The multi-epoch data favour a scenario in which the AGN is chemically homogeneous, and we find that a rapidly rotating black hole is preferred, with a* \u2265 0.7, but a slowly rotating black hole is not strongly excluded. In addition to the results for the inner disc, we also find that both the neutral and ionized absorbers vary from epoch to epoch, implying that both have some degree of inhomogeneity in their structure.",
"date": "2018-02-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "473",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4377-4391",
"id_number": "CaltechAUTHORS:20170608-112508378",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170608-112508378",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
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},
"doi": "10.1093/mnras/stx2659",
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"author_list": "Walton, D. J.; Brightman, M.; et el."
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"items": [
{
"id": "Bachetti-M",
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"given": "Matteo"
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},
"title": "No Time for Dead Time: Use the Fourier Amplitude Differences to Normalize Dead-time-affected Periodograms",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "methods: data analysis \u2013 X-rays: binaries \u2013 X-rays: general",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 September 27; revised 2018 January 15; accepted 2018 January 15; published 2018 January 30. \n\nWe thank the anonymous referee for providing very insightful feedback. We thank David W. Hogg for useful discussions on the topic of Fourier analysis, and Jeff Scargle for useful suggestions and comments. MB is supported in part by the Italian Space Agency through agreement ASI-INAF No. 2017-12-H.0 and ASI-INFN agreement No. 2017-13-H.0. D.H. is supported by the James Arthur Postdoctoral Fellowship and the Moore-Sloan Data Science Environment at New York University. D.H. acknowledges support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. \n\nSoftware: Astropy (Astropy Collaboration et al. 2013), Matplotlib (Hunter 2007), scipy & numpy (van der Walt et al. 2011), stingray (Huppenkothen et al. 2016), HENDRICS (Bachetti 2015, before name change), Jupyter notebooks (Kluyver et al. 2016).\n\nSubmitted - 1709.09700.pdf
",
"abstract": "Dead time affects many of the instruments used in X-ray astronomy, by producing a strong distortion in power density spectra. This can make it difficult to model the aperiodic variability of the source or look for quasi-periodic oscillations. Whereas in some instruments a simple a priori correction for dead-time-affected power spectra is possible, this is not the case for others such as NuSTAR, where the dead time is non-constant and long (~2.5 ms). Bachetti et al. (2015) suggested the cospectrum obtained from light curves of independent detectors within the same instrument as a possible way out, but this solution has always only been a partial one: the measured rms was still affected by dead time because the width of the power distribution of the cospectrum was modulated by dead time in a frequency-dependent way. In this Letter, we suggest a new, powerful method to normalize dead-time-affected cospectra and power density spectra. Our approach uses the difference of the Fourier amplitudes from two independent detectors to characterize and filter out the effect of dead time. This method is crucially important for the accurate modeling of periodograms derived from instruments affected by dead time on board current missions like NuSTAR and Astrosat, but also future missions such as IXPE.",
"date": "2018-02-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "853",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L21",
"id_number": "CaltechAUTHORS:20171002-135222252",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171002-135222252",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"doi": "10.3847/2041-8213/aaa83b",
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"pub_year": "2018",
"author_list": "Bachetti, Matteo and Huppenkothen, Daniela"
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"title": "NuSTAR spectral analysis of two bright Seyfert 1 galaxies: MCG +8-11-11 and NGC 6814",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual: MCG +8-11-11 \u2013 galaxies: individual: NGC 6814 \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 September 20; Received 2017 September 20; in original form 2017 July 14; Published: 02 October 2017.\n\nWe thank the anonymous referee for comments that helped improving the clarity of the paper. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTARDAS jointly developed by the ASDC (Italy) and the California Institute of Technology (USA). AT, AM and GM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13, and SB under grant ASI-INAF I/037/12/P1. Part of this work is based on archival data, software or online services provided by the ASDC. AT, SB, AM, GM and RM acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. POP acknowledges financial support from the CNES and the CNRS/PNHE. EP and SB acknowledge financial contribution from the agreement ASI-INAF I/037/12/0.\n\nSubmitted - 1709.07231.pdf
",
"abstract": "We report on the NuSTAR observations of two bright Seyfert 1 galaxies, namely MCG +8-11-11 (100 ks) and NGC 6814 (150 ks). The main goal of these observations was to investigate the Comptonization mechanisms acting in the innermost regions of an active galactic nucleus (AGN) which are believed to be responsible for the UV/X-ray emission. The spectroscopic analysis of the NuSTAR spectra of these two sources revealed that although they had different properties overall (black hole masses, luminosity and Eddington ratios), they had very similar coronal properties. Both presented a power-law spectrum with a high-energy cut-off at \u223c150\u2013200\u2009keV, a relativistically broadened Fe K\u2009\u03b1 line and the associated disc reflection component, plus a narrow iron line likely emitted in Compton thin and distant matter. The intrinsic continuum was well described by Comptonization models that show for MCG +8-11-11 a temperature of the coronal plasma of kT_e \u223c 60\u2009keV and an extrapolated optical depth \u03c4 = 1.8; for NGC 6814, the coronal temperature was kT_e \u223c 45\u2009keV with an extrapolated optical depth of \u03c4 = 2.5. We compare and discuss these values to some most common Comptonization models that aim at explaining the energy production and stability of coronae in AGNs.",
"date": "2018-01-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "473",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3104-3112",
"id_number": "CaltechAUTHORS:20170924-172902877",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170924-172902877",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/P1"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
}
]
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"doi": "10.1093/mnras/stx2457",
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"title": "NuSTAR + XMM-Newton monitoring of the neutron star transient AX J1745.6-2901",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 methods: observational \u2013 techniques: spectroscopic \u2013 stars: neutron \u2013 absorption lines \u2013X-rays: binaries",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 September 18. Received 2017 September 18; in original form 2017 May 13. Published: 22 September 2017. \n\nThe authors wish to thank Jan-Uwe Ness, Karl Foster, Ignacio de la Calle and the rest of the XMM-Newton and NuSTAR scheduling teams for the support that made the coordinated observations possible. We would like to thank the referee for the helpful comments and careful reading of the paper. The GC XMM-Newton monitoring project is supported by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408 and FKZ 50 OR 1408) and the Max Planck Society. SB acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0. TMD acknowledges support via a Ram\u00f3n y Cajal Fellowship (RYC-2015-18148). BDM acknowledges support from the European Union's Horizon 2020 research and innovation programme and the Polish National Science Centre grant Polonez 2016/21/P/ST9/04025. These results are based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NUSTARDAS jointly developed by the ASI Science Data Centre (ASDC, Italy) and the California Institute of Technology (USA). We thank the staff of the GMRT who have made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).\n\nPublished - stx2425.pdf
Accepted Version - 1709.06571.pdf
",
"abstract": "AX J1745.6-2901 is a high-inclination (eclipsing) transient neutron star (NS) low-mass X-ray binary showcasing intense ionized Fe K absorption. We present here the analysis of 11 XMM-Newton and 15 NuSTAR new data sets (obtained between 2013 and 2016), therefore tripling the number of observations of AX J1745.6-2901 in outburst. Thanks to simultaneous XMM-Newton and NuSTAR spectra, we greatly improve on the fitting of the X-ray continuum. During the soft state, the emission can be described by a disc blackbody (kT \u223c 1.1\u20131.2\u2009keV and inner disc radius rDBB \u223c 14 km), plus hot (kT \u223c 2.2\u20133.0\u2009keV) blackbody radiation with a small emitting radius (rBB \u223c 0.5 \u2212 0.8 km) likely associated with the boundary layer or NS surface, plus a faint Comptonization component. Imprinted on the spectra are clear absorption features created by both neutral and ionized matter. Additionally, positive residuals suggestive of an emission Fe K\u2009\u03b1 disc line and consistent with relativistic ionized reflection are present during the soft state, while such residuals are not significant during the hard state. The hard-state spectra are characterized by a hard (\u0393 \u223c 1.9\u20132.1) power law, showing no evidence for a high energy cut-off (kTe > 60\u2013140\u2009keV) and implying a small optical depth (\u03c4 < 1.6). The new observations confirm the previously witnessed trend of exhibiting strong Fe K absorption in the soft state that significantly weakens during the hard state. Optical (GROND) and radio (GMRT) observations suggest for AX J1745.6-2901 a standard broad-band spectral energy distribution as typically observed in accreting NSs.",
"date": "2018-01-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "473",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2304-2323",
"id_number": "CaltechAUTHORS:20170921-135527394",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170921-135527394",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "FKZ 50 OR 1408"
},
{
"agency": "Max Planck Society"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Ram\u00f3n y Cajal programme",
"grant_number": "RYC-2015-18148"
},
{
"agency": "European Union Horizon 2020 Research and Innovation Program"
},
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"agency": "National Science Centre (Poland)",
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},
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}
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"doi": "10.1093/mnras/stx2425",
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},
"title": "Reflection Spectra of the Black Hole Binary Candidate MAXI J1535-571 in the Hard State Observed by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 X-rays: binaries",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 November 2; revised 2018 January 2; accepted 2018 January 2; published 2018 January 12. \n\nWe thank the referee for constructive comments that improved the Letter. D.J.W. acknowledges support from STFC Ernest Rutherford Fellowship. J.A.G. acknowledges support from NASA grant No. 80NSSC17K0515 and the Alexander von Humboldt Foundation. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Xu_2018_ApJL_852_L34.pdf
Submitted - 1711.01346.pdf
",
"abstract": "We report on a Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the recently discovered bright black hole candidate MAXI J1535-571. NuSTAR observed the source on MJD 58003 (five days after the outburst was reported). The spectrum is characteristic of a black hole binary in the hard state. We observe clear disk reflection features, including a broad Fe K\u03b1 line and a Compton hump peaking around 30 keV. Detailed spectral modeling reveals a narrow Fe K\u03b1 line complex centered around 6.5 keV on top of the strong relativistically broadened Fe K\u03b1 line. The narrow component is consistent with distant reflection from moderately ionized material. The spectral continuum is well described by a combination of cool thermal disk photons and a Comptonized plasma with the electron temperature kT_e = 19.7 \u00b1 0.4 keV. An adequate fit can be achieved for the disk reflection features with a self-consistent relativistic reflection model that assumes a lamp-post geometry for the coronal illuminating source. The spectral fitting measures a black hole spin a > 0.84, inner disk radius R_(in) < 2.01 r_(ISCO) , and a lamp-post height h = 7.2^(+0.8)_(-2.0) r_g (statistical errors, 90% confidence), indicating no significant disk truncation and a compact corona. Although the distance and mass of this source are not currently known, this suggests the source was likely in the brighter phases of the hard state during this NuSTAR observation.",
"date": "2018-01-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "852",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L34",
"id_number": "CaltechAUTHORS:20180116-152713791",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180116-152713791",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "80NSSC17K0515"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
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"doi": "10.3847/2041-8213/aaa4b2",
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"pub_year": "2018",
"author_list": "Xu, Yanjun; Harrison, Fiona A.; et el."
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"items": [
{
"id": "Stiele-H",
"name": {
"family": "Stiele",
"given": "H."
}
},
{
"id": "Kong-Albert-K-H",
"name": {
"family": "Kong",
"given": "A. K. H."
},
"orcid": "0000-0002-5105-344X"
}
]
},
"title": "NuSTAR and Swift observations of Swift J1357.2-0933 during an early phase of its 2017 outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: close; stars: black holes; X-rays: binaries; X-rays: individual (Swift J1357.2-0933)",
"note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2017 June 29; revised 2017 November 10; accepted 2017 November 23; published 2018 January 3. \n\nWe thank Fiona Harrison, Brad Cenko, and the schedulers and SOC of Swift and NuSTAR for making these observations possible. This project is supported by the Ministry of Science and Technology of the Republic of China (Taiwan) through grants 105-2112-M-007-033-MY2 and 105-2811-M-007-065. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - .\n\nSubmitted - 1712.02804.pdf
",
"abstract": "We present a detailed spectral analysis of Swift and NuSTAR observations of the very faint X-ray transient and black hole system, Swift J1357.2\u20130933, during an early, low-hard state of its 2017 outburst. Swift J1357.2\u20130933 was observed at ~0.02% of the Eddington luminosity (for a distance of 2.3 kpc and a mass of 4 M_\u2299). Despite the low luminosity, the broadband X-ray spectrum between 0.3 and 78 keV requires the presence of a disk blackbody component with an inner disk temperature of T_(in) ~ 0.06 keV in addition to a thermal Comptonization component with a photon index of \u0393 ~ 1.70. Using a more physical model, which takes strong relativistic effects into account, and assuming a high inclination of 70\u00b0, which is motivated by the presence of dips in optical light curves, we find that the accretion disk is truncated within a few R_(ISCO) from the black hole, independent of the spin.",
"date": "2018-01-08",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "852",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 34",
"id_number": "CaltechAUTHORS:20171211-120811608",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171211-120811608",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "105-2112-M-007-033-MY2"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "105-2811-M-007-065"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa9d3e",
"primary_object": {
"basename": "1712.02804.pdf",
"url": "https://authors.library.caltech.edu/records/ss9ed-5jz07/files/1712.02804.pdf"
},
"pub_year": "2018",
"author_list": "Stiele, H. and Kong, A. K. H."
},
{
"id": "https://authors.library.caltech.edu/records/7a8az-prp88",
"eprint_id": 82157,
"eprint_status": "archive",
"datestamp": "2023-08-19 07:13:47",
"lastmod": "2023-10-17 22:04:28",
"type": "article",
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"creators": {
"items": [
{
"id": "Kammoun-E-S",
"name": {
"family": "Kammoun",
"given": "E. S."
}
},
{
"id": "Nardini-E",
"name": {
"family": "Nardini",
"given": "E."
},
"orcid": "0000-0001-9226-8992"
},
{
"id": "Risalti-G",
"name": {
"family": "Risaliti",
"given": "G."
}
},
{
"id": "Ghisellini-G",
"name": {
"family": "Ghisellini",
"given": "G."
}
},
{
"id": "Behar-E",
"name": {
"family": "Behar",
"given": "E."
}
},
{
"id": "Celotti-A",
"name": {
"family": "Celotti",
"given": "A."
}
}
]
},
"title": "Bulk Comptonization: new hints from the luminous blazar 4C+25.05",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 quasars: general \u2013 quasars: individual: 4C+25.05 \u2013X-rays: galaxies \u2013X-rays: general",
"note": "\u00a9 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 October 3. Received 2017 October 2; in original form 2017 September 9. Published: 05 October 2017.\n\nEN is supported by the EU through the Horizon 2020 Marie Sk\u0142odowska-Curie grant agreement no. 664931. EB is supported by the EU through the Horizon 2020 Marie Sk\u0142odowska-Curie grant agreement no. 655324. The results presented in this letter are based on data obtained with the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA; XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (Italy) and the California Institute of Technology (USA). The figures were generated using matplotlib (Hunter 2007), a PYTHON library for publication of quality graphics. The MCMC results were presented using the open source code corner.py (Foreman-Mackey 2016).\n\nAccepted Version - 1710.01748.pdf
",
"abstract": "Blazars are often characterized by a spectral break at soft X-rays, whose origin is still debated. While most sources show a flattening, some exhibit a blackbody-like soft excess with temperatures of the order of \u223c0.1\u2009keV, similar to low-luminosity, non-jetted Seyferts. Here, we present the analysis of the simultaneous XMM\u2013Newton and NuSTAR observations of the luminous flat-spectrum radio quasar 4C+25.05 (z = 2.368). The observed 0.3\u201330\u2009keV spectrum is best described by the sum of a hard X-ray power law (\u0393=1.38^(+0.05)_(\u22120.03)) and a soft component, approximated by a blackbody with kT_(BB)=0.66^(+0.05)_(\u22120.04) keV (rest frame). If the spectrum of 4C+25.05 is interpreted in the context of bulk Comptonization by cold electrons of broad-line region photons emitted in the direction of the jet, such an unusual temperature implies a bulk Lorentz factor of the jet of \u0393_(bulk) \u223c 11.7. Bulk Comptonization is expected to be ubiquitous on physical grounds, yet no clear signature of it has been found so far, possibly due to its transient nature and the lack of high-quality, broad-band X-ray spectra.",
"date": "2018-01-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "473",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L89-L93",
"id_number": "CaltechAUTHORS:20171006-100333383",
"issn": "1745-3933",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171006-100333383",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/slx164",
"primary_object": {
"basename": "1710.01748.pdf",
"url": "https://authors.library.caltech.edu/records/7a8az-prp88/files/1710.01748.pdf"
},
"pub_year": "2018",
"author_list": "Kammoun, E. S.; Nardini, E.; et el."
},
{
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"items": [
{
"id": "Porquet-D",
"name": {
"family": "Porquet",
"given": "D."
},
"orcid": "0000-0001-9731-0352"
},
{
"id": "Reeves-J-N",
"name": {
"family": "Reeves",
"given": "J. N."
}
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "A."
}
},
{
"id": "Nardini-E",
"name": {
"family": "Nardini",
"given": "E."
},
"orcid": "0000-0001-9226-8992"
},
{
"id": "Braito-V",
"name": {
"family": "Braito",
"given": "V."
},
"orcid": "0000-0002-2629-4989"
},
{
"id": "Lobban-A-P",
"name": {
"family": "Lobban",
"given": "A."
},
"orcid": "0000-0002-6433-1357"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tortosa-A",
"name": {
"family": "Tortosa",
"given": "A."
}
},
{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A deep X-ray view of the bare AGN Ark 120. IV. XMM-Newton and NuSTAR spectra dominated by two temperature (warm, hot) Comptonization processes",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: individuals: Ark 120 \u2013 galaxies: active \u2013 radiation mechanisms: general \u2013 accretion, accretion disks \u2013\nquasars: general",
"note": "\u00a9 2018 ESO. Article published by EDP Sciences.\n\nReceived 1 June 2017; Accepted 24 July 2017; Published online 05 January 2018.\n\nThe authors would like to deeply thank the anonymous referee for useful and constructive comments. The paper is based on observations obtained with the XMM-Newton, and ESA science mission with instruments and contributions directly funded by ESA member states and the USA (NASA). This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology. D.P. would like to acknowledge financial support from the French \"Programme National Hautes \u00c9nergies\" (PNHE). Part of the work was supported by the European Union Seventh Framework Program under the grant agreement No. 312789 (D.P., G.M., A.M., A.F.). J.N.R. acknowledges financial support via Chandra grant number GO4-15092X and NASA grant NNX15AF12G. J.N.R. and A.L. also acknowledge the support of the STFC, via the consolidated grant ST/M001040/1. G.M., A.M., A.T. and F.U. acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. E.N. acknowledges funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931.\n\nPublished - aa31290-17.pdf
Submitted - 1707.08907.pdf
",
"abstract": "Context. The physical characteristics of the material closest to supermassive black holes (SMBHs) are primarily studied through X-ray observations. However, the origins of the main X-ray components such as the soft X-ray excess, the Fe\u2009K\u03b1 line complex, and the hard X-ray excess are still hotly debated. This is particularly problematic for active galactic nuclei (AGN) showing a significant intrinsic absorption, either warm or neutral, which can severely distort the observed continuum. Therefore, AGN with no (or very weak) intrinsic absorption along the line of sight, so-called \"bare AGN\", are the best targets to directly probe matter very close to the SMBH.\nAims. We perform an X-ray spectral analysis of the brightest and cleanest bare AGN known so far, Ark\u2009120, in order to determine the process(es) at work in the vicinity of the SMBH.\nMethods. We present spectral analyses of data from an extensive campaign observing Ark\u2009120 in X-rays with XMM-Newton (4 \u00d7 120\u2009ks, 2014 March 18\u201324), and NuSTAR (65.5\u2009ks, 2014 March 22).\nResults. During this very deep X-ray campaign, the source was caught in a high-flux state similar to the earlier 2003 XMM-Newton observation, and about twice as bright as the lower-flux observation in 2013. The spectral analysis confirms the \"softer when brighter\" behavior of Ark\u2009120. The four XMM-Newton/pn spectra are characterized by the presence of a prominent soft X-ray excess and a significant Fe\u2009K\u03b1 complex. The continuum is very similar above about 3\u2009keV, while significant variability is present for the soft X-ray excess. We find that relativistic reflection from a constant-density, flat accretion disk cannot simultaneously produce the soft excess, broad Fe\u2009K\u03b1 complex, and hard X-ray excess. Instead, Comptonization reproduces the broadband (0.3\u201379 keV) continuum well, together with a contribution from a mildly relativistic disk reflection spectrum.\nConclusions. During this 2014 observational campaign, the soft X-ray spectrum of Ark 120 below ~0.5\u2009keV was found to be dominated by Comptonization of seed photons from the disk by a warm (kTe ~ 0.5\u2009keV), optically-thick corona (\u03c4 ~ 9). Above this energy, the X-ray spectrum becomes dominated by Comptonization from electrons in a hot optically thin corona, while the broad Fe\u2009K\u03b1 line and the mild Compton hump result from reflection off the disk at several tens of gravitational radii.",
"date": "2018-01",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "609",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A42",
"id_number": "CaltechAUTHORS:20180125-144741618",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180125-144741618",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Programme National Hautes \u00c9nergies (PNHE)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "NASA",
"grant_number": "GO4-15092X"
},
{
"agency": "NASA",
"grant_number": "NNX15AF12G"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/M001040/1"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "664931"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1051/0004-6361/201731290",
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"pub_year": "2018",
"author_list": "Porquet, D.; Reeves, J. N.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/6vcch-hm513",
"eprint_id": 82060,
"eprint_status": "archive",
"datestamp": "2023-08-19 06:58:58",
"lastmod": "2023-10-17 22:00:57",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Evans-P-A",
"name": {
"family": "Evans",
"given": "P. A."
},
"orcid": "0000-0002-8465-3353"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Y."
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Heida-M",
"name": {
"family": "Heida",
"given": "M."
},
"orcid": "0000-0002-1082-7496"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "H."
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Pike-S-N",
"name": {
"family": "Pike",
"given": "S."
},
"orcid": "0000-0002-8403-0041"
},
{
"id": "Rosswog-S",
"name": {
"family": "Rosswog",
"given": "S."
}
}
]
},
"title": "Swift and NuSTAR observations of GW170817: detection of a blue kilonova",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 American Association for the Advancement of Science. \n\nReceived 14 September 2017; accepted 4 October 2017; Published online 16 October 2017. \n\nWe acknowledge the leadership and scientific vision of Neil Gehrels (1952\u20132017), former PI of Swift, without whom the work we present here would not have been possible. Funding for the Swift mission in the UK is provided by the UK Space Agency. SRO gratefully acknowledges the support of the Leverhulme Trust Early Career Fellowship (SRO). The Swift team at the MOC at Penn State acknowledges support from NASA contract NAS5-00136. The Italian Swift team acknowledge support from ASI-INAF grant I/004/11/3. SR has been supported by the Swedish Research Council (VR) under grant number 2016-03657_3, by the Swedish National Space Board under grant number Dnr. 107/16 and by the research environment grant \"Gravitational Radiation and Electromagnetic Astrophysical Transients (GREAT)\" funded by the Swedish Research council (VR) under Dnr 2016- 06012. This research used resources provided by the Los Alamos National Laboratory Institutional Computing Program, which is supported by the U.S. Department of Energy National Nuclear Security Administration under Contract No. DE-AC52-06NA25396. VLT data were obtained under ESO program number 099.D-0668. NuSTAR acknowledges funding from NASA Contract No. NNG08FD60C. A.J.L. and N.R.T. acknowledge funding from the European Research Council under the European Union's Horizon 2020 programme, grant number 725246. Researchers at Los Alamos National Laboratory were supported by the National Nuclear Security Administration of the US Department of Energy under contract number DE-AC52-06NA25396. SWKE is supported by a Science and Technology Facilities Council studentship. The observations are archived at http://www.swift.ac.uk for Swift and https://heasarc.gsfc.nasa.gov/docs/nustar/nustar_archive.html for NuSTAR, under the observation IDs given in Table S2. Reduced photometry and surveyed areas are tabulated in the supplementary material. The BOXFIT software is available at http://cosmo.nyu.edu/afterglowlibrary/boxfit2011.html, SUPERNU at https://bitbucket.org/drrossum/supernu/wiki/Home, access to WINNET source code and input files will be granted upon request via: https://bitbucket.org/korobkin/winnet. The dynamical model ejecta are available at http://compact-merger.astro.su.se/downloads_fluid_trajectories.html (as run 12). The SUPERNU and BOXFIT input files are available in the supplementary materials.\n\nAccepted Version - 1710.05437.pdf
Supplemental Material - aap9580-Evans-SM.pdf
Supplemental Material - aap9580-Evans-SM_add_data.zip
",
"abstract": "With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW) astrophysics began. A complete picture of compact object mergers, however, requires the detection of an electromagnetic (EM) counterpart. We report ultraviolet (UV) and x-ray observations by Swift and the Nuclear Spectroscopic Telescope Array of the EM counterpart of the binary neutron star merger GW170817. The bright, rapidly fading UV emission indicates a high mass (\u22480.03 solar masses) wind-driven outflow with moderate electron fraction (Ye \u2248 0.27). Combined with the x-ray limits, we favor an observer viewing angle of \u224830\u00b0 away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultrarelativistic, highly collimated ejecta (a \u03b3-ray burst afterglow).",
"date": "2017-12-22",
"date_type": "published",
"publication": "Science",
"volume": "358",
"number": "6370",
"publisher": "American Association for the Advancement of Science",
"pagerange": "1565-1570",
"id_number": "CaltechAUTHORS:20171004-130639886",
"issn": "0036-8075",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171004-130639886",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "United Kingdom Space Agency (UKSA)"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "NASA",
"grant_number": "NAS5-00136"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/004/11/3"
},
{
"agency": "Swedish Research Council",
"grant_number": "2016-03657_3"
},
{
"agency": "Swedish National Space Board",
"grant_number": "Dnr. 107/16"
},
{
"agency": "Swedish Research Council",
"grant_number": "Dnr 2016-06012"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-AC52-06NA25396"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "725246"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1126/science.aap9580",
"primary_object": {
"basename": "aap9580-Evans-SM_add_data.zip",
"url": "https://authors.library.caltech.edu/records/6vcch-hm513/files/aap9580-Evans-SM_add_data.zip"
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"url": "https://authors.library.caltech.edu/records/6vcch-hm513/files/aap9580-Evans-SM.pdf"
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],
"pub_year": "2017",
"author_list": "Evans, P. A.; Madsen, K. K.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/hzbk4-x0h56",
"eprint_id": 77612,
"eprint_status": "archive",
"datestamp": "2023-08-19 06:57:16",
"lastmod": "2023-10-25 23:18:03",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Basak-R",
"name": {
"family": "Basak",
"given": "Rupal"
}
},
{
"id": "Zdziarski-A-A",
"name": {
"family": "Zdziarski",
"given": "Andrzej A."
}
},
{
"id": "Parker-M",
"name": {
"family": "Parker",
"given": "Michael"
}
},
{
"id": "Islam-N",
"name": {
"family": "Islam",
"given": "Nazma"
}
}
]
},
"title": "Analysis of NuSTAR and Suzaku observations of Cyg X-1 in the hard state: evidence for a truncated disc geometry",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013 stars: individual: Cyg X-1 \u2013 X-rays: binaries \u2013 X-rays: individual: Cyg X-1",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 September 1. Received 2017 September 1; in original form 2017 May 18. Published: 05 September 2017. \n\nWe thank John Tomsick for providing us with the wind-absorption model used in this work, Thomas Dauser, Chris Done, Javier Garc\u00eda, Andrzej Nied\u017awiecki, J\u00f6rn Wilms for valuable discussions, and the referee, Javier Garc\u00eda, for important suggestions. This research has used data obtained through the HEASARC Online Service, provided by the NASA/GSFC, in support of NASA High Energy Astrophysics Programs. RB has been supported by the 2016 START programme of the Polish Science Foundation. This research has been supported in part by the Polish National Science Centre grants 2013/10/M/ST9/00729, 2015/18/A/ST9/00746 and 2016/21/P/ST9/04025.\n\nAccepted Version - 1705.06638.pdf
",
"abstract": "The geometry of the accretion flow in black hole X-ray binaries in the hard state, in particular the position of the disc inner edge, has been a subject of intense debate in recent years. We address this issue by performing a spectral study of simultaneous observations of Cyg X-1 in the hard state by NuSTAR and Suzaku. The same data were analysed before, and modelled by a lamppost containing hybrid electrons and located very close to the horizon, whose emission was incident on a surrounding disc extending almost to the innermost stable circular orbit. We re-analyse the incident continuum model and show that it suffers from the lack of physical self-consistency. Still, the good fit to the data provided by this model indicates that the real continuum has a similar shape. We find it features a strong soft X-ray excess below a few keV, which we model as a soft thermal-Comptonization component, in addition to the main hard thermal-Compton component. This continuum model with reflection of both components yields the overall lowest \u03c7^2 and has a geometry with a hot inner accretion flow and a disc truncated at \u224313\u201320 gravitational radii. On the other hand, we have also found spectral solution with a lamppost at a large height and a disc that can extend to the innermost stable circular orbit, though somewhat statistically worse. Overall, we find that the fitted truncation radius depends on the assumed continuum and geometry.",
"date": "2017-12-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "472",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4220-4232",
"id_number": "CaltechAUTHORS:20170520-161631457",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170520-161631457",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx2283",
"primary_object": {
"basename": "1705.06638.pdf",
"url": "https://authors.library.caltech.edu/records/hzbk4-x0h56/files/1705.06638.pdf"
},
"pub_year": "2017",
"author_list": "Basak, Rupal; Zdziarski, Andrzej A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/xz4fh-5c285",
"eprint_id": 83958,
"eprint_status": "archive",
"datestamp": "2023-08-19 06:56:14",
"lastmod": "2023-10-18 14:33:50",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "Ashley L."
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Grinberg-V",
"name": {
"family": "Grinberg",
"given": "Victoria"
},
"orcid": "0000-0003-2538-0188"
}
]
},
"title": "Spectral and Timing Properties of IGR J17091\u20133624 in the Rising Hard State During Its 2016 Outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (IGR J17091\u20133624)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 August 10; revised 2017 November 2; accepted 2017 November 12; published 2017 December 18. \n\nWe thank the anonymous referee for detailed and helpful comments. D.J.W. acknowledges support from an STFC Ernest Rutherford Fellowship. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Xu_2017_ApJ_851_103.pdf
Submitted - 1711.04421.pdf
",
"abstract": "We present a spectral and timing study of the NuSTAR and Swift observations of the black hole candidate IGR J17091\u20133624 in the hard state during its outburst in 2016. Disk reflection is detected in each of the NuSTAR spectra taken in three epochs. Fitting with relativistic reflection models reveals that the accretion disk is truncated during all epochs with R_(in) > 10 r_g, with the data favoring a low disk inclination of ~30\u00b0\u201340\u00b0. The steepening of the continuum spectra between epochs is accompanied by a decrease in the high energy cutoff: the electron temperature kT_e drops from ~64 to ~26 keV, changing systematically with the source flux. We detect type-C QPOs in the power spectra with frequency varying between 0.131 and 0.327 Hz. In addition, a secondary peak is found in the power spectra centered at about 2.3 times the QPO frequency during all three epochs. The nature of this secondary frequency is uncertain; however, a non-harmonic origin is favored. We investigate the evolution of the timing and spectral properties during the rising phase of the outburst and discuss their physical implications.",
"date": "2017-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "851",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 103",
"id_number": "CaltechAUTHORS:20171219-092934959",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171219-092934959",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aa9ab4",
"primary_object": {
"basename": "1711.04421.pdf",
"url": "https://authors.library.caltech.edu/records/xz4fh-5c285/files/1711.04421.pdf"
},
"related_objects": [
{
"basename": "Xu_2017_ApJ_851_103.pdf",
"url": "https://authors.library.caltech.edu/records/xz4fh-5c285/files/Xu_2017_ApJ_851_103.pdf"
}
],
"pub_year": "2017",
"author_list": "Xu, Yanjun; Garc\u00eda, Javier A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/00251-1cy28",
"eprint_id": 81264,
"eprint_status": "archive",
"datestamp": "2023-08-19 06:49:19",
"lastmod": "2023-10-17 19:42:27",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kammoun-E-S",
"name": {
"family": "Kammoun",
"given": "E. S."
}
},
{
"id": "Papadakis-I-E",
"name": {
"family": "Papadakis",
"given": "I. E."
}
}
]
},
"title": "The nature of X-ray spectral variability in MCG-6-30-15",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual: MCG\u20136-30-15 \u2013 galaxies: nuclei \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 August 16. Received 2017 July 24; in original form 2017 June 20. Published: 24 August 2017. \n\nWe thank the anonymous referee for useful comments. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA; XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nAccepted Version - 1709.01059
",
"abstract": "The flux\u2013flux plot (FFP) method can provide model-independent clues regarding the X-ray variability of active galactic nuclei. To use it properly, the bin size of the light curves should be as short as possible, provided the average counts in the light-curve bins are larger than \u223c200. We apply the FFP method, performed in 2013, to the simultaneous XMM\u2013Newton and NuSTAR observations of the Seyfert galaxy MCG\u20136-30-15, in the 0.3\u201340\u2009keV range. The FFPs above \u223c1.6\u2009keV are well described by a straight line. This result rules out spectral slope variations and the hypothesis of absorption-driven variability. Our results are fully consistent with a power-law component varying in normalization only, with a spectral slope of \u223c2, plus a variable, relativistic reflection arising from the inner accretion disc around a rotating black hole. We also detect spectral components that remain constant over \u223c4.5\u2009d (at least). At energies above \u223c1.5\u2009keV, the stable component is consistent with reflection from distant, neutral material. The constant component at low energies is consistent with a blackbody spectrum of kTBB \u223c 100\u2009eV. The fluxes of these components are \u223c10\u201320% of the average continuum flux (in the respective bands). They should always be included in the models that are used to fit the spectrum of the source. The FFPs below 1.6\u2009keV are non-linear, which could be due to the variable warm absorber in this source.",
"date": "2017-12-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "472",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3131-3146",
"id_number": "CaltechAUTHORS:20170908-094351605",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170908-094351605",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx2181",
"primary_object": {
"basename": "1709.01059",
"url": "https://authors.library.caltech.edu/records/00251-1cy28/files/1709.01059"
},
"pub_year": "2017",
"author_list": "Kammoun, E. S. and Papadakis, I. E."
},
{
"id": "https://authors.library.caltech.edu/records/b403h-wn779",
"eprint_id": 83784,
"eprint_status": "archive",
"datestamp": "2023-09-22 22:39:48",
"lastmod": "2023-10-23 23:26:05",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Dallilar-Y",
"name": {
"family": "Dallilar",
"given": "Yigit"
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
}
]
},
"title": "A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 American Association for the Advancement of Science. \n\nReceived 22 February 2017; accepted 3 November 20. \n\nThe near-infrared light curve is based on observations made with the Gran Telescopio Canarias, installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias, in the island of La Palma, during science commissioning of CIRCE. Development of CIRCE was supported by the University of Florida and the National Science Foundation (grant AST-0352664), in collaboration with the Inter-University Centre for Astronomy and Astrophysics. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. The ULTRACAM team and P.G. (grant ST/J003697/2) acknowledge the financial support of the U.K. Science and Technology Facilities Council. This research has made use of data obtained with NuSTAR, a project led by the California Institute of Technology, funded by NASA and managed by NASA/Jet Propulsion Laboratory, and has used the NUSTARDAS software package, jointly developed by the Agenzia Spaziale Italiana Science Data Center (Italy) and California Institute of Technology (USA). A.J.C.-T. acknowledges support from the Spanish Ministry Project AYA2015-71718-R. We thank S. Markoff, C. Ceccobello, and T. Maccarone for comments on the scientific discussion. The multiwavelength lightcurves are provided as data file S1, and our derived measurements are listed in table S1. The observational data are available for each instrument: CIRCE at http://astro.ufl.edu/~ydallilar/Dallilar17/CIRCEraw; ULTRACAM at https://sotonac-my.sharepoint.com/personal/pg3e14_soton_ac_uk/Documents/Forms/All.aspx?slrid=603d299e%2D704d%2D4000%2Dbf01%2Dc1708c50f62d&RootFolder=%2Fpersonal%2Fpg3e14%5Fsoton%5Fac%5Fuk%2FDocuments%2Fv404&FolderCTID0x012000F83BE7EA86B4FE49BECFDAA6CEB2B068 (in ULTRACAM pipeline binary format); NuSTAR at https://heasarc.gsfc.nasa.gov/FTP/nustar/data/obs/01/9/90102007011; and AMI at www.tauceti.caltech.edu/kunal/uploads/SWIFT_643949-150625.fits (in radio Flexible Image Transport System format).\n\nSubmitted - science_manuscript_jun11.pdf
Supplemental Material - aan0249-Dallilar-SM.pdf
Supplemental Material - aan0249_Dallilar_SM-Data-File-S1.zip
",
"abstract": "Observations of binary stars containing an accreting black hole or neutron star often show x-ray emission extending to high energies (>10 kilo\u00ad\u2013electron volts), which is ascribed to an accretion disk corona of energetic particles akin to those seen in the solar corona. Despite their ubiquity, the physical conditions in accretion disk coronae remain poorly constrained. Using simultaneous infrared, optical, x-ray, and radio observations of the Galactic black hole system V404 Cygni, showing a rapid synchrotron cooling event in its 2015 outburst, we present a precise 461 \u00b1 12 gauss magnetic field measurement in the corona. This measurement is substantially lower than previous estimates for such systems, providing constraints on physical models of accretion physics in black hole and neutron star binary systems.",
"date": "2017-12-08",
"date_type": "published",
"publication": "Science",
"volume": "358",
"number": "6368",
"publisher": "American Association for the Advancement of Science",
"pagerange": "1299-1302",
"id_number": "CaltechAUTHORS:20171211-081010239",
"issn": "0036-8075",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171211-081010239",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "University of Florida"
},
{
"agency": "NSF",
"grant_number": "AST-0352664"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)",
"grant_number": "AYA2015-71718-R"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1126/science.aan0249",
"primary_object": {
"basename": "aan0249-Dallilar-SM.pdf",
"url": "https://authors.library.caltech.edu/records/b403h-wn779/files/aan0249-Dallilar-SM.pdf"
},
"related_objects": [
{
"basename": "aan0249_Dallilar_SM-Data-File-S1.zip",
"url": "https://authors.library.caltech.edu/records/b403h-wn779/files/aan0249_Dallilar_SM-Data-File-S1.zip"
},
{
"basename": "science_manuscript_jun11.pdf",
"url": "https://authors.library.caltech.edu/records/b403h-wn779/files/science_manuscript_jun11.pdf"
}
],
"pub_year": "2017",
"author_list": "Dallilar, Yigit and F\u00fcrst, Felix"
},
{
"id": "https://authors.library.caltech.edu/records/9htd6-rrg90",
"eprint_id": 80902,
"eprint_status": "archive",
"datestamp": "2023-08-19 06:13:17",
"lastmod": "2023-10-17 18:35:10",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "An elevation of 0.1 light-seconds for the optical jet base in an accreting Galactic black hole system",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 Macmillan Publishers Limited, part of Springer Nature. \n\nReceived: 24 February 2017; Accepted: 07 September 2017;\nPublished online: 30 October 2017.\n\nThis research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA), as well as the High Energy Astrophysics Science Archive Research Center. P.G. thanks the Science and Technology Facilities Council (STFC) for support (grant reference ST/J003697/2). ULTRACAM and V.S.D. are supported by STFC grant ST/M001350/1. P.G. thanks C.B. Markwardt, C.M. Boon, A.B. Hill, M. Fiocchi, K. Forster, A. Zoghbi and T. Mu\u00f1oz-Darias for help and discussions. J.C. acknowledges financial support from the Spanish Ministry of Economy, Industry and Competitiveness (MINECO) under the 2015 Severo Ochoa Program MINECO SEV-2015-0548, and to the Leverhulme Trust through grant VP2-2015-04. T.R.M. acknowledges STFC (ST/L000733/1). J.M. acknowledges financial support from the French National Research Agency (CHAOS project ANR-12-BS05-0009), and D.A. thanks the Royal Society. S.M. acknowledges support from Netherlands Organisation for Scientific Research (NWO) VICI grant no. 639.043.513. We thank P. Wallace for use of his SLA C library. P.A.C. is grateful to the Leverhulme Trust for the award of a Leverhulme Emeritus Fellowship. Part of this research was supported by the UK-India UKIERI/UGC Thematic Partnership grants UGC 2014-15/02 and IND/CONT/E/14-15/355. This work profited from discussions carried out during a meeting organized at the International Space Science Institute (ISSI) Beijing by T. Belloni and D. Bhattacharya.\n\nContributions: P.G. wrote the ULTRACAM proposal, analysed the data and wrote the paper. The ULTRACAM observations were coordinated and carried out by L.K.H., S.P.L., V.S.D. and T.R.M. The X-ray observations were proposed by D.J.W., coordinated by D.S., J.A.T. and F.A.H., and the timing data analysed by M.B. Radio data were obtained and analysed by R.P.F. and K.M. INTEGRAL data were arranged by E.K. The remaining authors provided insight into jet physics constraints (S.M., J.M., C.C.), cross-correlation analyses (P.C., R.I.H., C.K., C.F., M.P., F.V.) and placing the source in context (D.A., J.C., P.A.C., D.M.R., F.R., A.W.S.). All authors read and commented on multiple versions of the manuscript.\n\nCompeting interests: The authors declare no competing financial interests.\n\nAccepted Version - 1710.09838.pdf
Supplemental Material - 41550_2017_273_MOESM1_ESM.pdf
",
"abstract": "Relativistic plasma jets are observed in many systems that host accreting black holes. According to theory, coiled magnetic fields close to the black hole accelerate and collimate the plasma, leading to a jet being launched. Isolating emission from this acceleration and collimation zone is key to measuring its size and understanding jet formation physics. But this is challenging because emission from the jet base cannot easily be disentangled from other accreting components. Here, we show that rapid optical flux variations from an accreting Galactic black-hole binary are delayed with respect to X-rays radiated from close to the black hole by about 0.1\u2009seconds, and that this delayed signal appears together with a brightening radio jet. The origin of these subsecond optical variations has hitherto been controversial4. Not only does our work strongly support a jet origin for the optical variations but it also sets a characteristic elevation of \u227210^3 Schwarzschild radii for the main inner optical emission zone above the black hole, constraining both internal shock and magnetohydrodynamic models. Similarities with blazars suggest that jet structure and launching physics could potentially be unified under mass-invariant models. Two of the best-studied jetted black-hole binaries show very similar optical lags, so this size scale may be a defining feature of such systems.",
"date": "2017-12",
"date_type": "published",
"publication": "Nature Astronomy",
"volume": "1",
"number": "12",
"publisher": "Nature Publishing Group",
"pagerange": "859-864",
"id_number": "CaltechAUTHORS:20170829-115834040",
"issn": "2397-3366",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170829-115834040",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/M001350/1"
},
{
"agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)"
},
{
"agency": "Centro de Excelencia Severo Ochoa",
"grant_number": "SEV-2015-0548"
},
{
"agency": "Leverhulme Trust",
"grant_number": "VP2-2015-04"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L000733/1"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-12-BS05-0009"
},
{
"agency": "Royal Society"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)",
"grant_number": "639.043.513"
},
{
"agency": "UK India Education Research Initiative (UKIERI)",
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"doi": "10.1038/s41550-017-0273-3",
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"title": "Looking at A 0535+26 at low luminosities with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries / pulsars: individual: A 0535+26 / stars: neutron / accretion, accretion disks / stars: magnetic field",
"note": "\u00a9 ESO, 2017. \n\nReceived: 22 March 2017. Accepted: 10 July 2017. Published online 12 December 2017. \n\nWe thank Sebastian Falkner, Matthias K\u00fchnel, and Ingo Kreykenbohm for many fruitful discussions. We thank the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt for support under contract 50\u2009OR\u20091410. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nThis research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/).\n\nPublished - aa30845-17.pdf
Submitted - 1707.05648.pdf
",
"abstract": "We report on two NuSTAR observations of the high-mass X-ray binary A 0535+26 taken toward the end of its normal 2015 outburst at very low 3\u201350\u2009keV luminosities of ~1.4 \u00d7 10^(36) erg s^(-1) and ~5 \u00d7 10^(35) erg s^(-1), which are complemented by nine Swift observations. The data clearly confirm indications seen in earlier data that the source's spectral shape softens as it becomes fainter. The smooth exponential rollover at high energies seen in the first observation evolves to a much more abrupt steepening of the spectrum at 20\u201330\u2009keV. The continuum evolution can be nicely described with emission from a magnetized accretion column, modeled using the compmag model modified by an additional Gaussian emission component for the fainter observation. Between the two observations, the optical depth changes from 0.75 \u00b1 0.04 to 0.56^(+0.01)_(-0.04), the electron temperature remains constant, and there is an indication that the column decreases in radius. Since the energy-resolved pulse profiles remain virtually unchanged in shape between the two observations, the emission properties of the accretion column reflect the same accretion regime. This conclusion is also confirmed by our result that the energy of the cyclotron resonant scattering feature (CRSF) at ~45\u2009keV is independent of the luminosity, implying that the magnetic field in the region in which the observed radiation is produced is the same in both observations. Finally, we also constrain the evolution of the continuum parameters with the rotational phase of the neutron star. The width of the CRSF could only be constrained for the brighter observation. Based on Monte Carlo simulations of CRSF formation in single accretion columns, its pulse phase dependence supports a simplified fan beam emission pattern. The evolution of the CRSF width is very similar to that of the CRSF depth, which is, however, in disagreement with expectations.",
"date": "2017-12",
"date_type": "published",
"publication": "Astronomy & Astrophysics",
"volume": "608",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A105",
"id_number": "CaltechAUTHORS:20180104-163940808",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180104-163940808",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt",
"grant_number": "50\u2009OR\u20091410"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Gaia Multilateral Agreement"
}
]
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"doi": "10.1051/0004-6361/201730845",
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"author_list": "Ballhausen, Ralf; Pottschmidt, Katja; et el."
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"name": {
"family": "Boggs",
"given": "Steven E."
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"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
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"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
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"name": {
"family": "Hailey",
"given": "Charles J."
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"family": "Harrison",
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},
"title": "First NuSTAR Limits on Quiet Sun Hard X-Ray Transient Events",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: flares \u2013 Sun: X-rays, gamma rays",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 May 13; revised 2017 October 2; accepted 2017 October 2; published 2017 November 8. \n\nThis paper made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Some of the figures within this paper were produced using IDL color-blind-friendly color tables (Wright 2017). The authors would like to thank Albert Shih for helpful comments and suggestions. A.M. was supported by NASA Earth and Space Science Fellowship award NNX13AM41H. I.G.H. acknowledges support from a Royal Society University Research Fellowship. S.K. acknowledges support from the Swiss National Science Foundation (200021-140308). A.C. was supported by NASA grants NNX15AK26G and NNX14AH54G. L.G. was supported by an NSF Faculty Development Grant to UMN (AGS-1429512). P.J.W. was supported by an EPSRC/Royal Society Fellowship Engagement Award (EP/M00371X/1). This work was supported by NASA grants NNX12AJ36G and NNX14AG07G. \n\nFacility: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission.\n\nPublished - Marsh_2017_ApJ_849_131.pdf
Accepted Version - 1711.05385.pdf
",
"abstract": "We present the first results of a search for transient hard X-ray (HXR) emission in the quiet solar corona with the Nuclear Spectroscopic Telescope Array (NuSTAR) satellite. While NuSTAR was designed as an astrophysics mission, it can observe the Sun above 2 keV with unprecedented sensitivity due to its pioneering use of focusing optics. NuSTAR first observed quiet-Sun regions on 2014 November 1, although out-of-view active regions contributed a notable amount of background in the form of single-bounce (unfocused) X-rays. We conducted a search for quiet-Sun transient brightenings on timescales of 100 s and set upper limits on emission in two energy bands. We set 2.5\u20134 keV limits on brightenings with timescales of 100 s, expressed as the temperature T and emission measure EM of a thermal plasma. We also set 10\u201320 keV limits on brightenings with timescales of 30, 60, and 100 s, expressed as model-independent photon fluxes. The limits in both bands are well below previous HXR microflare detections, though not low enough to detect events of equivalent T and EM as quiet-Sun brightenings seen in soft X-ray observations. We expect future observations during solar minimum to increase the NuSTAR sensitivity by over two orders of magnitude due to higher instrument livetime and reduced solar background.",
"date": "2017-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "849",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 131",
"id_number": "CaltechAUTHORS:20171108-103806025",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171108-103806025",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX13AM41H"
},
{
"agency": "Royal Society"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "200021-140308"
},
{
"agency": "NASA",
"grant_number": "NNX15AK26G"
},
{
"agency": "NASA",
"grant_number": "NNX14AH54G"
},
{
"agency": "NSF",
"grant_number": "AGS-1429512"
},
{
"agency": "Engineering and Physical Sciences Research Council (EPSRC)",
"grant_number": "EP/M00371X/1"
},
{
"agency": "NASA",
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},
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"author_list": "Marsh, Andrew J.; Smith, David M.; et el."
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"id": "Del-Moro-Agnese",
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"family": "Del Moro",
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"orcid": "0000-0002-5896-6313"
},
{
"id": "Aird-James-A",
"name": {
"family": "Aird",
"given": "J. A."
},
"orcid": "0000-0003-1908-8463"
},
{
"id": "Bauer-Franz-E",
"name": {
"family": "Bauer",
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},
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{
"id": "Civano-Francesca",
"name": {
"family": "Civano",
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},
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"id": "Mullaney-James-R",
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"family": "Comastri",
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{
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"family": "Luo",
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{
"id": "Marchesi-Stefano",
"name": {
"family": "Marchesi",
"given": "S."
},
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"id": "Puccetti-Simonetta",
"name": {
"family": "Puccetti",
"given": "S."
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{
"id": "Ricci-Claudio",
"name": {
"family": "Ricci",
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{
"id": "Saez-Cristian",
"name": {
"family": "Saez",
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{
"id": "Stern-Daniel",
"name": {
"family": "Stern",
"given": "D."
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{
"id": "Treister-Ezequiel",
"name": {
"family": "Treister",
"given": "E."
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{
"id": "Zappacosta-Luca",
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},
"title": "The NuSTAR Extragalactic Survey: Average Broadband X-Ray Spectral Properties of the NuSTAR-detected AGNs",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 quasars: general \u2013 surveys \u2013 X-rays: galaxies",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 February 6; revised 2017 September 26; accepted 2017 October 2; published 2017 October 31.\n\nWe thank A. Corral for useful discussions about the spectral averaging method presented in her work. A.D.M. thanks the financial support from the Max Plank Society and the UK Science and Technology Facilities Council (STFC, ST/L00075X/1, A.D.M. and D.M.A.; ST/K501979/1, G.B.L.). F.E.B. and E.T. acknowledge support from CONICYT-Chile (Basal-CATA PFB-06/2007, \"EMBIGGEN\" Anillo ACT1101, FONDECYT Regular 1141218 [F.E.B.] and 1160999 [E.T.]); F.E.B. also thanks the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics (MAS). P.G. thanks the STFC for support (ST/J003697/2). W.N.B. acknowledges support from the Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. A.C. and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 011/13.\n\nThis work was supported under NASA contract no. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Del_Moro_2017_ApJ_849_57.pdf
Submitted - 1710.01041.pdf
",
"abstract": "We present a study of the average X-ray spectral properties of the sources detected by the NuSTARextragalactic survey, comprising observations of the Extended Chandra Deep Field South (E-CDFS), Extended Groth Strip (EGS), and the Cosmic Evolution Survey (COSMOS). The sample includes 182 NuSTAR sources (64 detected at 8\u201324 keV), with 3\u201324 keV fluxes ranging between f_(3-24 kev) \u2248 10^(-14) and 6 \u00d7 10^(\u221213) erg cm^(\u22122) s^(\u22121) (f_(8-24 kev) \u2248 3 x 10^(-14)-3 x 10^(-13) erg cm^(\u22122) s^(\u22121)) and redshifts in the range of z = 0.04-3.21. We produce composite spectra from the Chandra + NuSTAR data (E \u2248 2-40 keV, rest frame) for all the sources with redshift identifications (95%) and investigate the intrinsic, average spectra of the sources, divided into broad-line (BL) and narrow-line (NL) active galactic nuclei (AGNs), and also in different bins of X-ray column density and luminosity. The average power-law photon index for the whole sample is \u0393 = 1.65^(+0.03)_(-0.03), flatter than the \u0393 \u2248 1.8 typically found for AGNs. While the spectral slope of BL and X-ray unabsorbed AGNs is consistent with the typical values (\u0393 = 1.79^(+0.01)_(-0.01)), a significant flattening is seen in NL AGNs and heavily absorbed sources (\u0393 = 1.60^(+0.08)_(-0.05) and \u0393 = 1.38^(+0.12)_(-0.12), respectively), likely due to the effect of absorption and to the contribution from the Compton reflection component to the high-energy flux ( E > 10 keV). We find that the typical reflection fraction in our spectra is R \u2248 0.5 (for \u0393 = 1.8), with a tentative indication of an increase of the reflection strength with X-ray column density. While there is no significant evidence for a dependence of the photon index on X-ray luminosity in our sample, we find that R decreases with luminosity, with relatively high levels of reflection (R \u2248 1.2) for L_(10-40 kev) < 10^(44) erg s^(\u22121) and R \u2248 0.3 for L_(10-40 kev) > 10^(44) erg s^(\u22121) AGNs, assuming a fixed spectral slope of \u0393 = 1.8.",
"date": "2017-11-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "849",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 57",
"id_number": "CaltechAUTHORS:20171031-103333243",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171031-103333243",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Max Plank Society"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1160999"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0 011/13"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aa9115",
"primary_object": {
"basename": "1710.01041.pdf",
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"basename": "Del_Moro_2017_ApJ_849_57.pdf",
"url": "https://authors.library.caltech.edu/records/06jk0-sgg38/files/Del_Moro_2017_ApJ_849_57.pdf"
}
],
"pub_year": "2017",
"author_list": "Del Moro, A.; Alexander, D. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/3mcjy-rw478",
"eprint_id": 82404,
"eprint_status": "archive",
"datestamp": "2023-08-19 05:54:03",
"lastmod": "2023-10-17 22:15:47",
"type": "article",
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"creators": {
"items": [
{
"id": "Wong-Ka-Wah",
"name": {
"family": "Wong",
"given": "Ka-Wah"
},
"orcid": "0000-0002-5267-2867"
},
{
"id": "Nemmen-R-S",
"name": {
"family": "Nemmen",
"given": "Rodrigo S."
},
"orcid": "0000-0003-3956-0331"
},
{
"id": "Irwin-J-A",
"name": {
"family": "Irwin",
"given": "Jimmy A."
},
"orcid": "0000-0003-4307-8521"
},
{
"id": "Lin-Dacheng",
"name": {
"family": "Lin",
"given": "Dacheng"
},
"orcid": "0000-0001-5683-5339"
}
]
},
"title": "Hard X-ray Emission from the M87 AGN Detected with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: elliptical and lenticular, cD \u2013 galaxies: individual (M87) \u2013 galaxies: nuclei \u2013 X-rays: galaxies",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 September 16; revised 2017 October 5; accepted 2017 October 11; published 2017 October 26.\n\nWe thank the referee for helpful comments. This work was supported by NASA Chandra grant GO7-18085X and NASA NuSTAR grant NNX17GF12P.\n\nSubmitted - 1710.05031.pdf
",
"abstract": "M87 hosts a 3\u20136 billion solar mass black hole with a remarkable relativistic jet that has been regularly monitored in radio to TeV bands. However, hard X-ray emission \u227310 keV, which would be expected to primarily come from the jet or the accretion flow, had never been detected from its unresolved X-ray core. We report NuSTAR detection up to 40 keV from the the central regions of M87. Together with simultaneous Chandra observations, we have constrained the dominant hard X-ray emission to be from its unresolved X-ray core, presumably in its quiescent state. The core spectrum is well fitted by a power law with photon index \u0393 = 2.11^(+0.15)_(-0.11). The measured flux density at 40 keV is consistent with a jet origin, although emission from the advection-dominated accretion flow cannot be completely ruled out. The detected hard X-ray emission is significantly lower than that predicted by synchrotron self-Compton models introduced to explain emission above a GeV.",
"date": "2017-11-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "849",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L17",
"id_number": "CaltechAUTHORS:20171017-090307513",
"issn": "2041-8213",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171017-090307513",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "GO7-18085X"
},
{
"agency": "NASA",
"grant_number": "NNX17GF12P"
}
]
},
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"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8213/aa92c2",
"primary_object": {
"basename": "1710.05031.pdf",
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"pub_year": "2017",
"author_list": "Wong, Ka-Wah; Nemmen, Rodrigo S.; et el."
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"items": [
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "E. V."
},
"orcid": "0000-0003-3847-3957"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Hord-B-J",
"name": {
"family": "Hord",
"given": "Ben J."
}
},
{
"id": "de-O\u00f1a-Wilhelmi-E",
"name": {
"family": "de O\u00f1a Wilhelmi",
"given": "Emma"
}
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Zhang-Shuo",
"name": {
"family": "Zhang",
"given": "Shuo"
},
"orcid": "0000-0002-2967-790X"
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "Jaesub"
}
},
{
"id": "Garvin-A-M",
"name": {
"family": "Garvin",
"given": "Amani M."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Hard X-ray Observation of the Gamma-ray Binary Candidate HESS J1832-093",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "gamma rays: general \u2013 radiation mechanisms: non-thermal \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 June 16; revised 2017 August 19; accepted 2017 September 12; published 2017 October 13. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Mori_2017_ApJ_848_80.pdf
Submitted - 1710.02118.pdf
",
"abstract": "We present a hard X-ray observation of the TeV gamma-ray binary candidate HESS J1832\u2212093, which is coincident with the supernova remnant G22.7\u22120.2, using the Nuclear Spectroscopic Telescope Array. Non-thermal X-ray emission from XMMU J183245\u22120921539, the X-ray source associated with HESS J1832\u2212093, is detected up to ~30 keV and is well-described by an absorbed power-law model with a best-fit photon index \u0393 = 1.5 \u00b1 0.1. A re-analysis of archival Chandra and XMM-Newtondata finds that the long-term X-ray flux increase of XMMU J183245\u22120921539 is 50^(+40)_(-20)% (90% C.L.), much less than previously reported. A search for a pulsar spin period or binary orbit modulation yields no significant signal to a pulse fraction limit of f_p < 19% in the range 4 ms < P < 40 ks. No red noise is detected in the FFT power spectrum to suggest active accretion from a binary system. While further evidence is required, we argue that the X-ray and gamma-ray properties of XMMU J183245\u22120921539 are most consistent with a non-accreting binary generating synchrotron X-rays from particle acceleration in the shock formed as a result of the pulsar and stellar wind collision. We also report on three nearby hard X-ray sources, one of which may be associated with diffuse emission from a fast-moving supernova fragment interacting with a dense molecular cloud.",
"date": "2017-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "848",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 80",
"id_number": "CaltechAUTHORS:20171006-100701228",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171006-100701228",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aa8d15",
"primary_object": {
"basename": "1710.02118.pdf",
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"basename": "Mori_2017_ApJ_848_80.pdf",
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"pub_year": "2017",
"author_list": "Mori, Kaya; Gotthelf, E. V.; et el."
},
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"eprint_id": 81789,
"eprint_status": "archive",
"datestamp": "2023-08-19 05:35:07",
"lastmod": "2023-10-17 21:37:18",
"type": "article",
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"creators": {
"items": [
{
"id": "Kawamuro-Taiki",
"name": {
"family": "Kawamuro",
"given": "Taiki"
},
"orcid": "0000-0002-6808-2052"
},
{
"id": "Schirmer-M",
"name": {
"family": "Schirmer",
"given": "Mischa"
},
"orcid": "0000-0003-2568-9994"
},
{
"id": "Turner-J-E-H",
"name": {
"family": "Turner",
"given": "James E. H."
}
},
{
"id": "Davies-R-L",
"name": {
"family": "Davies",
"given": "Rebecca L."
},
"orcid": "0000-0002-3324-4824"
},
{
"id": "Ichikawa-Kohei",
"name": {
"family": "Ichikawa",
"given": "Kohei"
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"orcid": "0000-0002-4377-903X"
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},
"title": "NuSTAR hard X-ray data and Gemini 3D spectra reveal powerful AGN and outflow histories in two low-redshift Lyman-\u03b1 blobs",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual (SDSS J011341.11+010608.4, SDSS J115544.59\u2013014739.9) \u2013\nX-rays: galaxies",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 July 4; revised 2017 September 7; accepted 2017 September 19; published 2017 October 10.\n\nThis work was financially supported by the Grant-in-Aid for JSPS fellows for young researchers (T.K.) and also for Scientific Research 40756293 (K.I.). Further financial support was provided by the Gemini Observatory (T.K.). M.S. acknowledges support by the National Aeronautics and Space Administration through Chandra Award Number GO4-15110X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nAuthor contributions: T.K. reduced the NuSTAR and Chandra X-ray data and performed the joint spectral analysis; T.K. and M.S. wrote the manuscript; M.S. performed the analysis of the 3D spectra and led the NuSTAR, Chandra, and Gemini proposals; J.T. reduced the Gemini 3D spectra and obtained the [O iii]luminosities; and R.D. obtained the velocity, velocity dispersion, and line flux maps.\n\nM.S. thanks Claudio Ricci, Daniel Asmus, and Ai-Lei Sun for sharing their expertise on the subject.\n\nThis work is based on data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology.\n\nThis work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.\n\nBased on observations made by the Chandra X-ray Observatory, and on data obtained from the Chandra Data Archive. We also made use of the software provided by the Chandra X-ray Center (CXC) in the application packages CIAO.\n\nBased on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil).\n\nAccepted Version - 1709.07018.pdf
",
"abstract": "We have shown that Ly\u03b1 blobs (LABs) may still exist even at z ~ 0.3, about seven billion years later than most other LABs known (Shirmer et al.). Their luminous Ly\u03b1 and [O III] emitters at z ~ 0.3 offer new insights into the ionization mechanism. This paper focuses on the two X-ray brightest LABs at z ~ 0.3, SDSS J0113+0106 (J0113) and SDSS J1155\u22120147 (J1155), comparable in size and luminosity to \"B1,\" one of the best-studied LABs at z \u2273\n 2. Our NuSTAR hard X-ray (3\u201330 keV) observations reveal powerful active galactic nuclei (AGN) with L_(2-10 keV) = (0.5-3) x 10^(44) erg s^(\u22121). J0113 also faded by a factor of ~5 between 2014 and 2016, emphasizing that variable AGN may cause apparent ionization deficits in LABs. Joint spectral analyses including Chandra data constrain column densities of N_H = 5.1^(+3.1)_(-3.3) x 10^(23) cm^(\u22122) (J0113) and N_H = 6.0^(+1.4)_(-1.1) x 10^(22) cm^(\u22122) (J1155). J0113 is likely buried in a torus with a narrow ionization cone, but ionizing radiation is also leaking in other directions, as revealed by our Gemini/GMOS 3D spectroscopy. The latter shows a bipolar outflow over 10 kpc, with a peculiar velocity profile that is best explained by AGN flickering. X-ray analysis of J1155 reveals a weakly absorbed AGN that may ionize over a wide solid angle, consistent with our 3D spectra. Extinction-corrected [O III] log-luminosities are high, ~43.6. The velocity dispersions are low, ~100\u2013150 km s^(\u22121), even at the AGN positions. We argue that this is a combination of high extinction hiding the turbulent gas and previous outflows that have cleared the escape paths for their successors.",
"date": "2017-10-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "848",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 42",
"id_number": "CaltechAUTHORS:20170924-173321511",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170924-173321511",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
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},
"doi": "10.3847/1538-4357/aa8e46",
"primary_object": {
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"pub_year": "2017",
"author_list": "Kawamuro, Taiki; Schirmer, Mischa; et el."
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"id": "Younes-G",
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{
"id": "Kouveliotou-C",
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"family": "Kouveliotou",
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"orcid": "0000-0003-1443-593X"
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"family": "Baring",
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{
"id": "van-der-Horst-A-J",
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"family": "van der Horst",
"given": "Alexander J."
},
"orcid": "0000-0001-9149-6707"
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{
"id": "Harding-A-K",
"name": {
"family": "Harding",
"given": "Alice K."
},
"orcid": "0000-0001-6119-859X"
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{
"id": "Hessels-J-W-T",
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"family": "Hessels",
"given": "Jason W. T."
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"orcid": "0000-0003-2317-1446"
},
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"id": "Gehrels-N",
"name": {
"family": "Gehrels",
"given": "Neil"
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"family": "Gill",
"given": "Ramandeep"
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"orcid": "0000-0003-0516-2968"
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{
"id": "Huppenkothen-D",
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"family": "Huppenkothen",
"given": "Daniela"
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"orcid": "0000-0002-1169-7486"
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"id": "Granot-J",
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"orcid": "0000-0001-8530-8941"
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"id": "G\u00f6\u011f\u00fc\u015f-E",
"name": {
"family": "G\u00f6\u011f\u00fc\u015f",
"given": "Ersin"
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"orcid": "0000-0002-5274-6790"
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"id": "Lin-Lin",
"name": {
"family": "Lin",
"given": "Lin"
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"orcid": "0000-0001-6860-9566"
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},
"title": "X-ray and radio observations of the magnetar SGR J1935+2154 during its 2014, 2015, and 2016 outbursts",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "radio continuum: stars \u2013 stars: individual (SGR J1935+2154) \u2013 stars: magnetars \u2013 stars: neutron \u2013 X-rays: stars",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 February 14; revised 2017 August 28; accepted 2017 August 29; published 2017 September 25.\n\nWe thank NuSTAR PI Fiona Harrison and Belinda Wilkes for granting NuSTAR and Chandra DDT observations of SGR J1935+2154 during the 2015 and 2016 outbursts, respectively. We also thank the Swift team for performing the monitoring of the source during all of its outbursts. G.Y. and C.K. acknowledge support by NASA through grant NNH07ZDA001-GLAST. A.J. and J.W.T.H. acknowledge funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007\u20132013) ERC grant agreement no. 337062 (DRAGNET). The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968) and in alliance with Ana G. M\u00e9ndez-Universidad Metropolitana and the Universities Space Research Association. We would like to thank Arecibo observatory scheduler Hector Hernandez for the support during our observations. A.J. thanks Daniele Michilli for helping with the single-pulse search analysis. We thank the anonymous referee for their careful reading and insightful comments that improved the quality of the manuscript.\n\nSoftware: CIAO (http://cxc.harvard.edu/ciao/), SAS (v14.0.0, https://www.cosmos.esa.int/web/xmmnewton/sas), xrtpipeline (v13.2), nustardas (v1.5.1, https://heasarc.gsfc.nasa.gov/docs/nustar/analysis/), HEASOFT (v6.20, https://heasarc.nasa.gov/lheasoft/), ChaRT (http://cxc.harvard.edu/ciao/PSFs/chart2/) MARX (http://space.mit.edu/CXC/MARX/), PRESTO (Ransom 2001; Ransom et al. 2002, 2003), XSPEC (v12.9.0k; Arnaud 1996).\n\nSubmitted - 1702.04370.pdf
",
"abstract": "We analyzed broadband X-ray and radio data of the magnetar SGR J1935+2154 taken in the aftermath of its 2014, 2015, and 2016 outbursts. The source soft X-ray spectrum <10 keV is well described with a blackbody+power-law (BB+PL) or 2BB model during all three outbursts. Nuclear Spectroscopic Telescope Array observations revealed a hard X-ray tail, with a PL photon index \u0393 = 0.9, extending up to 50 keV, with flux comparable to the one detected <10 keV. Imaging analysis of Chandra data did not reveal small-scale extended emission around the source. Following the outbursts, the total 0.5\u201310 keV flux from SGR J1935+2154 increased in concordance to its bursting activity, with the flux at activation onset increasing by a factor of ~7 following its strongest 2016 June outburst. A Swift/X-Ray Telescope observation taken 1.5 days prior to the onset of this outburst showed a flux level consistent with quiescence. We show that the flux increase is due to the PL or hot BB component, which increased by a factor of 25 compared to quiescence, while the cold BB component kT = 0.47 keV remained more or less constant. The 2014 and 2015 outbursts decayed quasi-exponentially with timescales of ~40 days, while the stronger 2016 May and June outbursts showed a quick short-term decay with timescales of about four days. Our Arecibo radio observations set the deepest limits on the radio emission from a magnetar, with a maximum flux density limit of 14 \u03bcJy for the 4.6 GHz observations and 7 \u03bcJy for the 1.4 GHz observations. We discuss these results in the framework of the current magnetar theoretical models.",
"date": "2017-10-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "847",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 85",
"id_number": "CaltechAUTHORS:20170222-114618877",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-114618877",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
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}
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"doi": "10.3847/1538-4357/aa899a",
"primary_object": {
"basename": "1702.04370.pdf",
"url": "https://authors.library.caltech.edu/records/1xkba-ka856/files/1702.04370.pdf"
},
"pub_year": "2017",
"author_list": "Younes, George; Kouveliotou, Chryssa; et el."
},
{
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"eprint_id": 77902,
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"datestamp": "2023-08-19 05:29:04",
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"items": [
{
"id": "Ballo-L",
"name": {
"family": "Ballo",
"given": "L."
}
},
{
"id": "Severgnini-P",
"name": {
"family": "Severgnini",
"given": "P."
}
},
{
"id": "Della-Ceca-R",
"name": {
"family": "Della Ceca",
"given": "R."
}
},
{
"id": "Braito-V",
"name": {
"family": "Braito",
"given": "V."
},
"orcid": "0000-0002-2629-4989"
},
{
"id": "Campana-S",
"name": {
"family": "Campana",
"given": "S."
}
},
{
"id": "Moretti-A",
"name": {
"family": "Moretti",
"given": "A."
}
},
{
"id": "Vignali-C",
"name": {
"family": "Vignali",
"given": "C."
},
"orcid": "0000-0002-8853-9611"
},
{
"id": "Zaino-A",
"name": {
"family": "Zaino",
"given": "A."
}
}
]
},
"title": "XMM-Newton and NuSTAR joint observations of Mrk 915: a deep look into the X-ray properties",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active, X-rays: individual: Mrk 915",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 May 31. Received 2017 May 31; in original form 2017 February 1. Published: 03 June 2017.\n\nBased on observations obtained with the XMM\u2013Newton and the NuSTAR satellites.\n\nWe are grateful to the referee for her/his constructive comments that improved the paper. We warmly thank A. Caccianiga for the useful discussions and helpful suggestions.\n\nSupport from the Italian Space Agency is acknowledged (contract ASI INAF NuSTAR I/037/12/0).\n\nBased on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA, NASA. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology.\n\nThis research has made use of NASA's Astrophysics Data System.\n\nSubmitted - 1705.11114.pdf
",
"abstract": "We report on the X-ray monitoring programme (covering slightly more than 11\u2009d) carried out jointly by XMM\u2013Newton and NuSTAR on the intermediate Seyfert galaxy Mrk 915. The light curves extracted in different energy ranges show a variation in intensity but not a significant change in the spectral shape. The X-ray spectra reveal the presence of a two-phase warm absorber: a fully covering mildly ionized structure [log\u2009\u03be/(erg\u2009cm\u2009s^(\u22121)) \u223c 2.3, N_H \u223c 1.3 \u00d7 10^(21)\u2009cm^(\u22122)] and a partial covering (\u223c90\u2009per cent) lower ionized one [log\u2009\u03be/(erg\u2009cm\u2009s^(\u22121)) \u223c 0.6, N_H \u223c 2 \u00d7 10^(22)\u2009cm^(\u22122)]. A reflection component from distant matter is also present. Finally, a high-column density (N_H \u223c 1.5 \u00d7 10^(23)\u2009cm^(\u22122)) distribution of neutral matter covering a small fraction of the central region is observed, almost constant, in all observations. The main driver of the variations observed between the data sets is a decrease in the intrinsic emission by a factor of \u223c1.5. Slight variations in the partial covering ionized absorber are detected, while the data are consistent with no variation of the total covering absorber. The most likely interpretation of the present data locates this complex absorber closer to the central source than the narrow line region, possibly in the broad line region, in the innermost part of the torus, or in between. The neutral obscurer may either be part of this stratified structure or associated with the walls of the torus, grazed by (and partially intercepting) the line of sight.",
"date": "2017-10-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "470",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "3924-3939",
"id_number": "CaltechAUTHORS:20170601-153652302",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170601-153652302",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
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"doi": "10.1093/mnras/stx1360",
"primary_object": {
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"pub_year": "2017",
"author_list": "Ballo, L.; Severgnini, P.; et el."
},
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"items": [
{
"id": "Ludlam-R-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Sanna-A",
"name": {
"family": "Sanna",
"given": "A."
}
},
{
"id": "Cackett-E-M",
"name": {
"family": "Cackett",
"given": "E. M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Altamirano-D",
"name": {
"family": "Altamirano",
"given": "D."
},
"orcid": "0000-0002-3422-0074"
},
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "A. L."
}
}
]
},
"title": "Truncation of the Accretion Disk at One Third of the Eddington Limit in the Neutron Star Low-Mass X-ray Binary Aquila X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: individual (Aql X-1) \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 July 12; revised 2017 August 30; accepted 2017 September 5; published 2017 October 3. \n\nWe thank the referee for their prompt and thoughtful comments that have improved the quality of this work. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). N.D. is supported by a Vidi grant from the Netherlands Organization for Scientific Research (NWO). E.M.C. gratefully acknowledges support from the National Science Foundation through CAREER award number AST-1351222. D.A. acknowledges support from the Royal Society.\n\nPublished - Ludlam_2017_ApJ_847_135.pdf
Accepted Version - 1709.01559v1.pdf
",
"abstract": "We perform a reflection study on a new observation of the neutron star (NS) low-mass X-ray binary Aquila X-1 taken with NuSTAR during the 2016 August outburst and compare with the 2014 July outburst. The source was captured at ~32% L_(Edd), which is over four times more luminous than the previous observation during the 2014 outburst. Both observations exhibit a broadened Fe line profile. Through reflection modeling, we determine that the inner disk is truncated R_(in,2016) = 11^(+2)_(-1) R_g (where R_g= GM/c^2) and R_(in,2014) = 14 \u00b1 2 R_g (errors quoted at the 90% confidence level). Fiducial NS parameters (M_(NS) = 1.4 M\u2299, R_(NS) = 10 km) give a stellar radius of R_(NS) = 4.85 R g ; our measurements rule out a disk extending to that radius at more than the 6\u03c3 level of confidence. We are able to place an upper limit on the magnetic field strength of B \u2264 3.0\u20134.5 \u00d7 109 G at the magnetic poles, assuming that the disk is truncated at the magnetospheric radius in each case. This is consistent with previous estimates of the magnetic field strength for Aquila X-1. However, if the magnetosphere is not responsible for truncating the disk prior to the NS surface, we estimate a boundary layer with a maximum extent of R_(BL,2016) ~ 10 R_g and R_(BL,2014) ~ 6 R_g. Additionally, we compare the magnetic field strength inferred from the Fe line profile of Aquila X-1 and other NS low-mass X-ray binaries to known accreting millisecond X-ray pulsars.",
"date": "2017-10-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "847",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 135",
"id_number": "CaltechAUTHORS:20170907-090819705",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170907-090819705",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
},
{
"agency": "NSF",
"grant_number": "AST-1351222"
},
{
"agency": "Royal Society"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
},
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"doi": "10.3847/1538-4357/aa8b1b",
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"basename": "Ludlam_2017_ApJ_847_135.pdf",
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}
],
"pub_year": "2017",
"author_list": "Ludlam, R. M.; Miller, J. M.; et el."
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"items": [
{
"id": "Iwasawa-Kazushi",
"name": {
"family": "Iwasawa",
"given": "K."
},
"orcid": "0000-0002-4923-3281"
},
{
"id": "Spoon-H-W-W",
"name": {
"family": "Spoon",
"given": "H. W. W."
},
"orcid": "0000-0002-8712-369X"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Gilli-R",
"name": {
"family": "Gilli",
"given": "R."
}
},
{
"id": "Lanzuisi-G",
"name": {
"family": "Lanzuisi",
"given": "G."
},
"orcid": "0000-0001-9094-0984"
},
{
"id": "Piconcelli-E",
"name": {
"family": "Piconcelli",
"given": "E."
},
"orcid": "0000-0001-9095-2782"
},
{
"id": "Vignali-C",
"name": {
"family": "Vignali",
"given": "C."
},
"orcid": "0000-0002-8853-9611"
},
{
"id": "Brusa-Marcella",
"name": {
"family": "Brusa",
"given": "M."
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"orcid": "0000-0002-5059-6848"
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{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
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},
"title": "The active nucleus of the ULIRG IRAS F00183-7111 viewed by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual: IRAS F00183\u20137111 \u2013 X-rays: galaxies",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences.\n\nReceived 6 April 2017; Accepted 8 August; Published online 23 October 2017.\n\n\nThis research has also made use of data obtained from ESO telescopes at the La Silla Paranal Observatory. The ESO VLT data are under programme IDs 386.B-0346, 088.B-0405, and 090.B-0098.\n\nThe scientific results reported in this article are based on observations made by Chandra X-ray Observatory, Suzaku, NuSTAR and XMM-Newton, and has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. Support for this work was partially provided by NASA through Chandra Award Number GO2-13122X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. K.I. acknowledges support by the Spanish MINECO under grant AYA2016-76012-C3-1-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia \"Mar\u00eda de Maeztu\"). Support from the ASI/INAF grant I/037/12/0 \u2013 011/13 is acknowledged (A.C., M.B., E.P., G.L., R.G. and C.V.).\n\nPublished - aa30950-17.pdf
Submitted - 1709.01708.pdf
",
"abstract": "We present an X-ray study of the ultra-luminous infrared galaxy IRAS F00183\u20137111 (z = 0.327), using data obtained from NuSTAR, Chandra X-ray Observatory, Suzaku and XMM-Newton. The Chandra imaging shows that a point-like X-ray source is located at the nucleus of the galaxy at energies above 2 keV. However, the point source resolves into diffuse emission at lower energies, extending to the east, where the extranuclear [OIII]\u03bb5007 emission, presumably induced by a galactic-scale outflow, is present. The nuclear source is detected by NuSTAR up to the rest-frame 30 keV. The strong, high-ionization Fe K line, first seen by XMM-Newton, and subsequently by Suzaku and Chandra, is not detected in the NuSTAR data. The line flux appears to have been declining continuously between 2003 and 2016, while the continuum emission remained stable to within 30%. Further observations are needed to confirm this. The X-ray continuum below 10 keV is characterised by a hard spectrum caused by cold absorption of N_H\u2009~\u20091 \u00d7 10^(23) cm^(-2), compatible to that of the silicate absorption at 9.7 \u03bcm, and a broad absorption feature around 8 keV which we attribute to a high-ionization Fe K absorption edge. The latter is best described by a blueshifted, high-ionization (log \u03be ~ 3) absorber with a column density of N_H\u2009~\u20091 \u00d7 10^(24) cm^(-2), similar to the X-ray high-velocity outflows observed in a number of active nuclei. No extra hard component, which would arise from a strongly absorbed (i.e. Compton-thick) source, is seen in the NuSTAR data. While a pure reflection scenario (with a totally hidden central source) is viable, direct emission from the central source of L_(2\u221210 keV) \u2243 2 \u00d7 10^(44) erg\u2009s^(-1), behind layers of cold and hot absorbing gas may be an alternative explanation. In this case, the relative X-ray quietness (L_x/L_(bol,AGN) \u2264 6 \u00d7 10^(-3)), the high-ionization Fe line, strong outflows inferred from various observations, and other similarities to the well-studied ULIRG/QSO Mrk 231 point that the central source in this ULIRG might be accreting close to the Eddington limit.",
"date": "2017-10",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "606",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A117",
"id_number": "CaltechAUTHORS:20170907-090416528",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170907-090416528",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "GO2-13122X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)",
"grant_number": "AYA2016-76012-C3-1-P"
},
{
"agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)",
"grant_number": "MDM-2014-0369"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0 011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
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"doi": "10.1051/0004-6361/201730950",
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"pub_year": "2017",
"author_list": "Iwasawa, K.; Spoon, H. W. W.; et el."
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"items": [
{
"id": "Staubert-R",
"name": {
"family": "Staubert",
"given": "R."
}
},
{
"id": "Klochkov-D",
"name": {
"family": "Klochkov",
"given": "D."
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
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"id": "Rothschild-R-E",
"name": {
"family": "Rothschild",
"given": "R. E."
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"name": {
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},
"title": "Inversion of the decay of the cyclotron line energy in Hercules X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "magnetic fields \u2013 binaries: eclipsing \u2013 stars: neutron \u2013 radiation mechanisms: non-thermal \u2013 line: formation \u2013 X-rays: general",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 11 September 2017; Accepted 7 October 2017; Published online 27 October 2017. \n\nThe motivation for this paper are new observational data taken by the NASA satellite NuSTAR and the ESA satellite INTEGRAL. We would like to acknowledge the dedication of all the people who have contributed to the great success of these missions, especially the \"schedulers\" for their efforts with respect to the nonstandard scheduling of the observations of Her X-1. Earlier important data were provided by the equally successful NASA missions RXTE and Swift. We thank the anonymous referee for useful suggestions.\n\nPublished - aa31927-17.pdf
Accepted Version - 1710.05150.pdf
",
"abstract": "Recent observations of Her X-1 with NuSTAR and INTEGRAL in 2016 have provided\nevidence that the 20-year decay of the cyclotron line energy found between 1996\nand 2015 has ended and that an inversion with a new increase, possibly similar\nto the one observed around 1990-1993, has started. We consider this a strong\nmotivation for further observations and for enhanced efforts to significantly\nimprove our theoretical understanding of the accretion process in binary X-ray\npulsars. We speculate about the physics behind the long-term decay and its\ninversion, a possible cyclic behavior, and correlations with other variable\nobservables.",
"date": "2017-10",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "606",
"publisher": "EDP Sciences",
"pagerange": "Art. No. L13",
"id_number": "CaltechAUTHORS:20171017-090658993",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171017-090658993",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
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"doi": "10.1051/0004-6361/201731927",
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"pub_year": "2017",
"author_list": "Staubert, R.; Klochkov, D.; et el."
},
{
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"items": [
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
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{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
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{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl W."
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"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
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"orcid": "0000-0002-1984-2932"
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
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{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
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"orcid": "0000-0002-8074-4186"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram"
},
"orcid": "0000-0003-1703-8796"
}
]
},
"title": "Observational artifacts of Nuclear Spectroscopic Telescope Array: ghost rays and stray light",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Nuclear Spectroscopic Telescope Array; optics; satellite",
"note": "\u00a9 2017 The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI. \n\nPaper 17029P received Jun. 27, 2017; accepted for publication Oct. 3, 2017; published online Oct. 27, 2017. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology.\n\nPublished - 044003.pdf
Accepted Version - 1711.02719.pdf
",
"abstract": "The Nuclear Spectroscopic Telescope Array (NuSTAR) launched in June 2012, flies two conical approximation Wolter-I mirrors at the end of a 10.15-m mast. The optics are coated with multilayers of Pt/C and W/Si that operate from 3 to 80 keV. Since the optical path is not shrouded, aperture stops are used to limit the field of view (FoV) from background and sources outside the FoV. However, there is still a sliver of sky (\u223c1.0\u2009\u2009deg to 4.0 deg) where photons may bypass the optics altogether and fall directly on the detector array. We term these photons stray light. Additionally, there are also photons that do not undergo the focused double reflections in the optics, and we term these ghost rays. We present detailed analysis and characterization of these two components and discuss how they impact observations. Finally, we discuss how they could have been prevented and should be in future observatories.",
"date": "2017-10",
"date_type": "published",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"volume": "3",
"number": "4",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"pagerange": "Art. No. 044003",
"id_number": "CaltechAUTHORS:20180105-081533561",
"issn": "2329-4124",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180105-081533561",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1117/1.JATIS.3.4.044003",
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"basename": "044003.pdf",
"url": "https://authors.library.caltech.edu/records/4n7y1-j6b02/files/044003.pdf"
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{
"basename": "1711.02719.pdf",
"url": "https://authors.library.caltech.edu/records/4n7y1-j6b02/files/1711.02719.pdf"
}
],
"pub_year": "2017",
"author_list": "Madsen, Kristin K.; Christensen, Finn E.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/7w6je-qcy41",
"eprint_id": 78086,
"eprint_status": "archive",
"datestamp": "2023-08-19 05:11:17",
"lastmod": "2023-10-25 23:44:28",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Pahari-M",
"name": {
"family": "Pahari",
"given": "Mayukh"
}
},
{
"id": "McHardy-I-M",
"name": {
"family": "McHardy",
"given": "I. M."
}
},
{
"id": "Mallick-L",
"name": {
"family": "Mallick",
"given": "Labani"
}
},
{
"id": "Dewangan-G-C",
"name": {
"family": "Dewangan",
"given": "G. C."
}
},
{
"id": "Misra-R",
"name": {
"family": "Misra",
"given": "R."
}
}
]
},
"title": "Detection of the high energy cut-off from the Seyfert 1.5 galaxy NGC 5273",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disc \u2013 black hole physics \u2013 galaxies: individual: NGC 5273 \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 June 8. Received 2017 May 31; in original form 2017 March 5. Published: 12 June 2017.\n\nWe thank the referee for constructive comments and suggestions. We are thankful to NuSTAR team for making data publicly available. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). INTEGRAL/ISGRI and Swift/XRT data obtained through the High Energy Astrophysics Science Archive Research Center online service were provided by the NASA/Goddard Space Flight Center.\n\nAccepted Version - 1706.02489.pdf
",
"abstract": "We perform the NuSTAR and Swift/XRT joint energy spectral fitting of simultaneous observations from the broad-line Seyfert 1.5 galaxy NGC 5273. When fitted with the combination of an exponential cut-off power law and a reflection model, a high-energy cut-off is detected at 143\n^(+96)_(\u221240) keV with 2\u03c3 significance. Existence of such cut-off is also consistent with the observed Comptonizing electron temperature when fitted with a Comptonization model independently. We observe a moderate hard X-ray variability of the source over the time-scale of \u223c12 yr using INTEGRAL/ISGRI observations in the energy range of 20\u2013100 keV. When the hard-band count rate (6\u201320 keV) is plotted against the soft-band count rate (3\u20136 keV), a hard offset is observed. Our results indicate that the cut-off energy may not correlate with the coronal X-ray luminosity in a simple manner. Similarities in parameters that describe coronal properties indicate that the coronal structure of NGC 5273 may be similar to that of the broad-line radio galaxy 3C 390.3 and another galaxy MCG-5-23-16, where the coronal plasma is dominated by electrons, rather than electron\u2013positron pairs. Therefore, the coronal cooling is equally efficient to the heating mechanism keeping the cut-off energy at low even at the low accretion rate.",
"date": "2017-09-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "470",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3239-3248",
"id_number": "CaltechAUTHORS:20170612-081242471",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170612-081242471",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx1455",
"primary_object": {
"basename": "1706.02489.pdf",
"url": "https://authors.library.caltech.edu/records/7w6je-qcy41/files/1706.02489.pdf"
},
"pub_year": "2017",
"author_list": "Pahari, Mayukh; McHardy, I. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/eqcpz-9g325",
"eprint_id": 77370,
"eprint_status": "archive",
"datestamp": "2023-08-19 05:04:58",
"lastmod": "2023-10-25 22:58:33",
"type": "article",
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"creators": {
"items": [
{
"id": "D'Ai-Antonino",
"name": {
"family": "D'A\u00ec",
"given": "A."
},
"orcid": "0000-0002-5042-1036"
},
{
"id": "Cusumano-G",
"name": {
"family": "Cusumano",
"given": "G."
}
},
{
"id": "Del-Santo-M",
"name": {
"family": "Del Santo",
"given": "M."
}
},
{
"id": "La-Parola-V",
"name": {
"family": "La Parola",
"given": "V."
},
"orcid": "0000-0002-8087-6488"
},
{
"id": "Segreto-A",
"name": {
"family": "Segreto",
"given": "A."
}
}
]
},
"title": "A broad-band self-consistent modelling of the X-ray spectrum of 4U 1626\u221267",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "line: identification \u2013 line: formation \u2013 stars: individual (4U 1626\u201367)\u2014X-rays: binaries\u2014 X-rays: general",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 May 8. Received 2017 May 7; in original form 2016 December 28. Published: 11 May 2017.\n\nAD acknowledges contract ASI-INAF I/004/11/0.We acknowledge\nthe NASA High Energy Astrophysics Science Archive Research\nCenter (HEASARC) for developing and maintaining the HEASOFT\nsoftware that has been used in this study.\n\nAccepted Version - 1705.03404.pdf
",
"abstract": "The accretion-powered X-ray pulsar 4U 1626\u221267 is one of the few highly magnetized pulsars that accretes through Roche lobe overflow from a low-mass companion. The characteristics of its broad-band spectrum are similar to those of X-ray pulsars hosted in a high-mass X-ray binary system, with a broad resonant cyclotron scattering feature (CRSF) at \u223c37 keV. In this work, we examine the pulse-resolved and the pulse-averaged broad-band spectrum using data from NuSTAR and Swift. We use the Becker & Wolff model of bulk+thermal Comptonization to infer key physical parameters of the accretion column flow and a broad-band model for the disc-reflected spectrum. In the softer X-ray band, we need to add a soft blackbody component with kT_(bb) \u223c 0.5 keV, whose characteristics indicate a possible origin from the neutron star surface. Residuals suggest that the shape of the cyclotron line could be more satisfactorily fitted using a narrow core and broader wings and, at higher energies, a second harmonic could be present at \u223c61 keV.",
"date": "2017-09-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "470",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2457-2468",
"id_number": "CaltechAUTHORS:20170511-100805973",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170511-100805973",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx1146",
"primary_object": {
"basename": "1705.03404.pdf",
"url": "https://authors.library.caltech.edu/records/eqcpz-9g325/files/1705.03404.pdf"
},
"pub_year": "2017",
"author_list": "D'A\u00ec, A.; Cusumano, G.; et el."
},
{
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"eprint_id": 77702,
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"datestamp": "2023-08-19 04:59:36",
"lastmod": "2023-10-25 23:22:08",
"type": "article",
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"creators": {
"items": [
{
"id": "Pozzi-F",
"name": {
"family": "Pozzi",
"given": "F."
}
},
{
"id": "Vallini-L",
"name": {
"family": "Vallini",
"given": "L."
},
"orcid": "0000-0002-3258-3672"
},
{
"id": "Vignali-C",
"name": {
"family": "Vignali",
"given": "C."
},
"orcid": "0000-0002-8853-9611"
},
{
"id": "Talia-M",
"name": {
"family": "Talia",
"given": "M."
},
"orcid": "0000-0003-4352-2063"
},
{
"id": "Gruppioni-C",
"name": {
"family": "Gruppioni",
"given": "C."
},
"orcid": "0000-0002-5836-4056"
},
{
"id": "Mingozzi-M",
"name": {
"family": "Mingozzi",
"given": "M."
}
},
{
"id": "Massardi-M",
"name": {
"family": "Massardi",
"given": "M."
}
},
{
"id": "Andreani-P",
"name": {
"family": "Andreani",
"given": "P."
}
}
]
},
"title": "CO excitation in the Seyfert galaxy NGC 7130",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "photodissociation region (PDR) \u2013 galaxies: active \u2013 galaxies: ISM",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 May 11. Received 2017 May 9; in original form 2017 February 21. Published: 23 May 2017. \n\nWe acknowledge support from the Italian node of the Alma Regional Center. This Letter makes use of the ALMA data ADS/JAO.ALMA#2013.1.00524.S. FP kindly thanks the referees Matthew Malkan and Andrea Cimatti.\n\nSubmitted - 1705.08221.pdf
",
"abstract": "We present a coherent multiband modelling of the carbon monoxide (CO) spectral energy distribution of the local Seyfert galaxy NGC 7130 to assess the impact of the active galactic nucleus (AGN) activity on the molecular gas. We take advantage of all the available data from X-ray to the submillimetre, including ALMA data. The high-resolution (\u223c0.2\u2009arcsec) ALMA CO(6\u20135) data constrain the spatial extension of the CO emission down to an \u223c70 pc scale. From the analysis of the archival Chandra and NuSTAR data, we infer the presence of a buried, Compton-thick AGN of moderate luminosity, L_(2\u201310\u2009keV)\u2009 \u223c\u20091.6 \u00d7 10^(43) erg s^(\u22121). We explore photodissociation and X-ray-dominated-region (PDR and XDR) models to reproduce the CO emission. We find that PDRs can reproduce the CO lines up to J \u223c 6; however, the higher rotational ladder requires the presence of a separate source of excitation. We consider X-ray heating by the AGNs as a source of excitation, and find that it can reproduce the observed CO spectral energy distribution. By adopting a composite PDR+XDR model, we derive molecular cloud properties. Our study clearly indicates the capabilities offered by the current generation of instruments to shed light on the properties of nearby galaxies by adopting state-of-the-art physical modelling.",
"date": "2017-09-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "470",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L64-L68",
"id_number": "CaltechAUTHORS:20170524-093951443",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170524-093951443",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/slx077",
"primary_object": {
"basename": "1705.08221.pdf",
"url": "https://authors.library.caltech.edu/records/wq8vf-2be23/files/1705.08221.pdf"
},
"pub_year": "2017",
"author_list": "Pozzi, F.; Vallini, L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/kbd3a-2rb61",
"eprint_id": 80896,
"eprint_status": "archive",
"datestamp": "2023-08-19 05:00:39",
"lastmod": "2023-10-17 18:34:46",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "G. B."
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "The NuSTAR Serendipitous Survey: Hunting for the Most Extreme Obscured AGN at >10 keV",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 quasars: general \u2013 surveys \u2013 X-rays: galaxies",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 March 10; revised 2017 July 19; accepted 2017 July 19; published 2017 August 28. \n\nThe authors first thank the anonymous referee for the positive and constructive review. We acknowledge support from a Herchel Smith Postdoctoral Research Fellowship of the University of Cambridge (G.B.L.); the Science and Technology Facilities Council (STFC) grants ST/I001573/1 (D.M.A.) and ST/J003697/2 (P.G.); the ERC Advanced Grant FEEDBACK 340442 at the University of Cambridge (J.A.); the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.); CONICYT-Chile grants FONDECYT Regular 1141218 (F.E.B.), FONDECYT 1120061 and 1160999 (E.T.), and Anillo ACT1101 (F.E.B. and E.T.); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06; F.E.B. and E.T.); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics, MAS (F.E.B.); ASI/INAF contract I/037/12/0-011/13 (A.C., A.M., and L.Z.); and Chandra grants GO5-16154X and GO6-17135X (J.A.T.). We thank Yoshihiro Ueda and Roberto Gilli for providing number counts predictions. This work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: Chandra - , ESO La Silla - , Keck - , Magellan - , NuSTAR - , Palomar - , Pan-STARRS - , SDSS - , Swift - , WISE - , XMM-Newton.\n\nPublished - Lansbury_2017_ApJ_846_20.pdf
Submitted - 1707.06651.pdf
",
"abstract": "We identify sources with extremely hard X-ray spectra (i.e., with photon indices of \u0393 \u227e 0.6) in the 13 deg^2 NuSTAR serendipitous survey, to search for the most highly obscured active galactic nuclei (AGNs) detected at > 10 keV. Eight extreme NuSTAR sources are identified, and we use the NuSTARdata in combination with lower-energy X-ray observations (from Chandra, Swift XRT, and XMM-Newton) to characterize the broadband (0.5\u201324 keV) X-ray spectra. We find that all of the extreme sources are highly obscured AGNs, including three robust Compton-thick (CT; N_H > 1.5 x 10^(24) cm^(\u22122)) AGNs at low redshift (z < 0.1) and a likely CT AGN at higher redshift (z = 0.16). Most of the extreme sources would not have been identified as highly obscured based on the low-energy (< 10 keV) X-ray coverage alone. The multiwavelength properties (e.g., optical spectra and X-ray\u2013mid-IR luminosity ratios) provide further support for the eight sources being significantly obscured. Correcting for absorption, the intrinsic rest-frame 10\u201340 keV luminosities of the extreme sources cover a broad range, from \u22485 x 10^(42) to 10^(45) erg s^(\u22121). The estimated number counts of CT AGNs in the NuSTARserendipitous survey are in broad agreement with model expectations based on previous X-ray surveys, except for the lowest redshifts (z < 0.07), where we measure a high CT fraction of f^(obs)_(CT) = 30^(+16)_(-12)%. For the small sample of CT AGNs, we find a high fraction of galaxy major mergers (50% \u00b1 33%) compared to control samples of \"normal\" AGNs.",
"date": "2017-09-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "846",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 20",
"id_number": "CaltechAUTHORS:20170829-101443114",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170829-101443114",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "University of Cambridge"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1160999"
},
{
"agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Center of Excellence in Astrophysics and Associated Technologies (CATA)",
"grant_number": "PFB 06"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "NASA",
"grant_number": "GO5-16154X"
},
{
"agency": "NASA",
"grant_number": "GO6-17135X"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
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},
"doi": "10.3847/1538-4357/aa8176",
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"pub_year": "2017",
"author_list": "Lansbury, G. B.; Balokovi\u0107, M.; et el."
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"items": [
{
"id": "Tsygankov-S-S",
"name": {
"family": "Tsygankov",
"given": "S. S."
},
"orcid": "0000-0002-9679-0793"
},
{
"id": "Doroshenko-V",
"name": {
"family": "Doroshenko",
"given": "V."
}
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{
"id": "Lutovinov-A-A",
"name": {
"family": "Lutovinov",
"given": "A. A."
}
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{
"id": "Mushtukov-A-A",
"name": {
"family": "Mushtukov",
"given": "A. A."
}
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{
"id": "Poutanen-J",
"name": {
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},
"title": "SMC X-3: the closest ultraluminous X-ray source powered by a neutron star with non-dipole magnetic field",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 magnetic fields \u2013 X-rays: binaries \u2013 X-rays: individuals: SMC X-3",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 3 February 2017; Accepted 16 May 2017; Published online 05 September 2017. \n\nThis work was supported by the Russian Science Foundation grant 14-12-01287 (S.S.T., A.A.L., A.A.M.), the Foundations' Professor Pool, the Finnish Cultural Foundation and the Academy of Finland grant 268740 (J.P.). We also acknowledge the support from the COST Action MP1304.\n\nSubmitted - 1702.00966v1.pdf
",
"abstract": "Aims. The magnetic field of accreting neutron stars determines their overall behavior including the maximum possible luminosity. Some models require an above-average magnetic field strength (\u227310^(13) G) in order to explain super-Eddington mass accretion rate in the recently discovered class of pulsating ultraluminous X-ray sources (ULX). The peak luminosity of SMC\u2009X-3 during its major outburst in 2016\u20132017 reached ~2.5 \u00d7 10^(39) erg s^(-1) comparable to that in ULXs thus making this source the nearest ULX-pulsar. Determination of the magnetic field of SMC\u2009X-3 is the main goal of this paper.\nMethods. SMC\u2009X-3 belongs to the class of transient X-ray pulsars with Be optical companions, and exhibited a giant outburst in July 2016\u2013March 2017. The source has been observed over the entire outburst with the Swift/XRT and Fermi/GBM telescopes, as well as the NuSTAR observatory. Collected data allowed us to estimate the magnetic field strength of the neutron star in SMC\u2009X-3 using several independent methods.\nResults. Spin evolution of the source during and between the outbursts, and the luminosity of the transition to the so-called propeller regime in the range of (0.3\u20137) \u00d7 10^(35) erg s^(-1) imply a relatively weak dipole field of (1\u20135) \u00d7 10^(12) G. On the other hand, there is also evidence for a much stronger field in the immediate vicinity of the neutron star surface. In particular, transition from super- to sub-critical accretion regime associated with the cease of the accretion column and very high peak luminosity favor a field that is an order of magnitude stronger. This discrepancy makes SMC\u2009X-3 a good candidate for possessing significant non-dipolar components of the field, and an intermediate source between classical X-ray pulsars and accreting magnetars which may constitute an appreciable fraction of ULX population.",
"date": "2017-09",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "605",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A39",
"id_number": "CaltechAUTHORS:20170206-090626010",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170206-090626010",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"doi": "10.1051/0004-6361/201730553",
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"pub_year": "2017",
"author_list": "Tsygankov, S. S.; Doroshenko, V.; et el."
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"items": [
{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "E. V."
},
"orcid": "0000-0003-3847-3957"
},
{
"id": "Bogdanov-S",
"name": {
"family": "Bogdanov",
"given": "S."
},
"orcid": "0000-0002-9870-2742"
}
]
},
"title": "NuSTAR Hard X-ray Observations of the Energetic Millisecond Pulsars PSR B1821-24, PSR B1937+21, and PSR J0218+4232",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: general \u2013 pulsars: individual (PSR B1821-24, PSR B1937+21, PSR J0218+4232) \u2013 stars: neutron \u2013 X-rays: stars",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 April 11; revised 2017 July 12; accepted 2017 July 18; published 2017 August 22.\n\nWe greatly appreciate discussions with M. Bachetti and C. Markwardt concerning NuSTAR clock timing issues, and K. Forster for the necessary assistance in planning the PSR B1821-24 observations. We thank A. Harding for discussions regarding high-energy magnetospheric emission from pulsars. We also thank S. Ransom for supplying the radio ephemeris of PSR B1821-24. This work was supported under NuSTAR Cycle 1 Guest Observer Program grant NNX15AV29G awarded through Columbia University. E.V.G. thanks Josep Maria Paredes for hosting his sabbatical at the University of Barcelona Institut de Ci\u00e8ncies del Cosmos (ICCUB) and acknowledges support through the \"Programa Estatal de Foment de la Investigaci\u00f2 Cient\u00edfica i T\u00e8cnica d'Excell\u00e8ncia, Convocat\u00f2ria 2014, Unitats d'Excell\u00e8ncia Maria de Maeztu.\" The NuSTAR mission is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The scientific results reported in this article are based in part on data obtained from the Chandra Data Archive. A portion of the results presented are based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. This research has made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. We also acknowledge extensive use of arXiv and the NASA Astrophysics Data Service (ADS).\n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, CXO, XMM.\n\nAccepted Version - 1704.02964.pdf
",
"abstract": "We present Nuclear Spectroscopic Telescope Array (NuSTAR) hard X-ray timing and spectroscopy of the three exceptionally energetic rotation-powered millisecond pulsars PSRs B1821-24, B1937+21, and J0218+4232. By correcting for the frequency and phase drifts of the NuSTAR onboard clock, we are able to recover the intrinsic hard X-ray pulse profiles of all three pulsars with a resolution down to \u2a7d 15 \u00b5s. The substantial reduction of background emission relative to previous broadband X-ray observations allows us to detect for the first time pulsed emission up to ~50 keV, ~20 keV, and ~25 keV for the three pulsars, respectively. We conduct phase-resolved spectroscopy in the 0.5\u201379 keV range for all three objects, obtaining the best measurements yet of the broadband spectral shape and high-energy pulsed emission to date. We find extensions of the same power-law continua seen at lower energies, with no conclusive evidence for a spectral turnover or break. Extrapolation of the X-ray power-law spectrum to higher energies reveals that a turnover in the 100 keV to 100 MeV range is required to accommodate the high-energy \u03b3-ray emission observed with Fermi-LAT, similar to the spectral energy distribution observed for the Crab pulsar.",
"date": "2017-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "845",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 159",
"id_number": "CaltechAUTHORS:20170411-111011349",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170411-111011349",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
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}
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"doi": "10.3847/1538-4357/aa813c",
"primary_object": {
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"pub_year": "2017",
"author_list": "Gotthelf, E. V. and Bogdanov, S."
},
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"items": [
{
"id": "Wright-P-J",
"name": {
"family": "Wright",
"given": "Paul J."
},
"orcid": "0000-0001-9021-611X"
},
{
"id": "Hannah-I-G",
"name": {
"family": "Hannah",
"given": "Iain G."
},
"orcid": "0000-0003-1193-8603"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Glesener-L",
"name": {
"family": "Glesener",
"given": "Lindsay"
},
"orcid": "0000-0001-7092-2703"
},
{
"id": "Krucker-S",
"name": {
"family": "Krucker",
"given": "S\u00e4m"
}
},
{
"id": "Hudson-H-S",
"name": {
"family": "Hudson",
"given": "Hugh S."
},
"orcid": "0000-0001-5685-1283"
},
{
"id": "Smith-D-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
},
{
"id": "Marsh-A-J",
"name": {
"family": "Marsh",
"given": "Andrew J."
},
"orcid": "0000-0003-1086-6900"
},
{
"id": "White-S-M",
"name": {
"family": "White",
"given": "Stephen M."
},
"orcid": "0000-0002-8574-8629"
},
{
"id": "Kuhar-M",
"name": {
"family": "Kuhar",
"given": "Matej"
},
"orcid": "0000-0002-7210-180X"
}
]
},
"title": "Microflare Heating of a Solar Active Region Observed with NuSTAR, Hinode/XRT, and SDO/AIA",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: activity; Sun: corona; Sun: X-rays, gamma rays",
"note": "\u00a9 2017 American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2017 April 12. Accepted 2017 June 16. Published 2017 July 31. \n\nThis paper made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy), and the California Institute of Technology (USA). Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). The Atmospheric Imaging Assembly on the Solar Dynamics Observatory is part of NASA's Living with a Star program. CHIANTI is a collaborative project involving George Mason University and the University of Michigan (USA), and the University of Cambridge (UK). This research made extensive use of the IDL Astronomy Library, the SolarSoft IDL distribution (SSW), and NASA's Astrophysics Data System. \n\nP.J.W. was supported by an EPSRC/Royal Society Fellowship Engagement Award (EP/M00371X/1) and I.G.H. was supported by a Royal Society University Fellowship. M.K. and S.K. were supported by the Swiss National Science Foundation (project number 200021-140308 and 200020-169046). A.J.M. was supported by NASA Earth and Space Science Fellowship award NNX13AM41H. This work was also supported by NASA grants NNX12AJ36G and NNX14AG07G.\n\nThe authors thank the International Space Science Institute (ISSI) for support for the team \"New Diagnostics of Particle Acceleration in Solar Coronal Nanoflares from Chromospheric Observations and Modeling,\" where this work benefited from productive discussions. The authors also thank P. J. A. Sim\u00f5es, S. H. Saar, K. K. Reeves, and J. K. Vogel for their valuable comments. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Hinode (XRT) - , SDO (AIA) - , GOES.-\n\nPublished - Wright_2017_ApJ_844_132.pdf
Submitted - 1706.06108.pdf
",
"abstract": "NuSTAR is a highly sensitive focusing hard X-ray (HXR) telescope and has observed several small microflares in its initial solar pointings. In this paper, we present the first joint observation of a microflare with NuSTAR and Hinode/XRT on 2015 April 29 at ~11:29 UT. This microflare shows the heating of material to several million Kelvin, observed in soft X-rays with Hinode/XRT, and was faintly visible in the extreme ultraviolet with SDO/AIA. For three of the four NuSTAR observations of this region (pre-flare, decay, and post-flare phases), the spectrum is well fitted by a single thermal model of 3.2\u20133.5 MK, but the spectrum during the impulsive phase shows additional emission up to 10 MK, emission equivalent to the A0.1 GOES class. We recover the differential emission measure (DEM) using SDO/AIA, Hinode/XRT, and NuSTAR, giving unprecedented coverage in temperature. We find that the pre-flare DEM peaks at ~3 MK and falls off sharply by 5 MK; but during the microflare's impulsive phase, the emission above 3 MK is brighter and extends to 10 MK, giving a heating rate of about 2.5 x 10^(25) erg s^(\u22121). As the NuSTAR spectrum is purely thermal, we determined upper limits on the possible non-thermal bremsstrahlung emission. We find that for the accelerated electrons to be the source of heating, a power-law spectrum of \u03b4 \u2a7e 7 with a low-energy cutoff E_(c) \u227e 7 keV is required. In summary, this first NuSTAR microflare strongly resembles much more powerful flares.",
"date": "2017-08-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "844",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 132",
"id_number": "CaltechAUTHORS:20170801-090209507",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170801-090209507",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Engineering and Physical Sciences Research Council (EPSRC)",
"grant_number": "EP/M00371X/1"
},
{
"agency": "Royal Society"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "200021-140308"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "200020-169046"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX13AM41H"
},
{
"agency": "NASA",
"grant_number": "NNX12AJ36G"
},
{
"agency": "NASA",
"grant_number": "NNX14AG07G"
}
]
},
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"doi": "10.3847/1538-4357/aa7a59",
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"pub_year": "2017",
"author_list": "Wright, Paul J.; Hannah, Iain G.; et el."
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"items": [
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "P. G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Bucher-J",
"name": {
"family": "Buchner",
"given": "J."
},
"orcid": "0000-0003-0426-6634"
},
{
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"name": {
"family": "Brandt",
"given": "W. N."
},
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"name": {
"family": "Comastri",
"given": "A."
},
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"name": {
"family": "Del Moro",
"given": "A."
}
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"family": "Farrah",
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"name": {
"family": "Gandhi",
"given": "P."
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"name": {
"family": "Harrison",
"given": "F. A."
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"name": {
"family": "Koss",
"given": "M."
},
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"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "L."
},
"orcid": "0000-0002-3249-8224"
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"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
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"family": "Ricci",
"given": "C."
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"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
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"name": {
"family": "Vasudevan",
"given": "R."
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},
"title": "X-ray bolometric corrections for Compton-thick active galactic nuclei",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 galaxies: Seyfert",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 March 3; revised 2017 May 17; accepted 2017 May 19; published 2017 July 17. \n\nWe thank the referee for providing a constructive review of our manuscript, which improved its quality. We also thank Kohei Ichikawa for insights into IR torus modeling and Almudena Alonso-Herrero and Pat Roche for providing the IR data for Figure 1. M. Balokovi\u0107 acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. We acknowledge financial support from the ASI/INAF grant I/037/12/0\u2013011/13 (A.C., A.M.) and the Caltech Kingsley visitor program (A.C.). This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. Furthermore, this research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. \n\nFacility: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission.\n\nPublished - Brightman_2017_ApJ_844_10.pdf
Submitted - 1705.10804.pdf
",
"abstract": "We present X-ray bolometric correction factors, \u03ba_(Bol) (\u2261L_(Bol)/LX), for Compton-thick (CT) active galactic nuclei (AGN) with the aim of testing AGN torus models, probing orientation effects, and estimating the bolometric output of the most obscured AGN. We adopt bolometric luminosities, L_(Bol), from literature infrared (IR) torus modeling and compile published intrinsic 2\u201310 keV X-ray luminosities, L_X, from X-ray torus modeling of NuSTAR data. Our sample consists of 10 local CT AGN where both of these estimates are available. We test for systematic differences in \u03ba_(Bol) values produced when using two widely used IR torus models and two widely used X-ray torus models, finding consistency within the uncertainties. We find that the mean \u03ba_(Bol) of our sample in the range L_(Bol)\u2248 10^(42)\u221210^(45) erg s^\u22121 is log_(10)\u03ba_(Bol) = 1.44\u00b10.12 with an intrinsic scatter of \u223c 0.2 dex, and that our derived \u03ba_(Bol) values are consistent with previously established relationships between \u03ba_(Bol) and L_(Bol) and \u03ba_(Bol) and Eddington ratio (\u03bb_(Edd)). We investigate if \u03ba_(Bol) is dependent on N_H by comparing our results on CT AGN to published results on less-obscured AGN, finding no significant dependence. Since many of our sample are megamaser AGN, known to be viewed edge-on, and furthermore under the assumptions of AGN unification whereby unobscured AGN are viewed face-on, our result implies that\nthe X-ray emitting corona is not strongly anisotropic. Finally, we present \u03ba_(Bol) values for CT AGN identified in X-ray surveys as a function of their observed L_X, where an estimate of their intrinsic L_X is not available, and redshift, useful for estimating the bolometric output of the most obscured AGN across cosmic time.",
"date": "2017-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "844",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 10",
"id_number": "CaltechAUTHORS:20170601-152924591",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170601-152924591",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0\u2013011/13"
},
{
"agency": "Caltech Kingsley visitor program"
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{
"agency": "NASA",
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},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"id": "Space-Radiation-Laboratory"
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"doi": "10.3847/1538-4357/aa75c9",
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}
],
"pub_year": "2017",
"author_list": "Brightman, M.; Balokovi\u0107, M.; et el."
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"type": "article",
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"creators": {
"items": [
{
"id": "Li-Kwan-Lok",
"name": {
"family": "Li",
"given": "K. L."
},
"orcid": "0000-0001-8229-2024"
},
{
"id": "Kong-Albert-K-H",
"name": {
"family": "Kong",
"given": "A. K. H."
},
"orcid": "0000-0002-5105-344X"
},
{
"id": "Tam-Pak-Hin-Thomas",
"name": {
"family": "Tam",
"given": "P. H. T."
},
"orcid": "0000-0002-1262-7375"
},
{
"id": "Hou-Xian",
"name": {
"family": "Hou",
"given": "X."
},
"orcid": "0000-0003-0933-6101"
},
{
"id": "Takata-Jumpei",
"name": {
"family": "Takata",
"given": "J."
},
"orcid": "0000-0002-8731-0129"
},
{
"id": "Hui-David-C-Y",
"name": {
"family": "Hui",
"given": "C. Y."
},
"orcid": "0000-0003-1753-1660"
}
]
},
"title": "Swift, XMM-Newton, and NuSTAR observations of PSR J2032+4127/MT91 213",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (PSR J2032+4127) \u2013 stars: individual (MT91 213) \u2013 stars: winds, outflows \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 April 24; accepted 2017 June 8; published 2017 July 6. \n\nWe thank (i) Neil Gehrels and Brad Cenko for approving our Swift monitoring campaign, (ii) Fiona Harrison for approving the NuSTAR DDT request and Kristin Madsen for the technical support, and (iii) Norbert Schartel for approving the XMM-Newton DDT request and Rosario Gonzalez-Riestra for scheduling the observation. We acknowledge the support of the staff of the Lijiang 2.4 m telescope. Funding for the telescope has been provided by Chinese Academy of Sciences and the Peoples Government of Yunnan Province. The scientific results reported in this article are based in part on data obtained from the Chandra Data Archive. A.K.H.K. is supported by the Ministry of Science and Technology of Taiwan through grants 105-2112-M-007-033-MY2, 105-2119-M-007-028-MY3, and 106-2918-I-007-005. X.H. is supported by National Natural Science Foundation of China through grant 11503078. P.H.T. is supported by the National Science Foundation of China (NSFC) through grants 11633007 and 11661161010. J.T. is supported by NSFC grants of Chinese Government under 11573010 and U1631103. C.Y.H. is supported by the National Research Foundation of Korea through grants 2014R1A1A2058590 and 2016R1A5A1013277. \n\nFacilities: Swift, NuSTAR, XMM, YAO:2.4m, and CXO.\n\nSubmitted - 1705.09653.pdf
",
"abstract": "We report our recent Swift, NuSTAR, and XMM-Newton X-ray and Lijiang optical observations on PSR J2032+4127/MT91 213, the \u03b3-ray binary candidate with a period of 45\u201350 years. The coming periastron of the system was predicted to be in 2017 November, around which high-energy flares from keV to TeV are expected. Recent studies with Chandra and Swift X-ray observations taken in 2015/2016 showed that its X-ray emission has been brighter by a factors of ~10 than that before 2013, probably revealing some ongoing activities between the pulsar wind and the stellar wind. Our new Swift/XRT lightcurve shows no strong evidence of a single vigorous brightening trend, but rather several strong X-ray flares on weekly to monthly timescales with a slowly brightening baseline, namely the low state. The NuSTAR and XMM-Newton observations taken during the flaring and the low states, respectively, show a denser environment and a softer power-law index during the flaring state, implying that the pulsar wind interacted with the stronger stellar winds of the companion to produce the flares. These precursors would be crucial in studying the predicted giant outburst from this extreme \u03b3-ray binary during the periastron passage in late 2017.",
"date": "2017-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "843",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 85",
"id_number": "CaltechAUTHORS:20170531-104412423",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170531-104412423",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Chinese Academy of Sciences"
},
{
"agency": "Peoples Government of Yunnan Province"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "105-2112-M-007-033-MY2"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "105-2119-M-007-028-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "106-2918-I-007-005"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11503078"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11633007"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11661161010"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11573010"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "U1631103"
},
{
"agency": "National Research Foundation of Korea",
"grant_number": "2014R1A1A2058590"
},
{
"agency": "National Research Foundation of Korea",
"grant_number": "2016R1A5A1013277"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa784e",
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"pub_year": "2017",
"author_list": "Li, K. L.; Kong, A. K. H.; et el."
},
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"datestamp": "2023-08-21 21:25:15",
"lastmod": "2023-10-25 23:28:06",
"type": "article",
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"creators": {
"items": [
{
"id": "Kamraj-N",
"name": {
"family": "Kamraj",
"given": "N."
},
"orcid": "0000-0002-3233-2451"
},
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "E."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
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},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
}
]
},
"title": "The NuSTAR View of the Seyfert 2 Galaxy NGC 4388",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 4388); galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 April 22; Accepted 2017 May 25; Published 2017 July 6. \n\nWe have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). M. Balokovi\u0107 acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. \n\nFacility: NuSTAR.\n\nPublished - Kamraj_2017_ApJ_843_89.pdf
Submitted - 1705.09260.pdf
",
"abstract": "We present an analysis of NuSTAR X-ray observations in the 3\u201379 keV energy band of the Seyfert 2 galaxy NGC 4388, taken in 2013. The broadband sensitivity of NuSTAR, covering the Fe K\u03b1 line and Compton reflection hump, enables tight constraints to be placed on reflection features in AGN X-ray spectra, thereby providing insight into the geometry of the circumnuclear material. In this observation, we found the X-ray spectrum of NGC 4388 to be well described by a moderately absorbed power law with non-relativistic reflection. We fit the spectrum with phenomenological reflection models and a physical torus model and find the source to be absorbed by Compton-thin material (N_H = (6.5 \u00b1 0.8) \u00d7 10^(23) cm^(\u22122)) with a very weak Compton reflection hump (R < 0.09) and an exceptionally large Fe K\u03b1 line (EW = 368^(+56)_(-53)\neV) for a source with weak or no reflection. Calculations using a thin-shell approximation for the expected Fe K\u03b1 EW indicate that an Fe K\u03b1 line originating from Compton-thin material presents a possible explanation.",
"date": "2017-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "843",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 89",
"id_number": "CaltechAUTHORS:20170526-095619685",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170526-095619685",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
}
]
},
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"doi": "10.3847/1538-4357/aa7563",
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}
],
"pub_year": "2017",
"author_list": "Kamraj, N.; Rivers, E.; et el."
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"datestamp": "2023-08-19 04:04:36",
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"type": "article",
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"creators": {
"items": [
{
"id": "Zhang-Shuo",
"name": {
"family": "Zhang",
"given": "Shuo"
},
"orcid": "0000-0002-2967-790X"
},
{
"id": "Baganoff-F-K",
"name": {
"family": "Baganoff",
"given": "Frederick K."
}
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "Gabriele"
},
"orcid": "0000-0003-0293-3608"
},
{
"id": "Neilsen-J",
"name": {
"family": "Neilsen",
"given": "Joseph"
},
"orcid": "0000-0002-8247-786X"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
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"orcid": "0000-0001-5506-9855"
},
{
"id": "Dexter-J",
"name": {
"family": "Dexter",
"given": "Jason"
},
"orcid": "0000-0003-3903-0373"
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "Ma\u00efca"
},
"orcid": "0000-0003-0724-2742"
},
{
"id": "Markoff-S",
"name": {
"family": "Markoff",
"given": "Sera"
},
"orcid": "0000-0001-9564-0876"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Barri\u00e8re-N-M",
"name": {
"family": "Barri\u00e8re",
"given": "Nicolas M."
},
"orcid": "0000-0001-9407-9490"
},
{
"id": "Nowak-M-A",
"name": {
"family": "Nowak",
"given": "Michael A."
},
"orcid": "0000-0001-6923-1315"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Sagittarius A* High Energy X-ray Flare Properties During NuSTAR Monitoring of the Galactic Center from 2012 to 2015",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 quasars: supermassive black holes \u2013 radiation mechanisms: non-thermal \u2013\nX-rays: individual (sgra)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 April 12; revised 2017 May 19; accepted 2017 May 22; published 2017 July 10. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). S.Z. acknowledges support by NASA Headquarters under the NASA Earth and Space Science Fellowship Program\u2014Grant \"NNX13AM31H.\" J.N. acknowledges funding from NASA through the Einstein Postdoctoral Fellowship, grant PF2-130097, awarded by the CXC, which is operated by the SAO for NASA under contract NAS8-03060. G.P. acknowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1604) and the Max Planck Society. We thank all members of the Chandra Sgr A* XVP collaboration (http://www.sgra-star.com).\n\nPublished - Zhang_2017_ApJ_843_96.pdf
Submitted - 1705.08002.pdf
",
"abstract": "Understanding the origin of the flaring activity from the Galactic center supermassive black hole Sagittarius A* is a major scientific goal of the NuSTAR Galactic plane survey campaign. We report on the data obtained between 2012 July and 2015 April, including 27 observations on Sgr A*, with a total exposure of \u22431 Ms. We found a total of 10 X-ray flares detected in the NuSTAR observation window, with luminosities in the range of L_(3-79 keV) ~(0.2-4.0) x 10^(35) erg s^(-1). With this largest hard X-ray Sgr A* flare data set to date, we studied the flare spectral properties. Seven flares are detected above 5\u03c3 significance, showing a range of photon indices (\u0393 ~ 2.0\u20132.8) with typical uncertainties of \u00b10.5 (90% confidence level). We found no significant spectral hardening for brighter flares, as indicated by a smaller sample. The accumulation of all of the flare spectra in 1\u201379 keV can be well fit with an absorbed power-law model with \u0393 = 2.2 \u00b1 0.1, and does not require the existence of a spectral break. The lack of variation in the X-ray spectral index with luminosity would point to a single mechanism for the flares and is consistent with the synchrotron scenario. Lastly, we present the quiescent-state spectrum of Sgr A*, and derive an upper limit on the quiescent luminosity of Sgr A* above 10 keV to be L_(Xq,10-79 keV) \u2a7d (2.9 \u00b1 0.2) x 10^(34) erg s^(-1).",
"date": "2017-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "843",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 96",
"id_number": "CaltechAUTHORS:20170524-092936920",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170524-092936920",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX13AM31H"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF2-130097"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)",
"grant_number": "FKZ 50 OR 1604"
},
{
"agency": "Max Planck Society"
}
]
},
"local_group": {
"items": [
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"id": "Space-Radiation-Laboratory"
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"doi": "10.3847/1538-4357/aa74e8",
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],
"pub_year": "2017",
"author_list": "Zhang, Shuo; Baganoff, Frederick K.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-19 04:01:26",
"lastmod": "2023-10-23 22:56:01",
"type": "article",
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"creators": {
"items": [
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman"
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "Ma\u00efca"
},
"orcid": "0000-0003-0724-2742"
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "JaeSub"
}
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "Gabriele"
},
"orcid": "0000-0003-0293-3608"
},
{
"id": "Poutanen-J",
"name": {
"family": "Poutanen",
"given": "Juri"
},
"orcid": "0000-0002-0983-0049"
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Tsgankov-S",
"name": {
"family": "Tsygankov",
"given": "Sergey"
}
}
]
},
"title": "NuSTAR and XMM-Newton observations of the Arches cluster in 2015: fading hard X-ray emission from the molecular cloud",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "ISM: clouds \u2013X-rays: individual: Arches cluster",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 March 7. Received 2017 March 3; in original form 2016 December 10. Published: 09 March 2017. \n\nThis work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration, and re-observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). RK acknowledges support from the Russian Basic Research Foundation (grant 16-02-00294), the Program of the President of the Russian Federation for support of leading scientific schools (project NSh- 10222.2016.2), the Basic Research Program P-7 of the Presidium of the Russian Academy of Science, the Academy of Finland (grant 300005) and hospitality of the Tuorla Observatory, and thanks Eugene Churazov for the Monte Carlo X-ray reflection model used in the paper. GP acknowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408 and FKZ 50 OR 1604) and the Max Planck Society. The authors would like to thank the referee for valuable comments that helped to improve the paper.\n\nSubmitted - 1612.03320v1.pdf
",
"abstract": "We present results of long Nuclear Spectroscopic Telescope Array (NuSTAR; 200 ks) and XMM\u2013Newton (100 ks) observations of the Arches stellar cluster, a source of bright thermal (kT \u223c 2 keV) X-rays with prominent Fe XXV K\u03b1 6.7 keV line emission and a nearby molecular cloud, characterized by an extended non-thermal hard X-ray continuum and fluorescent Fe K\u03b1 6.4 keV line of a neutral or low-ionization state material around the cluster. Our analysis demonstrates that the non-thermal emission of the Arches cloud underwent a dramatic change, with its homogeneous morphology, traced by fluorescent Fe K\u03b1 line emission, vanishing after 2012, revealing three bright clumps. The declining trend of the cloud emission, if linearly fitted, is consistent with half-life decay time of \u223c8 yr. Such strong variations have been observed in several other molecular clouds in the Galactic Centre, including the giant molecular cloud Sgr B2, and point towards a similar propagation of illuminating fronts, presumably induced by the past flaring activity of Sgr A\u22c6. We also detect a significant drop of the equivalent width of the fluorescent Fe Ka line, which could mean either that the new clumps have a different position along the line of sight or that the contribution of cosmic ray has become more dominant.",
"date": "2017-07-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2822-2835",
"id_number": "CaltechAUTHORS:20161213-111643496",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161213-111643496",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx585",
"primary_object": {
"basename": "1612.03320v1.pdf",
"url": "https://authors.library.caltech.edu/records/gbbda-r0y05/files/1612.03320v1.pdf"
},
"pub_year": "2017",
"author_list": "Krivonos, Roman; Clavel, Ma\u00efca; et el."
},
{
"id": "https://authors.library.caltech.edu/records/08wx7-x6r95",
"eprint_id": 75236,
"eprint_status": "archive",
"datestamp": "2023-08-19 04:01:42",
"lastmod": "2023-10-25 14:52:30",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "Stefano"
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "Andrea"
}
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "Giorgio"
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Middei-R",
"name": {
"family": "Middei",
"given": "Riccardo"
},
"orcid": "0000-0001-9815-9092"
},
{
"id": "Barcons-X",
"name": {
"family": "Barcons",
"given": "Xavier"
}
},
{
"id": "Bassani-L",
"name": {
"family": "Bassani",
"given": "Loredana"
}
},
{
"id": "Carrera-F-J",
"name": {
"family": "Carrera",
"given": "Francisco J."
}
},
{
"id": "La-Franca-F",
"name": {
"family": "La Franca",
"given": "Fabio"
}
},
{
"id": "Panessa-F",
"name": {
"family": "Panessa",
"given": "Francesca"
}
}
]
},
"title": "The NuSTAR view of the true Type 2 Seyfert NGC 3147",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: Seyfert \u2013X-rays: individual: NGC 3147",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 March 14. Received 2017 March 13; in original form 2017 January 27. Published: 16 March 2017.\n\nWe would like to thank Kristin Kruse Madsen for her help in interpreting the discrepancy at the iron line energy between the two NuSTAR modules. SB acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0. AM and GM acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. AM acknowledges financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. FP acknowledges the ASI/INAF agreement number 2013-023-R1. XB and FJC acknowledge financial support through grant AYA2015-64346-C2-1-P (MINECO/FEDER).\n\nAccepted Version - 1703.04586.pdf
",
"abstract": "We present the first NuSTAR observation of a 'true' type 2 Seyfert galaxy. The 3\u201340 keV X-ray spectrum of NGC 3147 is characterized by a simple power-law, with a standard \u0393 \u223c 1.7 and an iron emission line, with no need for any further component up to \u223c40 keV. These spectral properties, together with significant variability on time-scales as short as weeks (as shown in a 2014 Swift monitoring campaign), strongly support an unobscured line of sight for this source. An alternative scenario in terms of a Compton-thick source is strongly disfavoured, requiring an exceptional geometrical configuration, whereas a large fraction of the solid angle to the source is filled by a highly ionized gas, whose reprocessed emission would dominate the observed luminosity. Moreover, in this scenario, the implied intrinsic X-ray luminosity of the source would be much larger than the value predicted by other luminosity proxies, like the [O III]\u03bb5007 emission-line extinction-corrected luminosity. Therefore, we confirm with high confidence that NGC 3147 is a true type 2 Seyfert galaxy, intrinsically characterized by the absence of a broad-line region.",
"date": "2017-07-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2740-2744",
"id_number": "CaltechAUTHORS:20170320-101557112",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170320-101557112",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx662",
"primary_object": {
"basename": "1703.04586.pdf",
"url": "https://authors.library.caltech.edu/records/08wx7-x6r95/files/1703.04586.pdf"
},
"pub_year": "2017",
"author_list": "Bianchi, Stefano; Marinucci, Andrea; et el."
},
{
"id": "https://authors.library.caltech.edu/records/508r1-mfq34",
"eprint_id": 75587,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:48:17",
"lastmod": "2023-10-25 15:09:45",
"type": "article",
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"creators": {
"items": [
{
"id": "Garc\u00eda-Bernete-I",
"name": {
"family": "Garc\u00eda-Bernete",
"given": "I."
}
},
{
"id": "Ramos-Almeida-C",
"name": {
"family": "Ramos Almeida",
"given": "C."
}
},
{
"id": "Landt-H",
"name": {
"family": "Landt",
"given": "H."
}
},
{
"id": "Ward-M-J",
"name": {
"family": "Ward",
"given": "M. J."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Acosta-Pulido-J-A",
"name": {
"family": "Acosta-Pulido",
"given": "J. A."
}
}
]
},
"title": "The infrared to X-ray correlation spectra of unobscured type 1 active galactic nuclei",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 infrared: galaxies \u2013X-rays: galaxies",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 March 28. Received 2017 March 28; in original form 2017 January 26. Published: 01 April 2017. \n\nIGB acknowledges financial support from the Instituto de Astrof\u00edsica de Canarias through Fundaci\u00f3n La Caixa. IGB also acknowledges the Durham University for their hospitality during his stay in 2015 March and April when this project was started. CRA acknowledges the Ram\u00f3n y Cajal Program of the Spanish Ministry of Economy and Competitiveness through project RYC-2014-15779 and also the Plan Nacional project AYA2016-76682-C3-2-P. MB acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. We finally acknowledge useful comments from the anonymous referee.\n\nPublished - stx795.pdf
Submitted - 1703.09660.pdf
",
"abstract": "We use new X-ray data obtained with the Nuclear Spectroscopic Telescope Array (NuSTAR), near-infrared (NIR) fluxes and mid-infrared (MIR) spectra of a sample of 24 unobscured type 1 active galactic nuclei (AGN) to study the correlation between various hard X-ray bands between 3 and 80 keV and the infrared (IR) emission. The IR to X-ray correlation spectrum (IRXCS) shows a maximum at \u223c15\u201320 \u03bcm, coincident with the peak of the AGN contribution to the MIR spectra of the majority of the sample. There is also an NIR correlation peak at \u223c2 \u03bcm, which we associate with the NIR bump observed in some type 1 AGN at \u223c1\u20135 \u03bcm and is likely produced by nuclear hot dust emission. The IRXCS shows practically the same behaviour in all the X-ray bands considered, indicating a common origin for all of them. We finally evaluated correlations between the X-ray luminosities and various MIR emission lines. All the lines show a good correlation with the hard X-rays (\u03c1 \u2265 0.7), but we do not find the expected correlation between their ionization potentials and the strength of the IRXCS.",
"date": "2017-07",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "469",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "110-126",
"id_number": "CaltechAUTHORS:20170331-105830442",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-105830442",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Fundaci\u00f3n La Caixa"
},
{
"agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)",
"grant_number": "RYC-2014-15779"
},
{
"agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)",
"grant_number": "AYA2016-76682-C3-2-P"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1093/mnras/stx795",
"primary_object": {
"basename": "1703.09660.pdf",
"url": "https://authors.library.caltech.edu/records/508r1-mfq34/files/1703.09660.pdf"
},
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"basename": "stx795.pdf",
"url": "https://authors.library.caltech.edu/records/508r1-mfq34/files/stx795.pdf"
}
],
"pub_year": "2017",
"author_list": "Garc\u00eda-Bernete, I.; Ramos Almeida, C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/jb8yc-zqb62",
"eprint_id": 76904,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:48:38",
"lastmod": "2023-10-25 16:58:32",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Enoto-Teruaki",
"name": {
"family": "Enoto",
"given": "Teruaki"
},
"orcid": "0000-0003-1244-3100"
},
{
"id": "Shibata-Shinpei",
"name": {
"family": "Shibata",
"given": "Shinpei"
},
"orcid": "0000-0002-8554-9240"
},
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "Takao"
}
},
{
"id": "Suwa-Yudai",
"name": {
"family": "Suwa",
"given": "Yudai"
}
},
{
"id": "Uchide-Takahiko",
"name": {
"family": "Uchide",
"given": "Takahiko"
}
},
{
"id": "Nishioka-Hiroyuki",
"name": {
"family": "Nishioka",
"given": "Hiroyuki"
}
},
{
"id": "Kisaka-Shota",
"name": {
"family": "Kisaka",
"given": "Shota"
}
},
{
"id": "Nakano-Toshio",
"name": {
"family": "Nakano",
"given": "Toshio"
}
},
{
"id": "Murakami-Hiroaki",
"name": {
"family": "Murakami",
"given": "Hiroaki"
}
},
{
"id": "Makishima-Kazuo",
"name": {
"family": "Makishima",
"given": "Kazuo"
}
}
]
},
"title": "Magnetar Broadband X-ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "catalogs \u2013 pulsars: general \u2013 stars: magnetars \u2013 stars: magnetic field \u2013 stars: neutron \u2013 X-rays: stars",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 October 28; revised 2017 April 20; accepted 2017 April 20; published 2017 July 19.\n\nThe authors would like to express their thanks to the Suzaku team for their prompt ToO observations, and to Prof. Hiroyuki Nakanishi for providing his hydrogen column density map of our Galaxy. This work was supported by JSPS KAKENHI grant numbers, 12J03320, 15H00845, 15H03653, 16H00869, 16H02198, 16K17665, 16J06773, 25105507, and 25400221, and the Hakubi project at Kyoto University. This research was also supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence \"Origin and Structure of the Universe.\"\n\nAccepted Version - 1704.07018.pdf
",
"abstract": "The 1\u201370 keV persistent spectra of 15 magnetars, observed with Suzaku from 2006 to 2013, were studied as a complete sample. Combined with early NuSTAR observations of four hard X-ray emitters, nine objects showed a hard power-law emission dominating at \u2273 10 keV with the 15\u201360 keV flux of ~1\u201311 x 10^(-11) erg s^(\u22121) cm^(\u22122). The hard X-ray luminosity L_h, relative to that of a soft-thermal surface radiation L_s, tends to become higher toward younger and strongly magnetized objects. Their hardness ratio, updated from a previous study and defined as \u03be = L_h/L_s, is correlated with the measured spin-down rate P as \u03be = 0.62 x (P/10^(-11)s s^(-1))^(0.72), corresponding to positive and negative correlations with the dipole field strength B_d (\u03be \u221d B^(1.41)_d) and the characteristic age \u03c4_c (\u03be \u221d \u03c4_c^(-0.68)), respectively. Among our sample, five transients were observed during X-ray outbursts, and the results are compared with their long-term 1\u201310 keV flux decays monitored with Swift/XRT and RXTE/PCA. Fading curves of three bright outbursts are approximated by an empirical formula used in the seismology, showing a ~10\u201340 day plateau phase. Transients show the maximum luminosities of L_s ~ 10^(35) erg s^(\u22121), which are comparable to those of persistently bright ones, and fade back to \u227e10^(32) erg s^(\u22121). Spectral properties are discussed in the framework of the magnetar hypothesis.",
"date": "2017-07",
"date_type": "published",
"publication": "Astrophysical Journal Supplement Series",
"volume": "231",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 8",
"id_number": "CaltechAUTHORS:20170425-091843035",
"issn": "1538-4365",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170425-091843035",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4365/aa6f0a",
"primary_object": {
"basename": "1704.07018.pdf",
"url": "https://authors.library.caltech.edu/records/jb8yc-zqb62/files/1704.07018.pdf"
},
"pub_year": "2017",
"author_list": "Enoto, Teruaki; Shibata, Shinpei; et el."
},
{
"id": "https://authors.library.caltech.edu/records/r2r9q-myg16",
"eprint_id": 75576,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:48:10",
"lastmod": "2023-10-25 15:09:25",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Lohfink-A",
"name": {
"family": "Lohfink",
"given": "A."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Tombesi-F",
"name": {
"family": "Tombesi",
"given": "F."
},
"orcid": "0000-0002-6562-8654"
},
{
"id": "Wilkins-D-R",
"name": {
"family": "Wilkins",
"given": "D. R."
}
}
]
},
"title": "The high-Eddington NLS1 Ark 564 has the coolest corona",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 X-rays: individual: Ark 564",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 March 28. Received 2017 March 27; in original form 2017 January 17. Published: 30 March 2017. \n\nEK thanks Julian Malzac, Pierre-Olivier Petrucci, Andrea Marinucci and the participants of the FERO8 meeting in Moravia, Czech Republic for interesting discussions on accretion disc coronae. EK thanks the NuSTAR GO Programme for support under grant NNX15AV26G. EK thanks the Hubble Fellowship Programme. Support for Programme number HST-HF2-51360.001-A was provided by NASA through a Hubble Fellowship grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. ACF acknowledges ERC Advanced Grant 340442. CSR acknowledges support from NASA under grant NNX17AF29G.\n\nPublished - stx792.pdf
Submitted - 1703.09815.pdf
",
"abstract": "Ark 564 is an archetypal Narrow line Seyfert 1 that has been well observed in\nsoft X-rays from 0.3-10 keV, revealing a steep spectrum, strong soft excess,\niron K emission line and dramatic variability on the order of hours. Because of\nits very steep spectrum, observations of the source above 10 keV have been\nsparse. We report here on the first NuSTAR observation of Ark 564. The source\nwas observed for 200 ks with NuSTAR, 50 ks of which were concurrent with Suzaku\nobservations. NuSTAR and Suzaku observed a dramatic flare, in which the hard\nemission is clearly delayed with respect to the soft emission, consistent with\nprevious detections of a low-frequency hard lag found in XMM-Newton data. The\nNuSTAR spectrum is well described by a low-temperature Comptonisation continuum\n(with an electron temperature of 15 +/- 2 keV), which irradiates a highly\nionised disc. No further relativistic broadening or ionized absorption is\nrequired. These spectral results show that Ark 564 has one of the lowest\ntemperature coronae observed by NuSTAR to date. We discuss possible reasons for\nlow-temperature coronae in high-Eddington sources.",
"date": "2017-07",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3489-3498",
"id_number": "CaltechAUTHORS:20170331-101614336",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-101614336",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AV26G"
},
{
"agency": "NASA Hubble Fellowship"
},
{
"agency": "NASA",
"grant_number": "HST-HF2-51360.001-A"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "NASA",
"grant_number": "NNX17AF29G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1093/mnras/stx792",
"primary_object": {
"basename": "1703.09815.pdf",
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"pub_year": "2017",
"author_list": "Kara, E.; Garc\u00eda, J. A.; et el."
},
{
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"eprint_id": 81061,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:56:55",
"lastmod": "2023-10-17 19:23:13",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Beuchert-T",
"name": {
"family": "Beuchert",
"given": "T."
}
},
{
"id": "Markowitz-A-G",
"name": {
"family": "Markowitz",
"given": "A. G."
}
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Keck-M-L",
"name": {
"family": "Keck",
"given": "M. L."
}
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Kadler-M",
"name": {
"family": "Kadler",
"given": "M."
}
},
{
"id": "Brenneman-L-W",
"name": {
"family": "Brenneman",
"given": "L. W."
}
},
{
"id": "Zdziarski-A-A",
"name": {
"family": "Zdziarski",
"given": "A. A."
}
}
]
},
"title": "A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 galaxies: individual: NGC4151 \u2013 galaxies: Seyfert \u2013 X-rays: galaxies",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived: 20 December 2016; Accepted: 27 March 2017; Published online 06 July 2017. \n\nWe thank the anonymous referee for providing us with a number of detailed comments that greatly improved the clarity of this manuscript. We made use of ISIS functions provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/) as well as the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank J. E. Davis for the development of the slxfig module that has been used to prepare the figures in this work. This work used data obtained with the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA) as well as XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.G.M. acknowledges support from NASA grant NNX15AE64G. A.A.Z. has been supported in part by the Polish National Science Centre grants 2013/10/M/ST9/00729 and 2015/18/A/ST9/00746.\n\nPublished - aa30293-16.pdf
Submitted - 1703.10856.pdf
",
"abstract": "We disentangle X-ray disk reflection from complex line-of-sight absorption in the nearby Seyfert NGC 4151, using a suite of Suzaku, NuSTAR, and XMM-Newton observations. Extending upon earlier published work, we pursue a physically motivated model using the latest angle-resolved version of the lamp-post geometry reflection model relxillCp_lp together with a Comptonization continuum. We use the long-look simultaneous Suzaku/NuSTAR observation to develop a baseline model wherein we model reflected emission as a combination of lamp-post components at the heights of 1.2 and 15.0 gravitational radii. We argue for a vertically extended corona as opposed to two compact and distinct primary sources. We find two neutral absorbers (one full-covering and one partial-covering), an ionized absorber (log\u2009\u03be = 2.8), and a highly-ionized ultra-fast outflow, which have all been reported previously. All analyzed spectra are well described by this baseline model. The bulk of the spectral variability between ~1\u2009keV and ~6\u2009keV can be accounted for by changes in the column density of both neutral absorbers, which appear to be degenerate and inversely correlated with the variable hard continuum component flux. We track variability in absorption on both short (2\u2009d) and long (~1\u2009yr) timescales; the observed evolution is either consistent with changes in the absorber structure (clumpy absorber at distances ranging from the broad line region to the inner torus or a dusty radiatively driven wind) or a geometrically stable neutral absorber that becomes increasingly ionized at a rising flux level. The soft X-rays below 1\u2009keV are dominated by photoionized emission from extended gas that may act as a warm mirror for the nuclear radiation.",
"date": "2017-07",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "603",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A50",
"id_number": "CaltechAUTHORS:20170901-090512733",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170901-090512733",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX15AE64G"
},
{
"agency": "National Science Centre (Poland)",
"grant_number": "2013/10/M/ST9/00729"
},
{
"agency": "National Science Centre (Poland)",
"grant_number": "2015/18/A/ST9/00746"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201630293",
"primary_object": {
"basename": "1703.10856.pdf",
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],
"pub_year": "2017",
"author_list": "Beuchert, T.; Markowitz, A. G.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/15rrr-a5g48",
"eprint_id": 74547,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:42:22",
"lastmod": "2023-10-24 22:45:05",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Pavlovi\u0107-M-Z",
"name": {
"family": "Pavlovi\u0107",
"given": "M. Z."
}
}
]
},
"title": "Hydrodynamical and radio evolution of young supernova remnant G1.9+0.3 based on the model of diffusive shock acceleration",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "acceleration of particles \u2013 hydrodynamics \u2013 radiation mechanisms: non-thermal \u2013 cosmic rays \u2013 ISM: individual objects: G1.9+0.3 \u2013 ISM: supernova remnants",
"note": "\u00a9 2017 The Author. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 February 23. Received 2017 February 9; in original form 2016 December 28, Published: 27 February 2017. \n\nThis work is part of project no. 176005 'Emission nebulae: structure and evolution' supported by the Ministry of Education, Science, and Technological Development of the Republic of Serbia. Numerical simulations were run on the PARADOX-IV supercomputing facility at the Scientific Computing Laboratory of the Institute of Physics Belgrade, supported in part by the Ministry of Education, Science and Technological Development of the Republic of Serbia under projects no. ON171017 and OI1611005. Simulations were also run on cluster Jason, belonging to Automated Reasoning Group (ARGO) based at the Department of Computer Science, Faculty of Mathematics, University of Belgrade. I thank the anonymous referee for the very constructive suggestions on this manuscript. I would like to thank D. Uro\u0161evi\u0107 and B. Arbutina for introducing me into this exciting field, continually supporting and encouraging me, but also for the careful reviewing and editing of the typescript. I acknowledge the hospitality of the Osservatorio Astronomico di Palermo where part of this work was carried out, special thanks to Salvatore Orlando and Marco Miceli for their illuminating contributions to this project and also for reading the manuscript. I am grateful to Gilles Ferrand for the extremely helpful discussions, advices and help during this work and its coding. Brian Reville provided valuable discussions on different approaches in SNR modelling. I am indebted to Tara Murphy for kindly providing the currently available MOST radio flux densities, to Dr. Wolfgang Reich for providing Effelsberg radio data and to Rui-Zhi Yang and Leonid Ksenofontov for sharing the X-ray data for G1.9+0.3 and useful explanations. PLUTO is developed at the Turin Astronomical Observatory in collaboration with the Department of Physics of Turin University.\n\nSubmitted - 1702.07418.pdf
",
"abstract": "The radio evolution of, so far the youngest known, Galactic supernova remnant (SNR) G1.9+0.3 is investigated by using three-dimensional (3D) hydrodynamic modelling and non-linear kinetic theory of cosmic ray (CR) acceleration in SNRs. We include consistent numerical treatment of magnetic field amplification (MFA) due to resonant streaming instability. Under the assumption that SNR G1.9+0.3 is the result of a Type Ia supernova explosion located near the Galactic Centre, using widely accepted values for explosion energy 10^(51) erg and ejecta mass 1.4 M\u2299, the non-thermal continuum radio emission is calculated. The main purpose of this paper is to explain radio flux brightening measured over recent decades and also predict its future temporal evolution. We estimate that the SNR is now \u223c120 yr old, expanding in an ambient density of 0.02 cm^(\u22123), and explain its steep radio spectral index only by means of efficient non-linear diffusive shock acceleration (NLDSA). We also make comparison between simulations and observations of this young SNR, in order to test the models and assumptions suggested. Our model prediction of a radio flux density increase of \u223c1.8 per cent yr^(\u22121) during the past two decades agrees well with the measured values. We synthesize the synchrotron spectrum from radio to X-ray and it fits well the Very Large Array, Molonglo Observatory Synthesis Telescope, Effelsberg, Chandra and NuSTAR measurements. We also propose a simplified evolutionary model of the SNR in gamma rays and suggest it may be a promising target for gamma-ray observations at TeV energies with the future generation of instruments like Cherenkov Telescope Array. SNR G1.9+0.3 is the only known Galactic SNR with the increasing flux density and we present here the prediction that the flux density will start to decrease approximately 500 yr from now. We conclude that this is a general property of SNRs in the free expansion phase.",
"date": "2017-06-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1616-1630",
"id_number": "CaltechAUTHORS:20170227-101954539",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170227-101954539",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx497",
"primary_object": {
"basename": "1702.07418.pdf",
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"author_list": "Pavlovi\u0107, M. Z."
},
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"lastmod": "2023-10-25 14:52:20",
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"creators": {
"items": [
{
"id": "Wang-Yanan",
"name": {
"family": "Wang",
"given": "Yanan"
}
},
{
"id": "M\u00e9ndez-M",
"name": {
"family": "M\u00e9ndez",
"given": "Mariano"
}
},
{
"id": "Sanna-A",
"name": {
"family": "Sanna",
"given": "Andrea"
}
},
{
"id": "Altamirano-D",
"name": {
"family": "Altamirano",
"given": "Diego"
},
"orcid": "0000-0002-3422-0074"
},
{
"id": "Belloni-T-M",
"name": {
"family": "Belloni",
"given": "T. M."
}
}
]
},
"title": "The reflection spectrum of the low-mass X-ray binary 4U 1636-53",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 X-rays: individual: 4U 1636\u221253",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 March 15. Received 2017 March 13; in original form 2016 December 23. Published: 17 March 2017.\n\nWe thank the referee for many invaluable comments and suggestions. We also thank, Thomas Dauser, for the kind explanation of their models, RELXILL and RELXILLLP. DA acknowledges support from the Royal Society. TMB acknowledges financial contribution from the agreement ASI-INAF I/037/12/0. This research is based on the data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA. This work has made use of data from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA/Goddard Space Flight Center (GSFC).\n\nSubmitted - 1703.05607.pdf
",
"abstract": "We present 3\u201379 keV NuSTAR observations of the neutron star low-mass X-ray binary 4U 1636\u221253 in the soft, transitional and hard state. The spectra display a broad emission line at 5\u201310 keV. We applied several models to fit this line: A GAUSSIAN line, a relativistically broadened emission line model, KYRLINE, and two models including relativistically smeared and ionized reflection off the accretion disc with different coronal heights, RELXILL and RELXILLLP. All models fit the spectra well; however, the KYRLINE and RELXILL models yield an inclination of the accretion disc of \u223c88\u00b0 with respect to the line of sight, which is at odds with the fact that this source shows no dips or eclipses. The RELXILLLP model, on the other hand, gives a reasonable inclination of \u223c56\u00b0. We discuss our results for these models in this source and the possible primary source of the hard X-rays.",
"date": "2017-06-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2256-2264",
"id_number": "CaltechAUTHORS:20170320-100112676",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170320-100112676",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx671",
"primary_object": {
"basename": "1703.05607.pdf",
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"pub_year": "2017",
"author_list": "Wang, Yanan; M\u00e9ndez, Mariano; et el."
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"items": [
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "G."
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"orcid": "0000-0003-0293-3608"
},
{
"id": "George-E",
"name": {
"family": "George",
"given": "E."
}
},
{
"id": "Scaringi-S",
"name": {
"family": "Scaringi",
"given": "S."
}
},
{
"id": "Zhang-S",
"name": {
"family": "Zhang",
"given": "S."
}
},
{
"id": "Jin-C",
"name": {
"family": "Jin",
"given": "C."
}
},
{
"id": "Dexter-J",
"name": {
"family": "Dexter",
"given": "J."
},
"orcid": "0000-0003-3903-0373"
},
{
"id": "Terrier-R",
"name": {
"family": "Terrier",
"given": "R."
}
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "M."
},
"orcid": "0000-0003-0724-2742"
},
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Eisenhauer-F",
"name": {
"family": "Eisenhauer",
"given": "F."
}
},
{
"id": "Genzel-R",
"name": {
"family": "Genzel",
"given": "R."
},
"orcid": "0000-0002-2767-9653"
},
{
"id": "Gillessen-S",
"name": {
"family": "Gillessen",
"given": "S."
}
},
{
"id": "Goldwurm-A",
"name": {
"family": "Goldwurm",
"given": "A."
}
},
{
"id": "Habibi-M",
"name": {
"family": "Habibi",
"given": "M."
}
},
{
"id": "Haggard-D",
"name": {
"family": "Haggard",
"given": "D."
},
"orcid": "0000-0001-6803-2138"
},
{
"id": "Hailey-C",
"name": {
"family": "Hailey",
"given": "C."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Merloni-A",
"name": {
"family": "Merloni",
"given": "A."
}
},
{
"id": "Mori-K",
"name": {
"family": "Mori",
"given": "K."
}
},
{
"id": "Nandra-K",
"name": {
"family": "Nandra",
"given": "K."
},
"orcid": "0000-0002-7150-9192"
},
{
"id": "Ott-T",
"name": {
"family": "Ott",
"given": "T."
}
},
{
"id": "Pfuhl-O",
"name": {
"family": "Pfuhl",
"given": "O."
}
},
{
"id": "Plewa-P-M",
"name": {
"family": "Plewa",
"given": "P. M."
}
},
{
"id": "Waisberg-I",
"name": {
"family": "Waisberg",
"given": "I."
}
}
]
},
"title": "A powerful flare from Sgr A* confirms the synchrotron nature of the X-ray emission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 methods: data analysis \u2013 Galaxy: centre",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 March 8. Received 2017 March 8; in original form 2016 October 12. Published: 10 March 2017.\n\nThe authors wish to thank Jan-Uwe Ness, Ignacio de la Calle, Karl Foster and the rest of the XMM\u2013Newton and NuSTAR scheduling teams for the enormous support that made this multiwavelength campaign possible, as well as the referee for the careful reading of the paper. GP thanks Mark R. Morris, Gabriele Ghisellini, Lorenzo Sironi, Hendrik J. van Eerten, Michi Baub\u00f6ck and Francesco Coti-Zelati, for useful discussion. RT and AG acknowledge support from CNES. This research has made use both of data obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and on data obtained from the Chandra Data Archive. The GC XMM\u2013Newton monitoring project is supported by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408 and FKZ 50 OR 1604) and the Max Planck Society.\n\nPublished - Ponti_2017p2447.pdf
Submitted - 1703.03410.pdf
",
"abstract": "We present the first fully simultaneous fits to the near-infrared (NIR) and X-ray spectral slope (and its evolution) during a very bright flare from Sgr A*, the supermassive black hole at the Milky Way's centre. Our study arises from ambitious multiwavelength monitoring campaigns with XMM\u2013Newton, NuSTAR and SINFONI. The average multiwavelength spectrum is well reproduced by a broken power law with \u0393_(NIR) = 1.7 \u00b1 0.1 and \u0393_X = 2.27 \u00b1 0.12. The difference in spectral slopes (\u0394\u0393 = 0.57 \u00b1 0.09) strongly supports synchrotron emission with a cooling break. The flare starts first in the NIR with a flat and bright NIR spectrum, while X-ray radiation is detected only after about 10^3 s, when a very steep X-ray spectrum (\u0394\u0393 = 1.8 \u00b1 0.4) is observed. These measurements are consistent with synchrotron emission with a cooling break and they suggest that the high-energy cut-off in the electron distribution (\u03b3_(max)) induces an initial cut-off in the optical\u2013UV band that evolves slowly into the X-ray band. The temporal and spectral evolution observed in all bright X-ray flares are also in line with a slow evolution of \u03b3_(max). We also observe hints for a variation of the cooling break that might be induced by an evolution of the magnetic field (from B \u223c 30 \u00b1 8 G to B \u223c 4.8 \u00b1 1.7 G at the X-ray peak). Such drop of the magnetic field at the flare peak would be expected if the acceleration mechanism is tapping energy from the magnetic field, such as in magnetic reconnection. We conclude that synchrotron emission with a cooling break is a viable process for Sgr A*'s flaring emission.",
"date": "2017-06-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2447-2468",
"id_number": "CaltechAUTHORS:20170314-130058938",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170314-130058938",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)",
"grant_number": "FKZ 50 OR 1408"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)",
"grant_number": "FKZ 50 OR 1604"
},
{
"agency": "Max Planck Society"
}
]
},
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"id": "Space-Radiation-Laboratory"
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{
"id": "Astronomy-Department"
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},
"doi": "10.1093/mnras/stx596",
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"pub_year": "2017",
"author_list": "Ponti, G.; George, E.; et el."
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"datestamp": "2023-08-19 03:40:34",
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"items": [
{
"id": "Gaggero-D",
"name": {
"family": "Gaggero",
"given": "Daniele"
}
},
{
"id": "Bertone-G",
"name": {
"family": "Bertone",
"given": "Gianfranco"
}
},
{
"id": "Calore-F",
"name": {
"family": "Calore",
"given": "Francesca"
}
},
{
"id": "Connors-R-M-T",
"name": {
"family": "Connors",
"given": "Riley M. T."
},
"orcid": "0000-0002-8908-759X"
},
{
"id": "Lovell-M",
"name": {
"family": "Lovell",
"given": "Mark"
}
},
{
"id": "Markoff-S",
"name": {
"family": "Markoff",
"given": "Sera"
},
"orcid": "0000-0001-9564-0876"
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"id": "Storm-E",
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},
"title": "Searching for Primordial Black Holes in the radio and X-ray sky",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 American Physical Society.\n\nReceived 9 December 2016; revised manuscript received 12 May 2017; published 12 June 2017.\n\nWe are indebted to M. Fornasa for verifying of the phase-space velocity at low radii with the Eddington formalism. We thank P.\u2009D. Serpico for his useful comments on the manuscript and D. Baumann, P. Crumley, B. Freivogel, A. King, A. Urbano, J. Vink, and C. Weniger for useful discussions. Finally, we thank the anonymous reviewers for their insightful comments and suggestions. R.\u2009C. is supported by the Netherlands Research School for Astronomy (NOVA). S.\u2009M. acknowledges support from the Netherlands Organization for Scientific Research (NWO) VICI Grant No. 639.043.513. E.\u2009S. is supported by the Netherlands Organization for Scientific Research (NWO) through a Vidi grant (PI: C. Weniger).\n\nSubmitted - 1612.00457v1.pdf
",
"abstract": "We model the accretion of gas onto a population of massive primordial black holes in the Milky Way and compare the predicted radio and x-ray emission with observational data. We show that, under conservative assumptions on the accretion process, the possibility that O(10)M\u2299 primordial black holes can account for all of the dark matter in the Milky Way is excluded at 5\u03c3 by a comparison with a Very Large Array radio catalog at 1.4 GHz and at \u224340\u03c3 by a comparison with a Chandra x-ray catalog (0.5\u20138 keV). We argue that this method can be used to identify such a population of primordial black holes with more sensitive future radio and x-ray surveys.",
"date": "2017-06-16",
"date_type": "published",
"publication": "Physical Review Letters",
"volume": "118",
"number": "24",
"publisher": "American Physical Society",
"pagerange": "Art. No. 241101",
"id_number": "CaltechAUTHORS:20161209-151329043",
"issn": "0031-9007",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161209-151329043",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1103/PhysRevLett.118.241101",
"primary_object": {
"basename": "1612.00457v1.pdf",
"url": "https://authors.library.caltech.edu/records/rf4wx-nn020/files/1612.00457v1.pdf"
},
"pub_year": "2017",
"author_list": "Gaggero, Daniele; Bertone, Gianfranco; et el."
},
{
"id": "https://authors.library.caltech.edu/records/stj7q-x3989",
"eprint_id": 73770,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:32:05",
"lastmod": "2023-10-24 16:26:08",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Belmont-R",
"name": {
"family": "Belmont",
"given": "R."
}
},
{
"id": "Malzac-J",
"name": {
"family": "Malzac",
"given": "J."
}
},
{
"id": "Coppi-P",
"name": {
"family": "Coppi",
"given": "P."
}
}
]
},
"title": "Properties of AGN coronae in the NuSTAR era \u2013 II. Hybrid plasma",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013X-rays: binaries",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 January 23. Received 2017 January 13; in original form 2016 December 14. Published: 09 February 2017.\n\nWe thank the referee for helpful comments. ACF and AL acknowledge support from ERC Advanced Grant FEEDBACK 340442. R. Belmont and J. Malzac acknowledge financial support from the French National Research Agency (CHAOS project ANR-12-BS05-0009).\n\nSubmitted - 1701.06774v1.pdf
",
"abstract": "The corona, a hot cloud of electrons close to the centre of the accretion disc, produces the hard X-ray power-law continuum commonly seen in luminous active galactic nuclei. The continuum has a high-energy turnover, typically in the range of one to several 100 keV and is suggestive of Comptonization by thermal electrons. We are studying hard X-ray spectra of AGN obtained with NuSTAR after correction for X-ray reflection and under the assumption that coronae are compact, being only a few gravitational radii in size as indicated by reflection and reverberation modelling. Compact coronae raise the possibility that the temperature is limited and indeed controlled by electron\u2013positron pair production, as explored earlier (Paper I). Here, we examine hybrid plasmas in which a mixture of thermal and non-thermal particles is present. Pair production from the non-thermal component reduces the temperature leading to a wider temperature range more consistent with observations.",
"date": "2017-06-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "467",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2566-2570",
"id_number": "CaltechAUTHORS:20170127-082425783",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-082425783",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx221",
"primary_object": {
"basename": "1701.06774v1.pdf",
"url": "https://authors.library.caltech.edu/records/stj7q-x3989/files/1701.06774v1.pdf"
},
"pub_year": "2017",
"author_list": "Fabian, A. C.; Lohfink, A. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/nqv24-2sh58",
"eprint_id": 77857,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:33:07",
"lastmod": "2023-10-25 23:31:00",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "Anne M."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "David R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "Peter"
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "Duncan"
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier"
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The X-Ray Reflection Spectrum of the Radio-loud Quasar 4C 74.26",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 quasars: individual (4C 74.26) \u2013 quasars: supermassive black holes \u2013 X-rays: individual (4C 74.26)",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 January 2; revised 2017 April 3; accepted 2017 April 10; published 2017 May 26.\n\nThe authors thank the referee for the useful comments that have helped to improve the manuscript. A.L. acknowledges support from the ERC Advanced Grant FEEDBACK 340442 and useful discussions with Niel Brandt. J.A.G. acknowledges partial funding provided by the Alexander von Humboldt Foundation. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Lohfink_2017_ApJ_841_80.pdf
Submitted - 1704.03673.pdf
",
"abstract": "The relativistic jets created by some active galactic nuclei are important agents of AGN feedback. In spite of this, our understanding of what produces these jets is still incomplete. X-ray observations, which can probe the processes operating in the central regions in the immediate vicinity of the supermassive black hole, the presumed jet launching point, are potentially particularly valuable in illuminating the jet formation process. Here, we present the hard X-ray NuSTAR observations of the radio-loud quasar 4C 74.26 in a joint analysis with quasi-simultaneous, soft X-ray Swift observations. Our spectral analysis reveals a high-energy cutoff of 183^(+51)_(-35) keV and confirms the presence of ionized reflection in the source. From the average spectrum we detect that the accretion disk is mildly recessed, with an inner radius of R_(in) = 4\u2013180 R_g. However, no significant evolution of the inner radius is seen during the three months covered by our NuSTAR campaign. This lack of variation could mean that the jet formation in this radio-loud quasar differs from what is observed in broad-line radio galaxies.",
"date": "2017-06-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "841",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 80",
"id_number": "CaltechAUTHORS:20170531-110427362",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170531-110427362",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aa6d07",
"primary_object": {
"basename": "Lohfink_2017_ApJ_841_80.pdf",
"url": "https://authors.library.caltech.edu/records/nqv24-2sh58/files/Lohfink_2017_ApJ_841_80.pdf"
},
"related_objects": [
{
"basename": "1704.03673.pdf",
"url": "https://authors.library.caltech.edu/records/nqv24-2sh58/files/1704.03673.pdf"
}
],
"pub_year": "2017",
"author_list": "Lohfink, Anne M.; Fabian, Andrew C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/xk78a-qg170",
"eprint_id": 77292,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:32:26",
"lastmod": "2023-10-25 22:03:13",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Pandey-Ashwani",
"name": {
"family": "Pandey",
"given": "Ashwani"
},
"orcid": "0000-0003-3590-4459"
},
{
"id": "Gupta-Alok-C",
"name": {
"family": "Gupta",
"given": "Alok C."
},
"orcid": "0000-0002-9331-4388"
},
{
"id": "Wiita-P-J",
"name": {
"family": "Wiita",
"given": "Paul J."
},
"orcid": "0000-0002-1029-3746"
}
]
},
"title": "X-ray Intraday Variability of Five TeV Blazars with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "BL Lacertae objects: general \u2013 BL Lacertae objects: individual (1ES 0229+200, Mrk 421, Mrk 501, 1ES 1959+650, PKS 2155\u2212304)",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 September 19; revised 2017 April 24; accepted 2017 April 27; published 2017 June 2.\n\nA.C.G. is partially supported by the Chinese Academy of Sciences (CAS) President's International Fellowship Initiative (PIFI; grant No. 2016VMB073). P.J.W. is grateful for hospitality at KIPAC, Stanford University, during a sabbatical. This research has made use of data obtained with NuSTAR, the first focusing hard X-ray mission managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA).\n\nAccepted Version - 1705.02719.pdf
",
"abstract": "We have examined 40 Nuclear Spectroscopic Telescope Array (NuSTAR) light curves (LCs) of five TeV emitting high synchrotron peaked blazars: 1ES 0229+200, Mrk 421, Mrk 501, 1ES 1959+650, and PKS 2155\u2212304. Four of the blazars showed intraday variability in the NuSTAR energy range of 3\u201379 keV. Using an autocorrelation function analysis we searched for intraday variability timescales in these LCs and found indications of several between 2.5 and 32.8 ks in eight LCs of Mrk 421, a timescale around 8.0 ks for one LC of Mrk 501, and timescales of 29.6 and 57.4 ks in two LCs of PKS 2155-304. The other two blazars' LCs do not show any evidence for intraday variability timescales shorter than the lengths of those observations; however, the data were both sparser and noisier for them. We found positive correlations with zero lag between soft (3\u201310 keV) and hard (10\u201379 keV) bands for most of the LCs, indicating that their emissions originate from the same electron population. We examined spectral variability using a hardness ratio analysis and noticed a general \"harder-when-brighter\" behavior. The 22 LCs of Mrk 421 observed between 2012 July and 2013 April show that this source was in a quiescent state for an extended period of time and then underwent an unprecedented double-peaked outburst while monitored on a daily basis during 2013 April 10\u201316. We briefly discuss models capable of explaining these blazar emissions.",
"date": "2017-06-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "841",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 123",
"id_number": "CaltechAUTHORS:20170509-092855159",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170509-092855159",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa705e",
"primary_object": {
"basename": "1705.02719.pdf",
"url": "https://authors.library.caltech.edu/records/xk78a-qg170/files/1705.02719.pdf"
},
"pub_year": "2017",
"author_list": "Pandey, Ashwani; Gupta, Alok C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/jx4ew-vh277",
"eprint_id": 77068,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:17:57",
"lastmod": "2023-10-25 17:16:27",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Annuar-A",
"name": {
"family": "Annuar",
"given": "A."
},
"orcid": "0000-0003-0387-1429"
},
{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "G. B."
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "P. G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Del-Moro-A",
"name": {
"family": "Del Moro",
"given": "A."
}
},
{
"id": "Elvis-M",
"name": {
"family": "Elvis",
"given": "M."
}
},
{
"id": "Guainazzi-M",
"name": {
"family": "Guainazzi",
"given": "M."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Lamperti-I",
"name": {
"family": "Lamperti",
"given": "I."
},
"orcid": "0000-0003-3336-5498"
},
{
"id": "Malaguti-G",
"name": {
"family": "Malaguti",
"given": "G."
}
},
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "E."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The weak Fe fluorescence line and long-term X-ray evolution of the Compton-thick active galactic nucleus in NGC 7674",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 February 8. Received 2017 February 7; in original form 2016 May 24. Published: 13 February 2017. \n\nThis research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester (Evans et al. 2009). PG thanks the Science and Technology Facilities Council (STFC) for support (grant reference ST/J003697/2). AC and AM acknowledge support from the ASI/INAF grant I/037/12/0-011/13. AC acknowledges the Caltech Kingsley visitor programme. We acknowledge financial support from Majlis Amanah Rakyat (MARA) Malaysia (AA), STFC grants ST/I0015731/1 (DMA) and ST/K501979/1 (GBL). WNB acknowledges California Institute of Technology (Caltech) NuSTAR subcontract 44A-1092750. SB acknowledges financial contribution from the agreement ASI-INAF I/037/12/0. We also acknowledge NASA NuSTAR A01 Award NNX15AV27G (FEB), CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB, CR), FONDECYT Regular 1141218 (FEB, CR), 'EMBIGGEN' Anillo ACT1101 (FEB, CR) and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). We thank the referee for detailed comments that helped us to make the presentation of results clearer and to place the discussion on a more robust footing.\n\nPublished - stx357.pdf
Submitted - 1605.08041.pdf
",
"abstract": "We present NuSTAR X-ray observations of the active galactic nucleus (AGN) in NGC\u20097674. The source shows a flat X-ray spectrum, suggesting that it is obscured by Compton-thick gas columns. Based upon long-term flux dimming, previous work suggested the alternate possibility that the source is a recently switched-off AGN with the observed X-rays being the lagged echo from the torus. Our high-quality data show the source to be reflection-dominated in hard X-rays, but with a relatively weak neutral Fe K\u03b1 emission line (equivalent width [EW] of \u2248 0.4 keV) and a strong Fe xxvi ionized line (EW \u2248 0.2 keV). We construct an updated long-term X-ray light curve of NGC\u20097674 and find that the observed 2\u201310 keV flux has remained constant for the past \u2248 20 yr, following a high-flux state probed by Ginga. Light travel time arguments constrain the minimum radius of the reflector to be \u223c 3.2 pc under the switched-off AGN scenario, \u2248 30 times larger than the expected dust sublimation radius, rendering this possibility unlikely. A patchy Compton-thick AGN (CTAGN) solution is plausible, requiring a minimum line-of-sight column density (N_H) of 3 \u00d7 10^(24) cm^(\u22122) at present, and yields an intrinsic 2\u201310 keV luminosity of (3\u20135) \u00d7 10^(43) erg\u2009s^(\u22121). Realistic uncertainties span the range of \u2248 (1\u201313) \u00d7 10^(43) erg\u2009s^(\u22121). The source has one of the weakest fluorescence lines amongst bona fide CTAGN, and is potentially a local analogue of bolometrically luminous systems showing complex neutral and ionized Fe emission. It exemplifies the difficulty of identification and proper characterization of distant CTAGN based on the strength of the neutral Fe K\u03b1 line.",
"date": "2017-06",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "467",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4606-4621",
"id_number": "CaltechAUTHORS:20170428-150646304",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170428-150646304",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Caltech Kingsley Visitor Program"
},
{
"agency": "Majlis Amanah Rakyat (MARA)"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I0015731/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "NASA",
"grant_number": "NNX15AV27G"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
}
]
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"doi": "10.1093/mnras/stx357",
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"family": "Harrison",
"given": "F. A."
},
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{
"id": "Ho-Luis-C",
"name": {
"family": "Ho",
"given": "L. C."
},
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"name": {
"family": "Iwasawa",
"given": "K."
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"family": "Sanders",
"given": "D. B."
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},
"title": "Growing supermassive black holes in the late stages of galaxy mergers are heavily obscured",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 The Authors. \n\nAccepted 2017 January 18. Received 2017 January 17; in original form 2016 December 2. \n\nWe thank the referee for the careful reading of the manuscript and\nfor the prompt report that helped us improve the quality of the\npaper. We thank the NuSTAR Cycle 1 TAC for the NuSTAR data\non which this paper is based, Chin-Shin Chang, George Lansbury,\nDave Alexander and Johannes Buchner for useful comments on the\nmanuscript. This work made use of data from the NuSTAR mission,\na project led by the California Institute of Technology, managed by\nthe Jet Propulsion Laboratory and funded by the National Aeronautics\nand Space Administration. We thank the NuSTAR Operations,\nSoftware and Calibration teams for support with the execution and\nanalysis of these observations. This research has made use of the\nNuSTAR Data Analysis Software (NUSTARDAS) jointly developed by\nthe ASI Science Data Center (ASDC, Italy) and the California Institute\nof Technology (Caltech, USA), and of the NASA/ IPAC\nInfrared Science Archive and NASA/IPAC Extragalactic Database\n(NED), which are operated by the Jet Propulsion Laboratory, California\nInstitute of Technology, under contract with the National\nAeronautics and Space Administration. We acknowledge financial\nsupport from the CONICYT-Chile grants 'EMBIGGEN' Anillo\nACT1101 (CR, FEB, ET), FONDECYT 1141218 (CR, FEB),\nFONDECYT 1160999 (ET), FONDECYT 3150361 (GP), Basal-\nCATA PFB\u201306/2007 (CR, FEB, ET), the NASA NuSTAR AO1\nAward NNX15AV27G (FEB), the China-CONICYT fund (CR),\nthe Swiss National Science Foundation (Grant PP00P2_138979/1\nand PP00P2_166159, KS), the Chinese Academy of Science grant\n\nPublished - stx173.pdf
",
"abstract": "Mergers of galaxies are thought to cause significant gas inflows to the inner parsecs, which\ncan activate rapid accretion on to supermassive black holes (SMBHs), giving rise to active\ngalactic nuclei (AGN). During a significant fraction of this process, SMBHs are predicted to\nbe enshrouded by gas and dust. Studying 52 galactic nuclei in infrared-selected local luminous\nand ultraluminous infrared galaxies in different merger stages in the hard X-ray band, where\nradiation is less affected by absorption, we find that the amount of material around SMBHs\nincreases during the last phases of the merger. We find that the fraction of Compton-thick\n(CT, NH \u2265 10^(24) cm^\u22122) AGN in late-merger galaxies is higher (fCT = 65+12\n\u221213 per cent) than\nin local hard X-ray selected AGN (f CT = 27 \u00b1 4 per cent), and that obscuration reaches\nits maximum when the nuclei of the two merging galaxies are at a projected distance of\nD12 \u2243 0.4\u201310.8 kpc (fCT = 77+13\n\u221217 per cent). We also find that all AGN of our sample in\nlate-merger galaxies have NH > 10^(23) cm^\u22122, which implies that the obscuring material covers\n95+4\n\u22128 per cent of the X-ray source. These observations show that the material is most effectively\nfunnelled from the galactic scale to the inner tens of parsecs during the late stages of\ngalaxy mergers, and that the close environment of SMBHs in advanced mergers is richer in\ngas and dust with respect to that of SMBHs in isolated galaxies, and cannot be explained by\nthe classical AGN unification model in which the torus is responsible for the obscuration.",
"date": "2017-06",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "468",
"publisher": "Royal Astronomical Society",
"pagerange": "1273-1299",
"id_number": "CaltechAUTHORS:20170525-121504076",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170525-121504076",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AV27G"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2_138979/1"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2_166159"
},
{
"agency": "Chinese Academy of Science",
"grant_number": "XDB09030102"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11473002"
},
{
"agency": "Ministry of Science and Technology (China)",
"grant_number": "2016YFA0400702"
},
{
"agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)",
"grant_number": "AYA2013-47447-C3-2-P"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.1093/mnras/stx173",
"primary_object": {
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"author_list": "Ricci, C.; Bauer, F. E.; et el."
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{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
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"orcid": "0000-0001-5506-9855"
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{
"id": "Lansbury-G-B",
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"given": "Ma\u00efca"
},
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},
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"name": {
"family": "Fornasini",
"given": "Francesca M."
}
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"family": "Hong",
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}
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"name": {
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{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "David M."
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},
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"name": {
"family": "Bodaghee",
"given": "Arash"
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"id": "Chiu-Jeng-Lun",
"name": {
"family": "Chiu",
"given": "Jeng-Lun"
}
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"name": {
"family": "Grindlay",
"given": "Jonathan E."
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"family": "Hailey",
"given": "Charles J."
}
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"name": {
"family": "Harrison",
"given": "Fiona A."
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"name": {
"family": "Krivonos",
"given": "Roman A."
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"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
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"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
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},
"title": "Galactic Sources Detected in the NuSTAR Serendipitous Survey",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: black holes \u2013 stars: neutron \u2013 surveys \u2013 white dwarfs \u2013 X-rays: stars",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 April 26; revised 2017 May 18; accepted 2017 May 23; published 2017 June 23. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Data from Swift, XMM, and Chandra were also used, and the work on serendipitous NuSTAR sources is partially funded by Chandra grants GO5-16154X and GO6-17135X. R.K. acknowledges support from Russian Science Foundation (grant 14-12-01315). We acknowledge useful discussions with A. Shaw, and we thank the referee for helpful comments. This work has made use of data from the European Space Agency (ESA) mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research had made use of the SIMBAD database and the VizieR catalog access tool, CDS, Strasbourg, France.\n\nPublished - Tomsick_2017_ApJS_230_25.pdf
Submitted - 1705.08476.pdf
",
"abstract": "The Nuclear Spectroscopic Telescope Array (NuSTAR) provides an improvement in sensitivity at energies above 10 keV by two orders of magnitude over non-focusing satellites, making it possible to probe deeper into the Galaxy and universe. Lansbury and collaborators recently completed a catalog of 497 sources serendipitously detected in the 3\u201324 keV band using 13 deg^2 of NuSTAR coverage. Here, we report on an optical and X-ray study of 16 Galactic sources in the catalog. We identify 8 of them as stars (but some or all could have binary companions), and use information from Gaia to report distances and X-ray luminosities for 3 of them. There are 4 CVs or CV candidates, and we argue that NuSTAR J233426\u20132343.9 is a relatively strong CV candidate based partly on an X-ray spectrum from XMM-Newton. NuSTAR J092418\u20133142.2, which is the brightest serendipitous source in the Lansbury catalog, and NuSTAR J073959\u20133147.8 are low-mass X-ray binary candidates, but it is also possible that these 2 sources are CVs. One of the sources is a known high-mass X-ray binary (HMXB), and NuSTAR J105008\u20135958.8 is a new HMXB candidate that has strong Balmer emission lines in its optical spectrum and a hard X-ray spectrum. We discuss the implications of finding these HMXBs for the surface density (log N\u2013log S) and luminosity function of Galactic HMXBs. We conclude that with the large fraction of unclassified sources in the Galactic plane detected by NuSTAR in the 8\u201324 keV band, there could be a significant population of low-luminosity HMXBs.",
"date": "2017-06",
"date_type": "published",
"publication": "Astrophysical Journal Supplement Series",
"volume": "230",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 25",
"id_number": "CaltechAUTHORS:20170525-114748455",
"issn": "1538-4365",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170525-114748455",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "GO5-16154X"
},
{
"agency": "NASA",
"grant_number": "GO6-17135X"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01315"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
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"id": "NuSTAR"
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"doi": "10.3847/1538-4365/aa7517",
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}
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"pub_year": "2017",
"author_list": "Tomsick, John A.; Lansbury, George B.; et el."
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"items": [
{
"id": "Bahramian-A",
"name": {
"family": "Bahramian",
"given": "Arash"
},
"orcid": "0000-0003-2506-6041"
},
{
"id": "Heinke-C-O",
"name": {
"family": "Heinke",
"given": "Craig O."
},
"orcid": "0000-0003-3944-6109"
},
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"id": "Tudor-V",
"name": {
"family": "Tudor",
"given": "Vlad"
}
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{
"id": "Miller-Jones-J-C-A",
"name": {
"family": "Miller-Jones",
"given": "James C. A."
},
"orcid": "0000-0003-3124-2814"
},
{
"id": "Bogdanov-S",
"name": {
"family": "Bogdanov",
"given": "Slavko"
},
"orcid": "0000-0002-9870-2742"
},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "Thomas J."
},
"orcid": "0000-0003-0976-4755"
},
{
"id": "Knigge-C",
"name": {
"family": "Knigge",
"given": "Christian"
}
},
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"id": "Sivakoff-G-R",
"name": {
"family": "Sivakoff",
"given": "Gregory R."
},
"orcid": "0000-0001-6682-916X"
},
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"id": "Chomiuk-L",
"name": {
"family": "Chomiuk",
"given": "Laura"
},
"orcid": "0000-0002-8400-3705"
},
{
"id": "Strader-J",
"name": {
"family": "Strader",
"given": "Jay"
},
"orcid": "0000-0002-1468-9668"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Kallman-Timothy-R",
"name": {
"family": "Kallman",
"given": "Timothy R."
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"orcid": "0000-0002-5779-6906"
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]
},
"title": "The ultracompact nature of the black hole candidate X-ray binary 47 Tuc X9",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 stars: Black holes \u2013 stars: neutron \u2013 globular clusters: individual: 47 Tuc \u2013X-rays: binaries",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 January 18. Received 2017 January 16; in original form 2016 August 2. Published: 24 February 2017.\n\nAB thanks E. W. Koch for help with computational aspects of this project, K. A. Arnaud for helpful discussion on spectral analysis and B. E. Tetarenko for help with the radio/X-ray luminosity plot. The authors thank F. A. Harrison for granting NuSTAR director's discretionary time for these observations and J. Tomsick for assisting in coordination of NuSTAR observations. JCAM-J is the recipient of an Australian Research Council Future Fellowship (FT 140101082). JS acknowledges support of NSF grant AST-1308124 and a Packard Fellowship. COH and GRS acknowledge support from NSERC Discovery Grants, and COH also acknowledges support from a Humboldt Fellowship. This work was funded in part by NASA Chandra grant GO4-15029A awarded through Columbia University and issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. \n\nThe scientific results reported in this article are based on observations made by the Chandra X-ray Observatory, NuSTAR observatory and Australia Telescope Compact Array, and archival data obtained from Chandra and Swift data archives. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. \n\nWe acknowledge use of the following packages/softwares for analysis: the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA); CIAO, provided by the Chandra X-ray Center (CXC); HEASOFT, provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division; PVM_XSTAR, developed at the MIT Kavli Institute for Astrophysics and funded in part by NASA and the Smithsonian Institution, through the AISRP grant NNG05GC23G and Smithsonian Astrophysical Observatory contract SV3-73016; ASTROPY (Astropy Collaboration et al. 2013); ASTROML (Vanderplas et al. 2012); GATSPY (Vanderplas 2015); and MATPLOTLIB (Hunter 2007). Our simulations were performed using Cybera cloud computing resources (http://www.cybera.ca/). We acknowledge extensive use of NASA's Astrophysics Data System and Arxiv.\n\nSubmitted - 1702.02167.pdf
",
"abstract": "47 Tuc X9 is a low-mass X-ray binary (LMXB) in the globular cluster 47 Tucanae, and was previously thought to be a cataclysmic variable. However, Miller-Jones et al. recently identified a radio counterpart to X9 (inferring a radio/X-ray luminosity ratio consistent with black hole LMXBs), and suggested that the donor star might be a white dwarf. We report simultaneous observations of X9 performed by Chandra, NuSTAR and Australia Telescope Compact Array. We find a clear 28.18 \u00b1 0.02-min periodic modulation in the Chandra data, which we identify as the orbital period, confirming this system as an ultracompact X-ray binary. Our X-ray spectral fitting provides evidence for photoionized gas having a high oxygen abundance in this system, which indicates a C/O white dwarf donor. We also identify reflection features in the hard X-ray spectrum, making X9 the faintest LMXB to show X-ray reflection. We detect an \u223c6.8-d modulation in the X-ray brightness by a factor of 10, in archival Chandra, Swiftand ROSAT data. The simultaneous radio/X-ray flux ratio is consistent with either a black hole primary or a neutron star primary, if the neutron star is a transitional millisecond pulsar. Considering the measured orbital period (with other evidence of a white dwarf donor), and the lack of transitional millisecond pulsar features in the X-ray light curve, we suggest that this could be the first ultracompact black hole X-ray binary identified in our Galaxy.",
"date": "2017-05-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "467",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2199-2216",
"id_number": "CaltechAUTHORS:20170213-092026356",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170213-092026356",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Australian Research Council",
"grant_number": "FT 140101082"
},
{
"agency": "NSF",
"grant_number": "AST-1308124"
},
{
"agency": "David and Lucile Packard Foundation"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "NASA",
"grant_number": "GO4-15029A"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Australian Government"
},
{
"agency": "Smithsonian Astrophysical Observatory",
"grant_number": "SV3-73016"
},
{
"agency": "NASA",
"grant_number": "NNG05GC23G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
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},
"doi": "10.1093/mnras/stx166",
"primary_object": {
"basename": "1702.02167.pdf",
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"pub_year": "2017",
"author_list": "Bahramian, Arash; Heinke, Craig O.; et el."
},
{
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"eprint_id": 77650,
"eprint_status": "archive",
"datestamp": "2023-08-21 21:05:27",
"lastmod": "2023-10-25 23:19:53",
"type": "article",
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"creators": {
"items": [
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
}
]
},
"title": "Measurement of the Absolute Crab Flux with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "space vehicles: instruments; X-rays: individual (Crab)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 January 9; revised 2017 March 10; accepted 2017 March 23; published 2017 May 23. \n\nWe thank the referee for the helpful comments and suggestions. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: CXO, NuSTAR, Swift, Suzaku, and XMM.\n\nPublished - Madsen_2017_ApJ_841_56.pdf
Submitted - 1703.10685.pdf
",
"abstract": "We present results from a Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the Crab made at a large off-axis angle of 1 5. At these angles, X-rays do not pass through the optics and instead illuminate the detectors directly, due to incomplete baffling. Due to the simplicity of the instrument response in this configuration and the good absolute calibration of the detectors, we are able to measure the absolute intrinsic flux of the Crab to better than 4%. We find the spectral parameters of the power law to be \u0393 = 2.106 \u00b1 0.006, N = 9.71 \u00b1 0.16, in agreement with the values measured 42 years ago by Toor & Seward. This suggests that the observed variability of the Crab is not part of a long-term trend, but instead results from fluctuations around a steady mean. The NuSTAR observation also enabled improved measurement of the detector absorption parameters without the added complications of the mirror response.",
"date": "2017-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "841",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 56",
"id_number": "CaltechAUTHORS:20170523-091449570",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170523-091449570",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aa6970",
"primary_object": {
"basename": "1703.10685.pdf",
"url": "https://authors.library.caltech.edu/records/bh8hg-gqd74/files/1703.10685.pdf"
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"related_objects": [
{
"basename": "Madsen_2017_ApJ_841_56.pdf",
"url": "https://authors.library.caltech.edu/records/bh8hg-gqd74/files/Madsen_2017_ApJ_841_56.pdf"
}
],
"pub_year": "2017",
"author_list": "Madsen, Kristin K.; Forster, Karl; et el."
},
{
"id": "https://authors.library.caltech.edu/records/65qg5-eb671",
"eprint_id": 77622,
"eprint_status": "archive",
"datestamp": "2023-08-21 21:05:15",
"lastmod": "2023-10-25 23:18:30",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Fornasini-F-M",
"name": {
"family": "Fornasini",
"given": "Francesca M."
}
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "Lorenzo"
},
"orcid": "0000-0002-6601-9543"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "An XMM-Newton and NuSTAR Study of IGR J18214-1318: A Non-pulsating High-mass X-Ray Binary with a Neutron Star",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: black holes; stars: individual (IGR J18214-1318); stars: neutron; X-rays: binaries",
"note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 August 23. Accepted 2017 April 25. Published 2017 May 22. \n\nWe thank the anonymous referee for suggestions that improved the clarity and thoroughness of this paper. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). In addition, F.M.F. acknowledges support from the National Science Foundation Graduate Research Fellowship. F.M.F. and J.A.T. acknowledge partial support from NASA under XMM Guest Observer grant NNX15AG31G. R.K. acknowledges support from the Russian Science Foundation (grant 14-12-01315). L.N. wishes to acknowledge financial support by ASI/INAF grant I/037/12/0.\n\nPublished - Fornasini_2017_ApJ_841_35.pdf
",
"abstract": "IGR J18214-1318, a Galactic source discovered by the International Gamma-Ray Astrophysics Laboratory, is a high-mass X-ray binary (HMXB) with a supergiant O-type stellar donor. We report on the XMM-Newton and NuSTAR observations that were undertaken to determine the nature of the compact object in this system. This source exhibits high levels of aperiodic variability, but no periodic pulsations are detected with a 90% confidence upper limit of 2% fractional rms between 0.00003\u201388 Hz, a frequency range that includes the typical pulse periods of neutron stars (NSs) in HMXBs (0.1\u201310^3 s). Although the lack of pulsations prevents us from definitively identifying the compact object in IGR J18214-1318, the presence of an exponential cutoff with e-folding energy \u227e30 keV in its 0.3\u201379 keV spectrum strongly suggests that the compact object is an NS. The X-ray spectrum also shows a Fe K\u03b1 emission line and a soft excess, which can be accounted for by either a partial-covering absorber with N_H \u2248 10^(23) cm^(\u22122), which could be due to the inhomogeneous supergiant wind, or a blackbody component with kT = 1.74_(-0.05)^(+0.04) keV and R_(BB) \u2248 0.3 km, which may originate from NS hot spots. Although neither explanation for the soft excess can be excluded, the former is more consistent with the properties observed in other supergiant HMXBs. We compare IGR J18214-1318 to other HMXBs that lack pulsations or have long pulsation periods beyond the range covered by our observations.",
"date": "2017-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "841",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 35",
"id_number": "CaltechAUTHORS:20170522-091006693",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170522-091006693",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NSF Graduate Research Fellowship"
},
{
"agency": "NASA",
"grant_number": "NNX15AG31G"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01315"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa6ff4",
"primary_object": {
"basename": "Fornasini_2017_ApJ_841_35.pdf",
"url": "https://authors.library.caltech.edu/records/65qg5-eb671/files/Fornasini_2017_ApJ_841_35.pdf"
},
"pub_year": "2017",
"author_list": "Fornasini, Francesca M.; Tomsick, John A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/dnb8c-4rs65",
"eprint_id": 66283,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:01:09",
"lastmod": "2023-10-18 17:19:35",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Mondal-A-S",
"name": {
"family": "Mondal",
"given": "Aditya S."
}
},
{
"id": "Pahari-M",
"name": {
"family": "Pahari",
"given": "Mayukh"
}
},
{
"id": "Dewangan-G-C",
"name": {
"family": "Dewangan",
"given": "G. C."
}
},
{
"id": "Misra-R",
"name": {
"family": "Misra",
"given": "R."
}
},
{
"id": "Raychaudhuri-B",
"name": {
"family": "Raychaudhuri",
"given": "B."
}
}
]
},
"title": "NuSTAR and Swift joint view of neutron star X-ray binary 4U 1728\u221234: disc reflection in the island and lower banana states",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual: 4U 1728\u201334",
"note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2017 January 6. Received 2017 January 6; in original form 2016 April 14. Published: 11 January 2017.\n\nWe are thankful to the referee for constructive and useful suggestions that help to improve the manuscript. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Centre (HEASARC). We also thank NuSTAR team for making NuSTAR data public. ASM would like to thank Inter-University Centre for Astronomy and Astrophysics (IUCAA) for hosting him during subsequent visits. MP is thankful to Diego Altamirano for useful and constructive discussions. BR likes to thank IUCAA for hospitality and other facilities extended to him during his visit.\n\nSubmitted - nustar_1.pdf
",
"abstract": "We analyse two simultaneous NuSTAR and Swift data of the Atoll-type neutron star (NS) X-ray binary 4U 1728\u221234 observed on 2013 October 1 and 3. We infer that the first and the second observations belong to the island state and the lower banana state, respectively. During island state, four type-I X-ray bursts are observed within 60 ks exposure. From the time-resolved spectral analysis of each burst with NuSTAR, the blackbody temperature kT_(bb) are found to vary between 1.3 and 3.0 keV, while the blackbody normalizations (km/10 kpc)^2 vary in the range 20\u2013200, which translates to blackbody radii of 3.5\u20137.4\u2009km for an assumed distance of 5 kpc. The persistent, joint energy spectra from Swift and NuSTAR for both observations in the energy band 1\u201379\u2009keV are well described with thermal emission from the NS surface (kT_(bb) \u2243 1\u20132.5\u2009keV), Comptonized emission of thermal seed photons from the hot boundary layer/corona and the strong reflection component from the accretion disc. We detect a broad iron line in the 5\u20138\u2009keV band and reflection hump in the 15\u201330\u2009keV band modelled by the relxill reflection model. Joint spectral fitting constrains the inclination angle of the binary system and inner disc radius to be 22\u00b0-40\u00b0 and (2.0\u20134.3) \u00d7 R_(ISCO), respectively. We estimate the magnetic field to be (1.8\u20136.5) \u00d7 108 G. The X-ray luminosity of the source during the island and lower banana states are found to be LX = 1.1 and 1.6 \u00d7 10^(37) erg s^(\u22121), respectively, which correspond to \u223c6\u2009per\u2009cent and \u223c9\u2009per\u2009cent of the Eddington luminosity.",
"date": "2017-05-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "466",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4991-5002",
"id_number": "CaltechAUTHORS:20160419-141608451",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160419-141608451",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stx039",
"primary_object": {
"basename": "nustar_1.pdf",
"url": "https://authors.library.caltech.edu/records/dnb8c-4rs65/files/nustar_1.pdf"
},
"pub_year": "2017",
"author_list": "Mondal, Aditya S.; Pahari, Mayukh; et el."
},
{
"id": "https://authors.library.caltech.edu/records/erprx-97909",
"eprint_id": 75406,
"eprint_status": "archive",
"datestamp": "2023-08-19 03:02:02",
"lastmod": "2023-10-25 15:01:28",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "LaMassa-S-M",
"name": {
"family": "LaMassa",
"given": "Stephanie M."
},
"orcid": "0000-0002-5907-3330"
},
{
"id": "Yaqoob-T",
"name": {
"family": "Yaqoob",
"given": "Tahir"
}
},
{
"id": "Kilgard-Roy",
"name": {
"family": "Kilgard",
"given": "Roy"
}
}
]
},
"title": "Insight Into \"Changing-Look\" AGN Mrk 1018 from the Fe K\u03b1 Line: The Reprocessing Gas Has Yet to Fully Respond to the Fading of the AGN",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: Seyfert \u2013 X-rays: individual (Mrk 1018)",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 March 6; revised 2017 March 19; accepted 2017 March 21; published 2017 April 27.\n\nWe thank the anonymous referee for a careful reading of this manuscript. S.M.L. is grateful for helpful conversations with J.R.R. Rigby when preparing this manuscript. The scientific results reported in this article are based to a significant degree on observations made by the Chandra X-ray Observatory. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa.\n\nFacilities: CXO - Chandra X-ray Observatory satellite, NuSTAR.\n\nAccepted Version - 1703.07410.pdf
",
"abstract": "Mrk 1018 is a \"changing-look\" active galactic nucleus (AGN) whose optical spectrum transitioned from a Type 1.9 to a Type 1 between 1979 and 1984, and then back to a Type 1.9 in 2015. This latest transition was accompanied by a decrease in X-ray flux. We analyze the Chandra spectra from 2010 and 2016 and NuSTAR spectra from 2016, with a careful treatment of pileup in the Chandraspectrum from 2010, and self-consistently model absorption, reflection, and Fe K\u03b1 line emission in the X-ray spectra from 2016. We demonstrate that while the 2\u201310 keV X-ray flux decreased by an order of magnitude (1.46^(+0.10)_(-0.13) x 10^(-11) -1.31^(+0.09)_(-0.04) erg s^(\u22121) cm^(\u22122)), the Fe K\u03b1 equivalent width (EW) increased from 0.18^(+0.17)_(-0.12) to 0.61^(+0.27)_(-0.25) keV due to a depressed AGN continuum. We jointly fit the Chandraand NuSTAR spectra from 2016 using the physically motivated MYTorus model, and find that the torus orientation is consistent with a face-on geometry and that lines of sight intersecting the torus are ruled out. While we measure no line-of-sight absorption, we do measure a column density of N_H = 5.38^(+14)_(-4.0) x 10^(22) cm^(\u22122) for gas out of the line of sight that reprocesses the X-ray emission. We find a high relative normalization between the Compton-scattered emission and transmitted continuum, which is indicative of time lags between the primary X-ray source and reprocessing gas. We predict that the Fe K\u03b1 line will respond to the decrease in AGN flux, which would manifest as a decrease in the Fe K\u03b1 EW.",
"date": "2017-05-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "840",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 11",
"id_number": "CaltechAUTHORS:20170327-090132926",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170327-090132926",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa68df",
"primary_object": {
"basename": "1703.07410.pdf",
"url": "https://authors.library.caltech.edu/records/erprx-97909/files/1703.07410.pdf"
},
"pub_year": "2017",
"author_list": "LaMassa, Stephanie M.; Yaqoob, Tahir; et el."
},
{
"id": "https://authors.library.caltech.edu/records/7wm1m-fev25",
"eprint_id": 73769,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:48:47",
"lastmod": "2023-10-24 16:26:04",
"type": "article",
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"creators": {
"items": [
{
"id": "Schwarm-F-W",
"name": {
"family": "Schwarm",
"given": "F.-W."
}
},
{
"id": "Balhausen-R",
"name": {
"family": "Ballhausen",
"given": "R."
}
},
{
"id": "Falkner-S",
"name": {
"family": "Falkner",
"given": "S."
},
"orcid": "0000-0001-5209-991X"
},
{
"id": "Sch\u00f6nherr-G",
"name": {
"family": "Sch\u00f6nherr",
"given": "G."
}
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "K."
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Wolff-M-T",
"name": {
"family": "Wolff",
"given": "M. T."
},
"orcid": "0000-0002-4013-5650"
},
{
"id": "Becker-P-A",
"name": {
"family": "Becker",
"given": "P. A."
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Marcu-Cheatham-D-M",
"name": {
"family": "Marcu-Cheatham",
"given": "D. M."
},
"orcid": "0000-0001-8061-611X"
},
{
"id": "Hemphill-P-B",
"name": {
"family": "Hemphill",
"given": "P. B."
},
"orcid": "0000-0002-1676-6954"
},
{
"id": "Sokolova-Lapa-E",
"name": {
"family": "Sokolova-Lapa",
"given": "E."
}
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Klochkov-D",
"name": {
"family": "Klochkov",
"given": "D."
}
},
{
"id": "Ferrigno-C",
"name": {
"family": "Ferrigno",
"given": "C."
}
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Cyclotron resonant scattering feature simulations. II. Description of the CRSF simulation process",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries \u2013 stars: neutron \u2013 methods: numerical",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences.\n\nReceived 14 December 2016; Accepted 23 January 2017; Published online 10 May 2017.\n\nThis work has been partially funded by the Deutsche Forschungsgemeinschaft under DFG grant number WI 1860/11-1 and by the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt under DLR grant numbers 50\u2009OR\u20091113, 50\u2009OR\u20091207, 50\u2009OR\u20091410, and 50\u2009OR\u20091411. We also acknowledge the Russian Foundation for Basic Research grant number 14-02-91345. M.T.W. is supported by the Chief of Naval Research and by the National Aeronautics and Space Administration Astrophysical Data Analysis Program. We thank the International Space Science Institute in Bern for inspiring team meetings. The fruitful discussions within the MAGNET collaboration also had a very positive impact on this work. The figures in this work have been produced using the slxfig package by Davis (2014).\n\nSubmitted - 1701.07669v1.pdf
",
"abstract": "Context. Cyclotron resonant scattering features (CRSFs) are formed by scattering of X-ray photons off quantized plasma electrons in the strong magnetic field (of the order 10^(12) G) close to the surface of an accreting X-ray pulsar. Due to the complex scattering cross-sections, the line profiles of CRSFs cannot be described by an analytic expression. Numerical methods, such as Monte Carlo (MC) simulations of the scattering processes, are required in order to predict precise line shapes for a given physical setup, which can be compared to observations to gain information about the underlying physics in these systems.\nAims. A versatile simulation code is needed for the generation of synthetic cyclotron lines. Sophisticated geometries should be investigatable by making their simulation possible for the first time.\nMethods. The simulation utilizes the mean free path tables described in the first paper of this series for the fast interpolation of propagation lengths. The code is parallelized to make the very time-consuming simulations possible on convenient time scales. Furthermore, it can generate responses to monoenergetic photon injections, producing Green's functions, which can be used later to generate spectra for arbitrary continua.\nResults. We develop a new simulation code to generate synthetic cyclotron lines for complex scenarios, allowing for unprecedented physical interpretation of the observed data. An associated XSPEC model implementation is used to fit synthetic line profiles to NuSTAR data of Cep X-4. The code has been developed with the main goal of overcoming previous geometrical constraints in MC simulations of CRSFs. By applying this code also to more simple, classic geometries used in previous works, we furthermore address issues of code verification and cross-comparison of various models. The XSPEC model and the Green's function tables are available online (see link in footnote, page 1).",
"date": "2017-05",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "601",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A99",
"id_number": "CaltechAUTHORS:20170127-081638965",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-081638965",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201630250",
"primary_object": {
"basename": "1701.07669v1.pdf",
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"pub_year": "2017",
"author_list": "Schwarm, F.-W.; Ballhausen, R.; et el."
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{
"id": "Vybornov-V",
"name": {
"family": "Vybornov",
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{
"id": "Klochkov-D",
"name": {
"family": "Klochkov",
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{
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"given": "M."
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"name": {
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"given": "E."
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{
"id": "Staubert-R",
"name": {
"family": "Staubert",
"given": "R."
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{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "K."
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"orcid": "0000-0002-4656-6881"
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{
"id": "Santangelo-A",
"name": {
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"given": "A."
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},
"title": "Luminosity-dependent changes of the cyclotron line energy and spectral hardness in Cepheus X-4",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries \u2013 X-rays: stars \u2013 stars: magnetic field \u2013 pulsars: individual: Cep X-4",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 17 December 2016; Accepted 8 February 2017; Published online 19 May 2017. \n\nThe research is supported by the joint DFG grant KL 2734/2-1 and Wi 1860 11-1 and the RFBR grants 14-02-91345 and 18-502-12025. We thank the anonymous referee for the useful comments and suggestions that substantially improved the manuscript. The research used the data obtained from HEASARC Online Service provided by the NASA/GSFC.\n\nSubmitted - 1702.06361v1.pdf
",
"abstract": "Context. X-ray spectra of accreting pulsars are generally observed to vary with their X-ray luminosity. In particular, the hardness of the X-ray continuum is found to depend on luminosity. In a few sources, the correlation between the energy of the cyclotron resonance scattering feature (CRSF) and the luminosity is clear. Different types (signs) of the correlation are believed to reflect different accretion modes.\n\nAims. We analyse two NuSTAR observations of the transient accreting pulsar Cep X-4 during its 2014 outburst. Our analysis is focused on a detailed investigation of the dependence of the CRSF energy and of the spectral hardness on X-ray luminosity, especially on short timescales.\n\nMethods. To investigate the spectral changes as a function of luminosity within each of the two observations, we used the intrinsic variability of the source on the timescale of individual pulse cycles (tens of seconds), the so-called pulse-to-pulse variability.\n\nResults. We find that the NuSTAR spectrum of Cep X-4 contains two CRSFs: the fundamental line at ~30 keV and its harmonic at ~55 keV. We find for the first time that the energy of the fundamental CRSF increases and the continuum becomes harder with increasing X-ray luminosity not only between the two observations, that is, on the long timescale, but also within an individual observation, on the timescale of a few tens of seconds. We investigate these dependencies in detail including their non-linearity. We discuss a possible physical interpretation of the observed behaviour in the frame of a simple one-dimensional model of the polar emitting region with a collisionless shock formed in the infalling plasma near the neutron star surface. With this model, we are able to reproduce the observed variations of the continuum hardness ratio and of the CRSF energy with luminosity.",
"date": "2017-05",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "601",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A126",
"id_number": "CaltechAUTHORS:20170222-114208640",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-114208640",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201630275",
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"pub_year": "2017",
"author_list": "Vybornov, V.; Klochkov, D.; et el."
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}
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{
"id": "Matt-G",
"name": {
"family": "Matt",
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"orcid": "0000-0002-2152-0916"
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
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{
"id": "La-Franca-F",
"name": {
"family": "La Franca",
"given": "F."
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{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
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{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "P. G."
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"orcid": "0000-0001-9379-4716"
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M. J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
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]
},
"title": "Broadband X-ray spectral analysis of the Seyfert 1 galaxy GRS 1734-292",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual: GRS 1734\u2212292 \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 December 14. Received 2016 December 14; in original form 2016 September 8. Published: 17 December 2016. \n\nWe thank the anonymous referee for comments that helped improving the clarity of the paper. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of theNuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work is also based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). AT, AM, GM and FU acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and SB under grant ASI-INAF I/037/12/P1. AT, AM, SB and GM acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789.\n\nPublished - stw3301.pdf
Submitted - 1612.05871.pdf
",
"abstract": "We discuss the broad-band X-ray spectrum of GRS 1734\u2212292 obtained from non-simultaneous XMM\u2013Newton and NuSTAR (Nuclear Spectroscopic Telescope Array) observations, performed in 2009 and 2014, respectively. GRS1734\u2212292 is a Seyfert 1 galaxy, located near the Galactic plane at z = 0.0214. The NuSTAR spectrum (3\u201380 keV) is dominated by a primary power-law continuum with \u0393 = 1.65 \u00b1 0.05 and a high-energy cut-off E_c=53^(+11)_(\u22128) keV, one of the lowest measured by NuSTAR in a Seyfert galaxy. Comptonization models show a temperature of the coronal plasma of \nkT_e=11.9^(+1.2)_(\u22120.9) keV and an optical depth, assuming a slab geometry, \u03c4=2.98^(+0.16)_(\u22120.19) or a similar temperature and \u03c4=6.7^(+0.3)_(\u22120.4) assuming a spherical geometry. The 2009 XMM\u2013Newton spectrum is well described by a flatter intrinsic continuum (\u0393=1.47^(+0.07)_(\u22120.03)) and one absorption line due to Fe XXV K\u03b1 produced by a warm absorber. Both data sets show a modest iron K\u03b1 emission line at 6.4 keV and the associated Compton reflection, due to reprocessing from neutral circumnuclear material.",
"date": "2017-05",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "466",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4193-4200",
"id_number": "CaltechAUTHORS:20170623-134323659",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170623-134323659",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/12/0-011/13"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI-INAF I/037/12/P1"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
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]
},
"doi": "10.1093/mnras/stw3301",
"primary_object": {
"basename": "1612.05871.pdf",
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"basename": "stw3301.pdf",
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],
"pub_year": "2017",
"author_list": "Tortosa, A.; Marinucci, A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/77jbv-94t54",
"eprint_id": 72696,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:41:20",
"lastmod": "2023-10-23 22:51:22",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Rani-P",
"name": {
"family": "Rani",
"given": "Priyanka"
}
},
{
"id": "Stalin-C-S",
"name": {
"family": "Stalin",
"given": "C. S."
},
"orcid": "0000-0002-4998-1861"
},
{
"id": "Rakshit-S",
"name": {
"family": "Rakshit",
"given": "Suvendu"
}
}
]
},
"title": "X-ray flux variability of active galactic nuclei observed using NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 BL Lacertae objects: general \u2013 galaxies: jets \u2013 galaxies: nuclei \u2013 galaxies: Seyfert \u2013X-rays: galaxies",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 December 8. Received 2016 December 8; in original form 2016 September 26. Published: 12 December 2016.\n\nWe thank the anonymous referee for his/her detailed comments that helped us to improve the manuscript. The comments by Dr. Markus Bottcher on an initial version of the manuscript is thankfully acknowledged. This research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology(USA).\n\nNote added in proof:\nWe thank Dr. Madsen of the NuSTAR operations team for bringing to our attention improved background filtering for South Atlantic Anomaly (SAA) passage made available since the work in this paper as well as the ways to identify flares due to SAA from inspection of the background light curves. All data have now been checked for the existence of such events in our analysis and the updated results are given in this version of the manuscript.\n\nSubmitted - 1612.02768v1.pdf
",
"abstract": "We present results of a systematic study of flux variability on hourly time-scales in a large sample of active galactic nuclei (AGN) in the 3\u221279 keV band using data from Nuclear Spectroscopic Telescope Array. Our sample consists of four BL Lac objects (BL Lacs), three flat spectrum radio quasars (FSRQs) 24 Seyfert 1, 42 Seyfert 2 and eight narrow line Seyfert 1 (NLSy1) galaxies. We find that in the 3\u221279 keV band, about 65 per cent of the sources in our sample show significant variations on hourly time-scales. Using the Mann\u2013Whitney U-test and the Kolmogorov\u2013Smirnov test, we find no difference in the variability behaviour between Seyfert 1 and 2 galaxies. The blazar sources (FSRQs and BL Lacs) in our sample are more variable than Seyfert galaxies that include Seyfert 1 and Seyfert 2 in the soft (3\u221210 keV), hard (10\u221279 keV) and total (3\u221279 keV) bands. NLSy1 galaxies show the highest duty cycle of variability (87 per cent), followed by BL Lacs (82 per cent), Seyfert galaxies (56 per cent) and FSRQs (23 per cent). We obtained flux doubling/halving time in the hard X-ray band less than 10 min in 11 sources. The flux variations between the hard and soft bands in all the sources in our sample are consistent with zero lag.",
"date": "2017-04-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "466",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3309-3322",
"id_number": "CaltechAUTHORS:20161209-150240501",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161209-150240501",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw3228",
"primary_object": {
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"pub_year": "2017",
"author_list": "Rani, Priyanka; Stalin, C. S.; et el."
},
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"items": [
{
"id": "Ferrigno-C",
"name": {
"family": "Ferrigno",
"given": "C."
}
},
{
"id": "Bozzo-E",
"name": {
"family": "Bozzo",
"given": "E."
}
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{
"id": "Sanna-A",
"name": {
"family": "Sanna",
"given": "A."
}
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{
"id": "Pintore-F",
"name": {
"family": "Pintore",
"given": "F."
}
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{
"id": "Papitto-A",
"name": {
"family": "Papitto",
"given": "A."
}
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{
"id": "Riggio-A",
"name": {
"family": "Riggio",
"given": "A."
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"family": "Burderi",
"given": "L."
}
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{
"id": "Di-Salvo-T",
"name": {
"family": "Di Salvo",
"given": "T."
}
},
{
"id": "Iaria-R",
"name": {
"family": "Iaria",
"given": "R."
}
},
{
"id": "D'Ai-Antonino",
"name": {
"family": "D'A\u00ec",
"given": "A."
},
"orcid": "0000-0002-5042-1036"
}
]
},
"title": "Discovery of a soft X-ray 8 mHz QPO from the accreting millisecond pulsar IGR J00291+5934",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron \u2013 pulsars: individual: IGR J00291+5934 \u2013X-rays: binaries",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 December 20. Received 2016 December 19; in original form 2016 September 23. Published: 23 December 2016.\n\nWe thank the anonymous referee and Phil Uttley for their precious suggestions. This work is based on observations obtained with XMM\u2013Newton (OBSID 0744840201) and NuSTAR (OBSID 90101010002); the former is an ESA science mission with instruments and contributions directly funded by ESA Member States and USA (NASA); the latter is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We also exploited the ISIS functions provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). AP is supported via an EU Marie Sk\u0142odowska-Curie fellowship under grant no. 660657-TMSP-H2020-MSCA-IF-2014. We acknowledge the International Space Science Institute (ISSI \u2013 Bern) that funded and hosted the international team 'The disk-magnetosphere interaction around transitional millisecond pulsars'.\n\nSubmitted - 1611.07075v1.pdf
",
"abstract": "We report on the analysis of the peculiar X-ray variability displayed by the accreting millisecond X-ray pulsar IGR J00291+5934 in a 80 ks-long joint NuSTAR and XMM\u2013Newton observation performed during the source outburst in 2015. The light curve of the source is characterized by a flaring-like behaviour, with typical rise and decay time-scales of \u223c120 s. The flares are accompanied by a remarkable spectral variability, with the X-ray emission being generally softer at the peak of the flares. A strong quasi-periodic oscillation (QPO) is detected at \u223c8 mHz in the power spectrum of the source and clearly associated with the flaring-like behaviour. This feature has the strongest power at soft X-rays ( \u2272 3 keV). We carried out a dedicated hardness-ratio-resolved spectral analysis and a QPO phase-resolved spectral analysis, together with an in-depth study of the source-timing properties, to investigate the origin of this behaviour. We suggest that the unusual variability of IGR J00291+5934 observed by XMM\u2013Newton and NuSTAR could be produced by a heartbeat-like mechanism, similar to that observed in black hole X-ray binaries. The possibility that this variability, and the associated QPO, are triggered by phases of quasi-stable nuclear burning, as sustained in the literature for a number of other neutron star binaries displaying a similar behaviour, cannot be solidly tested in the case of IGR J00291+5934 due to the paucity of type I X-ray bursts detected from this source.",
"date": "2017-04-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "466",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3450-3459",
"id_number": "CaltechAUTHORS:20161123-122237857",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161123-122237857",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw3344",
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"pub_year": "2017",
"author_list": "Ferrigno, C.; Bozzo, E.; et el."
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"id": "Walton-D-J",
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"family": "Walton",
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},
{
"id": "Mooley-Kunal-Prakash",
"name": {
"family": "Mooley",
"given": "K."
},
"orcid": "0000-0002-2557-5180"
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{
"id": "King-A-L",
"name": {
"family": "King",
"given": "A"
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{
"id": "Tomsick-J-A",
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"family": "Tomsick",
"given": "J. A."
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{
"id": "Miller-J-M",
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"family": "Miller",
"given": "J. M."
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"name": {
"family": "Dauser",
"given": "T."
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"orcid": "0000-0003-4583-9048"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J."
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"orcid": "0000-0003-3828-2448"
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{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
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{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
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{
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"family": "F\u00fcrst",
"given": "F."
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"name": {
"family": "Gandhi",
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"family": "Grefenstette",
"given": "B. W."
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
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"id": "Meier-D-L",
"name": {
"family": "Meier",
"given": "D. L."
}
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{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "L."
},
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},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "F."
},
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},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
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}
]
},
"title": "Living on a Flare: Relativistic Reflection in V404 Cyg Observed by NuSTAR During its Summer 2015 Outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (V404 Cyg)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 2; revised 2017 March 6; accepted 2017 March 17; published 2017 April 21. \n\nThe authors thank the anonymous reviewer for suggestions that helped to improve the manuscript. D.J.W., P.G., and M.J.M. acknowledge support from STFC Ernest Rutherford fellowships (grant ST/J003697/2). K.P.M. acknowledges support from the Hintze Foundation. A.L.K. acknowledges support from NASA through an Einstein Postdoctoral Fellowship (grant number PF4-150125) awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. A.C.F. acknowledges support from ERC Advanced Grant 340442. L.N. wishes to acknowledge the Italian Space Agency (ASI) for Financial support by ASI/INAF grant I/037/12/0-011/13. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data from AMI, which is supported by the ERC, and we thank the AMI staff for scheduling these radio observations. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, AMI - Arcminute MicroKelvin Imager.\n\nPublished - Walton_2017_ApJ_839_110.pdf
Submitted - 1609.01293v1.pdf
",
"abstract": "We present first results from a series of NuSTAR observations of the black hole X-ray binary V404 Cyg obtained during its summer 2015 outburst, primarily focusing on observations during the height of this outburst activity. The NuSTAR data show extreme variability in both the flux and spectral properties of the source. This is partly driven by strong and variable line-of-sight absorption, similar to previous outbursts. The latter stages of this observation are dominated by strong flares, reaching luminosities close to Eddington. During these flares, the central source appears to be relatively unobscured and the data show clear evidence for a strong contribution from relativistic reflection, providing a means to probe the geometry of the innermost accretion flow. Based on the flare properties, analogies with other Galactic black hole binaries, and also the simultaneous onset of radio activity, we argue that this intense X-ray flaring is related to transient jet activity during which the ejected plasma is the primary source of illumination for the accretion disk. If this is the case, then our reflection modeling implies that these jets are launched in close proximity to the black hole (as close as a few gravitational radii), consistent with expectations for jet launching models that tap either the spin of the central black hole, or the very innermost accretion disk. Our analysis also allows us to place the first constraints on the black hole spin for this source, which we find to be a* > 0.92 (99% statistical uncertainty, based on an idealized lamp-post geometry).",
"date": "2017-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "839",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 110",
"id_number": "CaltechAUTHORS:20161117-111407065",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161117-111407065",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "Hintze Foundation"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF4-150125"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.3847/1538-4357/aa67e8",
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}
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"pub_year": "2017",
"author_list": "Walton, D. J.; Mooley, K.; et el."
},
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"lastmod": "2023-10-25 15:09:22",
"type": "article",
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"items": [
{
"id": "Kong-Albert-K-H",
"name": {
"family": "Kong",
"given": "A. K. H."
},
"orcid": "0000-0002-5105-344X"
},
{
"id": "Hui-David-C-Y",
"name": {
"family": "Hui",
"given": "C. Y."
},
"orcid": "0000-0003-1753-1660"
},
{
"id": "Takata-Jumpei",
"name": {
"family": "Takata",
"given": "J."
},
"orcid": "0000-0002-8731-0129"
},
{
"id": "Li-Kwan-Lok",
"name": {
"family": "Li",
"given": "K. L."
},
"orcid": "0000-0001-8229-2024"
},
{
"id": "Tam-Pak-Hin-Thomas",
"name": {
"family": "Tam",
"given": "P. H. T."
},
"orcid": "0000-0002-1262-7375"
}
]
},
"title": "A NuSTAR Observation of the Gamma-ray Emitting Millisecond Pulsar PSR J1723-2837",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: close \u2013 pulsars: individual (PSR J1723\u20132837) \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 February 8; revised 2017 March 26; accepted 2017 March 29; published 2017 April 25.\n\nA.K.H.K. is supported by the Ministry of Science and Technology of the Republic of China (Taiwan) through grants 105-2112-M-007-033-MY2, 105-2119-M-007-028-MY3, and 106-2918-I-007-005. C.Y.H. is supported by the National Research Foundation of Korea through grants 2014R1A1A2058590 and 2016R1A5A1013277. J.T. is supported by NSFC grants of Chinese Government under 11573010 and U1631103.\n\nFacilities: NuSTAR, Swift.\n\nAccepted Version - 1703.10164.pdf
",
"abstract": "We report on the first NuSTAR observation of the gamma-ray emitting millisecond pulsar binary PSR J1723\u20132837. X-ray radiation up to 79 keV is clearly detected, and the simultaneous NuSTAR and Swift spectrum is well described by an absorbed power law with a photon index of ~1.3. We also find X-ray modulations in the 3\u201310, 10\u201320, 20\u201379, and 3\u201379 keV bands at the 14.8 hr binary orbital period. All of these are entirely consistent with previous X-ray observations below 10 keV. This new hard X-ray observation of PSR J1723\u20132837 provides strong evidence that the X-rays are from the intrabinary shock via an interaction between the pulsar wind and the outflow from the companion star. We discuss how the NuSTAR observation constrains the physical parameters of the intrabinary shock model.",
"date": "2017-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "839",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 130",
"id_number": "CaltechAUTHORS:20170331-101324182",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-101324182",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
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"id": "NuSTAR"
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"doi": "10.3847/1538-4357/aa6aa2",
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"author_list": "Kong, A. K. H.; Hui, C. Y.; et el."
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"lastmod": "2023-10-25 16:52:24",
"type": "article",
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"items": [
{
"id": "Marcotulli-L",
"name": {
"family": "Marcotulli",
"given": "L."
}
},
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"id": "Paliya-V-S",
"name": {
"family": "Paliya",
"given": "V. S."
},
"orcid": "0000-0001-7774-5308"
},
{
"id": "Ajello-M",
"name": {
"family": "Ajello",
"given": "M."
},
"orcid": "0000-0002-6584-1703"
},
{
"id": "Kaur-A",
"name": {
"family": "Kaur",
"given": "A."
}
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{
"id": "Hartmann-D-H",
"name": {
"family": "Hartmann",
"given": "D. H."
}
},
{
"id": "Gasparrini-D",
"name": {
"family": "Gasparrini",
"given": "D."
}
},
{
"id": "Greiner-J",
"name": {
"family": "Greiner",
"given": "J."
}
},
{
"id": "Rau-A",
"name": {
"family": "Rau",
"given": "A."
},
"orcid": "0000-0001-5990-6243"
},
{
"id": "Schady-P",
"name": {
"family": "Schady",
"given": "P."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G."
}
}
]
},
"title": "High-redshift Blazars through NuSTAR Eyes",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: jets \u2013 gamma rays: galaxies \u2013 quasars: individual (3FGL J0325.5+2223,\n3FGL J0449.0+1121, 3FGL J0453.2\u20132808)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 January 23; revised 2017 March 27; accepted 2017 March 27; published 2017 April 20. \n\nWe are thankful to the referee for a constructive report. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France. \n\nThis NuSTAR work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nWe thank the Swift team and the Swift PI (N. Gehrels) for promptly scheduling and executing the observations. \n\nPart of this work is based on archival data, software, or online services provided by the ASI Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS). Part of the funding for GROND (both hardware and personnel) was generously granted by the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). \n\nWe acknowledge funding from NASA contract NNX15AV09G. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. \n\nPart of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).\n\nPublished - Marcotulli_2017_ApJ_839_96.pdf
Submitted - 1703.10657.pdf
",
"abstract": "The most powerful sources among the blazar family are MeV blazars. Often detected at z > 2, they usually display high X- and \u03b3-ray luminosities, larger-than-average jet powers, and black hole masses \u227310^9 M\u2609. In the present work, we perform a multiwavelength study of three high-redshift blazars: 3FGL J0325.5+2223 (z = 2.06), 3FGL J0449.0+1121 (z = 2.15), and 3FGL J0453.2\u22122808 (z = 2.56), analyzing quasi-simultaneous data from GROND, Swift-UVOT and XRT, Nuclear Spectroscopic Telescope Array (NuSTAR), and Fermi-LAT. Our main focus is on the hard X-ray band recently unveiled by NuSTAR (3\u201379 keV) where these objects show a hard spectrum that enables us to constrain the inverse Compton (IC) peak and the jet power. We found that all three targets resemble the most powerful blazars, with the synchrotron peak located in the submillimeter range and the IC peak in the MeV range, and therefore belong to the MeV blazar class. Using a simple one-zone leptonic emission model to reproduce the spectral energy distributions, we conclude that a simple combination of synchrotron and accretion disk emission reproduces the infrared\u2013optical spectra, while the X-ray to \u03b3-ray part is well reproduced by the IC scattering of low-energy photons supplied by the broad-line region. The black hole masses for each of the three sources are calculated to be \u22734 \u00d7 10^8 M\u2609. The three studied sources have jet power at the level of, or beyond, the accretion luminosity.",
"date": "2017-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "839",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 96",
"id_number": "CaltechAUTHORS:20170421-080903620",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170421-080903620",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "HA 1850/28-1"
},
{
"agency": "NASA",
"grant_number": "NNX15AV09G"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
}
]
},
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"doi": "10.3847/1538-4357/aa6a17",
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"pub_year": "2017",
"author_list": "Marcotulli, L.; Paliya, V. S.; et el."
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{
"id": "Walton-D-J",
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"family": "Walton",
"given": "D. J."
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},
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"id": "Middleton-M-J",
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"family": "Middleton",
"given": "M. J."
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
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{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
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"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
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{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
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{
"id": "Tao-L",
"name": {
"family": "Tao",
"given": "L."
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},
"title": "The Broadband Spectral Variability of Holmberg IX X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (Holmberg IX X-1)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 October 19; revised 2017 March 15; accepted 2017 March 17; published 2017 April 21. \n\nThe authors would like to thank the anonymous reviewer, who provided useful suggestions for improving the final manuscript, and also Tim Roberts for useful discussion. D.J.W. and M.J.M. acknowledge support from STFC through Ernest Rutherford fellowships, A.C.F. acknowledges support from ERC Advanced Grant 340442, and D.B. acknowledges financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, and with Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). \n\nFacilites: NuSTAR, XMM, Suzaku.\n\nPublished - Walton_2017_ApJ_839_105.pdf
Submitted - 1610.06611.pdf
",
"abstract": "We present results from four new broadband X-ray observations of the extreme ultraluminous X-ray source Holmberg IX X-1 (L_X > 10^(40) erg s^(\u22121)), performed by Suzaku and NuSTAR in coordination. Combined with the archival data, we now have broadband observations of this remarkable source from six separate epochs. Two of these new observations probe lower fluxes than seen previously, allowing us to extend our knowledge of the broadband spectral variability exhibited. The spectra are well fit by two thermal blackbody components that dominate the emission below 10 keV, as well as a steep (\u0393 ~ 3.5) power-law tail that dominates above ~15 keV. Remarkably, while the 0.3\u201310.0 keV flux varies by a factor of ~3 between all these epochs, the 15\u201340 keV flux varies by only ~20%. Although the spectral variability is strongest in the ~1\u201310 keV band, both of the thermal components are required to vary when all epochs are considered. We also revisit the search for iron absorption features by leveraging the high-energy NuSTAR data to improve our sensitivity to extreme velocity outflows in light of the ultra-fast outflow recently detected in NGC 1313 X-1. Iron absorption from a similar outflow along our line of sight can be ruled out in this case. We discuss these results in the context of super-Eddington accretion models that invoke a funnel-like geometry for the inner flow, and propose a scenario in which we have an almost face-on view of a funnel that expands to larger radii with increasing flux, resulting in an increasing degree of geometrical collimation for the emission from intermediate-temperature regions.",
"date": "2017-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "839",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 105",
"id_number": "CaltechAUTHORS:20170421-141946967",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170421-141946967",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
}
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"author_list": "Walton, D. J.; F\u00fcrst, F.; et el."
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"id": "Doroshenko-V",
"name": {
"family": "Doroshenko",
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{
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"name": {
"family": "Tsygankov",
"given": "Sergey S."
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"orcid": "0000-0002-9679-0793"
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"id": "Mushtukov-A-A",
"name": {
"family": "Mushtukov",
"given": "Alexander A."
}
},
{
"id": "Lutovinov-A-A",
"name": {
"family": "Lutovinov",
"given": "Alexander A."
}
},
{
"id": "Santagelo-A",
"name": {
"family": "Santangelo",
"given": "Andrea"
}
},
{
"id": "Suleimanov-V-F",
"name": {
"family": "Suleimanov",
"given": "Valery F."
}
},
{
"id": "Poutanen-J",
"name": {
"family": "Poutanen",
"given": "Juri"
},
"orcid": "0000-0002-0983-0049"
}
]
},
"title": "Luminosity dependence of the cyclotron line and evidence for the accretion regime transition in V 0332+53",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries \u2013 X-rays: individual: V 0332+53",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 December 9. Received 2016 December 6; in original form 2016 April 29. Published: 14 December 2016. \n\nAuthors thank E. M. Churazov, who developed the INTEGRAL/SPI data analysis methods and provided the software. This research has made use of data provided by HEASARC (NASA/GSFC and Smithsonian Astrophysical Observatory). This work is based on observations with INTEGRAL, an ESA project with instruments and a science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), and with the participation of Russia and the USA. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The authors acknowledge support from the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR) through DLR-PT grant 50 OR 0702 (VD), Deutsche Forschungsgemeinschaft (DFG) through WE 1312/48-1 (VFS), the Russian Science Foundation through grant 14-12-01287 (AAM, SST and AAL), the Academy of Finland through grant 268740 and the Foundations' Professor Pool, the Finnish Cultural Foundation (JP).\n\nSubmitted - 1607.03933v1.pdf
",
"abstract": "We report on the analysis of NuSTAR observations of the Be-transient X-ray pulsar V 0332+53 during the giant outburst in 2015 and another minor outburst in 2016. We confirm the cyclotron-line energy\u2013luminosity correlation previously reported in the source and the line energy decrease during the giant outburst. Based on 2016 observations, we find that a year later the line energy has increased again essentially reaching the pre-outburst values. We discuss this behaviour and conclude that it is likely caused by a change of the emission region geometry rather than previously suggested accretion-induced decay of the neutron stars magnetic field. At lower luminosities, we find for the first time a hint of departure from the anticorrelation of line energy with flux, which we interpret as a transition from super- to sub-critical accretion associated with the disappearance of the accretion column. Finally, we confirm and briefly discuss the orbital modulation observed in the outburst light curve of the source.",
"date": "2017-04-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "466",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "2143-2150",
"id_number": "CaltechAUTHORS:20160715-085654157",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160715-085654157",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw3236",
"primary_object": {
"basename": "1607.03933v1.pdf",
"url": "https://authors.library.caltech.edu/records/4b3zj-t2p50/files/1607.03933v1.pdf"
},
"pub_year": "2017",
"author_list": "Doroshenko, Victor; Tsygankov, Sergey S.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/bfw9w-r1t21",
"eprint_id": 75586,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:34:45",
"lastmod": "2023-10-25 15:09:43",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Shidatsu-Megumi",
"name": {
"family": "Shidatsu",
"given": "M."
}
},
{
"id": "Ueda-Yoshihiro",
"name": {
"family": "Ueda",
"given": "Y."
},
"orcid": "0000-0001-7821-6715"
},
{
"id": "Fabrika-S",
"name": {
"family": "Fabrika",
"given": "S."
}
}
]
},
"title": "NuSTAR and Swift observations of the ultraluminous X-ray source IC 342 X-1 in 2016: witnessing spectral evolution",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (IC 342 X-1)",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 January 25; revised 2017 March 3; accepted 2017 March 17; published 2017 April 12.\n\nWe are grateful to the NuSTAR and Swift operation teams for carrying out the ToO observations. We thank Kirill Atapin for helpful comments and Ken Ohsuga and Tomohisa Kawashima for useful discussion of latest results from numerical simulations. M.S. acknowledges support by the Special Postdoctoral Researchers Program at RIKEN. This work is partly supported by a Grant-in-Aid for Young Scientists (B) 16K17672 (M.S.) and for Scientific Research 26400228 (Y.U.). S.F. acknowledges support by the the Russian RFBR grants 16-02-00567, 15-42-02573, and the Russian Science Foundation grant 14-50-00043. This research has made use of data supplied by the UK Swift Science Data Centre at the University of Leicester and data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center.\n\nAccepted Version - 1703.06399.pdf
",
"abstract": "We report on an X-ray observing campaign of the ultraluminous X-ray source IC 342 X-1 with NuSTAR and Swift in 2016 October, in which we captured the very moment when the source showed spectral variation. The Swift/XRT spectrum obtained in October 9\u201311 has a power-law shape and is consistent with those observed in the coordinated XMM-Newton and NuSTAR observations in 2012. In October 16\u201317, when the 3\u201310 keV flux became \u22484 times higher, we performed simultaneous NuSTAR and Swift observations. In this epoch, the source showed a more round-shaped spectrum like that seen with ASCA23 years ago. Thanks to the wide energy coverage and high sensitivity of NuSTAR, we obtained hard X-ray data covering up to ~30 keV for the first time during the high-luminosity state of IC 342 X-1. The observed spectrum has a broader profile than the multi-color disk blackbody model. The X-ray flux decreased again in the last several hours of the NuSTARobservation, when the spectral shape approached those seen in 2012 and 2016 October 9\u201311. The spectra obtained in our observations and in 2012 can be commonly described with disk emission and its Comptonization in cool (T_e \u2248 4 keV), optically thick (\u03c4 \u2248 5) plasma. The spectral turnover seen at around 5\u201310 keV shifts to higher energies as the X-ray luminosity decreases. This behavior is consistent with that predicted from recent numerical simulations of super-Eddington accretion flows with Compton-thick outflows. We suggest that the spectral evolution observed in IC 342 X-1 can be explained by a smooth change in mass-accretion rate.",
"date": "2017-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "839",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 46",
"id_number": "CaltechAUTHORS:20170331-105554581",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-105554581",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa67e7",
"primary_object": {
"basename": "1703.06399.pdf",
"url": "https://authors.library.caltech.edu/records/bfw9w-r1t21/files/1703.06399.pdf"
},
"pub_year": "2017",
"author_list": "Shidatsu, M.; Ueda, Y.; et el."
},
{
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"eprint_id": 75018,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:30:27",
"lastmod": "2023-10-20 23:29:14",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Matsuoka-Kenta",
"name": {
"family": "Matsuoka",
"given": "Kenta"
},
"orcid": "0000-0002-2689-4634"
},
{
"id": "Ueda-Yoshihiro",
"name": {
"family": "Ueda",
"given": "Yoshihiro"
},
"orcid": "0000-0001-7821-6715"
}
]
},
"title": "Nature of hard X-ray (3-24 keV) detected luminous infrared galaxies in the COSMOS field",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: evolution \u2013 infrared: galaxies",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 July 27; revised 2017 February 9; accepted 2017 February 28; published 2017 April 3. \n\nWe would like to thank Taiki Kawamuro, Atsushi Tanimoto, Kohei Ichikawa, and Tohru Nagao for helpful comments and suggestions, and Takamitsu Miyaji for his help on the energy responses of Chandra and XMM-Newton. We also thank the anonymous referee for useful comments and suggestions. This work was financially supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI Grant No. 14J01811 (K.M.) and 26400228 (Y.U.).\n\nAccepted Version - 1703.02975.pdf
Erratum - Matsuoka_2017_ApJ_844_172.pdf
",
"abstract": "We investigate the nature of far-infrared (70 \u03bcm) and hard X-ray (3\u201324 keV) selected galaxies in the COSMOS field detected with both Spitzer and the Nuclear Spectroscopic Telescope Array (NuSTAR). By matching the Spitzer-COSMOS catalog with the NuSTAR-COSMOS catalog, we obtain a sample consisting of a hyperluminous infrared galaxy with log(L_(IR)/L\u2299) \u2a7e 13, 12 ultraluminous infrared galaxies with 12 \u2a7d log (L_(IR)/L\u2299) \u2a7d 13, and 10 luminous infrared galaxies with 11\u2a7d log (L_(IR)/L\u2299 \u2a7d 12, i.e., 23 Hy/U/LIRGs in total. Using their X-ray hardness ratios, we find that 12 sources are obscured active galactic nuclei (AGNs) with absorption column densities of N_H > 10^(22) cm^(\u22122), including several Compton-thick (N_H ~ 10^(24) cm^(\u22122)) AGN candidates. On the basis of the infrared (60 \u03bcm) and intrinsic X-ray luminosities, we examine the relation between star formation (SF) and AGN luminosities of the 23 Hy/U/LIRGs. We find that the correlation is similar to that of the optically selected AGNs reported by Netzer, whereas local, far-infrared selected U/LIRGs show higher SF-to-AGN luminosity ratios than the average of our sample. This result suggests that our Hy/U/LIRGs detected both with Spitzer and NuSTAR are likely situated in a transition epoch between AGN-rising and cold-gas diminishing phases in SF-AGN evolutional sequences. The nature of a Compton-thick AGN candidate newly detected above 8 keV with NuSTAR (ID 245 in Civano et al.) is briefly discussed.",
"date": "2017-04-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "838",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 128",
"id_number": "CaltechAUTHORS:20170310-092959543",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170310-092959543",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa64d5",
"primary_object": {
"basename": "1703.02975.pdf",
"url": "https://authors.library.caltech.edu/records/t8a51-7mz48/files/1703.02975.pdf"
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{
"basename": "Matsuoka_2017_ApJ_844_172.pdf",
"url": "https://authors.library.caltech.edu/records/t8a51-7mz48/files/Matsuoka_2017_ApJ_844_172.pdf"
}
],
"pub_year": "2017",
"author_list": "Matsuoka, Kenta and Ueda, Yoshihiro"
},
{
"id": "https://authors.library.caltech.edu/records/tcrwb-8vw07",
"eprint_id": 70350,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:30:00",
"lastmod": "2023-10-20 22:51:54",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lutovinov-A-A",
"name": {
"family": "Lutovinov",
"given": "Alexander A."
}
},
{
"id": "Tsygankov-S-S",
"name": {
"family": "Tsygankov",
"given": "Sergey S."
},
"orcid": "0000-0002-9679-0793"
},
{
"id": "Postnov-K-A",
"name": {
"family": "Postnov",
"given": "Konstantin A."
}
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Molkov-S-V",
"name": {
"family": "Molkov",
"given": "Sergey V."
}
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
}
]
},
"title": "NuSTAR observations of the supergiant X-ray pulsar IGR J18027-2016: accretion from the stellar wind and possible cyclotron absorption line",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 magnetic fields \u2013 stars: individual: IGR J18027\u22122016 \u2013X-rays: binaries",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 November 21. Received 2016 November 21; in original form 2016 September 8. Published: 29 November 2016.\n\nThis work was supported by the Russian Science Foundation (grant 14-22-00271). Work of PK is partially supported by RSF grant 14-12-00657. We thank the anonymous referee for useful comments. The research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA).\n\nAccepted Version - 1609.02942v1.pdf
",
"abstract": "We report on the first focused hard X-ray view of the absorbed supergiant system IGR J18027\u22122016 performed with the Nuclear Spectroscopic Telescope Array observatory. The pulsations are clearly detected with a period of P_(spin)=139.866(1) s and a pulse fraction of about 50\u201360 per cent at energies from 3 to 80 keV. The source demonstrates an approximately constant X-ray luminosity on a time-scale of more than dozen years with an average spin-down rate of P \u2243 6x10^(-10) s s^(-1). This behaviour of the pulsar can be explained in terms of the wind accretion model in the settling regime. The detailed spectral analysis at energies above 10 keV was performed for the first time and revealed a possible cyclotron absorption feature at energy \u223c23 keV. This energy corresponds to the magnetic field B \u2243 3x10^(12) G at the surface of the neutron star, which is typical for X-ray pulsars.",
"date": "2017-04-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "466",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "593-599",
"id_number": "CaltechAUTHORS:20160914-124807381",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160914-124807381",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw3058",
"primary_object": {
"basename": "1609.02942v1.pdf",
"url": "https://authors.library.caltech.edu/records/tcrwb-8vw07/files/1609.02942v1.pdf"
},
"pub_year": "2017",
"author_list": "Lutovinov, Alexander A.; Tsygankov, Sergey S.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/nyxh5-fht27",
"eprint_id": 75235,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:30:45",
"lastmod": "2023-10-25 14:52:27",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Sidoli-L",
"name": {
"family": "Sidoli",
"given": "L."
},
"orcid": "0000-0001-9705-2883"
},
{
"id": "Tiengo-A",
"name": {
"family": "Tiengo",
"given": "A."
},
"orcid": "0000-0002-6038-1090"
},
{
"id": "Paizis-A",
"name": {
"family": "Paizis",
"given": "A."
},
"orcid": "0000-0001-5067-0377"
},
{
"id": "Sguera-V",
"name": {
"family": "Sguera",
"given": "V."
}
},
{
"id": "Lotti-S",
"name": {
"family": "Lotti",
"given": "S."
},
"orcid": "0000-0002-3088-1561"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "L."
},
"orcid": "0000-0002-6601-9543"
}
]
},
"title": "XMM-Newton and NuSTAR simultaneous X-ray observations of IGR J11215-5952",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual (IGR J11215-5952)",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 December 15; revised 2017 March 10; accepted 2017 March 13; published 2017 April 3.\n\nThis work is based on data from observations with XMM-Newton, NuSTAR and Swift. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). The NuSTAR mission is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research made use of the NuSTAR DAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). We thank N. Gehrels and the Swift team for making the Swift ToO possible. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank A. De Luca, S. Molendi (for helpful suggestions during EPIC data reduction), A. Bodaghee, F. F\u00fcrst, F. Gastaldello, K. Pottschmidt (for their useful advice on NuSTAR data), and K. Arnaud (for help with simftest in xspec). We are grateful to P. Esposito, S. Mereghetti and A.J. Bird for interesting and helpful discussions. We thank our anonymous referee for very constructive comments that helped to significantly improve the paper. We acknowledge financial contribution from the grant from PRIN-INAF 2014 \"Toward a unified picture of accretion in High Mass X-Ray Binaries\" (PI Sidoli) and from the agreement ASI-INAF NuSTAR I/037/12/0.\n\nAccepted Version - 1703.05030.pdf
",
"abstract": "We report the results of an XMM-Newton and NuSTAR coordinated observation of the Supergiant Fast X-ray Transient (SFXT) IGR J11215\u20135952, performed on 2016 February 14, during the expected peak of its brief outburst, which repeats every ~165 days. Timing and spectral analysis were performed simultaneously in the energy band 0.4\u201378 keV. A spin period of 187.0 (\u00b10.4) s was measured, consistent with previous observations performed in 2007. The X-ray intensity shows a large variability (more than one order of magnitude) on timescales longer than the spin period, with several luminous X-ray flares that repeat every 2\u20132.5 ks, some of which simultaneously observed by both satellites. The broadband (0.4\u201378 keV) time-averaged spectrum was well deconvolved with a double-component model (a blackbody plus a power law with a high energy cutoff) together with a weak iron line in emission at 6.4 keV (equivalent width, EW, of 40 \u00b1 10 eV). Alternatively, a partial covering model also resulted in an adequate description of the data. The source time-averaged X-ray luminosity was 10^(36) erg s^(\u22121) (0.1\u2013100 keV; assuming 7 kpc). We discuss the results of these observations in the framework of the different models proposed to explain SFXTs, supporting a quasi-spherical settling accretion regime, although alternative possibilities (e.g., centrifugal barrier) cannot be ruled out.",
"date": "2017-04-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "838",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 133",
"id_number": "CaltechAUTHORS:20170320-101004273",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170320-101004273",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa671a",
"primary_object": {
"basename": "1703.05030.pdf",
"url": "https://authors.library.caltech.edu/records/nyxh5-fht27/files/1703.05030.pdf"
},
"pub_year": "2017",
"author_list": "Sidoli, L.; Tiengo, A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/j1ejb-19r43",
"eprint_id": 75019,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:30:36",
"lastmod": "2023-10-25 14:40:04",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ludlam-R-M",
"name": {
"family": "Ludlam",
"given": "R. M."
},
"orcid": "0000-0002-8961-939X"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Cackett-E-C",
"name": {
"family": "Cackett",
"given": "E. C."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Bostrom-A-C",
"name": {
"family": "Bostrom",
"given": "A. C."
}
}
]
},
"title": "Relativistic Disk Reflection in the Neutron Star X-ray Binary XTE J1709-267 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: individual (XTE J1709-267) \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 December 2; revised 2017 March 4; accepted 2017 March 8; published 2017 March 29.\n\nWe thank the referee for their thoughtful comments that have led to the improvement of this work. R.M.L. would like to thank Fiona Harrison for the approval of the DDT that made this work possible. This research has made use of the NuSTAR Data Analysis Software, jointly developed by the ASI Science Data Center (Italy) and Caltech (USA). N.D. is supported by an NWO Vidi grant and a Marie Curie Intra-European Fellowship. E.M.C. gratefully acknowledges support from the National Science Foundation through CAREER award number AST-1351222.\n\nAccepted Version - 1703.03103.pdf
",
"abstract": "We perform the first reflection study of the soft X-ray transient and Type 1 burst source XTE J1709-267 using NuSTAR observations during its 2016 June outburst. There was an increase in flux near the end of the observations, which corresponds to an increase from ~0.04 L_(Edd) to ~0.06 L_(Edd) assuming a distance of 8.5 kpc. We have separately examined spectra from the low- and high-flux intervals, which are soft and show evidence of a broad Fe K line. Fits to these intervals with relativistic disk reflection models have revealed an inner-disk radius of 13.8^(+3.0)_(-1.8) Rg (where R_g = GM/c^2) for the low-flux spectrum and 23.4^(+15.6)_(-5.4) Rg for the high-flux spectrum at the 90% confidence level. The disk is likely truncated by a boundary layer surrounding the neutron star (NS) or the magnetosphere. Based on the measured luminosity and the accretion efficiency for a disk around an NS, we estimate that the theoretically expected size for the boundary layer would be ~0.9-1.1 R_g from the NS's surface, which can be increased by spin or viscosity effects. Another plausible scenario is that the disk could be truncated by the magnetosphere. We place a conservative upper limit on the strength of the magnetic field at the poles (assuming a* = 0 and M_(NS) = 1.4M\u2299) of B \u2a7d 0.75 \u2013 3.70 x 10^9 G, though X-ray pulsations have not been detected from this source.",
"date": "2017-04-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "838",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 79",
"id_number": "CaltechAUTHORS:20170310-093522243",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170310-093522243",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa661a",
"primary_object": {
"basename": "1703.03103.pdf",
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"pub_year": "2017",
"author_list": "Ludlam, R. M.; Miller, J. M.; et el."
},
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{
"id": "Matranga-M",
"name": {
"family": "Matranga",
"given": "M."
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{
"id": "Di-Salvo-T",
"name": {
"family": "Di Salvo",
"given": "T."
}
},
{
"id": "Iaria-R",
"name": {
"family": "Iaria",
"given": "R."
}
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"id": "Gambino-A-F",
"name": {
"family": "Gambino",
"given": "A. F."
}
},
{
"id": "Burderi-L",
"name": {
"family": "Burderi",
"given": "L."
}
},
{
"id": "Riggio-A",
"name": {
"family": "Riggio",
"given": "A."
}
},
{
"id": "Sanna-A",
"name": {
"family": "Sanna",
"given": "A."
}
}
]
},
"title": "A re-analysis of the NuSTAR and XMM-Newton broad-band spectrum of Serpens X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "line: formation \u2013 line: identification \u2013 stars: individual: Serpens X-1 \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: general",
"note": "\u00a9 2017 ESO. Article published by EDP Sciences.\n\nReceived 22 March 2016; Accepted 23 December 2016; Published online 22 March 2017.\n\nWe thank the anonymous referee for useful suggestions which helped to improve the manuscript. The High-Energy Astrophysics Group of Palermo acknowledges support from the Fondo Finalizzato alla Ricerca (FFR) 2012/13, project N. 2012-ATE-0390, founded by the University of Palermo. This work was partially supported by the Regione Autonoma della Sardegna through POR-FSE Sardegna 2007-2013, L.R. 7/2007, Progetti di Ricerca di Base e Orientata, Project N. CRP-60529. We also acknowledge financial contribution from the agreement ASI-INAF I/037/12/0.\n\nSubmitted - 1701.01069v1.pdf
",
"abstract": "Context. High-resolution X-ray spectra of neutron star low-mass X-ray binaries (LMXBs) in the energy range 6.4\u22126.97 keV are often characterized by the presence of K\u03b1 transition features of iron at different ionization stages. Since these lines are thought to originate by reflection of the primary Comptonization spectrum over the accretion disk, the study of these features allows us to investigate the structure of the accretion flow close to the central source. Thus, the study of these features gives us important physical information on the system parameters and geometry. Ser X-1 is a well studied LMXB that clearly shows a broad iron line. Several attempts to fit this feature as a smeared reflection feature have been performed on XMM-Newton, suzaku, NuSTAR, and, more recently, on Chandra data, finding different results for the inner radius of the disk and other reflection or smearing parameters. High-quality broad-band NuSTAR data on Ser X-1 have recently been published. Using relativistically smeared self-consistent reflection models, a value of R_(in) close to 1.0 R_(ISCO) (corresponding to 6 R_g, where R_g is the Gravitational radius, defined as usual R_g = GM/c^2) was found, as well as a low inclination angle of less than ~10\u00b0.\nAims. The aim of this paper is to probe to what extent the choice of reflection and continuum models (and uncertainties therein) can affect the conclusions about the disk parameters inferred from the reflection component. To this aim, we re-analyze all the available public NuSTAR and XMM-Newton observations, which have the best sensitivity at the iron line energy, of Ser X-1. Ser X-1 is a well studied source, its spectrum has been observed by several instruments, and is therefore one of the best sources for this study.\nMethods. We used slightly different continuum and reflection models with respect to those adopted in the literature for this source. In particular, we fit the iron line and other reflection features with self-consistent reflection models, such as reflionx (with a power-law illuminating continuum modified with a high-energy cutoff to mimic the shape of the incident Comptonization spectrum) and rfxconv. With these models, we fit NuSTAR and XMM-Newton spectra yielding consistent spectral results.\nResults. Our results are in line with those already found by Miller et al. (2013) but are less extreme. In particular, we find the inner disk radius to be ~13 R_g with an inclination angle with respect to the line of sight of ~27\u00b0. We conclude that, while the choice of the reflection model has little impact on the disk parameters, as soon as a self-consistent model is used, the choice of the continuum model can be important in the precise determination of the disk parameters from the reflection component. Hence broad-band X-ray spectra are highly preferable to constrain the continuum and disk parameters.",
"date": "2017-04",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "600",
"publisher": "EDP Sciences",
"pagerange": "Art. No. \tA24",
"id_number": "CaltechAUTHORS:20170105-131100985",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170105-131100985",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201628576",
"primary_object": {
"basename": "1701.01069v1.pdf",
"url": "https://authors.library.caltech.edu/records/fk9jx-44140/files/1701.01069v1.pdf"
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"pub_year": "2017",
"author_list": "Matranga, M.; Di Salvo, T.; et el."
},
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"items": [
{
"id": "Fornasini-F-M",
"name": {
"family": "Fornasini",
"given": "Francesca M."
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"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
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"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mao-Peter-H",
"name": {
"family": "Mao",
"given": "Peter H."
}
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram"
},
"orcid": "0000-0003-1703-8796"
}
]
},
"title": "The NuSTAR Hard X-Ray Survey of the Norma Arm Region",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 October 12. Accepted 2017 February 19. Published 2017 April 6.\n\nWe thank the referee for feedback that helped improve the clarity of the work presented in this paper. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software, and calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We also made use of observations taken by the Chandra X-ray Observatory and of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. This work also made use of data products from observations made with ESO telescopes at the La Silla or Paranal Observatories under ESO program ID 179.B-2002. In addition, F.M.F. acknowledges support from the National Science Foundation Graduate Research Fellowship and thanks G. K. Keating for helpful conversations on some of the statistical measures and figures in the paper. JAT acknowledges support from Chandra grants GO4-15138X and GO5-16152X. FEB acknowledges support from CONICYT-Chile grants Basal-CATA PFB-06/2007, FONDECYT Regular 1141218, \"EMBIGGEN\" Anillo ACT1101, and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics (MAS). JCS acknowledges support from FONDECYT 3140310. RK acknowledges support from the Russian Science Foundation (grant 14-12-01315). DB thanks the French Space Agency (CNES) for financial support.\n\nPublished - Fornasini_2017_ApJS_229_33.pdf
Submitted - 1703.00021.pdf
",
"abstract": "We present a catalog of hard X-ray sources in a square-degree region surveyed by the Nuclear Spectroscopic Telescope Array (NuSTAR) in the direction of the Norma spiral arm. This survey has a total exposure time of 1.7 Ms, and the typical and maximum exposure depths are 50 ks and 1 Ms, respectively. In the area of deepest coverage, sensitivity limits of 5 \u00d7 10^(\u221214) and 4 \u00d7 10^(\u221214) erg s^(\u22121) cm^(\u22122) in the 3\u201310 and 10\u201320 keV bands, respectively, are reached. Twenty-eight sources are firmly detected, and 10 are detected with low significance; 8 of the 38 sources are expected to be active galactic nuclei. The three brightest sources were previously identified as a low-mass X-ray binary, high-mass X-ray binary, and pulsar wind nebula. Based on their X-ray properties and multiwavelength counterparts, we identify the likely nature of the other sources as two colliding wind binaries, three pulsar wind nebulae, a black hole binary, and a plurality of cataclysmic variables (CVs). The CV candidates in the Norma region have plasma temperatures of \u224810\u201320 keV, consistent with the Galactic ridge X-ray emission spectrum but lower than the temperatures of CVs near the Galactic center. This temperature difference may indicate that the Norma region has a lower fraction of intermediate polars relative to other types of CVs compared to the Galactic center. The NuSTAR logN\u2013logS distribution in the 10\u201320 keV band is consistent with the distribution measured by Chandra at 2\u201310 keV if the average source spectrum is assumed to be a thermal model with kT \u2248 15 keV, as observed for the CV candidates.",
"date": "2017-04",
"date_type": "published",
"publication": "Astrophysical Journal Supplement Series",
"volume": "229",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 33",
"id_number": "CaltechAUTHORS:20170407-140117671",
"issn": "0067-0049",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170407-140117671",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/Caltech/JPL"
},
{
"agency": "NSF"
},
{
"agency": "NASA",
"grant_number": "GO4-15138X"
},
{
"agency": "NASA",
"grant_number": "GO5-16152X"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Millennium Institute of Astrophysics (MAS)"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "3140310"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01315"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
"local_group": {
"items": [
{
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},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4365/aa61fc",
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}
],
"pub_year": "2017",
"author_list": "Fornasini, Francesca M.; Forster, Karl; et el."
},
{
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"eprint_id": 72697,
"eprint_status": "archive",
"datestamp": "2023-08-19 02:07:13",
"lastmod": "2023-10-23 22:51:27",
"type": "article",
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"creators": {
"items": [
{
"id": "van-de-Eijnden-J",
"name": {
"family": "van de Eijnden",
"given": "J."
}
},
{
"id": "Bagnoli-T",
"name": {
"family": "Bagnoli",
"given": "T."
}
},
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Zand-J-J-M",
"name": {
"family": "Zand",
"given": "J. J. M."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
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"orcid": "0000-0002-9378-4072"
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},
"title": "A strongly truncated inner accretion disk in the Rapid Burster",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual: MXB 1730-335",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 December 1. Received 2016 November 28; in original form 2016 November 3. Published: 05 December 2016. \n\nWe thank the referee for comments on this Letter. JvdE and ND are supported by a Vidi grant from the Netherlands Organization for Scientific Research (NWO) awarded to ND. ND also acknowledges support via a Marie Curie fellowship (FP-PEOPLE-2013-IEF-627148) from the European Commission. ACF, AL and MP are supported by Advanced Grant Feedback 340442 from the European Research Counsil (ERC). TB acknowledges support from NewCompStar (COST Action MP1304). JvdE and TB acknowledge the hospitality of the Institute of Astronomy in Cambridge, where this research was carried out. We are grateful to Fiona Harrison, Norbert Schartel, Neil Gehrels and the observation planners for making these Director's Discretionary Time observations possible.\n\nAccepted Version - 1612.00384v1.pdf
",
"abstract": "The neutron star (NS) low-mass X-ray binary (LMXB) the Rapid Burster (RB; MXB 1730-335) uniquely shows both Type I and Type II X-ray bursts. The origin of the latter is ill-understood but has been linked to magnetospheric gating of the accretion flow. We present a spectral analysis of simultaneous Swift, NuSTARand XMM\u2013Newton observations of the RB during its 2015 outburst. Although a broad Fe K line has been observed before, the high quality of our observations allows us to model this line using relativistic reflection models for the first time. We find that the disc is strongly truncated at 41.8^(+6.7)_(\u22125.3) gravitational radii (\u223c87\u2009km), which supports magnetospheric Type II burst models and strongly disfavours models involving instabilities at the innermost stable circular orbit. Assuming that the RB magnetic field indeed truncates the disc, we find B = (6.2 \u00b1 1.5) \u00d7 10^8 G, larger than typically inferred for NS LMXBs. In addition, we find a low inclination (i=29\u00b0\u00b12\u00b0). Finally, we comment on the origin of the Comptonized and thermal components in the RB spectrum.",
"date": "2017-03-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "466",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L98-L102",
"id_number": "CaltechAUTHORS:20161209-150822081",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161209-150822081",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/slw244",
"primary_object": {
"basename": "1612.00384v1.pdf",
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"pub_year": "2017",
"author_list": "van de Eijnden, J.; Bagnoli, T.; et el."
},
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"items": [
{
"id": "Yukita-Mihoko",
"name": {
"family": "Yukita",
"given": "M."
},
"orcid": "0000-0001-6366-3459"
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "A. E."
},
"orcid": "0000-0001-8667-2681"
},
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"name": {
"family": "Wik",
"given": "D."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T. J."
},
"orcid": "0000-0003-0976-4755"
},
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"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "K."
},
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},
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"name": {
"family": "Zezas",
"given": "A."
},
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},
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"id": "Antoniou-V",
"name": {
"family": "Antoniou",
"given": "V."
},
"orcid": "0000-0001-7539-1593"
},
{
"id": "Ballhausen-R",
"name": {
"family": "Ballhausen",
"given": "R."
}
},
{
"id": "Lehmer-B-D",
"name": {
"family": "Lehmer",
"given": "B. D."
},
"orcid": "0000-0003-2192-3296"
},
{
"id": "Lien-A-Y",
"name": {
"family": "Lien",
"given": "A."
}
},
{
"id": "Williams-B-F",
"name": {
"family": "Williams",
"given": "B."
},
"orcid": "0000-0002-7502-0597"
},
{
"id": "Baganoff-F-K",
"name": {
"family": "Baganoff",
"given": "F."
}
},
{
"id": "Boyd-P-T",
"name": {
"family": "Boyd",
"given": "P. T."
},
"orcid": "0000-0003-0442-4284"
},
{
"id": "Enoto-Teruaki",
"name": {
"family": "Enoto",
"given": "T."
},
"orcid": "0000-0003-1244-3100"
},
{
"id": "Kennea-J-A",
"name": {
"family": "Kennea",
"given": "J."
},
"orcid": "0000-0002-6745-4790"
},
{
"id": "Page-K-L",
"name": {
"family": "Page",
"given": "K. L."
},
"orcid": "0000-0001-5624-2613"
},
{
"id": "Choi-Y",
"name": {
"family": "Choi",
"given": "Y."
}
}
]
},
"title": "Identification of the Hard X-ray Source Dominating the E > 25 keV Emission of the Nearby Galaxy M31",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: bulges \u2013 galaxies: individual (M31) \u2013 pulsars: general \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 16; revised 2017 February 17; accepted 2017 February 21; published 2017 March 22. \n\nWe would like to thank the referee for his/her comments, which improved our manuscript. We sincerely thank Neil Gehrels for approving the Swift DDT observations used in this work. We also thank NuSTAR and Swift mission planners for making the Swift and NuSTAR observations simultaneous. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). This work was supported by NuSTAR GO NNX15AV30G. We are grateful to Antara Basu-Zych, Hans Krimm, Craig Markwardt, Ryan Hickox, Dheeraj Pasham, Koji Mukai, Lennart van Haaften, and Panayiotis Tzanavaris for helpful discussions. K.L.P. acknowledges funding from the UK Space Agency. R.B. acknowledges funding from the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt grant 50 OR 1410. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift.\n\nAccepted Version - 1703.07318.pdf
",
"abstract": "We report the identification of a bright hard X-ray source dominating the M31 bulge above 25 keV from a simultaneous NuSTAR\u2013Swift observation. We find that this source is the counterpart to Swift J0042.6+4112, which was previously detected in the Swift BAT All-sky Hard X-ray Survey. This SwiftBAT source had been suggested to be the combined emission from a number of point sources; our new observations have identified a single X-ray source from 0.5 to 50 keV as the counterpart for the first time. In the 0.5\u201310 keV band, the source had been classified as an X-ray Binary candidate in various Chandra and XMM-Newton studies; however, since it was not clearly associated with Swift J0042.6+4112, the previous E < 10 keV observations did not generate much attention. This source has a spectrum with a soft X-ray excess (kT ~ 0.2 keV) plus a hard spectrum with a power law of and a cutoff around 15\u201320 keV, typical of the spectral characteristics of accreting pulsars. Unfortunately, any potential pulsation was undetected in the NuSTAR data, possibly due to insufficient photon statistics. The existing deep HST images exclude high-mass (>3 M\u2299) donors at the location of this source. The best interpretation for the nature of this source is an X-ray pulsar with an intermediate-mass (<3 M\u2299) companion or a symbiotic X-ray binary. We discuss other possibilities in more detail.",
"date": "2017-03-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "838",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 47",
"id_number": "CaltechAUTHORS:20170327-085423420",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170327-085423420",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/aa62a3",
"primary_object": {
"basename": "1703.07318.pdf",
"url": "https://authors.library.caltech.edu/records/fw8nj-kt455/files/1703.07318.pdf"
},
"pub_year": "2017",
"author_list": "Yukita, M.; Ptak, A.; et el."
},
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"eprint_id": 74645,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:55:24",
"lastmod": "2023-10-24 22:49:33",
"type": "article",
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"creators": {
"items": [
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "Michael L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "Ciro"
},
"orcid": "0000-0003-2532-7379"
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},
"title": "The response of relativistic outflowing gas to the inner accretion disk of a black hole",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2017 Macmillan Publishers Limited \n\nreceived 24 October 2016; accepted 9 January 2017. \n\nM.L.P., C.P., A.C.F. and A.L. acknowledge support from the European Research Council through Advanced Grant on Feedback 340492. W.N.A. and G.M. acknowledge support from the European Union Seventh Framework Programme (FP7/2013-2017) under grant agreement number 312789, StrongGravity. D.J.K.B. acknowledges support from the Science and Technology Facilities Council. This work is based on observations with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. D.R.W. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF6-170160, awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology. \n\nCode availability: All the code used for the data reduction is available from the respective websites. XSPEC and SPEX are freely available online. Code used for generating figures, calculating flux-resolved extraction intervals, and calculating line significance, is available upon request to M.L.P. \n\nData availability statement: All data used in this work is publicly available. The XMM-Newton observations can be accessed from the XMM-Newton science archive (http://nxsa.esac.esa.int/nxsa-web/) and the NuSTAR data from the HEASARC archive (http://heasarc.gsfc.nasa.gov/docs/archive.html). Figure data are available from the authors. \n\nAuthor Contributions: \nM.L.P. wrote the manuscript with comments from all authors and performed the flux-resolved EPIC-pn analysis and line detections. C.P. analysed the RGS data and did the physical modelling. A.C.F. led the XMM-Newton proposal. All authors were involved with the proposal at various stages. \n\nThe authors declare no competing financial interests. \n\nReviewer Information: Nature thanks G. Risaliti and the other anonymous reviewer(s) for their contribution to the peer review of this work.\n\nSupplemental Material - nature21385-sf1.jpg
Supplemental Material - nature21385-sf2.jpg
Supplemental Material - nature21385-sf3.jpg
Supplemental Material - nature21385-sf4.jpg
Supplemental Material - nature21385-sf5.jpg
Supplemental Material - nature21385-st1.jpg
Supplemental Material - nature21385-st2.jpg
",
"abstract": "The brightness of an active galactic nucleus is set by the gas falling onto it from the galaxy, and the gas infall rate is regulated by the brightness of the active galactic nucleus; this feedback loop is the process by which supermassive black holes in the centres of galaxies may moderate the growth of their hosts1. Gas outflows (in the form of disk winds) release huge quantities of energy into the interstellar medium2, potentially clearing the surrounding gas. The most extreme (in terms of speed and energy) of these\u2014the ultrafast outflows\u2014are the subset of X-ray-detected outflows with velocities higher than 10,000 kilometres per second, believed to originate in relativistic (that is, near the speed of light) disk winds a few hundred gravitational radii from the black hole3. The absorption features produced by these outflows are variable4, but no clear link has been found between the behaviour of the X-ray continuum and the velocity or optical depth of the outflows, owing to the long timescales of quasar variability. Here we report the observation of multiple absorption lines from an extreme ultrafast gas flow in the X-ray spectrum of the active galactic nucleus IRAS 13224\u22123809, at 0.236\u2009\u00b1\u20090.006 times the speed of light (71,000 kilometres per second), where the absorption is strongly anti-correlated with the emission of X-rays from the inner regions of the accretion disk. If the gas flow is identified as a genuine outflow then it is in the fastest five per cent of such winds, and its variability is hundreds of times faster than in other variable winds, allowing us to observe in hours what would take months in a quasar. We find X-ray spectral signatures of the wind simultaneously in both low- and high-energy detectors, suggesting a single ionized outflow, linking the low- and high-energy absorption lines. That this disk wind is responding to the emission from the inner accretion disk demonstrates a connection between accretion processes occurring on very different scales: the X-ray emission from within a few gravitational radii of the black hole ionizing the disk wind hundreds of gravitational radii further away as the X-ray flux rises.",
"date": "2017-03-01",
"date_type": "published",
"publication": "Nature",
"volume": "543",
"number": "7643",
"publisher": "Nature Publishing Group",
"pagerange": "83-86",
"id_number": "CaltechAUTHORS:20170301-125605305",
"issn": "0028-0836",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-125605305",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "340492"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "PF6-170160"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
}
]
},
"collection": "CaltechAUTHORS",
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"value": "Astronomy Department"
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]
},
"doi": "10.1038/nature21385",
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"pub_year": "2017",
"author_list": "Parker, Michael L.; Pinto, Ciro; et el."
},
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"datestamp": "2023-08-19 01:55:04",
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"items": [
{
"id": "Xu-Yanjun",
"name": {
"family": "Xu",
"given": "Yanjun"
},
"orcid": "0000-0003-2443-3698"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
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{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
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},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
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},
"title": "Evidence for Relativistic Disk Reflection in the Seyfert 1h Galaxy/ULIRG IRAS 05189\u20132524 Observed by NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: active \u2013 galaxies: individual (IRAS 05189\u20132524) \u2013 galaxies: Seyfert \u2013 X-rays: galaxies",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 4; revised 2017 January 31; accepted 2017 January 31; published 2017 February 28. \n\nWe thank the anonymous referee for helpful comments that improved the paper. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. This work was supported under NASA Contract no. NNG08FD60C and made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA, and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States.\n\nPublished - Xu_2017_ApJ_837_21.pdf
Submitted - 1702.00073.pdf
",
"abstract": "We present a spectral analysis of the NuSTAR and XMM-Newton observations of the Seyfert 1h galaxy/ULIRG IRAS 05189\u20132524 taken in 2013. We find evidence for relativistic disk reflection in the broadband X-ray spectrum: a highly asymmetric broad Fe K\u03b1 emission line extending down to 3 keV and a Compton scattering component above 10 keV. Physical modeling with a self-consistent disk reflection model suggests that the accretion disk is viewed at an intermediate angle with a supersolar iron abundance, and a mild constraint can be put on the high-energy cutoff of the power-law continuum. We test the disk reflection modeling under different absorption scenarios. A rapid black hole spin is favored; however, we cannot place a model-independent tight constraint on the value. The high reflection fraction (R_(ref) \u2243 2.0\u20133.2) suggests that the coronal illuminating source is compact and close to the black hole (lying within 8.7 R_g above the central black hole), where light-bending effects are important.",
"date": "2017-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "837",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 21",
"id_number": "CaltechAUTHORS:20170228-110354967",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170228-110354967",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Alexander von Humboldt Foundation"
},
{
"agency": "Swiss National Science Foundation (SNSF)"
}
]
},
"collection": "CaltechAUTHORS",
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"doi": "10.3847/1538-4357/aa5df4",
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"pub_year": "2017",
"author_list": "Xu, Yanjun; Balokovi\u0107, Mislav; et el."
},
{
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"id": "Bult-P",
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},
"title": "The stochastic X-ray variability of the accreting millisecond pulsar MAXI J0911-655",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: individual (MAXI J0911-655) \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 January 5; revised 2017 February 3; accepted 2017 February 8; published 2017 March 3. \n\nI would like to thank Marieke van Doesburgh for sharing some of the data behind Figure 4 and the referee for constructive feedback that helped improve the paper. This work was supported by an NPP fellowship at NASA Goddard Space Flight Center.\n\nAccepted Version - 1702.04182.pdf
",
"abstract": "In this work, I report on the stochastic X-ray variability of the 340 Hz accreting millisecond pulsar MAXI J0911\u2013655. Analyzing pointed observations of the XMM-Newton and NuSTAR observatories, I find that the source shows broad band-limited stochastic variability in the 0.01-10 Hz range with a total fractional variability of ~24% rms in the 0.4-3 keV energy band that increases to ~40% rms in the 3\u201310 keV band. Additionally, a pair of harmonically related quasi-periodic oscillations (QPOs) are discovered. The fundamental frequency of this harmonic pair is observed between frequencies of 62 and 146 mHz. Like the band-limited noise, the amplitudes of the QPOs show a steep increase as a function of energy; this suggests that they share a similar origin, likely the inner accretion flow. Based on their energy dependence and frequency relation with respect to the noise terms, the QPOs are identified as low-frequency oscillations and discussed in terms of the Lense\u2013Thirring precession model.",
"date": "2017-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "837",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 61",
"id_number": "CaltechAUTHORS:20170222-115108839",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-115108839",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"doi": "10.3847/1538-4357/aa607f",
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{
"id": "Chen-Chien-Ting-J",
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"given": "C.-T. J."
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"name": {
"family": "Reines",
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"id": "Del-Moro-A",
"name": {
"family": "Del Moro",
"given": "A."
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"id": "Gandhi-Poshak",
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"family": "Gandhi",
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"family": "Koss",
"given": "M. J."
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{
"id": "Lanz-L",
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"family": "Lanz",
"given": "L."
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"name": {
"family": "Luo",
"given": "B."
},
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{
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"name": {
"family": "Mullaney",
"given": "J. R."
},
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"name": {
"family": "Ricci",
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"family": "Trump",
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},
"title": "Hard X-Ray-selected AGNs in Low-mass Galaxies from the NuSTAR Serendipitous Survey",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: dwarf; X-rays: galaxies",
"note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 October 11; revised 2017 January 24; accepted 2017 January 27; published 2017 March 1. \n\nWe thank the referee for carefully reading the manuscript and providing helpful comments. This work was supported under NASA contract no. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). C.-T.J.C. and W.N.B. acknowledge support from Caltech NuSTAR subcontract 44A-1092750. Support for A.E.R. was provided by NASA through Hubble Fellowship grant HST-HF2-51347.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. D.M.A. gratefully acknowledges support from Science and Technology Facilities Council (ST/L00075X/1). F.E.B. and C.R. acknowledge support from NASA NuSTAR A01 Award NNX15AV27G, CONICYT-Chile grants Basal-CATA PFB-06/2007, FONDECYT Regular 1141218 and 1151408, China-CONICYT Fellowship, and the Ministry of Economy, Development, and Tourisms Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics, MAS. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. This research has made use of the \"Aladin sky atlas\" developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000). This work has also made use of observations made with the Spitzer Space Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Chandra - , XMM-Newton - Newton X-Ray Multimirror Mission satellite, Swift/BAT - Swift Gamma-Ray Burst Mission, Swift/XRT - , WISE - Wide-field Infrared Survey Explorer, Keck - , NTT - New Techology Telescope, Palomar - . \n\nSoftware: Astropy, CIAO, HEAsoft, XMMSAS, XSPEC.\n\nPublished - Chen__2017_ApJ_837_48.pdf
Submitted - 1701.08768v1.pdf
Submitted - ctc_nustardwarf_figset.pdf
",
"abstract": "We present a sample of 10 low-mass active galactic nuclei (AGNs) selected from the 40-month Nuclear Spectroscopic Telescope Array (NuSTAR) serendipitous survey. The sample is selected to have robust NuSTAR detections at 3-24 keV, to be at z < 0.3, and to have optical r-band magnitudes at least 0.5 mag fainter than an L_\u2605 galaxy at its redshift. The median values of absolute magnitude, stellar mass, and 2\u201310 X-ray luminosity of our sample are \u3008 M_\u2605\u3009 = -20.03, M_r\u3009 = 4.6 x 10^9 M_\u2299, and \u3008L_(2-10 keV)\u3009 = 3.1 x 10^(42) erg s^(\u22121), respectively. Five objects have detectable broad H\u03b1 emission in their optical spectra, indicating black hole masses of (1.1--10.4) x 10^6 M_\u2299. We find that 30_(-10)^(+17)% of the galaxies in our sample do not show AGN-like optical narrow emission lines, and one of the 10 galaxies in our sample, J115851+4243.2, shows evidence for heavy X-ray absorption. This result implies that a non-negligible fraction of low-mass galaxies might harbor accreting massive black holes that are missed by optical spectroscopic surveys and < 10 keV X-ray surveys. The mid-IR colors of our sample also indicate that these optically normal low-mass AGNs cannot be efficiently identified with typical AGN selection criteria based on Wide Field Infrared Survey Explorer colors. While the hard (> 10 keV) X-ray-selected low-mass AGN sample size is still limited, our results show that sensitive NuSTAR observations are capable of probing faint hard X-ray emission originating from the nuclei of low-mass galaxies out to moderate redshift (z > 0.3), thus providing a critical step in understanding AGN demographics in low-mass galaxies.",
"date": "2017-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "837",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 48",
"id_number": "CaltechAUTHORS:20170201-075210760",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170201-075210760",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51347.001-A"
},
{
"agency": "NASA",
"grant_number": "NAS 5-26555"
},
{
"agency": "NASA",
"grant_number": "NNX15AV27G"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1151408"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "China-CONICYT Fellowship"
},
{
"agency": "NSF"
},
{
"agency": "Alfred P. Sloan Foundation"
},
{
"agency": "Participating Institutions"
},
{
"agency": "Department of Energy (DOE)"
}
]
},
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"id": "Space-Radiation-Laboratory"
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"id": "NuSTAR"
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{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/aa5d5b",
"primary_object": {
"basename": "Chen__2017_ApJ_837_48.pdf",
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"basename": "1701.08768v1.pdf",
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"pub_year": "2017",
"author_list": "Chen, C.-T. J.; Brandt, W. N.; et el."
},
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{
"id": "Shtykovsky-A-E",
"name": {
"family": "Shtykovsky",
"given": "A. E."
}
},
{
"id": "Lutovinov-A-A",
"name": {
"family": "Lutovinov",
"given": "A. A."
}
},
{
"id": "Arefiev-V-A",
"name": {
"family": "Arefiev",
"given": "V. A."
}
},
{
"id": "Molkov-S-V",
"name": {
"family": "Molkov",
"given": "S. V."
}
},
{
"id": "Tsygankov-S-S",
"name": {
"family": "Tsygankov",
"given": "S. S."
},
"orcid": "0000-0002-9679-0793"
},
{
"id": "Revnivtsev-M-G",
"name": {
"family": "Revnivtsev",
"given": "M. G."
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"title": "NuSTAR observations of the X-ray pulsar LMC X-4: A constraint on the magnetic field and tomography of the system in the fluorescent iron line",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "neutron stars, magnetic field, X-ray pulsars, LMC X-4",
"note": "\u00a9 2017 Pleiades Publishing, Inc. \n\nOriginal Russian Text \u00a9 A.E. Shtykovsky, A.A. Lutovinov, V.A. Arefiev, S.V. Molkov, S.S. Tsygankov, M.G. Revnivtsev, 2017, published in Pis'ma v Astronomicheskii Zhurnal, 2017, Vol. 43, No. 3, pp. 203\u2013213. \n\nReceived: 27 September 2016; First Online: 11 March 2017. \n\nThis work was supported by the Russian Science Foundation (project no. 14-12-01287). We used data from the NuSTAR observatory, a project led by Caltech, funded by NASA, and managed by NASA/JPL. The data were reduced using the NUSTARDAS package, jointly developed by ASDC (Italy) and Caltech (USA). We thank R.A. Krivonos for his help in processing the NuSTAR data.\n\nAccepted Version - 1610.08092v1.pdf
",
"abstract": "We present the results of the spectral and timing analysis of the X-ray pulsar LMC X-4 based on data from the NuSTAR observatory in the broad X-ray energy range 3-79 keV. Along with a detailed analysis of the source's averaged spectrum, high-precision spectra corresponding to different phases of the neutron star spin cycle have been obtained for the first time. The Comptonization model is shown to describe best the source's spectrum, and the evolution of its parameters as a function of the pulse phase has been traced. For all spectra (the averaged and phase-resolved ones) in the energy range 5-55 keV we have searched for the cyclotron absorption line. The derived upper limit on the optical depth of the cyclotron line \u03c4 0.15 (3 \u03c3) points to the absence of this feature in the given energy range, which provides a constraint on the magnetic field of the neutron star: B < 3 \u00d7 10^(11) or > 6.5 \u00d7 10^(12) G. The latter constraint is consistent with the magnetic field estimate obtained by analyzing the pulsar's power spectrum, B \u2245 3 \u00d7 10^(13) G. Based on our analysis of the phase-resolved spectra, we have determined the delay between the emission peaks and the equivalent width of the fluorescent iron line. This delay depends on the orbital phase and is apparently associated with the travel time of photons between the emitting regions in the vicinity of the neutron star and the region where the flux is reflected (presumably in the inflowing stream or at the place of interaction between the stream and the outer edge of the accretion disk).",
"date": "2017-03",
"date_type": "published",
"publication": "Astronomy Letters",
"volume": "43",
"number": "3",
"publisher": "Springer",
"pagerange": "175-185",
"id_number": "CaltechAUTHORS:20161027-094005120",
"issn": "1063-7737",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161027-094005120",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1134/S1063773717030069",
"primary_object": {
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"author_list": "Shtykovsky, A. E.; Lutovinov, A. A.; et el."
},
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{
"id": "Reynolds-C",
"name": {
"family": "Reynolds",
"given": "Cormac"
},
"orcid": "0000-0002-1510-4860"
},
{
"id": "Punsly-B",
"name": {
"family": "Punsly",
"given": "Brian"
},
"orcid": "0000-0002-9448-2527"
},
{
"id": "Miniutti-G",
"name": {
"family": "Miniutti",
"given": "Giovanni"
}
},
{
"id": "O'Dea-C-P",
"name": {
"family": "O'Dea",
"given": "Christopher P."
},
"orcid": "0000-0001-6421-054X"
},
{
"id": "Hurley-Walker-N",
"name": {
"family": "Hurley-Walker",
"given": "Natasha"
},
"orcid": "0000-0002-5119-4808"
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]
},
"title": "The Relativistic Jet-accretion Flow-wind Connection in Mrk 231",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: jets \u2013 quasars: absorption lines \u2013 quasars: general",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 15; revised 2016 December 28; accepted 2016 December 28; published 2017 February 16. \n\nThis research made use of data obtained with NuSTAR, a\nproject led by Caltech, funded by NASA and managed by\nNASA/JPL, and utilized the NUSTARDAS software package,\njointly developed by the ASDC (Italy) and Caltech (USA). We\nalso made use of data obtained with XMM-Newton, an ESA\nscience mission with instruments and contributions directly\nfunded by ESA Member States. This work made use of\nDirector's Discretionary Time on both NuSTAR and XMMNewton for which we thank Fiona Harrison and Norbert\nSchartel for approving, as well as the NuSTAR and XMMNewton SOC for implementing and coordinating the observations. We would like to thank S. Veilleux and M. Melendez for\nsharing their G130M data. The National Radio Astronomy\nObservatory is a facility of the National Science Foundation\noperated under cooperative agreement by Associated Universities,\nInc. This research has made use of NASA's Astrophysics\nData System Bibliographic Services. This work made use of\nthe Swinburne University of Technology software correlator,\ndeveloped as part of the Australian Major National Research\nFacilities Programme and operated under licence.\n\nSubmitted - 1701.03190v1.pdf
",
"abstract": "Long-term radio monitoring of the broad absorption line (BAL) quasar Mrk 231 at 17.6 GHz detected a strong flare in 2015. This triggered four epochs of Very Long Baseline Array (VLBA) observations from 8.4 to 43 GHz as well as three epochs of X-ray observations with NuSTAR and two with XMM over a 15 week period. Two ejected components were detected by the VLBA observations. A conservative lower bound on the apparent speed of the first ejection is attained by assuming that it was ejected when the flare began, \u03bd_(app) > 3.15c. Serendipitous far-UV Hubble Space Telescopeobservations combined with our long-term radio monitoring seem to indicate that episodes of relativistic ejections suppress flux that is emitted at wavelengths shortward of the peak of the far-UV spectral energy distribution, similar to what has been observed in radio-loud quasars. Episodes of strong jet production also seem to suppress the high-ionization BAL wind seen in weak jet states. We found a statistically significant increase (~25%) of the 3\u201312 keV flux during the radio flare relative to a quiescent radio state. This is explained by an ultra-fast (~0.06c) X-ray-absorbing photoionized wind that is significantly detected only in the low-radio state (similar to Galactic black holes). Mrk 231 is becoming more radio loud. We found that the putative parsec-scale radio lobe doubled in brightness in nine years. Furthermore, large flares are more frequent, with three major flares occurring at ~2 year intervals.",
"date": "2017-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 155",
"id_number": "CaltechAUTHORS:20170113-142207861",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170113-142207861",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
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"doi": "10.3847/1538-4357/836/2/155",
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"author_list": "Reynolds, Cormac; Punsly, Brian; et el."
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"id": "Alexander-D-M",
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"family": "Boorman",
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"family": "Stanley",
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"family": "Zhang",
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},
"title": "A New Compton-thick AGN in Our Cosmic Backyard: Unveiling the Buried Nucleus in NGC 1448 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 techniques: spectroscopic \u2013 X-rays: galaxies \u2013 X-rays: individual\n(NGC 1448)",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 July 27; revised 2016 December 20; accepted 2016 December 27; published 2017 February 17.\n\nWe thank the anonymous referee for useful comments which have helped to improve the paper. We acknowledge financial support from Majlis Amanah Rakyat (MARA) Malaysia (A.A.), the Science and Technology Facilities Council (STFC) grant ST/L00075X/1 (D.M.A.), ST/J003697/1 (P.G.), and ST/K501979/1 (G.B.L.). F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT Regular 1141218, \"EMBIGGEN\" Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. P.B. would like to thank the STFC for funding. S.M.L.'s research was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by the Universities Space Research Association under contract with NASA. M.K. acknowledges support from the Swiss National Science Foundation and Ambizione fellowship grant PZ00P2_154799/1. We acknowledge financial support from the CONICYT-Chile grants \"EMBIGGEN\" Anillo ACT1101 (C.R.), FONDECYT 1141218 (C.R.), Basal-CATA PFB\u201306/2007 (C.R.) and from the China-CONICYT fund (C.R.).\n\nNuSTAR is a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). We thank the NuSTAR Operations, Software and Calibrations teams for support with these observations. This research has made use of the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research also made use of the data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) Online Service, provided by the NASA/Goddard Space Flight Center, and the NASA/IPAC extragalactic Database (NED) operated by JPL, Caltech under contract with NASA.\n\nFacilities: Chandra - , Gemini:South - , NTT - , NuSTAR.\n\nPublished - Annuar_2017_ApJ_836_165.pdf
Submitted - 1701.00497.pdf
",
"abstract": "NGC 1448 is one of the nearest luminous galaxies (L_(8\u20131000\u03bcm) > 10^9 L\u2299) to ours (z = 0.00390), and yet the active galactic nucleus (AGN) it hosts was only recently discovered, in 2009. In this paper, we present an analysis of the nuclear source across three wavebands: mid-infrared (MIR) continuum, optical, and X-rays. We observed the source with the Nuclear Spectroscopic Telescope Array (NuSTAR), and combined these data with archival Chandra data to perform broadband X-ray spectral fitting (\u22480.5\u201340 keV) of the AGN for the first time. Our X-ray spectral analysis reveals that the AGN is buried under a Compton-thick (CT) column of obscuring gas along our line of sight, with a column density of N H(los) \u2273 2.5 \u00d7 10^(24) cm^(\u22122). The best-fitting torus models measured an intrinsic 2\u201310 keV luminosity of L_(2-10,int) (3.5\u20137.6) \u00d7 10^(40) erg s^(\u22121), making NGC 1448 one of the lowest luminosity CTAGNs known. In addition to the NuSTAR observation, we also performed optical spectroscopy for the nucleus in this edge-on galaxy using the European Southern Observatory New Technology Telescope. We re-classify the optical nuclear spectrum as a Seyfert on the basis of the Baldwin\u2013Philips\u2013Terlevich diagnostic diagrams, thus identifying the AGN at optical wavelengths for the first time. We also present high spatial resolution MIR observations of NGC 1448 with Gemini/T-ReCS, in which a compact nucleus is clearly detected. The absorption-corrected 2\u201310 keV luminosity measured from our X-ray spectral analysis agrees with that predicted from the optical [O III]\u03bb5007 \u00c5 emission line and the MIR 12 \u03bcm continuum, further supporting the CT nature of the AGN.",
"date": "2017-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 165",
"id_number": "CaltechAUTHORS:20170222-080503232",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-080503232",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Majlis Amanah Rakyat (MARA)"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Basal-CATA PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Ministry of Economy, Development, and Tourism's Millennium Science Initiative",
"grant_number": "IC120009"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PZ00P2_154799/1"
},
{
"agency": "China-CONICYT Fund"
},
{
"agency": "NASA/JPL/Caltech"
}
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"url": "https://authors.library.caltech.edu/records/41w38-pgh85/files/Annuar_2017_ApJ_836_165.pdf"
}
],
"pub_year": "2017",
"author_list": "Annuar, A.; Alexander, D. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/74d9r-sq998",
"eprint_id": 72775,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:35:48",
"lastmod": "2023-10-23 22:55:56",
"type": "article",
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"creators": {
"items": [
{
"id": "Secrest-N-J",
"name": {
"family": "Secrest",
"given": "Nathan J."
},
"orcid": "0000-0002-4902-8077"
},
{
"id": "Schmitt-H-R",
"name": {
"family": "Schmitt",
"given": "Henrique R."
},
"orcid": "0000-0001-7376-8481"
},
{
"id": "Blecha-L",
"name": {
"family": "Blecha",
"given": "Laura"
},
"orcid": "0000-0002-2183-1087"
},
{
"id": "Rothberg-B",
"name": {
"family": "Rothberg",
"given": "Barry"
},
"orcid": "0000-0003-2283-2185"
},
{
"id": "Fischer-J",
"name": {
"family": "Fischer",
"given": "Jacqueline"
},
"orcid": "0000-0001-6697-7808"
}
]
},
"title": "Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: bulges \u2013 galaxies: dwarf \u2013 galaxies: interactions \u2013 galaxies: nuclei \u2013 galaxies: Seyfert",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 March 23; revised 2016 December 8; accepted 2016 December 9; published 2017 February 17.\n\nWe thank the anonymous referee for their thorough review of our manuscript. We also thank Shai Kaspi (Tel Aviv University) for his advice regarding the L_(2-10 KeV)\u2013R_(BLR) relation, Ren\u00e9 Andrae (Max-Planck-Institut f\u00fcr Astronomie) for his helpful discussion of statistical methods, and Sara Ellison (University of Victoria) for her helpful input during the completion of this work. Finally, we are indebted to Teznie Pugh and Jason Sanborn for their invaluable guidance during our observing run at the DCT.\nThis research has made use of the NuSTAR Data Analysis Software, jointly developed by the ASI Science Data Center (Italy) and the California Institute of Technology (USA) as well as the UK Swift Science Data Centre at the University of Leicester. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. The UKIDSS project is defined in Lawrence et al. (2007). UKIDSS uses the UKIRT Wide-Field Camera (WFCAM; Casali et al. 2007). The photometric system is described in Hewett et al. (2006), and the calibration is described in Hodgkin et al. (2009). The WFCAM science archive is described in Hambly et al. (2008). This research made use of Astropy, a community-developed core Python package for astronomy (Astropy Collaboration et al. 2013), and APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. This research has also made use of the NASA/IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\nN.J.S. held an NRC Research Associateship award at Naval Research Laboratory during the course of this research. Basic research in astronomy at the Naval Research Laboratory is funded by the Office of Naval Research.\n\nSubmitted - 1612.03163v1.pdf
",
"abstract": "We present a combined morphological and X-ray analysis of Was 49, an isolated, dual-AGN system notable for the presence of a dominant AGN, Was 49b, in the disk of the primary galaxy, Was 49a, at a projected radial distance of 8 kpc from the nucleus. Using X-ray data from Chandra, the Nuclear Spectroscopic Telescope Array, and Swift, we find that this AGN has a bolometric luminosity of L_(bol) ~ 10^(45) erg s^(\u22121), with a black hole mass of M_(BH) = 1.3^(+2.9)_(-0.9) x 10^8 M\u2299. Despite the large mass, our analysis of optical data from the Discovery Channel Telescope shows that the supermassive black hole (SMBH) is hosted by a stellar counterpart with a mass of only 5.6^(+4.9)_(-2.6) x 10^9 M\u2299, which makes the SMBH potentially larger than expected from SMBH\u2013galaxy scaling relations, and the stellar counterpart exhibits a morphology that is consistent with dwarf elliptical galaxies. Our analysis of the system in the r and Kbands indicates that Was 49 is a minor merger, with the mass ratio of Was 49b to Was 49a between ~1:7 and ~1:15. This is in contrast with findings that the most luminous merger-triggered AGNs are found in major mergers and that minor mergers predominantly enhance AGN activity in the primary galaxy.",
"date": "2017-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 183",
"id_number": "CaltechAUTHORS:20161213-111233599",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161213-111233599",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/836/2/183",
"primary_object": {
"basename": "1612.03163v1.pdf",
"url": "https://authors.library.caltech.edu/records/74d9r-sq998/files/1612.03163v1.pdf"
},
"pub_year": "2017",
"author_list": "Secrest, Nathan J.; Schmitt, Henrique R.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/gdyrx-37562",
"eprint_id": 71505,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:27:54",
"lastmod": "2023-10-23 15:50:44",
"type": "article",
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"creators": {
"items": [
{
"id": "Keek-L",
"name": {
"family": "Keek",
"given": "L."
}
},
{
"id": "Iwakiri-Wataru",
"name": {
"family": "Iwakiri",
"given": "W."
}
},
{
"id": "Serino-M",
"name": {
"family": "Serino",
"given": "M."
}
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "in-'t-Zand-J-J-M",
"name": {
"family": "in 't Zand",
"given": "J. J. M."
}
},
{
"id": "Strohmayer-T-E",
"name": {
"family": "Strohmayer",
"given": "T. E."
},
"orcid": "0000-0001-7681-5845"
}
]
},
"title": "X-ray Reflection and An Exceptionally Long Thermonuclear Helium Burst from IGR J17062-6143",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: individual (IGR J17062-6143) \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: bursts",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 October 24; revised 2017 January 13; accepted 2017 January 16; published 2017 February 13. \n\nL.K. is supported by NASA under award number NNG06EO90A. L.K. thanks the International Space Science Institute in Bern, Switzerland for hosting an International Team on X-ray bursts. This work benefited from events supported by the National Science Foundation under Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). This research has made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. We thank the Swift observatory for performing the observations described in this paper.\n\nAccepted Version - 1610.07608v1.pdf
",
"abstract": "Thermonuclear X-ray bursts from accreting neutron stars power brief but strong irradiation of their surroundings, providing a unique way to study accretion physics. We analyze MAXI/Gas Slit Camera and Swift/XRT spectra of a day-long flash observed from IGR J17062-6143 in 2015. It is a rare case of recurring bursts at a low accretion luminosity of 0.15% Eddington. Spectra from MAXI, Chandra, and NuSTAR observations taken between the 2015 burst and the previous one in 2012 are used to determine the accretion column. We find it to be consistent with the burst ignition column of 5 \u00d7 10^(10) g cm^(\u22122), which indicates that it is likely powered by burning in a deep helium layer. The burst flux is observed for over a day, and decays as a straight power law: F \u221d t^(-1.15). The burst and persistent spectra are well described by thermal emission from the neutron star, Comptonization of this emission in a hot optically thin medium surrounding the star, and reflection off the photoionized accretion disk. At the burst peak, the Comptonized component disappears, when the burst may dissipate the Comptonizing gas, and it returns in the burst tail. The reflection signal suggests that the inner disk is truncated at ~102 gravitational radii before the burst, but may move closer to the star during the burst. At the end of the burst, the flux drops below the burst cooling trend for 2 days, before returning to the pre-burst level.",
"date": "2017-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 111",
"id_number": "CaltechAUTHORS:20161026-134501476",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161026-134501476",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/836/1/111",
"primary_object": {
"basename": "1610.07608v1.pdf",
"url": "https://authors.library.caltech.edu/records/gdyrx-37562/files/1610.07608v1.pdf"
},
"pub_year": "2017",
"author_list": "Keek, L.; Iwakiri, W.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/harj1-hyn54",
"eprint_id": 74293,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:29:18",
"lastmod": "2023-10-24 22:17:22",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "G. B."
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Jiang-B",
"name": {
"family": "Jiang",
"given": "B."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "The NuSTAR Serendipitous Survey: The 40-month Catalog and the Properties of the Distant High-energy X-Ray Source Population",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "catalogs \u2013 galaxies: active \u2013 galaxies: nuclei \u2013 quasars: general \u2013 surveys \u2013 X-rays: general",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 2; revised 2016 November 18; accepted 2016 December 7; published 2017 February 10. \n\nThe authors first thank the anonymous referee for the constructive comments. We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A.), and ST/J003697/2 (P.G.); a Herchel Smith Postdoctoral Fellowship of the University of Cambridge (G.B.L.); the ERC Advanced Grant FEEDBACK 340442 at the University of Cambridge (J.A.); a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University (J.A.); the Leverhulme Trust (D.M.A.); CONICYT-Chile grants FONDECYT 1120061 and 1160999 (E.T.), 3140534 (S.S.), and Anillo ACT1101 (E.T. and F.E.B.); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06; E.T. and F.E.B.); and the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.). We extend gratitude to Felipe Ardila, Roberto Assef, Eduardo Ba\u00f1ados, Stanislav George Djorgovski, Andrew Drake, Jack Gabel, Audrey Galametz, Daniel Gawerc, David Girou, Marianne Heida, Nikita Kamraj, Peter Kosec, Thomas Kr\u00fchler, Ashish Mahabal, Alessandro Rettura, and Aaron Stemo for their support during the ground-based follow-up observations. We thank John Lucey for unearthing the J1410 spectrum, and Sophie Reed, David Rosario, Mara Salvato, and Martin Ward for the informative discussions. Additional thanks to Eden Stern for lending a hand during the 2015 August Keck run. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: Chandra, ESO La Silla, Gemini, Keck, Magellan, NuSTAR, Palomar, SDSS, Swift, WISE, XMM-Newton.\n\nPublished - Lansbury_2017_ApJ_836_99.pdf
Submitted - 1612.06389.pdf
",
"abstract": "We present the first full catalog and science results for the Nuclear Spectroscopic Telescope Array (NuSTAR) serendipitous survey. The catalog incorporates data taken during the first 40 months of NuSTAR operation, which provide \u224820 Ms of effective exposure time over 331 fields, with an areal coverage of 13 deg^2, and 497 sources detected in total over the 3\u201324 keV energy range. There are 276 sources with spectroscopic redshifts and classifications, largely resulting from our extensive campaign of ground-based spectroscopic follow-up. We characterize the overall sample in terms of the X-ray, optical, and infrared source properties. The sample is primarily composed of active galactic nuclei (AGNs), detected over a large range in redshift from z = 0.002 to 3.4 (median of \u3008z\u3009= 0.56), but also includes 16 spectroscopically confirmed Galactic sources. There is a large range in X-ray flux, from log(f_(3-24 keV)/erg s^(-1) cm^(-2) \u2248 -14 to \u221211, and in rest-frame 10\u201340 keV luminosity, from log(L_(10-40 keV)/erg s^(-1) \u2248 39 to 46, with a median of 44.1. Approximately 79% of the NuSTAR sources have lower-energy (<10 keV) X-ray counterparts from XMM-Newton, Chandra, and Swift XRT. The mid-infrared (MIR) analysis, using WISE all-sky survey data, shows that MIR AGN color selections miss a large fraction of the NuSTAR-selected AGN population, from \u224815% at the highest luminosities (L_X > 10^(44) erg s^(\u22121)) to \u224880% at the lowest luminosities (L_X > 10^(43) erg s^(\u22121)). Our optical spectroscopic analysis finds that the observed fraction of optically obscured AGNs (i.e., the type 2 fraction) is F_(Type 2) = 53^(+14)_(-15)%, for a well-defined subset of the 8\u201324 keV selected sample. This is higher, albeit at a low significance level, than the type 2 fraction measured for redshift- and luminosity-matched AGNs selected by <10 keV X-ray missions.",
"date": "2017-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 99",
"id_number": "CaltechAUTHORS:20170214-093358892",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170214-093358892",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "University of Cambridge"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Durham University"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1160999"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "3140534"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Center of Excellence in Astrophysics and Associated Technologies",
"grant_number": "PFB 06"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/836/1/99",
"primary_object": {
"basename": "Lansbury_2017_ApJ_836_99.pdf",
"url": "https://authors.library.caltech.edu/records/harj1-hyn54/files/Lansbury_2017_ApJ_836_99.pdf"
},
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{
"basename": "1612.06389.pdf",
"url": "https://authors.library.caltech.edu/records/harj1-hyn54/files/1612.06389.pdf"
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],
"pub_year": "2017",
"author_list": "Lansbury, G. B.; Harrison, F. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/632g1-ha040",
"eprint_id": 74094,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:28:42",
"lastmod": "2023-10-24 22:05:18",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Zoghbi-A",
"name": {
"family": "Zoghbi",
"given": "Abderahmen"
},
"orcid": "0000-0002-0572-9613"
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J. A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M. J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A Long Look at MCG-5-23-16 with NuSTAR. I. Relativistic Reflection and Coronal Properties",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 galaxies: active \u2013 galaxies: individual (MCG-5-23-16) \u2013 galaxies: Seyfert",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 22; revised 2017 January 3; accepted 2017 January 6; published 2017 February 3. \n\nWe thank the referee, A. Zdziarski, for the useful comments and suggestions that helped with the interpretation of the data. This work has been partly supported by NASA grant NNX14AF89G. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Zoghbi_2017_ApJ_836_2.pdf
Submitted - 1701.02309.pdf
",
"abstract": "MCG-5-23-16 was targeted in early 2015 with a half mega-second observing campaign using NuSTAR. Here we present the spectral analysis of these data sets along with an earlier observation and study the relativistic reflection and the primary coronal source. The data show strong reflection features in the form of both narrow and broad iron lines plus a Compton reflection hump. A cutoff energy is significantly detected in all exposures. The shape of the reflection spectrum does not change in the two years spanned by the observations, suggesting a stable geometry. A strong positive correlation is found between the cutoff energy and both the hard X-ray flux and spectral index. The measurements imply that the coronal plasma is not at the runaway electron\u2013positron pair limit, and instead contains mostly electrons. The observed variability in the coronal properties is driven by a variable optical depth. A constant heating-to-cooling ratio is measured, implying that there is a feedback mechanism in which a significant fraction of the photons cooling the corona are due to reprocessed hard X-rays.",
"date": "2017-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 2",
"id_number": "CaltechAUTHORS:20170206-142411468",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170206-142411468",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX14AF89G"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"collection": "CaltechAUTHORS",
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory",
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"pub_year": "2017",
"author_list": "Zoghbi, Abderahmen; Matt, G.; et el."
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"id": "Ludlam-R-M",
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"title": "A Hard Look at the Neutron Stars and Accretion Disks in 4U 1636-53, GX 17+2, and 4U 1705-44 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: neutron \u2013 X-rays: binaries \u2013 X-rays: individual (4U 1636-53, GX 17\n+2, 4U 1705-44)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 August 5; revised 2017 January 4; accepted 2017 January 6; published 2017 February 14. \n\nThis research has made use of the NuSTAR. Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). J.M.M. gratefully acknowledges support through the NuSTAR guest observer program. N.D. is supported via an NWO Vidi grant and an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE- 2013-IEF-627148. E.M.C. gratefully acknowledges support from the National Science Foundation through CAREER award number AST-1351222.\n\nSubmitted - 1701.01774v1.pdf
",
"abstract": "We present NuSTAR observations of neutron star (NS) low-mass X-ray binaries: 4U 1636-53, GX 17+2, and 4U 1705-44. We observed 4U 1636-53 in the hard state, with an Eddington fraction, F_(Edd), of 0.01; GX 17+2 and 4U 1705-44 were in the soft state with fractions of 0.57 and 0.10, respectively. Each spectrum shows evidence for a relativistically broadened Fe K \u03b1 line. Through accretion disk reflection modeling, we constrain the radius of the inner disk in 4U 1636-53 to be R_(in) = 1.03 \u00b1 0.03 ISCO (innermost stable circular orbit), assuming a dimensionless spin parameter a* = cJ/GM^2 = 0.0, and R_(in) = 1.08 \u00b1 0.06 ISCO for a* = 0.3 (errors quoted at 1\u03c3). This value proves to be model independent. For a* = 0.3 and M = 1.4 M\u2299, for example, 1.08 \u00b1 0.06 ISCO translates to a physical radius of R = 10.8 \u00b1 0.6 km, and the NS would have to be smaller than this radius (other outcomes are possible for allowed spin parameters and masses). For GX 17+2, R_(in) = 1.00-1.04 ISCO for a* = 0.0 and R_(in) = 1.03-1.30 ISCO for a* = 0.3. For a* = 0.3 and M = 1.4 M\u2299, R_(in) = 1.03-1.30 ISCO translates to R = 10.3-13.0 km. The inner accretion disk in 4U 1705-44 may be truncated just above the stellar surface, perhaps by a boundary layer or magnetosphere; reflection models give a radius of 1.46\u20131.64 ISCO for a* = 0.0 and 1.69\u20131.93 ISCO for a* = 0.3. We discuss the implications our results may have on the equation of state of ultradense, cold matter and our understanding of the innermost accretion flow onto NSs with low surface magnetic fields, and systematic errors related to the reflection models and spacetime metric around less idealized NSs.",
"date": "2017-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "836",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 140",
"id_number": "CaltechAUTHORS:20170111-113848710",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170111-113848710",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"doi": "10.3847/1538-4357/836/1/140",
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"author_list": "Ludlam, R. M.; Miller, J. M.; et el."
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"items": [
{
"id": "Margutti-Raffaella",
"name": {
"family": "Margutti",
"given": "Raffaella"
},
"orcid": "0000-0003-4768-7586"
},
{
"id": "Kamble-Atish",
"name": {
"family": "Kamble",
"given": "A."
},
"orcid": "0000-0003-0861-5168"
},
{
"id": "Milisavljevic-Dan",
"name": {
"family": "Milisavljevic",
"given": "D."
},
"orcid": "0000-0002-0763-3885"
},
{
"id": "Zapartas-Emmanouil",
"name": {
"family": "Zapartas",
"given": "E."
}
},
{
"id": "de-Mink-Selma-E",
"name": {
"family": "de Mink",
"given": "S.E."
},
"orcid": "0000-0001-9336-2825"
},
{
"id": "Drout-Maria-R",
"name": {
"family": "Drout",
"given": "M."
},
"orcid": "0000-0001-7081-0082"
},
{
"id": "Chornock-Ryan",
"name": {
"family": "Chornock",
"given": "R."
},
"orcid": "0000-0002-7706-5668"
},
{
"id": "Risaliti-Guido",
"name": {
"family": "Risaliti",
"given": "G."
}
},
{
"id": "Zauderer-B-Ashley",
"name": {
"family": "Zauderer",
"given": "B. A."
},
"orcid": "0000-0003-1152-518X"
},
{
"id": "Bietenholz-Michael-F",
"name": {
"family": "Bietenholz",
"given": "M."
},
"orcid": "0000-0002-0592-4152"
},
{
"id": "Cantiello-Matteo",
"name": {
"family": "Cantiello",
"given": "M."
},
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"id": "Chakraborti-Sankhamala",
"name": {
"family": "Chakraborti",
"given": "S."
}
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"id": "Chomiuk-Laura",
"name": {
"family": "Chomiuk",
"given": "L."
},
"orcid": "0000-0002-8400-3705"
},
{
"id": "Fong-Wen-Fai",
"name": {
"family": "Fong",
"given": "W."
},
"orcid": "0000-0002-7374-935X"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Guidorzi-Cristiano",
"name": {
"family": "Guidorzi",
"given": "C."
},
"orcid": "0000-0001-6869-0835"
},
{
"id": "Kirshner-Robert-P",
"name": {
"family": "Kirshner",
"given": "R. P."
},
"orcid": "0000-0002-1966-3942"
},
{
"id": "Parrent-Jerod-T",
"name": {
"family": "Parrent",
"given": "J. T."
}
},
{
"id": "Patnaude-D",
"name": {
"family": "Patnaude",
"given": "D."
}
},
{
"id": "Soderberg-Alicia-M",
"name": {
"family": "Soderberg",
"given": "A. M."
}
},
{
"id": "Gehrels-Neil",
"name": {
"family": "Gehrels",
"given": "N. C."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
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"orcid": "0000-0003-2992-8024"
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},
"title": "Ejection of the massive Hydrogen-rich envelope timed with the collapse of the stripped SN2014C",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "supernovae: individual (SN 2014C)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 January 20; revised 2016 December 18; accepted 2016 December 20; published 2017 January 24. \n\nWe are indebted to David Arnett, Chris Kochanek, Ori Fox, Avishy Gal-Yam, Chris Matzner, Maryam Modjaz, Andrea Pastorello, Jeff Silverman, Nathan Smith, Kris Stanek, and Noam Soker for their insightful comments and suggestions. \n\nR.M. acknowledges generous support from the James Arthur Fellowship at NYU. S.d.M. acknowledges support by a Marie Sklodowska-Curie Reintegration Fellowship (H2020 MSCA-IF-2014, project id 661502). M.Z. acknowledges support by the Netherlands Research School for Astronomy (NOVA). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory under programs GO 15500831 and DDT 15508491. This work was partially supported under NASA No. NNX15AV38G, and made use of data from the Nuclear Spectroscopic Array (NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This work was supported in part by National Science Foundation Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. We thank the Chandra, NuSTAR, and Swift teams for support with the execution of the observations.\n\nPublished - Margutti_2017_ApJ_835_140.pdf
Accepted Version - nihms860580.pdf
Submitted - 1601.06806v1.pdf
",
"abstract": "We present multi-wavelength observations of SN 2014C during the first 500 days. These observations represent the first solid detection of a young extragalactic stripped-envelope SN out to high-energy X-rays ~40 keV. SN 2014C shows ordinary explosion parameters (Ek ~ 1.8 \u00d7 10\u2075\u00b9 erg and M_(ej) ~ 1.7 M_\u2299). However, over an ~1 year timescale, SN 2014C evolved from an ordinary hydrogen-poor supernova into a strongly interacting, hydrogen-rich supernova, violating the traditional classification scheme of type-I versus type-II SNe. Signatures of the SN shock interaction with a dense medium are observed across the spectrum, from radio to hard X-rays, and revealed the presence of a massive shell of ~1 M_\u2299 of hydrogen-rich material at ~6 \u00d7 10\u00b9\u2076) cm. The shell was ejected by the progenitor star in the decades to centuries before collapse. This result challenges current theories of massive star evolution, as it requires a physical mechanism responsible for the ejection of the deepest hydrogen layer of H-poor SN progenitors synchronized with the onset of stellar collapse. Theoretical investigations point at binary interactions and/or instabilities during the last nuclear burning stages as potential triggers of the highly time-dependent mass loss. We constrain these scenarios utilizing the sample of 183 SNe Ib/c with public radio observations. Our analysis identifies SN 2014C-like signatures in ~10% of SNe. This fraction is reasonably consistent with the expectation from the theory of recent envelope ejection due to binary evolution if the ejected material can survive in the close environment for 10\u00b3\u201310\u2074 years. Alternatively, nuclear burning instabilities extending to core C-burning might play a critical role.",
"date": "2017-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "835",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 140",
"id_number": "CaltechAUTHORS:20160127-094616076",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160127-094616076",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "James Arthur Fellowship"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "H2020-MSCA-IF-2014"
},
{
"agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)"
},
{
"agency": "NASA",
"grant_number": "NNX15AV38G"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NSF",
"grant_number": "PHYS-1066293"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-24",
"name": "Space Radiation Laboratory"
}
]
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"doi": "10.3847/1538-4357/835/2/140",
"pmcid": "PMC5495200",
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"pub_year": "2017",
"author_list": "Margutti, Raffaella; Kamble, A.; et el."
},
{
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"eprint_status": "archive",
"datestamp": "2023-08-19 01:22:42",
"lastmod": "2023-10-25 15:09:34",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "Ashley L."
}
},
{
"id": "Lohfink-A",
"name": {
"family": "Lohfink",
"given": "Anne"
}
},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "Erin"
},
"orcid": "0000-0003-0172-0854"
}
]
},
"title": "AGN Coronae through a Jet Perspective",
"ispublished": "pub",
"full_text_status": "restricted",
"note": "\u00a9 2017. The American Astronomical Society. \n\nThe authors would like to thank the anonymous referee for\ninsightful and helpful comments. The authors would also like\nto thank Dan Wilkins for productive discussions regarding this\nmanuscript. A.L.K. would like to thank the support provided\nby NASA through Einstein Postdoctoral Fellowship grant\nnumber PF4-150125 awarded by the Chandra X-ray Center,\noperated by the Smithsonian Astrophysical Observatory for\nNASA under contract NAS8-03060. A.L. acknowledges\nsupport from the ERC Advanced Grant FEEDBACK. E.K.\nwould like to thank the Hubble Fellowship program. Support\nfor program number HST-HF2-51360.001-A was provided by\nNASA through a Hubble Fellowship grant from the Space\nTelescope Science Institute, which is operated by the Association\nof Universities for Research in Astronomy, Incorporated,\nunder NASA contract NAS5-26555.",
"abstract": "This paper presents an in-depth look at the jet and coronal properties of 41 active galactic nuclei (AGNs). Utilizing the highest quality NuSTAR, XMM-Newton, and NRAO VLA Sky Survey 1.4 GHz data, we find that the radio Eddington luminosity inversely scales with X-ray reflection fraction, and positively scales with the distance between the corona and the reflected regions in the disk. We next investigate a model fit to the data that predicts the corona is outflowing and propagates into the large-scale jet. We find this model describes the data well and predicts that the corona has mildly relativistic velocities, 0.04< \u03b2 < 0.40. We discuss our results in the context of disk\u2013jet connections in AGNs.",
"date": "2017-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "835",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 226",
"id_number": "CaltechAUTHORS:20170331-102733529",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-102733529",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
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}
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"doi": "10.3847/1538-4357/835/2/226",
"pub_year": "2017",
"author_list": "King, Ashley L.; Lohfink, Anne; et el."
},
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"eprint_id": 75577,
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"datestamp": "2023-08-22 19:40:33",
"lastmod": "2023-10-25 15:09:27",
"type": "article",
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"creators": {
"items": [
{
"id": "Oda-Saeko",
"name": {
"family": "Oda",
"given": "Saeko"
}
},
{
"id": "Tanimoto-Atsushi",
"name": {
"family": "Tanimoto",
"given": "Atsushi"
},
"orcid": "0000-0002-0114-5581"
},
{
"id": "Ueda-Yoshihiro",
"name": {
"family": "Ueda",
"given": "Yoshihiro"
},
"orcid": "0000-0001-7821-6715"
},
{
"id": "Imanishi-Masatoshi",
"name": {
"family": "Imanishi",
"given": "Masatoshi"
},
"orcid": "0000-0001-6186-8792"
},
{
"id": "Terashima-Yuichi",
"name": {
"family": "Terashima",
"given": "Yuichi"
},
"orcid": "0000-0003-1780-5481"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
}
]
},
"title": "Shedding Light on the Compton-thick Active Galactic Nucleus in the Ultraluminous Infrared Galaxy UGC 5101 with Broadband X-Ray Spectroscopy",
"ispublished": "pub",
"full_text_status": "restricted",
"keywords": "galaxies: active; galaxies: individual (UGC 5101); X-rays: galaxies",
"note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 September 28; revised 2016 December 10; accepted 2016 December 18; published 2017 January 30. \n\nThis research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy, and the California Institute of Technology [Caltech], USA). Part of this work was financially supported by the Grant-in-Aid for Scientific Research 26400228 (Y.U.), 15K05030 (M.I.), and 15H02070 (Y.T.) from the Japan Society for the Promotion of Science (JSPS), and by the CONICYT-Chile grants \"EMBIGGEN\" Anillo ACT1101 (C.R.), FONDECYT 1141218 (C.R.), and Basal-CATA PFB\u201306/2007 (C.R.). C.R. acknowledges support from the China-CONICYT fund.",
"abstract": "We report the broadband X-ray spectra of the ultraluminous infrared galaxy (ULIRG) UGC 5101 in the 0.25\u2013100 keV band observed with the Swift/Burst Alert Telescope (BAT), Nuclear Spectroscopic Telescope Array (NuSTAR), Suzaku, XMM-Newton, and Chandra. A Compton-thick active galactic nucleus (AGN) obscured with a hydrogen column density of \u2248 1.3 \u00d7 10^(24) cm^(-2) is detected above 10 keV. A spectral fit with a numerical torus model favors a large half-opening angle of the torus, > 41\u00b0, suggesting that the covering fraction of material heavily obscuring the X-ray source is moderate. The intrinsic 2\u201310 keV luminosity is determined to be \u2248 1.4\u00d7 10^(43) erg s^(\u20111), which is \u2248 2.5 times larger than the previous estimate using only data below 10 keV with a simple spectral model. We find that UGC 5101 shows the ratio between the [O iv] 26 \u03bcm line and 2\u201310 keV luminosities similar to those of normal Seyfert galaxies, along with other ULIRGs observed with NuSTAR, indicating that a significant portion of local ULIRGs are not really \"X-ray faint\" with respect to the flux of forbidden lines originating from the narrow-line region. We propose a possible scenario that (1) the AGN in UGC 5101 is surrounded not only by Compton-thick matter located close to the equatorial plane but also by Compton-thin (N_H \u223c 10^(21) cm^(\u20112)) matter in the torus-hole region and (2) it is accreting at a high Eddington rate with a steep UV to X-ray spectral energy distribution. Nevertheless, we argue that AGNs in many ULIRGs do not look extraordinary (i.e., extremely X-ray faint), as suggested by recent works, compared with normal Seyferts.",
"date": "2017-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "835",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. no. 179",
"id_number": "CaltechAUTHORS:20170331-102221840",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-102221840",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "26400228"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "15K05030"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "15H02070"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB\u201306/2007"
},
{
"agency": "China-CONICYT fund"
}
]
},
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"doi": "10.3847/1538-4357/835/2/179",
"pub_year": "2017",
"author_list": "Oda, Saeko; Tanimoto, Atsushi; et el."
},
{
"id": "https://authors.library.caltech.edu/records/0z0s7-e1219",
"eprint_id": 75369,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:17:05",
"lastmod": "2023-10-25 14:59:29",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kammoun-E-S",
"name": {
"family": "Kammoun",
"given": "E. S."
}
},
{
"id": "Risaliti-G",
"name": {
"family": "Risaliti",
"given": "G."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Jun-Hyunsung-David",
"name": {
"family": "Jun",
"given": "H. D."
},
"orcid": "0000-0003-1470-5901"
},
{
"id": "Graham-M",
"name": {
"family": "Graham",
"given": "M."
}
},
{
"id": "Celotti-A",
"name": {
"family": "Celotti",
"given": "A."
}
},
{
"id": "Behar-E",
"name": {
"family": "Behar",
"given": "E."
}
},
{
"id": "Elvis-M",
"name": {
"family": "Elvis",
"given": "M."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Coronal properties of the luminous radio-quiet quasar QSO B2202\u2013209",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active, galaxies: nuclei, quasars: individual: QSO B2202\u2013209, X-rays: galaxies",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nReceived: 23 July 2016. Revision Received: 05 November 2016. Accepted: 07 November 2016. Published: 10 November 2016. \n\nThis research made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA, XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and the Hale Telescope at Palomar Observatory. This research has made use of the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We like to acknowledge S.G. Djorgovski for providing the Palomar observations. We thank the anonymous referee for comments and suggestions, which significantly contributed to improving the quality of the manuscript. EB received funding from the European Union Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement no. 655324. \n\nFacilities: NuSTAR, Palomar: DBSP, XMM\u2013Newton.\n\nPublished - stw2897.pdf
Submitted - 1611.02306.pdf
",
"abstract": "We present an analysis of the joint XMM\u2013Newton and NuSTAR observations of the radio-quiet quasar QSO B2202\u2013209. Using an optical observation from the Hale Telescope at the Palomar Observatory, we revise the redshift of the source from the previously reported z = 1.77 to z = 0.532, and we estimate the mass of the central black hole, log\u2009(M_(BH)/M_\u2299) = 9.08 \u00b1 0.18. The X-ray spectrum of this source can be well described by a power law of photon index \u0393 = 1.82 \u00b1 0.05 with \nE_(cut) = 152^(+103)_(\u221254) keV, in the rest frame of the source. Assuming a Comptonization model, we estimate the coronal temperature to be kT_e = 42 \u00b1 3\u2009keV and kT_e = 56 \u00b1 3\u2009keV for a spherical and a slab geometry, respectively. The coronal properties are comparable to the ones derived for local active galactic nuclei, despite a difference of around one order of magnitude in black hole mass and X-ray luminosity (L_(2 \u2212 10) = 1.93 \u00d7 10^(45)\u2009erg\u2009s^(\u22121)). The quasar is X-ray loud, with an unusually flat observed optical-to-X-ray spectral slope \u03b1_(OX) = 1.00 \u00b1 0.02, and has an exceptionally strong optical [O\u2009iii] line. Assuming that both the X-ray emission and the [O\u2009iii] line are isotropic, these two extreme properties can be explained by a nearly edge-on disc, leading to a reduction in the observed ultraviolet continuum light.",
"date": "2017-02",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "465",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1665-1671",
"id_number": "CaltechAUTHORS:20170324-073204061",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170324-073204061",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "Hale Telescope at Palomar Observatory"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "655324"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1093/mnras/stw2897",
"primary_object": {
"basename": "1611.02306.pdf",
"url": "https://authors.library.caltech.edu/records/0z0s7-e1219/files/1611.02306.pdf"
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{
"basename": "stw2897.pdf",
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}
],
"pub_year": "2017",
"author_list": "Kammoun, E. S.; Risaliti, G.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/8eyfa-jbx23",
"eprint_id": 70919,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:09:35",
"lastmod": "2023-10-23 15:07:44",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ingram-A",
"name": {
"family": "Ingram",
"given": "Adam"
},
"orcid": "0000-0002-5311-9078"
},
{
"id": "van-der-Klis-M",
"name": {
"family": "van der Klis",
"given": "Michiel"
},
"orcid": "0000-0003-0070-9872"
},
{
"id": "Middleton-M",
"name": {
"family": "Middleton",
"given": "Matthew"
}
},
{
"id": "Altamirano-D",
"name": {
"family": "Altamirano",
"given": "Diego"
},
"orcid": "0000-0002-3422-0074"
},
{
"id": "Uttley-P",
"name": {
"family": "Uttley",
"given": "Phil"
}
}
]
},
"title": "Tomographic reflection modelling of quasi-periodic oscillations in the black hole binary H 1743-322",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs, black hole physics, X-rays: individual: H 1743\u2212322",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 October 6. Received 2016 October 4; in original form 2016 July 29; Editorial Decision 2016 October 4. Published: 08 October 2016.\n\nAccepted Version - 1610.00948v1.pdf
",
"abstract": "Accreting stellar mass black holes (BHs) routinely exhibit Type-C quasi-periodic oscillations (QPOs). These are often interpreted as Lense\u2013Thirring precession of the inner accretion flow, a relativistic effect whereby the spin of the BH distorts the surrounding space\u2013time, inducing nodal precession. The best evidence for the precession model is the recent discovery, using a long joint XMM\u2013Newton and NuSTAR observation of H 1743\u2212322, that the centroid energy of the iron florescence line changes systematically with QPO phase. This was interpreted as the inner flow illuminating different azimuths of the accretion disc as it precesses, giving rise to a blueshifted/redshifted iron line when the approaching/receding disc material is illuminated. Here, we develop a physical model for this interpretation, including a self-consistent reflection continuum, and fit this to the same H 1743\u2212322 data. We use an analytic function to parametrize the asymmetric illumination pattern on the disc surface that would result from inner flow precession, and find that the data are well described if two bright patches rotate about the disc surface. This model is preferred to alternatives considering an oscillating disc ionization parameter, disc inner radius and radial emissivity profile. We find that the reflection fraction varies with QPO phase (3.5\u03c3), adding to the now formidable body of evidence that Type-C QPOs are a geometric effect. This is the first example of tomographic QPO modelling, initiating a powerful new technique that utilizes QPOs in order to map the dynamics of accreting material close to the BH.",
"date": "2017-01-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "464",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2979-2991",
"id_number": "CaltechAUTHORS:20161006-121429546",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161006-121429546",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw2581",
"primary_object": {
"basename": "1610.00948v1.pdf",
"url": "https://authors.library.caltech.edu/records/8eyfa-jbx23/files/1610.00948v1.pdf"
},
"pub_year": "2017",
"author_list": "Ingram, Adam; van der Klis, Michiel; et el."
},
{
"id": "https://authors.library.caltech.edu/records/5ab7d-18246",
"eprint_id": 73826,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:08:39",
"lastmod": "2023-10-24 16:30:19",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "NuSTAR Observations of WISE J1036+0449, a Galaxy at z ~ 1 Obscured by Hot Dust",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "infrared: galaxies \u2013 galaxies: active \u2013 galaxies: evolution \u2013 galaxies: high-redshift \u2013 quasars: general \u2013 quasars: individual (WISE J1036+0449)",
"note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 3; revised 2016 October 27; accepted 2016 November 10; published 2017 January 20. \n\nWe thank the referee for a very prompt report that helped to improve the article. This work makes use of data products from the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology (Caltech). WISE is funded by the National Aeronautics and Space Administration (NASA). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership between Caltech, the University of California, and NASA. Use of the observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work makes use of data from the NuSTAR mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for their support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software, jointly developed by the ASI Science Data Center (Italy) and Caltech. This work has made use of the NASA/IPAC Infrared Science Archive and NASA/IPAC Extragalactic Database, which are operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. This material is based upon work supported by NASA under Proposal No. 13-ADAP13-0092, issued through the Astrophysics Data Analysis Program. We thank M. Karouzos and C.S. Chang for their comments on the manuscript. We acknowledge financial support from CONICYT-Chile grants \"EMBIGGEN\" Anillo ACT1101 (C.R., E.T., F.E.B.); FONDECYT 1141218 (C.R., F.E.B.), 3140436 (R.N.), and 1151408 (R.A.); and Basal-CATA PFB\u201306/2007 (C.R., F.E.B., E.T.) and from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics (F.E.B.). C.R. acknowledges support from the China-CONICYT fund. P.G. thanks the STFC for their support [grant reference ST/J003697/2], and W.N.B. acknowledges financial support from NuSTAR subcontract 44A\u20131092750. P.B. is supported by an STFC studentship. A.C. acknowledges support from ASI/INAF grant I/037/12/0011/13 and the Caltech Kingsley visitor program. T.D.-S. acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT 1151239. S.M.L. is supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by the Universities Space Research Association under contract with NASA. \n\nFacilities: Chandra - , NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, XMM-Newton - Newton X-Ray Multimirror Mission satellite, WISE - Wide-field Infrared Survey Explorer, Keck\n\nPublished - Ricci_2017_ApJ_835_105.pdf
Submitted - 1609.04808v2.pdf
",
"abstract": "Hot dust-obscured galaxies (hot DOGs), selected from Wide-Field Infrared Survey Explorer's all-sky infrared survey, host some of the most powerful active galactic nuclei known and may represent an important stage in the evolution of galaxies. Most known hot DOGs are located at z > 1.5, due in part to a strong bias against identifying them at lower redshift related to the selection criteria. We present a new selection method that identifies 153 hot DOG candidates at z ~ 1, where they are significantly brighter and easier to study. We validate this approach by measuring a redshift z = 1.009 and finding a spectral energy distribution similar to that of higher-redshift hot DOGs for one of these objects, WISE J1036+0449 (L_(Bol \u2243 8 x 10^(46) erg s^(-1)). We find evidence of a broadened component in Mg II, which would imply a black hole mass of M_(BH) \u2243 2 x 10^8 M\u2299 and an Eddington ratio of \u03bb_(Edd) \u2243 2.7. WISE J1036+0449 is the first hot DOG detected by the Nuclear Spectroscopic Telescope Array, and observations show that the source is heavily obscured, with a column density of N_H \u2243 (2-15) x 10^(23) cm^(-2). The source has an intrinsic 2\u201310 keV luminosity of ~6 x 10^(44) erg s^(-1), a value significantly lower than that expected from the mid-infrared/X-ray correlation. We also find that other hot DOGs observed by X-ray facilities show a similar deficiency of X-ray flux. We discuss the origin of the X-ray weakness and the absorption properties of hot DOGs. Hot DOGs at z \u227e 1 could be excellent laboratories to probe the characteristics of the accretion flow and of the X-ray emitting plasma at extreme values of the Eddington ratio.",
"date": "2017-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "835",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 105",
"id_number": "CaltechAUTHORS:20170130-141550926",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170130-141550926",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "W. M. Keck Foundation"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "13-ADAP13-0092"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "3140436"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1151408"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "NuSTAR",
"grant_number": "44A-1092750"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0011/13"
},
{
"agency": "Caltech Kingsley Visitor Program"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "31130005"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1151239"
},
{
"agency": "NASA Postdoctoral Program"
}
]
},
"collection": "CaltechAUTHORS",
"local_group": {
"items": [
{
"id": "NuSTAR",
"value": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory",
"value": "Space Radiation Laboratory"
},
{
"id": "Astronomy-Department",
"value": "Astronomy Department"
}
]
},
"doi": "10.3847/1538-4357/835/1/105",
"primary_object": {
"basename": "1609.04808v2.pdf",
"url": "https://authors.library.caltech.edu/records/5ab7d-18246/files/1609.04808v2.pdf"
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"basename": "Ricci_2017_ApJ_835_105.pdf",
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}
],
"pub_year": "2017",
"author_list": "Ricci, C.; Brightman, M.; et el."
},
{
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"eprint_id": 73571,
"eprint_status": "archive",
"datestamp": "2023-08-22 19:33:35",
"lastmod": "2023-10-24 15:29:10",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kuhar-M",
"name": {
"family": "Kuhar",
"given": "Matej"
},
"orcid": "0000-0002-7210-180X"
},
{
"id": "Krucker-S",
"name": {
"family": "Krucker",
"given": "S\u00e4m"
}
},
{
"id": "Hannah-I-G",
"name": {
"family": "Hannah",
"given": "Iain G."
},
"orcid": "0000-0003-1193-8603"
},
{
"id": "Glesener-L",
"name": {
"family": "Glesener",
"given": "Lindsay"
},
"orcid": "0000-0001-7092-2703"
},
{
"id": "Saint-Hilaire-P",
"name": {
"family": "Saint-Hilaire",
"given": "Pascal"
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hudson-H-S",
"name": {
"family": "Hudson",
"given": "Hugh S."
},
"orcid": "0000-0001-5685-1283"
},
{
"id": "White-S-M",
"name": {
"family": "White",
"given": "Stephen M."
},
"orcid": "0000-0002-8574-8629"
},
{
"id": "Smith-D-M",
"name": {
"family": "Smith",
"given": "David M."
},
"orcid": "0000-0002-0542-5759"
},
{
"id": "Marsh-A-J",
"name": {
"family": "Marsh",
"given": "Andrew J."
},
"orcid": "0000-0003-1086-6900"
},
{
"id": "Wright-P-J",
"name": {
"family": "Wright",
"given": "Paul J."
},
"orcid": "0000-0001-9021-611X"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Evidence of Significant Energy Input in the Late Phase of a Solar Flare from NuSTAR X-Ray Observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays",
"note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 October 20. Accepted 2016 November 30. Published 2017 January 16. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). M.K. and S.K. acknowledge funding from the Swiss National Science Foundation (200021-140308). Funding for this work was also provided under NASA grants NNX12AJ36G and NNX14AG07G. A.J.M.'s participation was supported by NASA Earth and Space Science Fellowship award NNX13AM41H. I.G.H. is supported by a Royal Society University Research Fellowship. P.J.W. is supported by an EPSRC-Royal Society fellowship engagement grant. FOXSI was funded by NASA LCAS grant NNX11AB75G. We would also like to thank the anonymous referee for the helpful comments.\n\nPublished - Kuhar_2017_ApJ_835_6.pdf
",
"abstract": "We present observations of the occulted active region AR 12222 during the third Nuclear Spectroscopic Telescope ARray (NuSTAR) solar campaign on 2014 December 11, with concurrent Solar Dynamics Observatory (SDO)/AIA and FOXSI-2 sounding rocket observations. The active region produced a medium-size solar flare 1 day before the observations, at ~18 UT on 2014 December 10, with the post-flare loops still visible at the time of NuSTAR observations. The time evolution of the source emission in the SDO/AIA 335 \u00c5 channel reveals the characteristics of an extreme-ultraviolet late-phase event, caused by the continuous formation of new post-flare loops that arch higher and higher in the solar corona. The spectral fitting of NuSTAR observations yields an isothermal source, with temperature 3.8\u20134.6 MK, emission measure (0.3\u20131.8) \u00d7 10^(46) cm^(\u22123), and density estimated at (2.5\u20136.0) \u00d7 10^8 cm^(\u22123). The observed AIA fluxes are consistent with the derived NuSTAR temperature range, favoring temperature values in the range of 4.0\u20134.3 MK. By examining the post-flare loops' cooling times and energy content, we estimate that at least 12 sets of post-flare loops were formed and subsequently cooled between the onset of the flare and NuSTAR observations, with their total thermal energy content an order of magnitude larger than the energy content at flare peak time. This indicates that the standard approach of using only the flare peak time to derive the total thermal energy content of a flare can lead to a large underestimation of its value.",
"date": "2017-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "835",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 6",
"id_number": "CaltechAUTHORS:20170120-102600412",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170120-102600412",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "200021-140308"
},
{
"agency": "NASA",
"grant_number": "NNX12AJ36G"
},
{
"agency": "NASA",
"grant_number": "NNX14AG07G"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX13AM41H"
},
{
"agency": "Royal Society"
},
{
"agency": "Engineering and Physical Sciences Research Council (EPSRC)"
},
{
"agency": "NASA",
"grant_number": "NNX11AB75G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/835/1/6",
"primary_object": {
"basename": "Kuhar_2017_ApJ_835_6.pdf",
"url": "https://authors.library.caltech.edu/records/96zph-x1z84/files/Kuhar_2017_ApJ_835_6.pdf"
},
"pub_year": "2017",
"author_list": "Kuhar, Matej; Krucker, S\u00e4m; et el."
},
{
"id": "https://authors.library.caltech.edu/records/k8991-07z84",
"eprint_id": 71909,
"eprint_status": "archive",
"datestamp": "2023-08-19 01:02:32",
"lastmod": "2023-10-23 17:40:20",
"type": "article",
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"items": [
{
"id": "Plotkin-R-M",
"name": {
"family": "Plotkin",
"given": "R. M."
},
"orcid": "0000-0002-7092-0326"
},
{
"id": "Miller-Jones-J-C-A",
"name": {
"family": "Miller-Jones",
"given": "J. C. A."
},
"orcid": "0000-0003-3124-2814"
},
{
"id": "Gallo-E",
"name": {
"family": "Gallo",
"given": "E."
}
},
{
"id": "Jonker-P-G",
"name": {
"family": "Jonker",
"given": "P. G."
},
"orcid": "0000-0001-5679-0695"
},
{
"id": "Homan-J",
"name": {
"family": "Homan",
"given": "J."
},
"orcid": "0000-0001-8371-2713"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Kaaret-P",
"name": {
"family": "Kaaret",
"given": "P."
},
"orcid": "0000-0002-3638-0637"
},
{
"id": "Russell-D-M",
"name": {
"family": "Russell",
"given": "D. M."
},
"orcid": "0000-0002-3500-631X"
},
{
"id": "Heinz-S",
"name": {
"family": "Heinz",
"given": "S."
},
"orcid": "0000-0002-8433-8652"
},
{
"id": "Hodges-Kluck-E-J",
"name": {
"family": "Hodges-Kluck",
"given": "E. J."
},
"orcid": "0000-0002-2397-206X"
},
{
"id": "Markoff-S",
"name": {
"family": "Markoff",
"given": "S."
},
"orcid": "0000-0001-9564-0876"
},
{
"id": "Sivakoff-G-R",
"name": {
"family": "Sivakoff",
"given": "G. R."
},
"orcid": "0000-0001-6682-916X"
},
{
"id": "Altamirano-D",
"name": {
"family": "Altamirano",
"given": "D."
},
"orcid": "0000-0002-3422-0074"
},
{
"id": "Neilsen-J",
"name": {
"family": "Neilsen",
"given": "J."
},
"orcid": "0000-0002-8247-786X"
}
]
},
"title": "The 2015 Decay of the Black Hole X-ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition into Quiescence",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: black holes \u2013 stars: individual (V404 Cygni) \u2013 X-rays: binaries",
"note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 September 14; revised 2016 October 25; accepted 2016 November 3; published 2017 January 5.\n\nWe thank the anonymous referee for constructive comments that improved this manuscript. We are especially grateful to the Chandra, VLA, and Swift teams for coordinating these observations, particularly Belinda Wilkes and Neil Gehrels for approving the Chandra and Swift observations, and especially Scott Wolk for patiently assisting with multiple iterations of our Chandra observing setup. We also thank Mark Claussen, Gustaaf van Moorsel, and Heidi Medlin for their assistance with the VLA observations. We thank Arash Bahramian for helpful discussions on the X-ray decay timescale that assisted the timing of our trigger, and Thomas Russell for assistance with the radio data reduction. R.M.P. acknowledges support from Curtin University through the Peter Curran Memorial Fellowship. J.C.A.M.-J. is supported by an Australian Research Council Future Fellowship (FT140101082). G.R.S. acknowledges support from NSERC Discovery Grants. D.A. acknowledges support from the Royal Society. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO5-16032A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The scientific results reported in this article are based to a significant degree on observations made by the Chandra X-ray Observatory. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nFacilities: CXO - Chandra X-ray Observatory satellite, NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, VLA. - Very Large Array\n\nSoftware: CIAO (v4.8; Fruscione et al. 2006), HEASOFT, NUSTARDAS (v1.6.0), ISIS (Houck & Denicola 2000), CASA (v4.5; McMullin et al. 2007).\n\nAccepted Version - 1611.02810v1.pdf
",
"abstract": "We present simultaneous X-ray and radio observations of the black hole X-ray binary V404 Cygni at the end of its 2015 outburst. From 2015 July 11\u2013August 5, we monitored V404 Cygni with Chandra, Swift, and NuSTAR in the X-ray, and with the Karl G. Jansky Very Large Array and the Very Long Baseline Array in the radio, spanning a range of luminosities that were poorly covered during its previous outburst in 1989 (our 2015 campaign covers 2 x 10^(33) \u227e L_X \u227e 10^(34) erg s^(-1)). During our 2015 campaign, the X-ray spectrum evolved rapidly from a hard photon index of \u0393 \u2248 1.6 (at L_X \u2248 10^(34) erg s^(-1)) to a softer \u0393 \u2248 2 (at L_X \u2248 3 x 10^(33) erg s^(-1)). We argue that V404 Cygni reaching \u0393 \u2248 2 marks the beginning of the quiescent spectral state, which occurs at a factor of \u22483\u20134 higher X-ray luminosity than the average pre-outburst luminosity of \u22488 x 10^(32) erg s^(-1). V404 Cygni falls along the same radio/X-ray luminosity correlation that it followed during its previous outburst in 1989, implying a robust disk-jet coupling. We exclude the possibility that a synchrotron-cooled jet dominates the X-ray emission in quiescence, leaving synchrotron self-Compton from either a hot accretion flow or from a radiatively cooled jet as the most likely sources of X-ray radiation, and/or particle acceleration along the jet becoming less efficient in quiescence. Finally, we present the first indications of correlated radio and X-ray variability on minute timescales in quiescence, tentatively measuring the radio emission to lag the X-ray by 15 \u00b1 4 minute, suggestive of X-ray variations propagating down a jet with a length of <3.0 au.",
"date": "2017-01-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "834",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 104",
"id_number": "CaltechAUTHORS:20161110-080756178",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161110-080756178",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/834/2/104",
"primary_object": {
"basename": "1611.02810v1.pdf",
"url": "https://authors.library.caltech.edu/records/k8991-07z84/files/1611.02810v1.pdf"
},
"pub_year": "2017",
"author_list": "Plotkin, R. M.; Miller-Jones, J. C. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/34ffb-qzm49",
"eprint_id": 70425,
"eprint_status": "archive",
"datestamp": "2023-08-19 00:56:03",
"lastmod": "2023-10-20 22:57:12",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Wijnands-R",
"name": {
"family": "Wijnands",
"given": "R."
}
},
{
"id": "Altamirano-D",
"name": {
"family": "Altamirano",
"given": "D."
},
"orcid": "0000-0002-3422-0074"
},
{
"id": "Paerels-F",
"name": {
"family": "Paerels",
"given": "F."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "D."
},
"orcid": "0000-0001-8804-8946"
}
]
},
"title": "An in-depth study of a neutron star accreting at low Eddington rate: On the possibility of a truncated disk and an outflow",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 stars: individual: (IGR J17062-6143) \u2013 stars: neutron \u2013 pulsars: general \u2013X-rays: binaries \u2013 X-rays: bursts",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 September 14. Received 2016 September 12; in original form 2016 August 16. Published: 15 September 2016.\n\nND is supported by an NWO Vidi grant and an EU Marie Curie\nIntra-European fellowship (contract no. FP-PEOPLE-2013-IEF-\n627148). ND acknowledges valuable discussions with Anne Lohfink, \nVictor Doroshenko, and Caroline D'Angelo. CP and ACF \nare supported by ERC Advanced Grant Feedback 340442. JMM\nacknowledges support from the Chandra guest observer program. \nDA acknowledges support from the Royal Society. RW is supported \nby an NWO Top grant, module 1. We thank the referee for useful \ncomments. This work is based on data from the NuSTAR mission, \na project led by California Institute of Technology, managed by the \nJet Propulsion Laboratory, and funded by NASA. We thank Neil \nGehrels and the Swift duty scientists for rapid scheduling of observations \nand acknowledge the use of the Swift public data archive.\n\nAccepted Version - 1609.04816v1.pdf
",
"abstract": "Due to observational challenges, our knowledge of low-level accretion flows around neutron stars is limited. We present NuSTAR, Swift and Chandraobservations of the low-mass X-ray binary IGR J17062-6143, which has been persistently accreting at \u22430.1 per cent of the Eddington limit since 2006. Our simultaneous NuSTAR/Swift observations show that the 0.5\u201379 keV spectrum can be described by a combination of a power law with a photon index of \u0393 \u2243 2, a blackbody with a temperature of kT_(bb) \u2243 0.5 keV (presumably arising from the neutron star surface) and disc reflection. Modelling the reflection spectrum suggests that the inner accretion disc was located at R_(in) \u2273 100\u2009GM/c^2 (\u2273225 km) from the neutron star. The apparent truncation may be due to evaporation of the inner disc into a radiatively-inefficient accretion flow, or due to the pressure of the neutron star magnetic field. Our Chandra gratings data reveal possible narrow emission lines near 1 keV that can be modelled as reflection or collisionally ionized gas, and possible low-energy absorption features that could point to the presence of an outflow. We consider a scenario in which this neutron star has been able to sustain its low accretion rate through magnetic inhibition of the accretion flow, which gives some constraints on its magnetic field strength and spin period. In this configuration, IGR J17062-6143 could exhibit a strong radio jet as well as a (propeller-driven) wind-like outflow.",
"date": "2017-01-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "464",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "398-409",
"id_number": "CaltechAUTHORS:20160919-103607188",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160919-103607188",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw2355",
"primary_object": {
"basename": "1609.04816v1.pdf",
"url": "https://authors.library.caltech.edu/records/34ffb-qzm49/files/1609.04816v1.pdf"
},
"pub_year": "2017",
"author_list": "Degenaar, N.; Pinto, C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/z7pqn-3md96",
"eprint_id": 71568,
"eprint_status": "archive",
"datestamp": "2023-08-22 19:28:05",
"lastmod": "2023-10-23 15:55:01",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Huppenkothen-D",
"name": {
"family": "Huppenkothen",
"given": "D."
},
"orcid": "0000-0002-1169-7486"
},
{
"id": "Younes-G",
"name": {
"family": "Younes",
"given": "G."
},
"orcid": "0000-0002-7991-028X"
},
{
"id": "Ingram-A-R",
"name": {
"family": "Ingram",
"given": "A."
},
"orcid": "0000-0002-5311-9078"
},
{
"id": "Kouveliotou-C",
"name": {
"family": "Kouveliotou",
"given": "C."
},
"orcid": "0000-0003-1443-593X"
},
{
"id": "G\u00f6\u011f\u00fc\u015f-E",
"name": {
"family": "G\u00f6\u011f\u00fc\u015f",
"given": "E."
},
"orcid": "0000-0002-5274-6790"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "S\u00e1nchez-Fern\u00e1ndez-C",
"name": {
"family": "S\u00e1nchez-Fern\u00e1ndez",
"given": "C."
}
},
{
"id": "Chenevez-J",
"name": {
"family": "Chenevez",
"given": "J."
},
"orcid": "0000-0002-4397-8370"
},
{
"id": "Motta-S",
"name": {
"family": "Motta",
"given": "S."
}
},
{
"id": "van-der-Klis-M",
"name": {
"family": "van der Klis",
"given": "M."
},
"orcid": "0000-0003-0070-9872"
},
{
"id": "Granot-J",
"name": {
"family": "Granot",
"given": "J."
},
"orcid": "0000-0001-8530-8941"
},
{
"id": "Gehrels-N",
"name": {
"family": "Gehrels",
"given": "N."
}
},
{
"id": "Kuulkers-E",
"name": {
"family": "Kuulkers",
"given": "E."
}
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "Detection of Very Low-frequency, Quasi-periodic Oscillations in the 2015 Outburst of V404 Cygni",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "methods: statistical; relativistic processes; stars: black holes; X-rays: binaries",
"note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 May 12; revised 2016 October 24; accepted 2016 October 26; published 2017 January 4. \n\nWe thank the anonymous referee for very helpful comments and suggestions. We thank Victoria Grinberg for very informative and useful discussions on INTEGRAL calibration and timing with IBIS/ISGRI. D.H. acknowledges support by the Moore-Sloan Data Science Environment at NYU. Partly based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain) and with the participation of Russia and the USA. AI acknowledges support from the Netherlands Organization for Scientific Research (NWO) Veni Fellowship, grant number 639.041.437. M.B. was supported in part by the Sardinian Region, in the framework of the Regional Fundamental Research funds (L.R. 7/2007). J.C. thanks financial support from ESA/PRODEX Nr. 90057.\n\nPublished - Huppenkothen_2017_ApJ_834_90.pdf
Submitted - 1610.08653v1.pdf
",
"abstract": "In 2015 June, the black hole X-ray binary (BHXRB) V404 Cygni went into outburst for the first time since 1989. Here, we present a comprehensive search for quasi-periodic oscillations (QPOs) of V404 Cygni during its recent outburst, utilizing data from six instruments on board five different X-ray missions: Swift/XRT, Fermi/GBM, Chandra/ACIS, INTEGRAL's IBIS/ISGRI and JEM-X, and NuSTAR. We report the detection of a QPO at 18 mHz simultaneously with both Fermi/GBM and Swift/XRT, another example of a rare but slowly growing new class of mHz-QPOs in BHXRBs linked to sources with a high orbital inclination. Additionally, we find a duo of QPOs in a Chandra/ACIS observation at 73 mHz and 1.03 Hz, as well as a QPO at 136 mHz in a single Swift/XRT observation that can be interpreted as standard Type-C QPOs. Aside from the detected QPOs, there is significant structure in the broadband power, with a strong feature observable in the Chandra observations between 0.1 and 1 Hz. We discuss our results in the context of current models for QPO formation.",
"date": "2017-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "934",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 90",
"id_number": "CaltechAUTHORS:20161028-100132024",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161028-100132024",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "New York University (NYU)"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)",
"grant_number": "639.041.437"
},
{
"agency": "Sardinian Region",
"grant_number": "L.R. 7/2007"
},
{
"agency": "ESA/PRODEX",
"grant_number": "90057"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/834/1/90",
"primary_object": {
"basename": "1610.08653v1.pdf",
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}
],
"pub_year": "2017",
"author_list": "Huppenkothen, D.; Younes, G.; et el."
},
{
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"eprint_id": 73210,
"eprint_status": "archive",
"datestamp": "2023-08-22 19:29:00",
"lastmod": "2023-10-24 15:07:50",
"type": "article",
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"creators": {
"items": [
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Fryer-C-L",
"name": {
"family": "Fryer",
"given": "Chris L."
},
"orcid": "0000-0003-2624-0056"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Delaney-T",
"name": {
"family": "Delaney",
"given": "Tracey"
}
},
{
"id": "Laming-J-M",
"name": {
"family": "Laming",
"given": "J. Martin"
},
"orcid": "0000-0002-3362-7040"
},
{
"id": "Reynolds-S-P",
"name": {
"family": "Reynolds",
"given": "Stephen P."
}
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "David M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Giommi-P",
"name": {
"family": "Giommi",
"given": "Paolo"
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Hornstrup-A",
"name": {
"family": "Hornstrup",
"given": "Alan"
}
},
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "Takao"
}
},
{
"id": "Koglin-J-E",
"name": {
"family": "Koglin",
"given": "J. E."
}
},
{
"id": "Lopez-L-A",
"name": {
"family": "Lopez",
"given": "Laura"
},
"orcid": "0000-0002-1790-3148"
},
{
"id": "Mao-Peter-H",
"name": {
"family": "Mao",
"given": "Peter H."
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Perri-M",
"name": {
"family": "Perri",
"given": "Matteo"
}
},
{
"id": "Pivovaroff-M-J",
"name": {
"family": "Pivovaroff",
"given": "Michael J."
}
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "Simonetta"
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram"
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Westergaard-N-J",
"name": {
"family": "Westergaard",
"given": "Niels J."
}
},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "Daniel R."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
},
{
"id": "Zoglauer-A-C",
"name": {
"family": "Zoglauer",
"given": "Andreas"
}
}
]
},
"title": "The distribution of radioactive ^(44)Ti in Cassiopeia A",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "gamma rays: general; ISM: supernova remnants; nuclear reactions, nucleosynthesis, abundances; X-rays: individual (Cassiopeia A)",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 August 30; revised 2016 October 17; accepted 2016 October 29; published 2016 December 27. \n\nWe would like thank Dan Milisavljevic for providing the [S iii] data files, as well as Thomas Janka, Raph Hix, and Adam Burrows for their helpful comments. This work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. J.M.L. was supported by the NASA ADAP grant NNH16AC24I.\n\nWe thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research also made extensive use of the IDL Astronomy Library (http://idlastro.gsfc.nasa.gov/). Additional figures were produced using the Veusz plotting package (\u00a9 2003\u20132016 Jeremy Sanders). 3D figures and movies were produced via the Anaconda Software Distribution (https://www.continuum.io) of python and mayavi2 (Ramachandran & Varoquaux 2011).\n\nFacilities: NuSTAR, Chandra, Spitzer.\n\nPublished - Grefenstette_2017_ApJ_834_19.pdf
",
"abstract": "The distribution of elements produced in the innermost layers of a supernova explosion is a key diagnostic for studying the collapse of massive stars. Here we present the results of a 2.4 Ms NuSTAR observing campaign aimed at studying the supernova remnant Cassiopeia A (Cas A). We perform spatially resolved spectroscopic analyses of the ^(44)Ti ejecta, which we use to determine the Doppler shift and thus the three-dimensional (3D) velocities of the ^(44)Ti ejecta. We find an initial ^(44)Ti mass of (1.54 \u00b1 0.21) \u00d7 10^(\u22124) M_\u2299, which has a present-day average momentum direction of 340\u00b0 \u00b1 15\u00b0 projected onto the plane of the sky (measured clockwise from celestial north) and is tilted by 58\u00b0 \u00b1 20\u00b0 into the plane of the sky away from the observer, roughly opposite to the inferred direction of motion of the central compact object. We find some ^(44)Ti ejecta that are clearly interior to the reverse shock and some that are clearly exterior to it. Where we observe ^(44)Ti ejecta exterior to the reverse shock we also see shock-heated iron; however, there are regions where we see iron but do not observe ^(44)Ti. This suggests that the local conditions of the supernova shock during explosive nucleosynthesis varied enough to suppress the production of ^(44)Ti by at least a factor of two in some regions, even in regions that are assumed to be the result of processes like \u03b1-rich freezeout that should produce both iron and titanium.",
"date": "2017-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "834",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 19",
"id_number": "CaltechAUTHORS:20170104-115334892",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170104-115334892",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNH16AC24I"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/834/1/19",
"primary_object": {
"basename": "Grefenstette_2017_ApJ_834_19.pdf",
"url": "https://authors.library.caltech.edu/records/bnqx7-zrw84/files/Grefenstette_2017_ApJ_834_19.pdf"
},
"pub_year": "2017",
"author_list": "Grefenstette, Brian W.; Fryer, Chris L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/4a4g6-ntk38",
"eprint_id": 73278,
"eprint_status": "archive",
"datestamp": "2023-09-28 01:15:30",
"lastmod": "2023-10-24 15:24:08",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
}
]
},
"title": "Spectral Changes in the Hyperluminous Pulsar in NGC 5907 as a Function of Super-Orbital Phase",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; pulsars: individual (NGC 5907 ULX1); X-rays: binaries",
"note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 September 30; revised 2016 November 11; accepted 2016 November 11; published 2017 January 4. \n\nWe thank the referee for useful comments that helped to improve the manuscript. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work.The Swift/BAT transient monitor results were provided by the Swift/BAT team. \n\nFacilities: NuSTAR, XMM, Chandra, Swift.\n\nPublished - Furst_2017_ApJ_834_77.pdf
Draft - 1610_00258.pdf
",
"abstract": "We present broadband, multi-epoch X-ray spectroscopy of the pulsating ultra-luminous X-ray source (ULX) in NGC 5907. Simultaneous XMM-Newton and NuSTAR data from 2014 are best described by a multicolor blackbody model with a temperature gradient as a function of accretion disk radius significantly flatter than expected for a standard thin accretion disk (T(r) \u03b1 r^(-p), with p = 0.608__(-0.012)^(+0.014)). Additionally, we detect a hard power-law tail at energies above 10 keV, which we interpret as being due to Comptonization. We compare this observation to archival XMM-Newton, Chandra, and NuSTAR data from 2003, 2012, and 2013, and investigate possible spectral changes as a function of phase over the 78-day super-orbital period of this source. We find that observations taken around phases 0.3\u20130.4 show very similar temperature profiles, even though the observed flux varies significantly, while one observation taken around phase 0 has a significantly steeper profile. We discuss these findings in light of the recent discovery that the compact object is a neutron star and show that precession of the accretion disk or the neutron star can self-consistently explain most observed phenomena.",
"date": "2017-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "834",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 77",
"id_number": "CaltechAUTHORS:20170105-135606067",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170105-135606067",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "ESA Member States"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-4357/834/1/77",
"primary_object": {
"basename": "1610_00258.pdf",
"url": "https://authors.library.caltech.edu/records/4a4g6-ntk38/files/1610_00258.pdf"
},
"related_objects": [
{
"basename": "Furst_2017_ApJ_834_77.pdf",
"url": "https://authors.library.caltech.edu/records/4a4g6-ntk38/files/Furst_2017_ApJ_834_77.pdf"
}
],
"pub_year": "2017",
"author_list": "F\u00fcrst, F.; Walton, D. J.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/8v31b-0cy48",
"eprint_id": 75208,
"eprint_status": "archive",
"datestamp": "2023-08-19 00:52:28",
"lastmod": "2023-10-25 14:50:48",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Landt-H",
"name": {
"family": "Landt",
"given": "H."
}
},
{
"id": "Ward-M-J",
"name": {
"family": "Ward",
"given": "M. J."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Kynoch-D",
"name": {
"family": "Kynoch",
"given": "D."
}
},
{
"id": "Storchi-Bergmann-T",
"name": {
"family": "Storchi-Bergmann",
"given": "T."
}
},
{
"id": "Boisson-C",
"name": {
"family": "Boisson",
"given": "C."
}
},
{
"id": "Done-C",
"name": {
"family": "Done",
"given": "C."
}
},
{
"id": "Schimoia-J",
"name": {
"family": "Schimoia",
"given": "J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
}
]
},
"title": "On the black hole mass of the \u03b3-ray emitting narrow-line Seyfert 1 galaxy 1H 0323+342",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "uasars: emission lines, quasars: individual: 1H 0323+342, galaxies: Seyfert, infrared: galaxies, X-rays: galaxies",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 September 23. Received 2016 September 20; in original form 2016 August 25. \n\nMJW and DK would like to thank the Observatoire de Paris for its hospitality and support during some months of this work in the framework of the Laboratoire Europ\u00e9en Associ\u00e9 (LEA) ELGA (European Laboratory for Gamma-ray Astronomy). We thank Maria March\u00e3 for kindly making their optical spectrum available to us in electronic format. HL is supported by a European Union COFUND/Durham Junior Research Fellowship (under EU grant agreement number 267209). MB acknowledges support from the National Aeronautics and Space Administration (NASA) Headquarters under the NASA Earth and Space Science Fellowship Program grant no. NNX14AQ07H. DK acknowledges the receipt of an STFC studentship. This work is partly based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA.\n\nPublished - stw2447.pdf
",
"abstract": "Narrow-line Seyfert 1 galaxies have been identified by the Fermi Gamma-Ray Space Telescope as a rare class of \u03b3-ray emitting active galactic nuclei. The lowest redshift candidate among them is the source 1H 0323+342. Here we present quasi-simultaneous Gemini near-infrared and Keck optical spectroscopy for it, from which we derive a black hole mass based on both the broad Balmer and Paschen emission lines. We supplement these observations with a Nuclear Spectroscopic Telescope Array X-ray spectrum taken about two years earlier, from which we constrain the black hole mass based on the short time-scale spectral variability. Our multiwavelength observations suggest a black hole mass of \u223c2 \u00d7 10^7 M_\u2299, which agrees well with previous estimates. We build the spectral energy distribution and show that it is dominated by the thermal and reprocessed emission from the accretion disc rather than the non-thermal jet component. A detailed spectral fitting with the energy-conserving accretion disc model of Done et al. constrains the Eddington ratio to L/LEdd \u223c 0.5 for a (non-rotating) Schwarzschild black hole and to L/LEdd \u223c 1 for a Kerr black hole with dimensionless spin of a^\u2605 = 0.8. Higher spin values and so higher Eddington ratios are excluded, since they would strongly overpredict the observed soft X-ray flux.",
"date": "2017-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "464",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2565-2576",
"id_number": "CaltechAUTHORS:20170317-130508222",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170317-130508222",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Laboratoire Europ\u00e9en Associ\u00e9"
},
{
"agency": "COFUND/Durham Junior Research Fellowship",
"grant_number": "267209"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "W. M. Keck Foundation"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw2447",
"primary_object": {
"basename": "stw2447.pdf",
"url": "https://authors.library.caltech.edu/records/8v31b-0cy48/files/stw2447.pdf"
},
"pub_year": "2017",
"author_list": "Landt, H.; Ward, M. J.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/7b6g3-xtd65",
"eprint_id": 74002,
"eprint_status": "archive",
"datestamp": "2023-08-19 00:49:13",
"lastmod": "2023-10-24 21:59:36",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Beardmore-A-P",
"name": {
"family": "Beardmore",
"given": "Andrew P."
}
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Guainazzi-M",
"name": {
"family": "Guainazzi",
"given": "Matteo"
}
},
{
"id": "Marshall-H-L",
"name": {
"family": "Marshall",
"given": "Herman L."
}
},
{
"id": "Miller-E-D",
"name": {
"family": "Miller",
"given": "Eric D."
}
},
{
"id": "Page-K-L",
"name": {
"family": "Page",
"given": "Kim L."
},
"orcid": "0000-0001-5624-2613"
},
{
"id": "Stuhlinger-M",
"name": {
"family": "Stuhlinger",
"given": "Martin"
}
}
]
},
"title": "IACHEC Cross-Calibration of Chandra, NuSTAR, Swift, Suzaku, and XMM-Newton with 3C 273 and PKS 2155-304",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "space vehicles: instruments",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 August 1. Accepted 2016 September 27. Published 2016 December 14. \n\nK.K.M. was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. \n\nH.L.M. was supported by the National Aeronautics and Space Administration (NASA) through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of the Chandra X-Ray Center (CXC), which is operated by SAO for and on behalf of NASA under contract NAS8-03060. \n\nA.P.B. and K.L.P. acknowledge support from the UK Space Agency. \n\nE.D.M. acknowledges funding from NASA grant NNX09AE58G to MIT to support the Suzaku XIS. \n\nWe thank the IACHEC for organizing the campaigns and providing the forum for development and discussion of the cross-calibration results that have led to this paper, and thank the referee for comments and suggestions. \n\nFacilities: Chandra - , NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, Suzaku - Suzaku (ASTRO-EII), and XMM-Newton. - Newton X-Ray Multimirror Mission satellite\n\nPublished - Madsen_2017_AJ_153_2.pdf
Submitted - 1609.09032v1.pdf
",
"abstract": "On behalf of the International Astronomical Consortium for High Energy Calibration, we present results from the cross-calibration campaigns in 2012 on 3C 273 and in 2013 on PKS 2155-304 between the then active X-ray observatories Chandra, NuSTAR, Suzaku, Swift, and XMM-Newton. We compare measured fluxes between instrument pairs in two energy bands, 1\u20135 keV and 3\u20137 keV, and calculate an average cross-normalization constant for each energy range. We review known cross-calibration features and provide a series of tables and figures to be used for evaluating cross-normalization constants obtained from other observations with the above mentioned observatories.",
"date": "2017-01",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "153",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 2",
"id_number": "CaltechAUTHORS:20170203-081053097",
"issn": "1538-3881",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170203-081053097",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Smithsonian Astrophysical Observatory",
"grant_number": "SV3-73016"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "United Kingdom Space Agency (UKSA)"
},
{
"agency": "NASA",
"grant_number": "NNX09AE58G"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-3881/153/1/2",
"primary_object": {
"basename": "1609.09032v1.pdf",
"url": "https://authors.library.caltech.edu/records/7b6g3-xtd65/files/1609.09032v1.pdf"
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"basename": "Madsen_2017_AJ_153_2.pdf",
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}
],
"pub_year": "2017",
"author_list": "Madsen, Kristin K.; Beardmore, Andrew P.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/bd5gs-63h22",
"eprint_id": 75028,
"eprint_status": "archive",
"datestamp": "2023-08-19 00:51:52",
"lastmod": "2023-10-25 14:40:48",
"type": "article",
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"creators": {
"items": [
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Guainazzi-M",
"name": {
"family": "Guainazzi",
"given": "M."
}
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "P. G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M. J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "LaMassa-S-M",
"name": {
"family": "LaMassa",
"given": "S. M."
},
"orcid": "0000-0002-5907-3330"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Phoenix galaxy as seen by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active / galaxies: Seyfert / X-rays: galaxies",
"note": "\u00a9 ESO, 2017. \n\nReceived: 1 August 2016. Accepted: 1 September 2016. Published online 11 January 2017. \n\nWe thank the anonymous referee for useful suggestions that helped to improve the paper. This work was supported under NASA Contract NNG08FD60C, and it made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has also made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC). A.M., A.C., and S.P. acknowledge support from the ASI/INAF grant I/037/12/0-011/13. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. P.G. and P.B. thank STFC for support (grant ST/J003697/2). S.L.M. is supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Universities Space Research Association under contract with NASA. We acknowledge support from NASA NuSTAR A01 Award NNX15AV27G (F.E.B.), CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., C.R.), FONDECYT Regular 1141218 (F.E.B., C.R.), \"EMBIGGEN\" Anillo ACT1101 (F.E.B., C.R.), the China-CONICYT fund (C.R.), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.).\n\nPublished - aa29444-16.pdf
",
"abstract": "Aims. We study the long-term variability of the well-known Seyfert\u20092 galaxy Mrk\u20091210 (also known as UGC\u20094203, or the Phoenix galaxy). \n\nMethods. The source was observed by many X-ray facilities in the last 20 yr. Here we present a NuSTAR observation and put the results in the context of previously published observations. \n\nResults. NuSTAR observed Mrk\u20091210 in 2012 for 15.4 ks. The source showed Compton-thin obscuration similar to that observed by Chandra, Suzaku, BeppoSAX and XMM-Newton over the past two decades, but different from the first observation by ASCA in 1995, in which the active nucleus was caught in a low flux state or was obscured by Compton-thick matter with a reflection-dominated spectrum. Thanks to the high-quality hard X-ray spectrum obtained with NuSTAR and exploiting the long-term spectral coverage spanning 16.9 yr, we can precisely disentangle the transmission and reflection components and put constraints on both the intrinsic long-term variability and hidden nucleus scenarios. In the former case, the distance between the reflector and the source must be at least ~2 pc, while in the latter the eclipsing cloud may be identified with a water maser-emitting clump.",
"date": "2017-01",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "597",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A100",
"id_number": "CaltechAUTHORS:20170310-121538992",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170310-121538992",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "NASA",
"grant_number": "NNX15AV27G"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.1051/0004-6361/201629444",
"primary_object": {
"basename": "aa29444-16.pdf",
"url": "https://authors.library.caltech.edu/records/bd5gs-63h22/files/aa29444-16.pdf"
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"pub_year": "2017",
"author_list": "Masini, A.; Comastri, A.; et el."
},
{
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"eprint_id": 72906,
"eprint_status": "archive",
"datestamp": "2023-08-19 00:36:18",
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"type": "article",
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"items": [
{
"id": "Zoghbi-A",
"name": {
"family": "Zoghbi",
"given": "Abderahmen"
},
"orcid": "0000-0002-0572-9613"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "A. L."
}
},
{
"id": "Miller-M-C",
"name": {
"family": "Miller",
"given": "M. C."
},
"orcid": "0000-0002-2666-728X"
},
{
"id": "Proga-D",
"name": {
"family": "Proga",
"given": "D."
}
},
{
"id": "Kallman-Timothy-R",
"name": {
"family": "Kallman",
"given": "T."
},
"orcid": "0000-0002-5779-6906"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kaastra-J-S",
"name": {
"family": "Kaastra",
"given": "J."
},
"orcid": "0000-0001-5540-2822"
},
{
"id": "Raymond-J",
"name": {
"family": "Raymond",
"given": "J."
}
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Disk\u2013Wind Connection during the Heartbeats of GRS 1915+105",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 instabilities \u2013 X-rays: binaries \u2013 X-rays: individual (GRS 1915+105)",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 April 13; revised 2016 September 27; accepted 2016 October 17; published 2016 December 15. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This work is also based on observations made by the Chandra X-ray Observatory.\n\nPublished - Zoghbi_2016_ApJ_833_165.pdf
Submitted - 1610.05772v1.pdf
",
"abstract": "Disk and wind signatures are seen in the soft state of Galactic black holes, while the jet is seen in the hard state. Here we study the disk\u2013wind connection in the \u03c1 class of variability in GRS 1915+105 using a joint NuSTAR\u2013Chandra observation. The source shows 50 s limit cycle oscillations. By including new information provided by the reflection spectrum and using phase-resolved spectroscopy, we find that the change in the inner disk inferred from the blackbody emission is not matched by reflection measurements. The latter is almost constant, independent of the continuum model. The two radii are comparable only if the disk temperature color correction factor changes, an effect that could be due to the changing opacity of the disk caused by changes in metal abundances. The disk inclination is similar to that inferred from the jet axis, and oscillates by ~10\u00b0. The simultaneous Chandra data show the presence of two wind components with velocities between 500 and 5000 km s^(\u22121), and possibly two more with velocities reaching 20,000 km s^(\u22121) (~0.06 c). The column densities are ~5 \u00d7 10^(22) cm^(\u22122). An upper limit to the wind response time of 2 s is measured, implying a launch radius of <6 \u00d7 10^(10) cm. The changes in wind velocity and absorbed flux require the geometry of the wind to change during the oscillations, constraining the wind to be launched from a distance of 290\u20131300 r_g from the black hole. Both data sets support fundamental model predictions in which a bulge originates in the inner disk and moves outward as the instability progresses.",
"date": "2016-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "833",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 165",
"id_number": "CaltechAUTHORS:20161216-100202166",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161216-100202166",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/1538-4357/833/2/165",
"primary_object": {
"basename": "1610.05772v1.pdf",
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"basename": "Zoghbi_2016_ApJ_833_165.pdf",
"url": "https://authors.library.caltech.edu/records/re7f6-yw491/files/Zoghbi_2016_ApJ_833_165.pdf"
}
],
"pub_year": "2016",
"author_list": "Zoghbi, Abderahmen; Miller, J. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/wj6ag-e1t40",
"eprint_id": 72962,
"eprint_status": "archive",
"datestamp": "2023-08-22 19:19:06",
"lastmod": "2023-10-23 23:27:29",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Boorman-P-G",
"name": {
"family": "Boorman",
"given": "Peter G."
},
"orcid": "0000-0001-9379-4716"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Annuar-A",
"name": {
"family": "Annuar",
"given": "A."
},
"orcid": "0000-0003-0387-1429"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "H\u00f6nig-S-F",
"name": {
"family": "H\u00f6nig",
"given": "S. F."
}
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "LaMassa-S-M",
"name": {
"family": "LaMassa",
"given": "S. M."
},
"orcid": "0000-0002-5907-3330"
},
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Risaliti-G",
"name": {
"family": "Risaliti",
"given": "G."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "IC 3639\u2014A New Bona Fide Compton-Thick AGN Unveiled by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: nuclei; galaxies: Seyfert; techniques: spectroscopic; X-rays: galaxies; X-rays: individual (IC 3639)",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 June 27. Accepted 2016 October 26. Published 2016 December 20. \n\nWe thank the anonymous referee for the invaluable comments that helped to improve this paper. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The scientific results reported in this article are based on observations made by the ChandraX-ray Observatory. \n\nThis research has made use of data, software, and/or Web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. \n\nThis research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. \n\nThis research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). \n\nThis publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. \n\nP.B. thanks STFC and the RAS for funding. \n\nP.G. thanks STFC for support (grant reference ST/J003697/2). \n\nA.A. acknowledges financial support from Majlis Amanah Rakyat (MARA), Malaysia. \n\nD. M. A. acknowledges the Science and Technology Facilities Council (DMA; ST/L00075X/1). \n\nW.N.B. acknowledges Caltech NuSTAR subcontract 44A-1092750 and the VM Willaman Endowment. \n\nS.F.H. acknowledges support from the European Research Council under Horizon 2020 grant ERC-2015-StG-677117. \n\nM.K. acknowledges support from the Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant PZ00P2_154799/1. \n\nS.M.L. acknowledges support by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by the Universities Space Research Association under contract with NASA. \n\nA.M. acknowledges support from the ASI/INAF grant I/037/12/0-011/13. \n\nF.E.B. and C.R. acknowledge support from NASA NuSTAR A01 Award NNX15AV27G, CONICYT-Chile grants Basal-CATA PFB-06/2007, FONDECYT Regular 1141218 and 1151408, \"EMBIGGEN\" Anillo ACT1101, the China-CONICYT, and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. \n\nFacilities: NuSTAR, Suzaku, Chandra.\n\nPublished - Boorman_2016_ApJ_833_245.pdf
Submitted - 1610.08997v1.pdf
",
"abstract": "We analyze high-quality NuSTAR observations of the local (z = 0.011) Seyfert 2 active galactic nucleus (AGN) IC 3639, in conjunction with archival Suzaku and Chandra data. This provides the first broadband X-ray spectral analysis of the source, spanning nearly two decades in energy (0.5\u201330 keV). Previous X-ray observations of the source below 10 keV indicated strong reflection/obscuration on the basis of a pronounced iron fluorescence line at 6.4 keV. The hard X-ray energy coverage of NuSTAR, together with self-consistent toroidal reprocessing models, enables direct broadband constraints on the obscuring column density of the source. We find the source to be heavily Compton-thick (CTK) with an obscuring column in excess of 3.6 x 10^(24) cm^(\u22122), unconstrained at the upper end. We further find an intrinsic 2\u201310 keV luminosity of log_(10)(L_(2-10keV) [erg s^(-1)])={43.4}_(-1.1)^(+0.6 to 90% confidence, almost 400 times the observed flux, and consistent with various multiwavelength diagnostics. Such a high ratio of intrinsic to observed flux, in addition to an Fe-K\u03b1 fluorescence line equivalent width exceeding 2 keV, is extreme among known bona fide CTK AGNs, which we suggest are both due to the high level of obscuration present around IC 3639. Our study demonstrates that broadband spectroscopic modeling with NuSTAR enables large corrections for obscuration to be carried out robustly and emphasizes the need for improved modeling of AGN tori showing intense iron fluorescence.",
"date": "2016-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "833",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 245",
"id_number": "CaltechAUTHORS:20161220-081623292",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161220-081623292",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Royal Astronomical Society"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "Majlis Amanah Rakyat (MARA)"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "Caltech VM Willaman Endowmnent"
},
{
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"title": "GRS 1739-278 Observed at Very Low Luminosity with XMM-Newton and NuSTAR",
"ispublished": "pub",
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"keywords": "accretion, accretion disks \u2013 stars: black holes \u2013 X-rays: binaries \u2013 X-rays: individual (GRS 1739-278)",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 August 2; revised 2016 September 20; accepted 2016 September 22; published 2016 November 22. \n\nWe thank the referee for their helpful comments. We thank the schedulers and SOC of XMM-Newton and NuSTAR for making these observations possible. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work is based upon work supported by NASA under award No. NNX16AH17G. J.A.T. acknowledges partial support from NASA under Swift Guest Observer grants NNX15AB81G and NNX15AR52G. E.K. acknowledges support of TUBITAK Project No 115F488. S.C. and A.L. acknowledge funding support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 and the UnivEarthS Labex program of Sorbonne Paris Cit\u00e9 (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). J.C.A.M.-J. is the recipient of an Australian Research Council Future Fellowship (FT140101082). This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. This research has made use of MAXI data provided by RIKEN, JAXA and the MAXI team. The Swift/BAT transient monitor results were provided by the Swift/BAT team. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/).\n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM.\n\nPublished - F\u00fcrst_2016_ApJ_832_115.pdf
Submitted - 1609.07530v1.pdf
",
"abstract": "We present a detailed spectral analysis of XMM-Newton and NuSTAR observations of the accreting transient black hole GRS 1739\u2212278 during a very faint low hard state at ~0.02% of the Eddington luminosity (for a distance of 8.5 kpc and a mass of 10 M\u2299). The broadband X-ray spectrum between 0.5 and 60 keV can be well-described by a power-law continuum with an exponential cutoff. The continuum is unusually hard for such a low luminosity, with a photon index of \u0393 = 1.39 \u00b1 0.04. We find evidence for an additional reflection component from an optically thick accretion disk at the 98% likelihood level. The reflection fraction is low, with R_(refl) = 0.043^(+0.033)_(-0.023). In combination with measurements of the spin and inclination parameters made with NuSTAR during a brighter hard state by Miller et al., we seek to constrain the accretion disk geometry. Depending on the assumed emissivity profile of the accretion disk, we find a truncation radius of 15\u201335 R_g(5\u201312 R_(ISCO)) at the 90% confidence limit. These values depend strongly on the assumptions and we discuss possible systematic uncertainties.",
"date": "2016-12-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "832",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 115",
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"agency": "T\u00fcrkiye Bilimsel ve Teknolojik Ara\u015ft\u0131rma Kurumu (T\u00dcB\u0130TAK)",
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"title": "Multi-wavelength observations of IGR J17544-2619 from quiescence to outburst",
"ispublished": "pub",
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"keywords": "X-rays: binaries",
"note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 14 July 2016; Accepted 9 October 2016; Published online 22 November 2016.\n\nWe warmly thank the XMM-Newton and NuSTAR teams for their efforts in scheduling the simultaneous observations of IGR\u2009J17544-2619. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We also made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This publication was motivated by a team meeting sponsored by the International Space Science Institute in Bern, Switzerland. E.B., L.O., and A.M. thank ISSI for their financial support during their stay in Bern. V.B. and J.A.T. thank Brian Grefenstette and Kristin Madsen for help with planning the NuSTAR observations and Lorenzo Natalucci and David Smith for useful discussions. P.R. acknowledges contract ASI-INAF I/004/11/0 and financial contribution from the agreement ASI-INAF I/037/12/0. A.M. acknowledges support from the Polish NCN grant 2013/08/A/ST9/00795. S.C. is grateful to the Centre National d'\u00c9tudes Spatiales (CNES) for the funding of MINE (Multi-wavelength INTEGRAL Network). We thank the anonymous referee for detailed and useful referee report that helped improve the paper.\n\nAccepted Version - 1610.02648v1.pdf
",
"abstract": "In this paper we report on a long multi-wavelength observational campaign of the supergiant fast X-ray transient prototype IGR\u2009J17544-2619. A 150 ks-long observation was carried out simultaneously with XMM-Newton and NuSTAR, catching the source in an initial faint X-ray state and then undergoing a bright X-ray outburst lasting approximately 7 ks. We studied the spectral variability during outburst and quiescence by using a thermal and bulk Comptonization model that is typically adopted to describe the X-ray spectral energy distribution of young pulsars in high mass X-ray binaries. Although the statistics of the collected X-ray data were relatively high, we could neither confirm the presence of a cyclotron line in the broad-band spectrum of the source (0.5\u221240 keV), nor detect any of the previously reported tentative detections of the source spin period. The monitoring carried out with Swift\u2009/XRT during the same orbit of the system observed by XMM-Newton and NuSTAR revealed that the source remained in a low emission state for most of the time, in agreement with the known property of all supergiant fast X-ray transients being significantly sub-luminous compared to other supergiant X-ray binaries. Optical and infrared observations were carried out for a total of a few thousand seconds during the quiescence state of the source detected by XMM-Newton and NuSTAR. The measured optical and infrared magnitudes were slightly lower than previous values reported in the literature, but compatible with the known micro-variability of supergiant stars. UV observations obtained with the UVOT telescope on-board Swift did not reveal significant changes in the magnitude of the source in this energy domain compared to previously reported values.",
"date": "2016-12",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "596",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A16",
"id_number": "CaltechAUTHORS:20161011-074320835",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161011-074320835",
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},
"title": "The NuSTAR view of the non-thermal emission from PSR J0437-4715",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron \u2013 pulsars: individual: PSR 0437\u22124715",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 August 26. Received 2016 August 26; in original form 2015 December 12. \n\nThe authors thank the referee, Slavko Bogdanov, for very useful suggestions that significantly improved this paper. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. The data analysis was performed with the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). SG is a FONDECYT post-doctoral fellow, funded by grant # 3150428. VMK receives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.\n\nPublished - stw2194.pdf
Submitted - 1512.03957v1.pdf
",
"abstract": "We present a hard X-ray Nuclear Spectroscopic Telescope Array (NuSTAR) observation of PSR J0437\u22124715, the nearest millisecond pulsar. The known pulsations at the apparent pulse period \u223c5.76ms are observed with a significance of 3.7\u03c3, at energies up to 20\u2009keV above which the NuSTAR background dominates. We measure a photon index \u0393 = 1.50 \u00b1 0.25 (90 per cent confidence) for the power-law fit to the non-thermal emission. It had been shown that spectral models with two or three thermal components fit the XMM\u2013Newton spectrum of PSR J0437\u22124715, depending on the slope of the power-law component, and the amount of absorption of soft X-rays. The new constraint on the high-energy emission provided by NuSTAR removes ambiguities regarding the thermal components of the emission below 3keV. We performed a simultaneous spectral analysis of the XMM\u2013Newton and NuSTAR data to confirm that three thermal components and a power law are required to fit the 0.3\u201320\u2009keV emission of PSR J0437\u22124715. Adding a ROSAT-PSPC spectrum further confirmed this result and allowed us to better constrain the temperatures of the three thermal components. A phase-resolved analysis of the NuSTAR data revealed no significant change in the photon index of the high-energy emission. This NuSTAR observation provides further impetus for future observations with the NICER mission (Neutron Star Interior Composition Explorer) whose sensitivity will provide much stricter constraints on the equation of state of nuclear matter by combining model fits to the pulsar's phase-folded light curve with the pulsar's well-defined mass and distance from radio timing observations.",
"date": "2016-12",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "463",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2612-2622",
"id_number": "CaltechAUTHORS:20160115-070419376",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-070419376",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
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{
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{
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"doi": "10.1093/mnras/stw2194",
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"author_list": "Guillot, S.; Kaspi, V. M.; et el."
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"id": "Ursini-F",
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}
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"family": "Matt",
"given": "G."
},
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{
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"name": {
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{
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"name": {
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{
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"name": {
"family": "De Marco",
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}
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{
"id": "De-Rosa-A",
"name": {
"family": "De Rosa",
"given": "A."
},
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{
"id": "Malzac-J",
"name": {
"family": "Malzac",
"given": "J."
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{
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"name": {
"family": "Marinucci",
"given": "A."
}
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{
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"family": "Ponti",
"given": "G."
},
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},
{
"id": "Tortosa-A",
"name": {
"family": "Tortosa",
"given": "A."
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]
},
"title": "High-energy monitoring of NGC 4593 with XMM-Newton and NuSTAR. X-ray spectral analysis",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: Seyfert \u2013X-rays: galaxies \u2013X-rays: individual: NGC 4593",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 August 9. Received 2016 August 9; in original form 2016 July 4. Published: 12 August 2016. \n\nWe thank the anonymous referee for helpful comments and suggestions that improved the paper. \n\nThis work is based on observations obtained with: the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA; XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of data, software and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. FU, P-OP, GM, SB, MC, ADR and JM acknowledge support from the French\u2013Italian International Project of Scientific Collaboration: PICS-INAF project number 181542. FU and P-OP acknowledge support from CNES. FU acknowledges support from Universit\u00e9 Franco-Italienne (Vinci PhD fellowship). FU and GM acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. P-OP acknowledges financial support from the Programme National Hautes Energies. SB, MC and ADR acknowledge financial support from the Italian Space Agency under grant ASI-INAF I/037/12/P1. GP acknowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society.\n\nAccepted Version - 1608.02847v1.pdf
",
"abstract": "We present results from a joint XMM\u2013Newton/NuSTAR monitoring of the Seyfert 1 NGC 4593, consisting of 5 \u00d7 20 ks simultaneous observations spaced by 2 d, performed in 2015 January. The source is variable, both in flux and spectral shape, on time-scales down to a few ks and with a clear softer-when-brighter behaviour. In agreement with past observations, we find the presence of a warm absorber well described by a two-phase ionized outflow. The source exhibits a cold, narrow and constant Fe K\u03b1 line at 6.4 keV, and a broad component is also detected. The broad-band (0.3\u201379 keV) spectrum is well described by a primary power law with \u0393 \u2243 1.6\u20131.8 and an exponential cut-off varying from 90^(+40_+(\u221220) to >700 keV, two distinct reflection components, and a variable soft excess correlated with the primary power law. This campaign shows that probing the variability of Seyfert 1 galaxies on different time-scales is of prime importance to investigate the high-energy emission of active galactic nuclei.",
"date": "2016-11-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "463",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "382-392",
"id_number": "CaltechAUTHORS:20160816-122629700",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160816-122629700",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw2022",
"primary_object": {
"basename": "1608.02847v1.pdf",
"url": "https://authors.library.caltech.edu/records/8y5yh-3sd16/files/1608.02847v1.pdf"
},
"pub_year": "2016",
"author_list": "Ursini, F.; Petrucci, P.-O.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/crvh7-5qd48",
"eprint_id": 69992,
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"datestamp": "2023-08-19 00:07:38",
"lastmod": "2023-10-20 21:18:58",
"type": "article",
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"creators": {
"items": [
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman"
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Sazonov-S",
"name": {
"family": "Sazonov",
"given": "Sergey"
}
}
]
},
"title": "NuSTAR and XMM-Newton observations of the ultraluminous X-ray source NGC 5643 X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 galaxies: individual: NGC 5643 \u2013 X-rays: binaries \u2013 X-rays: individual: NGC 5643 X-1",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 August 12. Received 2016 July 19; in original form 2016 June 17. Published: 16 August 2016.\n\nThis work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration, and re-observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The research has made use of the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work was supported by the Russian Science Foundation (grant 14-12-01315).\n\nAccepted Version - 1608.07445v1.pdf
",
"abstract": "We present a high-quality hard X-ray spectrum of the ultraluminous X-ray source (ULX) NGC 5643 X-1 measured with NuSTAR in 2014 May\u2013June. We have obtained this spectrum by carefully separating the signals from the ULX and from the active nucleus of its host galaxyNGC 5643 located 0.8 arcmin away. Together with long XMM\u2013Newton observations performed in 2009 July and 2014 August, the NuSTAR data confidently reveal a high-energy cutoff in the spectrum of NGC 5643 X-1 above \u223c10 keV, which is a characteristic signature of ULXs. The NuSTAR and XMM\u2013Newton data are consistent with the source having a constant luminosity \u223c1.5 \u00d7 10^(40) erg s^(\u22121) (0.2\u201312 keV) in all but the latest observation (2014 August) when it brightened to \u223c3 \u00d7 10^(40) erg s^(\u22121). This increase is associated with the dominant, hard spectral component (presumably collimated emission from the inner regions of a supercritical accretion disc), while an additional, soft component (with a temperature \u223c0.3 keV if described by multicolour disc emission), possibly associated with a massive wind outflowing from the disc, is also evident in the spectrum but does not exhibit significant variability.",
"date": "2016-11-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "463",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "756-762",
"id_number": "CaltechAUTHORS:20160829-141753109",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160829-141753109",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
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}
]
},
"doi": "10.1093/mnras/stw2058",
"primary_object": {
"basename": "1608.07445v1.pdf",
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"pub_year": "2016",
"author_list": "Krivonos, Roman and Sazonov, Sergey"
},
{
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"eprint_id": 67639,
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"items": [
{
"id": "D'Ai-Antonino",
"name": {
"family": "D'A\u00ec",
"given": "A."
},
"orcid": "0000-0002-5042-1036"
},
{
"id": "Burderi-L",
"name": {
"family": "Burderi",
"given": "L."
}
},
{
"id": "Di-Salvo-T",
"name": {
"family": "Di Salvo",
"given": "T."
}
},
{
"id": "Iaria-R",
"name": {
"family": "Iaria",
"given": "R."
}
},
{
"id": "Pintore-F",
"name": {
"family": "Pintore",
"given": "F."
}
},
{
"id": "Riggio-A",
"name": {
"family": "Riggio",
"given": "A."
}
},
{
"id": "Sanna-A",
"name": {
"family": "Sanna",
"given": "A."
}
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},
"title": "Discovery of hard phase lags in the pulsed emission of GRO J1744-28",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "line: formation \u2013 line: identification \u2013 stars: individual: (GRO J1744\u221228) \u2013 X-rays: binaries \u2013 X-rays: general",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 June 1. Received 2016 June 1; in original form 2016 March 31. Published: 17 June 2016. \n\nThe High-Energy Astrophysics Group of Palermo acknowledges support from the Fondo Finalizzato alla Ricerca (FFR) 2012/13, project N. 2012-ATE-0390, founded by the University of Palermo. \n\nAR gratefully acknowledges the Sardinia Regional Government for the financial support (P.O.R. Sardegna F.S.E. Operational Programme of the Autonomous Region of Sardinia, European Social Fund 2007\u20132013 \u2013 Axis IV Human Resources, Objective l.3, Line of Activity l.3.1). \n\nThe Palermo and Cagliari University groups acknowledge financial contribution from the agreement ASI-INAF I/037/12/0.\n\nSubmitted - 1606.00194v1.pdf
",
"abstract": "We report on the discovery and energy dependence of hard phase lags in the 2.14 Hz pulsed profiles of GRO J1744\u221228. We used data from XMM\u2013Newton and NuSTAR. We were able to well constrain the lag spectrum with respect to the softest (0.3\u20132.3 keV) band: the delay shows increasing lag values reaching a maximum delay of \u223c12 ms, between 6 and 6.4 keV. After this maximum, the value of the hard lag drops to \u223c7 ms, followed by a recovery to a plateau at \u223c9 ms for energies above 8 keV. NuSTAR data confirm this trend up to 30 keV, but the measurements are statistically poorer, and therefore, less constraining. The lag-energy pattern up to the discontinuity is well described by a logarithmic function. Assuming this is due to a Compton reverberation mechanism, we derive a size for the Compton cloud Rcc \u223c 120 Rg, consistent with previous estimates on the magnetospheric radius. In this scenario, the sharp discontinuity at \u223c6.5 keV appears difficult to interpret and suggests the possible influence of the reflected component in this energy range. We therefore propose the possible coexistence of both Compton and disc reverberation to explain the scale of the lags and its energy dependence.",
"date": "2016-11-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "463",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L84-L88",
"id_number": "CaltechAUTHORS:20160603-084223310",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160603-084223310",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/slw112",
"primary_object": {
"basename": "1606.00194v1.pdf",
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},
"pub_year": "2016",
"author_list": "D'A\u00ec, A.; Burderi, L.; et el."
},
{
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"datestamp": "2023-08-19 00:00:28",
"lastmod": "2023-10-20 21:57:37",
"type": "article",
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"creators": {
"items": [
{
"id": "Lobban-A-P",
"name": {
"family": "Lobban",
"given": "A. P."
},
"orcid": "0000-0002-6433-1357"
},
{
"id": "Pounds-K",
"name": {
"family": "Pounds",
"given": "K."
}
},
{
"id": "Vaughan-S",
"name": {
"family": "Vaughan",
"given": "S."
}
},
{
"id": "Reeves-J-N",
"name": {
"family": "Reeves",
"given": "J. N."
}
}
]
},
"title": "Testing relativistic reflection and resolving outflows in PG 1211+143 with XMM-Newton and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: active \u2013 galaxies: individual (PG 1211+143) \u2013 quasars: absorption lines",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 April 6; revised 2016 August 22; accepted 2016 September 5; published 2016 November 9. \n\nThis research has made use of the NASA Astronomical Data System (ADS), the NASA Extragalactic Database (NED) and is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL). APL and SV acknowledge support from STFC consolidated grant ST/K001000/1 and JNR acknowledges financial support via NASA grant NNX15AF12G. We thank an anonymous referee for highly constructive comments which helped improve the clarity of the paper. \n\nFacilities: XMM-Newton (EPIC), NuSTAR.\n\nAccepted Version - 1609.01674v1.pdf
",
"abstract": "We analyze the broad-band X-ray spectrum (0.3\u201350 keV) of the luminous Seyfert 1/quasar PG 1211+143\u2014the archetypal source for high-velocity X-ray outflows\u2014using near-simultaneous XMM-Newton and NuSTAR observations. We compare pure relativistic reflection models with a model including the strong imprint of photoionized emission and absorption from a high-velocity wind, finding a spectral fit that extrapolates well over the higher photon energies covered by NuSTAR. Inclusion of the high signal-to-noise ratio XMM-Newton spectrum provides much tighter constraints on the model parameters, with a much harder photon index/lower reflection fraction compared to that from the NuSTAR data alone. We show that pure relativistic reflection models are not able to account for the spectral complexity of PG 1211+143 and that wind absorption models are strongly required to match the data in both the soft X-ray and Fe K spectral regions. In confirming the significance of previously reported ionized absorption features, the new analysis provides a further demonstration of the power of combining the high throughput and resolution of long-look XMM-Newton observations with the unprecedented spectral coverage of NuSTAR.",
"date": "2016-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "831",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 201",
"id_number": "CaltechAUTHORS:20160908-134633517",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160908-134633517",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/0004-637X/831/2/201",
"primary_object": {
"basename": "1609.01674v1.pdf",
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"pub_year": "2016",
"author_list": "Lobban, A. P.; Pounds, K.; et el."
},
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"eprint_id": 71748,
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"datestamp": "2023-08-19 00:01:09",
"lastmod": "2023-10-23 17:02:24",
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{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
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{
"id": "Stern-D",
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"family": "Stern",
"given": "D."
},
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"name": {
"family": "Barret",
"given": "D."
},
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{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "K."
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Webb-N-A",
"name": {
"family": "Webb",
"given": "N."
}
}
]
},
"title": "Discovery of Coherent Pulsations from the Ultraluminous X-Ray Source NGC 7793 P13",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 pulsars: individual (NGC 7793 P13) \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 September 22; revised 2016 October 10; accepted 2016 October 15; published 2016 November 3. \n\nWe would like the thank the referee for the helpful comments. M.J.M. acknowledges support from an STFC Ernest Rutherford fellowship, A.C.F. acknowledges support from ERC Advanced Grant 340442, and D.B. acknowledges financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the nustardas software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, and also made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). \n\nFacilities: NuSTAR, XMM, Swift.\n\nPublished - F\u00fcrst_2016_ApJL_831_L14.pdf
Submitted - 1609.07129v2.pdf
",
"abstract": "We report the detection of coherent pulsations from the ultraluminous X-ray source (ULX) NGC 7793 P13. The \u22480.42 s nearly sinusoidal pulsations were initially discovered in broadband X-ray observations using XMM-Newton and NuSTAR taken in 2016. We subsequently also found pulsations in archival XMM-Newton data taken in 2013 and 2014. The significant (\u226b5\u03c3) detection of coherent pulsations demonstrates that the compact object in P13 is a neutron star, and given the observed peak luminosity of \u224810^(40) erg s^(-1) (assuming isotropy), it is well above the Eddington limit for a 1.4 M\u2299 accretor. This makes P13 the second ULX known to be powered by an accreting neutron star. The pulse period varies between epochs, with a slow but persistent spin-up over the 2013\u20132016 period. This spin-up indicates a magnetic field of B \u2248 1.5 \u00d7 10^(12) G, typical of many Galactic accreting pulsars. The most likely explanation for the extreme luminosity is a high degree of beaming; however, this is difficult to reconcile with the sinusoidal pulse profile.",
"date": "2016-11-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "831",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L14",
"id_number": "CaltechAUTHORS:20161104-130329124",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161104-130329124",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.3847/2041-8205/831/2/L14",
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"pub_year": "2016",
"author_list": "F\u00fcrst, F.; Walton, D. J.; et el."
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"id": "Wolff-M-T",
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{
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},
"title": "The NuSTAR X-ray Spectrum of Hercules X-1: A Radiation-Dominated Radiative Shock",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "methods: data analysis; X-rays: binaries; stars: individual (Her X-1); stars: neutron; radiative transfer",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 September 24; revised 2016 August 22; accepted 2016 August 23; published 2016 November 8. \n\nThe authors thank Dr. Carlo Ferrigno and Dr. Kenneth Wolfram for valuable help in formulating the numerical implementation of many of the analytical expressions. We thank Dr. Richard Rothschild for a number of stimulating discussions. We also thank an anonymous referee for a number of insightful comments that helped improve the manuscript. This research was supported by the National Aeronautics and Space Administration Astrophysical Data Analysis Program under Grant 12-ADAP12-0118. MTW and KSW are also supported by the Chief of Naval Research. JW and F-WS are grateful for support by the Deutsche Forschungsgemeinschaft. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - Wolff_2016_ApJ_831_194.pdf
Submitted - 1608.08978v1.pdf
",
"abstract": "We report on new spectral modeling of the accreting X-ray pulsar Hercules X-1. Our radiation-dominated radiative shock model is an implementation of the analytic work of Becker & Wolff on Comptonized accretion flows onto magnetic neutron stars. We obtain a good fit to the spin-phase-averaged 4\u201378 keV X-ray spectrum observed by the Nuclear Spectroscopic Telescope Array during a main-on phase of the Her X-1 35 day accretion disk precession period. This model allows us to estimate the accretion rate, the Comptonizing temperature of the radiating plasma, the radius of the magnetic polar cap, and the average scattering opacity parameters in the accretion column. This is in contrast to previous phenomenological models that characterized the shape of the X-ray spectrum, but could not determine the physical parameters of the accretion flow. We describe the spectral fitting details and discuss the interpretation of the accretion flow physical parameters.",
"date": "2016-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "831",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 194",
"id_number": "CaltechAUTHORS:20161109-092115164",
"issn": "0004-637X",
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"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
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"agency": "NASA",
"grant_number": "12-ADAP12-0118"
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{
"agency": "Chief of Naval Research"
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{
"agency": "Deutsche Forschungsgemeinschaft (DFG)"
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{
"agency": "NASA/JPL/Caltech"
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"doi": "10.3847/0004-637X/831/2/194",
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"author_list": "Wolff, Michael T.; Becker, Peter A.; et el."
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"title": "First NuSTAR observations of the BL Lac-type blazar PKS~2155-304: constraints on the jet content and distribution of radiating particles",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "BL Lacertae objects: individual (PKS 2155-304); galaxies: active; galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 August 2; revised 2016 August 25; accepted 2016 August 29; published 2016 November 3. \n\nThe Fermi-LAT Collaboration acknowledges support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. This work was partially supported under the NASA contract No. NNG08FD60C, and made use of observations from the NuSTAR mission, a project led by California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support in the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). K.N. was supported by NASA through Einstein Postdoctoral Fellowship grant number PF3-140130 awarded by the Chandra X-ray Center, and by the Polish National Science Centre grant 2015/18/E/ST9/00580. M.B. acknowledges support from NASA under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.\n\nPublished - Madejski_2016_ApJ_831_142.pdf
Submitted - 1609.02203v1.pdf
",
"abstract": "We report the first hard X-ray observations with NuSTAR of the BL Lac-type blazar PKS 2155-304, augmented with soft X-ray data from XMM-Newton and \u03b3-ray data from the Fermi Large Area Telescope, obtained in 2013 April when the source was in a very low flux state. A joint NuSTAR and XMM spectrum, covering the energy range 0.5\u201360 keV, is best described by a model consisting of a log-parabola component with curvature \u03b2 = 0.3_(-0.1)^(+0.2) and a (local) photon index 3.04 \u00b1 0.15 at photon energy of 2 keV, and a hard power-law tail with photon index 2.2 \u00b1 0.4. The hard X-ray tail can be smoothly joined to the quasi-simultaneous \u03b3-ray spectrum by a synchrotron self-Compton component produced by an electron distribution with index p = 2.2. Assuming that the power-law electron distribution extends down to \u03b3 min = 1 and that there is one proton per electron, an unrealistically high total jet power of L_p ~ 10^(47) erg s^(\u22121) is inferred. This can be reduced by two orders of magnitude either by considering a significant presence of electron\u2013positron pairs with lepton-to-proton ratio n_(e + e-)/n_p ~ 30, or by introducing an additional, low-energy break in the electron energy distribution at the electron Lorentz factor \u03b3_(br1) ~ 100. In either case, the jet composition is expected to be strongly matter-dominated.",
"date": "2016-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "831",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 142",
"id_number": "CaltechAUTHORS:20161104-080424476",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161104-080424476",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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{
"agency": "Department of Energy (DOE)"
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{
"agency": "Commissariat \u00e0 l'Energie Atomique (CEA)"
},
{
"agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)"
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{
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{
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{
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{
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{
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{
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{
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{
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{
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"grant_number": "2015/18/E/ST9/00580"
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{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
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{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
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{
"agency": "Institut de recherche sur les lois fondamentales de l'Univers (Irfu)"
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{
"agency": "Swedish National Space Board (SNSB)"
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"title": "The NuSTAR Extragalactic Surveys: The Number Counts of Active Galactic Nuclei and the Resolved Fraction of the Cosmic X-ray Background",
"ispublished": "pub",
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"keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 galaxies: Seyfert \u2013 surveys \u2013 X-rays: diffuse background \u2013 X-rays: galaxies",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 October 29; revised 2016 August 23; accepted 2016 August 24; published 2016 November 7. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J.A. acknowledges support from ERC Advanced Grant FEEDBACK at the University of Cambridge and a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University.\n\nPublished - Harrison_2016_ApJ_831_185.pdf
Submitted - 1511.04183v1.pdf
",
"abstract": "We present the 3\u20138 keV and 8\u201324 keV number counts of active galactic nuclei (AGNs) identified in the Nuclear Spectroscopic Telescope Array (NuSTAR) extragalactic surveys. NuSTAR has now resolved 33%\u201339% of the X-ray background in the 8\u201324 keV band, directly identifying AGNs with obscuring columns up to ~10^(25) cm^(-2). In the softer 3\u20138 keV band the number counts are in general agreement with those measured by XMM-Newton and Chandra over the flux range 5 x 10^(-15) \u227eS(3\u20138 keV)/erg s^(-1) cm^(-2) \u227e10^(-12) probed by NuSTAR. In the hard 8\u201324 keV band NuSTAR probes fluxes over the range 2 x 10^(-14) \u227e S(8\u201324 keV)/ erg s^(-1) cm^(-2) \u227e 10^_12), a factor ~100 fainter than previous measurements. The 8\u201324 keV number counts match predictions from AGN population synthesis models, directly confirming the existence of a population of obscured and/or hard X-ray sources inferred from the shape of the integrated cosmic X-ray background. The measured NuSTAR counts lie significantly above simple extrapolation with a Euclidian slope to low flux of the Swift/BAT 15\u201355 keV number counts measured at higher fluxes (S(15\u201355 keV) \u227310^(\u221211) erg s^(-1) cm^(-2)), reflecting the evolution of the AGN population between the Swift/BAT local (z < 0.1) sample and NuSTAR's z ~ 1 sample. CXB synthesis models, which account for AGN evolution, lie above the Swift/BAT measurements, suggesting that they do not fully capture the evolution of obscured AGNs at low redshifts.",
"date": "2016-11-10",
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},
"orcid": "0000-0003-0624-3276"
},
{
"id": "Pitchford-K",
"name": {
"family": "Pitchford",
"given": "Kate"
}
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William"
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: evolution; galaxies: individual (IRAS 09104+4109); galaxies: Seyfert; galaxies: starburst; infrared: galaxies; X-rays: galaxies",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 February 22; revised 2016 June 14; accepted 2016 June 14; published 2016 October 27. \n\nWe thank the referee for a very helpful report. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Part of this work is based on archival data, software, and online services provided by the ASDC. This research has made use of NASA's Astrophysics Data System. We acknowledge support from the NASA Earth and Space Science Fellowship Program grant NNX14AQ07H (M.B.), CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., C.R.), FONDECYT Regular 1141218 (F.E.B., C.R.), \"EMBIGGEN\" Anillo ACT1101 (F.E.B., C.R.), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.). A.C.F. acknowledges ERC Advanced Grant Feedback 340442. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - , Suzaku - , Chandra - , Spitzer - , Herschel - , Palomar - .\n\nPublished - Farrah_2016_ApJ_831_76.pdf
",
"abstract": "We study the geometry of the active galactic nucleus (AGN) obscurer in IRAS 09104+4109, an IR-luminous, radio-intermediate FR-I source at z = 0.442, using infrared data from Spitzer and Herschel, X-ray data from NuSTAR, Swift, Suzaku, and Chandra, and an optical spectrum from Palomar. The infrared data imply a total rest-frame 1\u20131000 \u03bcm luminosity of 5.5 \u00d7 10^(46) erg s^(\u22121) and require both an AGN torus and a starburst model. The AGN torus has an anisotropy-corrected IR luminosity of 4.9 \u00d7 10^(46) erg s^(\u22121) and a viewing angle and half-opening angle both of approximately 36\u00b0 from pole-on. The starburst has a star formation rate of (110 \u00b1 34) M_\u2299 yr^(\u22121) and an age of <50 Myr. These results are consistent with two epochs of luminous activity in IRAS 09104+4109: one approximately 150 Myr ago, and one ongoing. The X-ray data suggest a photon index of \u0393 \u2243 1.8 and a line-of-sight column density of N_H \u2243 5 \u00d7 10^(23) cm^(\u22122). This argues against a reflection-dominated hard X-ray spectrum, which would have implied a much higher N_H and luminosity. The X-ray and infrared data are consistent with a bolometric AGN luminosity of L(bol) ~ (0.5\u20132.5) \u00d7 10^(47) erg s^(\u22121). The X-ray and infrared data are further consistent with coaligned AGN obscurers in which the line of sight \"skims\" the torus. This is also consistent with the optical spectra, which show both coronal iron lines and broad lines in polarized but not direct light. Combining constraints from the X-ray, optical, and infrared data suggest that the AGN obscurer is within a vertical height of 20 pc, and a radius of 125 pc, of the nucleus.",
"date": "2016-11-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "831",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 76",
"id_number": "CaltechAUTHORS:20161027-143757170",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161027-143757170",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Basal-CATA PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
}
]
},
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"doi": "10.3847/0004-637X/831/1/76",
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},
"pub_year": "2016",
"author_list": "Farrah, Duncan; Balokovi\u0107, Mislav; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-18 23:55:10",
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"items": [
{
"id": "Strader-J",
"name": {
"family": "Strader",
"given": "Jay"
},
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},
{
"id": "Li-Kwan-Lok",
"name": {
"family": "Li",
"given": "Kwan-Lok"
},
"orcid": "0000-0001-8229-2024"
},
{
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"name": {
"family": "Chomiuk",
"given": "Laura"
},
"orcid": "0000-0002-8400-3705"
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{
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"name": {
"family": "Heinke",
"given": "Craig O."
},
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},
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"id": "Udalski-A",
"name": {
"family": "Udalski",
"given": "Andrzej"
},
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},
{
"id": "Peacock-M",
"name": {
"family": "Peacock",
"given": "Mark"
},
"orcid": "0000-0001-9767-8499"
},
{
"id": "Shishokovsky-L",
"name": {
"family": "Shishkovsky",
"given": "Laura"
}
},
{
"id": "Tremou-E",
"name": {
"family": "Tremou",
"given": "Evangelia"
},
"orcid": "0000-0002-4039-6703"
}
]
},
"title": "A new \u03b3-ray loud, eclipsing low-mass X-ray binary",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: spectroscopic \u2013 pulsars: general \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 July 27; revised 2016 August 5; accepted 2016 August 11; published 2016 October 28. \n\nWe thank an anonymous referee for helpful comments that improved the paper. We thank C. C. Cheung, R. Corbet, T. Maccarone, D. Nidever, T. Tauris, and L. van Haaften for useful conversations, F. Walter for providing routines and advice for the reduction of ANDICAM photometry, and R. J. Foley and Y-C. Pan for data acquisition. This project made use of NuSTAR mission data, a project led by the California Institute of Technology and managed by the Jet Propulsion Laboratory. We sincerely thank F. Harrison, K. Forster, and the NuSTAR team for scheduling and executing the NuSTAR observations. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist\u00e9rio da Ci\u00eancia, Tecnologia, e Inova\u00e7\u00e3o (MCTI) da Rep\u00fablica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. We acknowledge the use of public data from the Swift data archive. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. Support from NASA grant NNX15AU83G is gratefully acknowledged.\n\nSubmitted - 1608.02583v3.pdf
",
"abstract": "We report the discovery of an eclipsing low-mass X-ray binary at the center of the 3FGL error ellipse of the unassociated Fermi/Large Area Telescope \u03b3-ray source 3FGL J0427.9\u20136704. Photometry from OGLE and the SMARTS 1.3 m telescope and spectroscopy from the SOAR telescope have allowed us to classify the system as an eclipsing low-mass X-ray binary (P = 8.8 hr) with a main-sequence donor and a neutron-star accretor. Broad double-peaked H and He emission lines suggest the ongoing presence of an accretion disk. Remarkably, the system shows separate sets of absorption lines associated with the accretion disk and the secondary, and we use their radial velocities to find evidence for a massive (~1.8\u20131.9 M\u2299) neutron-star primary. In addition to a total X-ray eclipse with a duration of ~2200 s observed with NuSTAR, the X-ray light curve also shows properties similar to those observed among known transitional millisecond pulsars: short-term variability, a hard power-law spectrum (\u0393 ~ 1.7), and a comparable 0.5\u201310 keV luminosity (~2.4 x 10^(33) erg s^(\u22121)). We find tentative evidence for a partial (~60%) \u03b3-ray eclipse at the same phase as the X-ray eclipse, suggesting the \u03b3-ray emission may not be confined to the immediate region of the compact object. The favorable inclination of this binary is promising for future efforts to determine the origin of \u03b3-rays among accreting neutron stars.",
"date": "2016-11-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "831",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 89",
"id_number": "CaltechAUTHORS:20160816-122133622",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160816-122133622",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
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"doi": "10.3847/0004-637X/831/1/89",
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"pub_year": "2016",
"author_list": "Strader, Jay; Li, Kwan-Lok; et el."
},
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"items": [
{
"id": "Sbarrato-T",
"name": {
"family": "Sbarrato",
"given": "T."
}
},
{
"id": "Ghisellini-G",
"name": {
"family": "Ghisellini",
"given": "G."
}
},
{
"id": "Tagliaferri-G",
"name": {
"family": "Tagliaferri",
"given": "G."
}
},
{
"id": "Perri-M",
"name": {
"family": "Perri",
"given": "M."
}
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{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G. M."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Extremes of the jet-accretion power relation of blazars, as explored by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active quasars: general quasars: individual: B0222+185 quasars: individual: S5 0014+813 X-rays: general",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 July 14. Received 2016 July 12; in original form 2016 April 1. First published online July 18, 2016. \n\nWe thank the referee for her/his comments, that helped us to improve the paper. We acknowledge financial support from the ASI-INAF grant I/037/12/0. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software and calibration teams for support with the execution and analysis of these observations. This research has made also use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Part of this work is based on archival data, software or online services provided by the ASDC. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy.\n\nPublished - MNRAS-2016-Sbarrato-1542-50.pdf
Submitted - 1510.08849v1.pdf
",
"abstract": "Hard X-ray observations are crucial to study the non-thermal jet emission from high-redshift, powerful blazars. We observed two bright z > 2 flat-spectrum radio quasars (FSRQs) in hard X-rays to explore the details of their relativistic jets and their possible variability. S5 0014+81 (at z = 3.366) and B0222+185 (at z = 2.690) have been observed twice by the Nuclear Spectroscopic Telescope Array (NuSTAR) simultaneously with Swift/X-ray Telescope, showing different variability behaviours. We found that NuSTAR is instrumental to explore the variability of powerful high-redshift blazars, even when no \u03b3-ray emission is detected. The two sources have proven to have respectively the most luminous accretion disc and the most powerful jet among known blazars. Thanks to these properties, they are located at the extreme end of the jet\u2013accretion disc relation previously found for \u03b3\u2013ray detected blazars, to which they are consistent.",
"date": "2016-10-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "462",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1542-1550",
"id_number": "CaltechAUTHORS:20160128-140129459",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-140129459",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"id": "2015-70",
"name": "Space Radiation Laboratory"
}
]
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{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
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},
"doi": "10.1093/mnras/stw1730",
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}
],
"pub_year": "2016",
"author_list": "Sbarrato, T.; Ghisellini, G.; et el."
},
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"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
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"given": "D."
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"family": "Gusinskaia",
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"title": "Disk reflection and a possible disk wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9-342058",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion: accretion disks \u2013 stars: individual (1RXS J180408.9\u2013342058) \u2013 stars:\nneutron \u2013 stars: winds, outflows \u2013 X-rays: binaries",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 June 30. Received 2016 June 30; in original form 2016 May 4. Published: 04 July 2016. \n\nWe are grateful to Belinda Wilkes, Fiona Harrison, Neil Gehrels and the Chandra, NuSTAR and Swift teams for carrying out these DDT observations. We thank the anonymous referee for constructive comments. ND thanks Ciro Pinto, Matt Middleton and Anne Lohfink for useful discussions. ND is supported by an NWO/Vidi grant and an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2013-IEF-627148. DA acknowledges support from the Royal Society. JCAMJ is supported by an Australian Research Council (ARC) Future Fellowship (FT140101082) and an ARC Discovery Grant (DP120102393). RW and AP are supported by an NWO/TOP grant, module 1, awarded to RW. COH is supported by an NSERC Discovery Grant. ATD is supported by an NWO/Veni grant. JWTH is supported by NWO/Vidi and ERC/starting (337062) grants.\n\nSubmitted - 1607.01780v1.pdf
",
"abstract": "1RXS J180408.9\u2013342058 is a transient neutron star low-mass X-ray binary that exhibited a bright accretion outburst in 2015. We present NuSTAR, Swift, and Chandra observations obtained around the peak brightness of this outburst. The source was in a soft X-ray spectral state and displayed an X-ray luminosity of L_X \u2243 (2\u20133) \u00d7 10^(37)(D/5.8\u2009kpc)^2\u2009erg\u2009s^(\u22121) (0.5\u201310 keV). The NuSTAR data reveal a broad Fe\u2013K emission line that we model as relativistically broadened reflection to constrain the accretion geometry. We found that the accretion disc is viewed at an inclination of i \u2243 27\u00b0\u201335\u00b0 and extended close to the neutron star, down to R_(in) \u2243 5\u20137.5 gravitational radii (\u224311\u201317 km). This inner disc radius suggests that the neutron star magnetic field strength is B \u2272 2 \u00d7 10^8 G. We find a narrow absorption line in the Chandra/HEG data at an energy of \u22437.64 keV with a significance of \u22434.8\u03c3. This feature could correspond to blueshifted Fe XXVI and arise from an accretion disc wind, which would imply an outflow velocity of v_(out) \u2243 0.086c (\u224325 800\u2009km\u2009s^(\u22121)). However, this would be extreme for an X-ray binary and it is unclear if a disc wind should be visible at the low inclination angle that we infer from our reflection analysis. Finally, we discuss how the X-ray and optical properties of 1RXS J180408.9\u2013342058 are consistent with a relatively small (P_(orb) \u2272 3 h) binary orbit.",
"date": "2016-10-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "461",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4049-4058",
"id_number": "CaltechAUTHORS:20160708-151940241",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160708-151940241",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
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"id": "NuSTAR"
}
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"doi": "10.1093/mnras/stw1593",
"primary_object": {
"basename": "1607.01780v1.pdf",
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},
"pub_year": "2016",
"author_list": "Degenaar, N.; Altamirano, D.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/47dmq-xcs04",
"eprint_id": 70639,
"eprint_status": "archive",
"datestamp": "2023-08-22 18:44:35",
"lastmod": "2023-10-20 23:17:19",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Davis-S-W",
"name": {
"family": "Davis",
"given": "Shane W."
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "Matthew"
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tao-Lian",
"name": {
"family": "Tao",
"given": "Lian"
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "A broadband X-ray spectral study of the intermediate-mass black hole candidate M82 X-1 with NuSTAR, Chandra and Swift",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; X-rays: binaries; X-rays: individual (M82 X-1)",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 June 2; revised 2016 July 11; accepted 2016 July 13; published 2016 September 20. \n\nThis work made use of Director's Discretionary Time on Chandra, for which we thank Belinda Wilkes for approving and the Chandra X-ray Center for implementing. We also use Director's Discretionary Time on NuSTAR, for which we thank Fiona Harrison for approving and the NuSTAR SOC for co-ordinating with Chandra. The NuSTAR mission is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.Z. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 617001. \n\nFacilities: Chandra (ACIS) - , NuSTAR - , Swift (XRT).\n\nPublished - apj_829_1_28.pdf
Submitted - 1607.03903v1.pdf
",
"abstract": "M82 X-1 is one of the brightest ultraluminous X-ray sources (ULXs) known, which, assuming Eddington-limited accretion and other considerations, makes it one of the best intermediate-mass black-hole (IMBH) candidates. However, the ULX may still be explained by super-Eddington accretion onto a stellar remnant black hole. We present simultaneous NuSTAR, Chandra, and Swift/XRT observations during the peak of a flaring episode with the aim of modeling the emission of M82 X-1 and yielding insights into its nature. We find that thin accretion disk models all require accretion rates at or above the Eddington limit in order to reproduce the spectral shape, given a range of black-hole masses and spins. Since at these high Eddington ratios the thin-disk model breaks down due to radial advection in the disk, we discard the results of the thin-disk models as unphysical. We find that the temperature profile as a function of disk radius (T(r) \u221d r^(-p)) is significantly flatter (p = 0.55_(-0.04)^(+0.07)) than expected for a standard thin disk (p = 0.75). A flatter profile is instead characteristic of a slim disk, which is highly suggestive of super-Eddington accretion. Furthermore, radiation hydrodynamical simulations of super-Eddington accretion have shown that the predicted spectra of these systems are very similar to what we observe for M82 X-1. We therefore conclude that M82 X-1 is a super-Eddington accretor. Our mass estimates inferred from the inner disk radius imply a stellar remnant black hole (M_(BH) = 26_(-6)^(+9 M_\u2299) when assuming zero spin and face-on inclination, or an IMBH for maximal spin and a highly inclined disk.",
"date": "2016-09-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "829",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 28",
"id_number": "CaltechAUTHORS:20160928-115009615",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160928-115009615",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "617001"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/0004-637X/829/1/28",
"primary_object": {
"basename": "1607.03903v1.pdf",
"url": "https://authors.library.caltech.edu/records/47dmq-xcs04/files/1607.03903v1.pdf"
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"related_objects": [
{
"basename": "apj_829_1_28.pdf",
"url": "https://authors.library.caltech.edu/records/47dmq-xcs04/files/apj_829_1_28.pdf"
}
],
"pub_year": "2016",
"author_list": "Brightman, Murray; Harrison, Fiona A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/fbq52-zfn22",
"eprint_id": 69450,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:51:17",
"lastmod": "2023-10-20 19:04:15",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Archibald-R-F",
"name": {
"family": "Archibald",
"given": "R. F."
},
"orcid": "0000-0002-4017-8837"
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "V. M."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "S. P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "Scholz-P",
"name": {
"family": "Scholz",
"given": "P."
},
"orcid": "0000-0002-7374-7119"
}
]
},
"title": "A Magnetar-like Outburst from a High-B Radio Pulsar",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: general \u2013 pulsars: individual (PSR J1119-6127) \u2013 stars: magnetars",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 August 2; revised 2016 August 30; accepted 2016 August 30; published 2016 September 21. \n\nThe authors thank the operations teams of NuSTAR, particularly Karl Forster, and Swift for their speed and flexibility scheduling these observations. We thank the Fermi LAT Collaboration for the public data and tools used in this work. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the NASA. We acknowledge the use of public data from the Swift data archive. R.F.A. acknowledges support from an NSERC CGSD. V.M.K. receives support from an NSERC Discovery Grant, an Accelerator Supplement and from the Gerhard Herzberg Award, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. S.P.T. acknowledges support from a McGill Astrophysics postdoctoral fellowship. P.S. acknowledges support from a Schulich Graduate Fellowship.\n\nSubmitted - 1608.01007v1.pdf
",
"abstract": "Radio pulsars are believed to have their emission powered by the loss of rotational kinetic energy. By contrast, magnetars show intense X-ray and \u03b3-ray radiation whose luminosity greatly exceeds that due to spin down and magnetar luminosity is believed to be powered by intense internal magnetic fields. A basic prediction of this picture is that radio pulsars of high magnetic field should show magnetar-like emission. Here we report on a magnetar-like X-ray outburst from the radio pulsar PSR J1119\u20136127, heralded by two short bright X-ray bursts on 2016 July 27 and 28. Using target of opportunity data from the Swift X-ray Telescope and NuSTAR, we show that this pulsar's flux has brightened by a factor of >160 in the 0.5\u201310 keV band, and that its previously soft X-ray spectrum has undergone a strong hardening with strong pulsations appearing for the first time above 2.5 keV, with phase-averaged emission detectable up to 25 keV. By comparing Swift-XRT and NuSTAR timing data with a pre-outburst ephemeris derived from Fermi Large Area Telescope data, we find that the source has contemporaneously undergone a large spin-up glitch of amplitude \u0394\u03bd/\u03bd = 5.74(8) x 10^(-6). The collection of phenomena observed thus far in this outburst strongly mirrors those in most magnetar outbursts and provides an unambiguous connection between the radio pulsar and magnetar populations.",
"date": "2016-09-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "829",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L21",
"id_number": "CaltechAUTHORS:20160804-143354943",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160804-143354943",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8205/829/1/L21",
"primary_object": {
"basename": "1608.01007v1.pdf",
"url": "https://authors.library.caltech.edu/records/fbq52-zfn22/files/1608.01007v1.pdf"
},
"pub_year": "2016",
"author_list": "Archibald, R. F.; Kaspi, V. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/g5b7j-a4t28",
"eprint_id": 68501,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:46:59",
"lastmod": "2023-10-19 22:14:42",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Mondal-A-S",
"name": {
"family": "Mondal",
"given": "Aditya S."
}
},
{
"id": "Dewangan-G-C",
"name": {
"family": "Dewangan",
"given": "G. C."
}
},
{
"id": "Pahari-M",
"name": {
"family": "Pahari",
"given": "M."
}
},
{
"id": "Misra-R",
"name": {
"family": "Misra",
"given": "R."
}
},
{
"id": "Kembhavi-A-K",
"name": {
"family": "Kembhavi",
"given": "A. K."
}
},
{
"id": "Raychaudhuri-B",
"name": {
"family": "Raychaudhuri",
"given": "B."
}
}
]
},
"title": "Broad-band X-ray emission and the reality of the broad iron line from the neutron star\u2013white dwarf X-ray binary 4U 1820\u221230",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: individual: 4U 1820\u221230 \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 June 16. Received 2016 June 16; in original form 2015 September 8. Published: 20 June 2016. \n\nWe are thankful to the anonymous referee whose detail in-depth comments helped us in improving the paper. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Centre (HEASARC). ASM would like to thank Inter-University Centre for Astronomy and Astrophysics (IUCAA) for hosting him during subsequent visits. BR likes to thank IUCAA for hospitality and other facilities extended to him during his visit under their visiting Associateship programme.\n\nAccepted Version - 1606.05307v1.pdf
",
"abstract": "Broad relativistic iron lines from neutron star X-ray binaries are important probes of the inner accretion disc. The X-ray reflection features can be weakened due to strong magnetic fields or very low iron abundances such as is possible in X-ray binaries with low mass, first generation stars as companions. Here, we investigate the reality of the broad iron line detected earlier from the neutron-star low-mass X-ray binary 4U 1820\u221230 with a degenerate helium dwarf companion. We perform a comprehensive, systematic broad-band spectral study of the atoll source using Suzaku and simultaneous NuSTAR and Swift observations. We have used different continuum models involving accretion disc emission, thermal blackbody and thermal Comptonization of either disc or blackbody photons. The Suzaku data show positive and negative residuals in the region of Fe K band. These features are well described by two absorption edges at 7.67 \u00b1 0.14\u2009keV and 6.93 \u00b1 0.07\u2009keV or partial covering photoionized absorption or by blurred reflection. Though, the simultaneous Swift and NuSTAR data do not clearly reveal the emission or absorption features, the data are consistent with the presence of either absorption or emission features. Thus, the absorption based models provide an alternative to the broad iron line or reflection model. The absorption features may arise in winds from the inner accretion disc. The broad-band spectra appear to disfavour continuum models in which the blackbody emission from the neutron-star surface provides the seed photons for thermal Comptonization. Our results suggest emission from a thin accretion disc (kT_(disc) \u223c 1\u2009keV), Comptonization of disc photons in a boundary layer most likely covering a large fraction of the neutron-star surface and innermost parts of the accretion disc, and blackbody emission (kT_(bb) \u223c 2\u2009keV) from the polar regions.",
"date": "2016-09-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "461",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1917-1926",
"id_number": "CaltechAUTHORS:20160620-070445495",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160620-070445495",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw1464",
"primary_object": {
"basename": "1606.05307v1.pdf",
"url": "https://authors.library.caltech.edu/records/g5b7j-a4t28/files/1606.05307v1.pdf"
},
"pub_year": "2016",
"author_list": "Mondal, Aditya S.; Dewangan, G. C.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/b5amr-d5h71",
"eprint_id": 69177,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:47:07",
"lastmod": "2023-10-20 16:37:28",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ingram-A",
"name": {
"family": "Ingram",
"given": "Adam"
},
"orcid": "0000-0002-5311-9078"
},
{
"id": "van-der-Klis-M",
"name": {
"family": "van der Klis",
"given": "Michiel"
},
"orcid": "0000-0003-0070-9872"
},
{
"id": "Middleton-M",
"name": {
"family": "Middleton",
"given": "Matthew"
}
},
{
"id": "Done-C",
"name": {
"family": "Done",
"given": "Chris"
}
},
{
"id": "Altamirano-D",
"name": {
"family": "Altamirano",
"given": "Diego"
},
"orcid": "0000-0002-3422-0074"
},
{
"id": "Heil-L",
"name": {
"family": "Heil",
"given": "Lucy"
}
},
{
"id": "Uttley-P",
"name": {
"family": "Uttley",
"given": "Phil"
}
},
{
"id": "Axelsson-M",
"name": {
"family": "Axelsson",
"given": "Magnus"
}
}
]
},
"title": "A quasi-periodic modulation of the iron line centroid energy in the \n black hole binary H 1743-322",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013 relativistic processes \u2013 X-rays: individual: H1743\u2212322",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 May 19. Received 2016 May 19; in original form 2016 April 15. Published: 25 May 2016. \n\nAI acknowledges support from the Netherlands Organisation for Scientific Research (NWO) Veni Fellowship, grant number 639.041.437. He thanks Martin Heemskerk for assistance making the plots in this paper. He also acknowledges useful conversations with Dom Walton, Matteo Bachetti and Brian Grefenstette about NuSTAR data reduction, and useful conversations with Andrew King about disc warping. MJM appreciates support via an STFC Ernest Rutherford Fellowship. CD acknowledges support from the STFC consolidated grant ST/L00075X/1. DA acknowledges support from the Royal Society. MA is an International Research Fellow of the Japan Society for the Promotion of Science. We thank the anonymous referee for constructive comments.\n\nSubmitted - 1607.02866v1.pdf
",
"abstract": "Accreting stellar-mass black holes often show a 'Type-C' quasi-periodic oscillation (QPO) in their X-ray flux and an iron emission line in their X-ray spectrum. The iron line is generated through continuum photons reflecting off the accretion disc, and its shape is distorted by relativistic motion of the orbiting plasma and the gravitational pull of the black hole. The physical origin of the QPO has long been debated, but is often attributed to Lense\u2013Thirring precession, a General Relativistic effect causing the inner flow to precess as the spinning black hole twists up the surrounding space\u2013time. This predicts a characteristic rocking of the iron line between red- and blueshift as the receding and approaching sides of the disc are respectively illuminated. Here we report on XMM\u2013Newton and NuSTAR observations of the black hole binary H1743\u2212322 in which the line energy varies systematically over the \u223c4 s QPO cycle (3.70\u03c3 significance), as predicted. This provides strong evidence that the QPO is produced by Lense\u2013Thirring precession, constituting the first detection of this effect in the strong gravitation regime. There are however elements of our results harder to explain, with one section of data behaving differently than all the others. Our result enables the future application of tomographic techniques to map the inner regions of black hole accretion discs.",
"date": "2016-09-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "461",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1967-1980",
"id_number": "CaltechAUTHORS:20160722-150519999",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160722-150519999",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw1245",
"primary_object": {
"basename": "1607.02866v1.pdf",
"url": "https://authors.library.caltech.edu/records/b5amr-d5h71/files/1607.02866v1.pdf"
},
"pub_year": "2016",
"author_list": "Ingram, Adam; van der Klis, Michiel; et el."
},
{
"id": "https://authors.library.caltech.edu/records/9rerp-saa27",
"eprint_id": 69176,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:41:24",
"lastmod": "2023-10-20 16:37:22",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Rea-N",
"name": {
"family": "Rea",
"given": "N."
},
"orcid": "0000-0003-2177-6388"
},
{
"id": "Borghese-A",
"name": {
"family": "Borghese",
"given": "A."
},
"orcid": "0000-0001-8785-5922"
},
{
"id": "Esposito-P",
"name": {
"family": "Esposito",
"given": "P."
},
"orcid": "0000-0003-4849-5092"
},
{
"id": "Coti-Zelati-F",
"name": {
"family": "Coti Zelati",
"given": "F."
},
"orcid": "0000-0001-7611-1581"
},
{
"id": "Bashetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Israel-G-L",
"name": {
"family": "Israel",
"given": "G. L."
}
},
{
"id": "De-Luca-A",
"name": {
"family": "De Luca",
"given": "A."
}
}
]
},
"title": "Magnetar-like activity from the central compact object in the SNR RCW103",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: individual (1E 161348\u20135055) \u2013 stars: neutron \u2013 X-rays: stars",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 July 13; revised 2016 August 12; accepted 2016 August 12; published 2016 August 29. \n\nWe are grateful to Dr. Belinda Wilkes and Dr. Fiona Harrison for accepting our Director Discretionary Time requests, and to the Chandra and NuSTAR teams for the large efforts in scheduling these simultaneous observations on such a short timescale. We also acknowledge the Swift team for promptly announce new transient events, allowing rapid follow-up observations. N.R., A.B., P.E., and F.C.Z. acknowledge funding in the framework of the NWO Vidi award A.2320.0076 (PI: N. Rea), and via the European COST Action MP1304 (NewCOMPSTAR). N.R. is also supported by grants AYA2015-71042-P and SGR2014-1073. We acknowledge J. Pons and J. Elfritz for useful discussions and valuable comments, and the referee for suggestions.\n\nSubmitted - 1607.04107v1.pdf
",
"abstract": "The 6.67 hr periodicity and the variable X-ray flux of the central compact object (CCO) at the center of the supernova remnant RCW 103, named 1E 161348\u20135055, have been always difficult to interpret within the standard scenarios of an isolated neutron star (NS) or a binary system. On 2016 June 22, the Burst Alert Telescope (BAT) on board Swift detected a magnetar-like short X-ray burst from the direction of 1E 161348\u20135055, also coincident with a large long-term X-ray outburst. Here, we report on Chandra, Nuclear Spectroscopic Telescope Array, and Swift (BAT and XRT) observations of this peculiar source during its 2016 outburst peak. In particular, we study the properties of this magnetar-like burst, we discover a hard X-ray tail in the CCO spectrum during outburst, and we study its long-term outburst history (from 1999 to 2016 July). We find the emission properties of 1E 161348\u20135055 consistent with it being a magnetar. However, in this scenario, the 6.67 hr periodicity can only be interpreted as the rotation period of this strongly magnetized NS, which therefore represents the slowest pulsar ever detected, by orders of magnitude. We briefly discuss the viable slow-down scenarios, favoring a picture involving a period of fall-back accretion after the supernova explosion, similarly to what is invoked (although in a different regime) to explain the \"anti-magnetar\" scenario for other CCOs.",
"date": "2016-09-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "828",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L13",
"id_number": "CaltechAUTHORS:20160722-150054988",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160722-150054988",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/2041-8205/828/1/L13",
"primary_object": {
"basename": "1607.04107v1.pdf",
"url": "https://authors.library.caltech.edu/records/9rerp-saa27/files/1607.04107v1.pdf"
},
"pub_year": "2016",
"author_list": "Rea, N.; Borghese, A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/bkb83-x4372",
"eprint_id": 77611,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:43:39",
"lastmod": "2023-10-25 23:17:58",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Jaisawal-G-K",
"name": {
"family": "Jaisawal",
"given": "Gaurava K."
},
"orcid": "0000-0002-6789-2723"
},
{
"id": "Naik-S",
"name": {
"family": "Naik",
"given": "Sachindra"
},
"orcid": "0000-0003-2865-4666"
}
]
},
"title": "Detection of Cyclotron Resonance Scattering Feature in High Mass X-ray Binary Pulsar SMC X-2",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: neutron \u2013 pulsars: individual: SMC X-2 \u2013 X-rays: stars",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 May 23. Received 2016 May 23; in original form 2016 May 4. Published: 25 May 2016.\n\nWe sincerely thank the referee for his/her valuable comments and suggestions which improved the Letter. The research work at Physical Research Laboratory is funded by the Department of Space, Government of India. The authors would like to thank all the NuSTAR and Swift team members for ToO observations. This research has made use of data from HEASARC Online Service, and the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nAccepted Version - 1705.05544.pdf
",
"abstract": "We report broad-band spectral properties of the high-mass X-ray binary pulsar SMC X-2 by using three simultaneous Nuclear Spectroscopy Telescope Array and Swift/XRT observations during its 2015 outburst. The pulsar was significantly bright, reaching a luminosity up to as high as \u223c5.5 \u00d7 10^(38) erg s^(\u22121) in 1\u201370 keV range. Spin period of the pulsar was estimated to be 2.37 s. Pulse profiles were found to be strongly luminosity dependent. The 1\u201370 keV energy spectrum of the pulsar was well described with three different continuum models such as (i) negative and positive power law with exponential cutoff, (ii) Fermi-Dirac cutoff power law and (iii) cutoff power-law models. Apart from the presence of an iron line at \u223c6.4 keV, a model independent absorption like feature at \u223c27 keV was detected in the pulsar spectrum. This feature was identified as a cyclotron absorption line and detected for the first time in this pulsar. Corresponding magnetic field of the neutron star was estimated to be \u223c2.3 \u00d7 10^(12) G. The cyclotron line energy showed a marginal negative dependence on the luminosity. The cyclotron line parameters were found to be variable with pulse phase and interpreted as due to the effect of emission geometry or complicated structure of the pulsar magnetic field.",
"date": "2016-09-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "461",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L97-L101",
"id_number": "CaltechAUTHORS:20170520-161330425",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170520-161330425",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/slw108",
"primary_object": {
"basename": "1705.05544.pdf",
"url": "https://authors.library.caltech.edu/records/bkb83-x4372/files/1705.05544.pdf"
},
"pub_year": "2016",
"author_list": "Jaisawal, Gaurava K. and Naik, Sachindra"
},
{
"id": "https://authors.library.caltech.edu/records/qw8mx-qdx98",
"eprint_id": 70399,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:35:53",
"lastmod": "2023-10-20 22:55:30",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Husemann-B",
"name": {
"family": "Husemann",
"given": "B."
},
"orcid": "0000-0003-2901-6842"
},
{
"id": "Urrutia-T",
"name": {
"family": "Urrutia",
"given": "T."
},
"orcid": "0000-0001-6746-9936"
},
{
"id": "Tremblay-G-R",
"name": {
"family": "Tremblay",
"given": "G. R."
}
},
{
"id": "Krumpe-M",
"name": {
"family": "Krumpe",
"given": "M."
}
},
{
"id": "Dexter-J",
"name": {
"family": "Dexter",
"given": "J."
},
"orcid": "0000-0003-3903-0373"
},
{
"id": "Busch-G",
"name": {
"family": "Busch",
"given": "G."
}
},
{
"id": "Combes-F",
"name": {
"family": "Combes",
"given": "F."
},
"orcid": "0000-0003-2658-7893"
},
{
"id": "Croom-S-M",
"name": {
"family": "Croom",
"given": "S. M."
},
"orcid": "0000-0003-2880-9197"
},
{
"id": "Davis-T-A",
"name": {
"family": "Davis",
"given": "T. A."
}
},
{
"id": "Eckart-A",
"name": {
"family": "Eckart",
"given": "A."
}
},
{
"id": "McElroy-R-E",
"name": {
"family": "McElroy",
"given": "R. E."
}
},
{
"id": "P\u00e9rez-Torres-M-A",
"name": {
"family": "P\u00e9rez-Torres",
"given": "M."
}
},
{
"id": "Powell-M",
"name": {
"family": "Powell",
"given": "M."
}
},
{
"id": "Scharw\u00e4chter-J",
"name": {
"family": "Scharw\u00e4chter",
"given": "J."
}
}
]
},
"title": "The Close AGN Reference Survey (CARS) - What is causing Mrk 1018's return to the shadows after 30 years?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 galaxies: nuclei \u2013 galaxies: Seyfert \u2013 galaxies: individual: Mrk 1018",
"note": "\u00a9 2016 ESO.\n\nReceived: 4 July 2016;\nAccepted: 16 August 2016;\nPublished online 20 September 2016.\n\n\nBased on Cycle 17 DDT program (ID: 18789, PI: G. Tremblay) approved\nby the Chandra Director, Dr. Belinda Wilkes. Based on Cycle 23\nDDT project with the NASA/ESA Hubble Space Telescope (ID: 14486,\nPI: B. Husemann) approved by HST Director Dr. Kenneth Sembach.\n\nWe thank the anonymous referee for very constructive comments\nand suggestions that significantly helped to improve this Letter. GRT\nacknowledges support from the NASA through the Einstein Postdoctoral Fellowship\nAward Number PF-150128, issued by the Chandra X-ray Observatory\nCenter, which is operated by the Smithsonian Astrophysical Observatory for\nand on behalf of NASA under contract NAS8-03060. MK acknowledges support\nby DFG grant KR 3338/3-1. MAPT acknowledges support from the Spanish\nMINECO through grants AYA2012-38491-C02-02 and AYA2015-63939-\nC2-1-P. TAD acknowledges support from a Science and Technology Facilities\nCouncil Ernest Rutherford Fellowship. Parts of this research were conducted by\nthe Australian Research Council Centre of Excellence for All-sky Astrophysics\n(CAASTRO), through project number CE110001020.\n\nPublished - aa29245-16.pdf
",
"abstract": "We recently discovered that the active galactic nucleus (AGN) of Mrk 1018 has changed optical type again after 30 yr as a type 1 AGN. Here we combine Chandra, NuStar, Swift, Hubble Space Telescope and ground-based observations to explore the cause of this change. The 2\u201310\u2009keV flux declines by a factor of ~8 between 2010 and 2016. We show with our X-ray observation that this is not caused by varying neutral hydrogen absorption along the line-of-sight up to the Compton-thick level. The optical-UV spectral energy distributions are well fit with a standard geometrically thin optically thick accretion disc model that seems to obey the expected L ~ T^4 relation. It confirms that a decline in accretion disc luminosity is the primary origin for the type change. We detect a new narrow-line absorber in Ly\u03b1 blue-shifted by ~700\u2009km s^(-1) with respect to the systemic velocity of the galaxy. This new Ly\u03b1 absorber could be evidence for the onset of an outflow or a companion black hole with associated gas that could be related to the accretion rate change. However, the low column density of the absorber means that it is not the direct cause for Mrk 1018's changing-look nature.",
"date": "2016-09",
"date_type": "published",
"publication": "Astronomy & Astrophysics",
"volume": "593",
"publisher": "EDP Sciences",
"pagerange": "Art No. L9",
"id_number": "CaltechAUTHORS:20160916-110635722",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160916-110635722",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201629245",
"primary_object": {
"basename": "aa29245-16.pdf",
"url": "https://authors.library.caltech.edu/records/qw8mx-qdx98/files/aa29245-16.pdf"
},
"pub_year": "2016",
"author_list": "Husemann, B.; Urrutia, T.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/fvacf-2j790",
"eprint_id": 67428,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:27:57",
"lastmod": "2023-10-18 21:10:53",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Luangtip-W",
"name": {
"family": "Luangtip",
"given": "Wasutep"
}
},
{
"id": "Roberts-T-P",
"name": {
"family": "Roberts",
"given": "Timothy P."
},
"orcid": "0000-0001-8252-6337"
},
{
"id": "Done-C",
"name": {
"family": "Done",
"given": "Chris"
}
}
]
},
"title": "The X-ray spectral evolution of the ultraluminous X-ray source Holmberg IX X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013X-rays: binaries \u2013 X-rays: individual: Holmberg IX X-1",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 May 26. Received 2016 May 26; in original form 2015 September 24. Published: 30 May 2016. \n\nWe thank the anonymous referee for their comments, that have helped improve this paper. WL acknowledges financial support in the form of funding for a PhD studentship from the Royal Thai Government. TPR and CD thank STFC for support as part of the consolidated grant ST/L00075X/1. We also would like to thank Matthew Middleton and Dominic Walton for helpful discussions. This work is in part based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has also made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA).\n\nSubmitted - 1605.08246v1.pdf
Supplemental Material - stw1282_Supplementary_Data.zip
",
"abstract": "We present a new analysis of X-ray spectra of the archetypal ultraluminous X-ray source (ULX) Holmberg IX X-1 obtained by the Swift, XMM\u2013Newton and NuSTAR observatories. This ULX is a persistent source, with a typical luminosity of \u223c10^(40) erg s^(\u22121), that varied by a factor of 4\u20135 over eight years. We find that its spectra tend to evolve from relatively flat or two-component spectra in the medium energy band (1\u20136 keV), at lower luminosities, to a spectrum that is distinctly curved and disc-like at the highest luminosities, with the peak energy in the curved spectrum tending to decrease with increased luminosity. We argue that the spectral evolution of the ULX can be explained by super-Eddington accretion models, where in this case we view the ULX down the evacuated funnel along its rotation axis, bounded by its massive radiatively driven wind. The spectral changes then originate in enhanced geometric beaming as the accretion rate increases and wind funnel narrows, causing the scattered flux from the central regions of the supercritical flow to brighten faster than the isotropic thermal emission from the wind, and so the curved hard spectral component to dominate at the highest luminosities. The wind also Compton down-scatters photons at the edge of the funnel, resulting in the peak energy of the spectrum decreasing. We also confirm that Holmberg IX X-1 displays spectral degeneracy with luminosity, and suggest that the observed differences are naturally explained by precession of the black hole rotation axis for the suggested wind geometry.",
"date": "2016-08-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "460",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4417-4432",
"id_number": "CaltechAUTHORS:20160527-090731589",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-090731589",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Royal Thai Government"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw1282",
"primary_object": {
"basename": "1605.08246v1.pdf",
"url": "https://authors.library.caltech.edu/records/fvacf-2j790/files/1605.08246v1.pdf"
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"basename": "stw1282_Supplementary_Data.zip",
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}
],
"pub_year": "2016",
"author_list": "Luangtip, Wasutep; Roberts, Timothy P.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/2naak-kw015",
"eprint_id": 69708,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:27:30",
"lastmod": "2023-10-20 20:30:27",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Sleator-C-C",
"name": {
"family": "Sleator",
"given": "Clio C."
}
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "Ashley L."
}
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Chenevez-J",
"name": {
"family": "Chenevez",
"given": "J\u00e9r\u00f4me"
},
"orcid": "0000-0002-4397-8370"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel K."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A NuSTAR Observation of the Reflection Spectrum of the Low-mass X-Ray Binary 4U 1728-34",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 9; revised 2016 June 17; accepted 2016 June 25; published 2016 August 18. \n\nWe thank Michael Parker and Andy Fabian for the particular version of the reflionx model used in this analysis. We thank Kristin Madsen for her help identifying the calibration issue in the NuSTAR data between 3\u20134.5 keV. J.C. thanks ESA/PRODEX for financial support. This work is based on data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA.\n\nPublished - apj_827_2_134.pdf
Submitted - 1605.02137v2.pdf
",
"abstract": "We report on a simultaneous NuSTAR and Swift observation of the neutron star low-mass X-ray binary 4U 1728-34. We identified and removed four Type I X-ray bursts during the observation in order to study the persistent emission. The continuum spectrum is hard and described well by a blackbody with kT = 1.5 keV and a cutoff power law with \u0393 = 1.5, and a cutoff temperature of 25 keV. Residuals between 6 and 8 keV provide strong evidence of a broad Fe K\u03b1 line. By modeling the spectrum with a relativistically blurred reflection model, we find an upper limit for the inner disk radius of R_(in) \u2a7d 2R_(ISCO). Consequently, we find that R_(NS) \u2a7d 23 km, assuming M = 1.4 M_\u2299 and a = 0.15. We also find an upper limit on the magnetic field of B \u2a7d 2 \u00d7 10^8 G.",
"date": "2016-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "827",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 134",
"id_number": "CaltechAUTHORS:20160817-123809585",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160817-123809585",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA-PRODEX (Belgium)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/0004-637X/827/2/134",
"primary_object": {
"basename": "1605.02137v2.pdf",
"url": "https://authors.library.caltech.edu/records/2naak-kw015/files/1605.02137v2.pdf"
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"basename": "apj_827_2_134.pdf",
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}
],
"pub_year": "2016",
"author_list": "Sleator, Clio C.; Tomsick, John A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/e8abs-3tt54",
"eprint_id": 67950,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:21:46",
"lastmod": "2023-10-19 22:08:13",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Kataoka-Jun",
"name": {
"family": "Kataoka",
"given": "Jun"
},
"orcid": "0000-0003-2819-6415"
},
{
"id": "Stawarz-\u0141",
"name": {
"family": "Stawarz",
"given": "\u0141ukasz"
}
}
]
},
"title": "Inverse Compton X-Ray Emission from TeV Blazar Mrk 421 During a Historical Low-flux State Observed with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "acceleration of particles \u2013 BL Lacertae objects: individual (Mrk 421) \u2013 galaxies: active \u2013 galaxies: jets \u2013 radiation mechanisms: non-thermal",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 May 12; revised 2016 June 7; accepted 2016 June 10; published 2016 August 8. \n\n\u0141.S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083.\n\nSubmitted - 1606.03659v1.pdf
",
"abstract": "We report on the detection of excess hard X-ray emission from the TeV BL Lac object Mrk 421 during the historical low-flux state of the source in 2013 January. Nuclear Spectroscopic Telescope Array observations were conducted four times between MJD 56294 and MJD 56312 with a total exposure of 80.9 ks. The source flux in the 3\u201340 keV range was nearly constant, except for MJD 56307 when the average flux level increased by a factor of three. Throughout the exposure, the X-ray spectra of Mrk 421 were well represented by a steep power-law model with a photon index of \u0393 \u2243 3.1, although a significant excess was noted above 20 keV in the MJD 56302 data when the source was in its faintest state. Moreover, Mrk 421 was detected at more than the 4\u03c3 level in the 40\u201379 keV count maps for both MJD 56307 and MJD 56302 but not during the remaining two observations. The detected excess hard X-ray emission connects smoothly with the extrapolation of the high-energy \u03b3-ray continuum of the blazar constrained by Fermi-LAT during source quiescence. These findings indicate that while the overall X-ray spectrum of Mrk 421 is dominated by the highest-energy tail of the synchrotron continuum, the variable excess hard X-ray emission above 20 keV (on the timescale of a week) is related to the inverse Compton emission component. We discuss the resulting constraints on the variability and spectral properties of the low-energy segment of the electron energy distribution in the source.",
"date": "2016-08-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "827",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 55",
"id_number": "CaltechAUTHORS:20160615-154451842",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160615-154451842",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "National Science Centre (Poland)",
"grant_number": "DEC-2012/04/A/ST9/00083"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/0004-637X/827/1/55",
"primary_object": {
"basename": "1606.03659v1.pdf",
"url": "https://authors.library.caltech.edu/records/e8abs-3tt54/files/1606.03659v1.pdf"
},
"pub_year": "2016",
"author_list": "Kataoka, Jun and Stawarz, \u0141ukasz"
},
{
"id": "https://authors.library.caltech.edu/records/wgdyh-cfv18",
"eprint_id": 69311,
"eprint_status": "archive",
"datestamp": "2023-08-20 13:14:46",
"lastmod": "2023-10-20 16:47:27",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
}
]
},
"title": "An Iron K Component to the Ultrafast Outflow in NGC 1313 X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (NGC 1313 X-1)",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 June 30; revised 2016 July 6; accepted 2016 July 6; published 2016 July 29. \n\nThe authors would like to thank the anonymous referee for their extremely timely and positive feedback, which helped improve the final manuscript. M.J.M. acknowledges support from an STFC Ernest Rutherford fellowship, C.P. and A.C.F. acknowledge support from ERC Advanced Grant 340442, and D.B. acknowledges financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA, and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. \n\nFacilities: NuSTAR, XMM.\n\nPublished - apjl_826_2_L26.pdf
Submitted - 1607.03124v1.pdf
",
"abstract": "We present the detection of an absorption feature at E = 8.77^(+0.05)_(-0.06) keV in the combined X-ray spectrum of the ultraluminous X-ray source NGC 1313 X-1 observed with XMM-Newton and NuSTAR, significant at the 3\u03c3 level. If associated with blueshifted ionized iron, the implied outflow velocity is ~0.2c for Fe xxvi, or ~0.25c for Fe xxv. These velocities are similar to the ultrafast outflow seen in absorption recently discovered in this source at lower energies by XMM-Newton, and we therefore conclude that this is an iron component to the same outflow. Photoionization modeling marginally prefers the Fe xxv solution, but in either case the outflow properties appear to be extreme, potentially supporting a super-Eddington hypothesis for NGC 1313 X-1.",
"date": "2016-08-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "826",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L26",
"id_number": "CaltechAUTHORS:20160729-114600441",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160729-114600441",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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{
"id": "2016-51",
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}
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"doi": "10.3847/2041-8205/826/2/L26",
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"pub_year": "2016",
"author_list": "Walton, D. J.; Middleton, M. J.; et el."
},
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},
"orcid": "0000-0002-6404-4737"
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"name": {
"family": "Canipe",
"given": "Alicia M."
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"name": {
"family": "Hong",
"given": "Jaesub"
}
},
{
"id": "Tomsick-J-A",
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"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Boggs-S-E",
"name": {
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"given": "Steven E."
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"given": "Finn E."
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"name": {
"family": "Craig",
"given": "William W."
}
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"id": "Fornasini-F-M",
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"given": "Francesca"
}
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
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},
{
"id": "Nynka-M",
"name": {
"family": "Nynka",
"given": "Melania"
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"orcid": "0000-0002-3310-1946"
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{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-Shuo",
"name": {
"family": "Zhang",
"given": "Shuo"
},
"orcid": "0000-0002-2967-790X"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Evidence for Intermediate Polars as the Origin of the Galactic Center Hard X-ray Emission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center \u2013 novae, cataclysmic variables \u2013 X-rays: diffuse background",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 December 4; revised 2016 May 16; accepted 2016 May 19; published 2016 July 28. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors thank K Mukai and QD Wang for valuable discussions.\n\nPublished - apj_826_2_160.pdf
Submitted - 1605.06066v1.pdf
",
"abstract": "Recently, unresolved hard (20\u201340 keV) X-ray emission has been discovered within the central 10 pc of the Galaxy, possibly indicating a large population of intermediate polars (IPs). Chandra and XMM-Newton measurements in the surrounding ~50 pc imply a much lighter population of IPs with\u3008M_(WD)\u3009 \u2248 0.5M\u2299. Here we use broadband NuSTAR observations of two IPs: TV Columbae, which has a fairly typical but widely varying reported mass of M_(WD) \u2248 0.5-1.0M\u2299, and IGR J17303\u20130601, with a heavy reported mass of M_(WD) \u2248 1.0-1.2M\u2299. We investigate how varying spectral models and observed energy ranges influences estimated white dwarf mass. Observations of the inner 10 pc can be accounted for by IPs with M_(WD) \u2248 0.9M\u2299, consistent with that of the CV population in general and the X-ray observed field IPs in particular. The lower mass derived by Chandra and XMM-Newton appears to be an artifact of narrow energy-band fitting. To explain the (unresolved) central hard X-ray emission (CHXE) by IPs requires an X-ray (2\u20138 keV) luminosity function (XLF) extending down to at least 5 \u00d7 10^(31) erg s^(\u22121). The CHXE XLF, if extended to the surrounding ~50 pc observed by Chandra and XMM-Newton, requires that at least ~20%\u201340% of the ~9000 point sources are IPs. If the XLF extends just a factor of a few lower in luminosity, then the vast majority of these sources are IPs. This is in contrast to recent observations of the Galactic ridge, where the bulk of the 2\u20138 keV emission is ascribed to non-magnetic CVs.",
"date": "2016-08-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "826",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 160",
"id_number": "CaltechAUTHORS:20160729-154753481",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160729-154753481",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-52",
"name": "Space Radiation Laboratory"
}
]
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}
]
},
"doi": "10.3847/0004-637X/826/2/160",
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"pub_year": "2016",
"author_list": "Hailey, Charles J.; Mori, Kaya; et el."
},
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"items": [
{
"id": "Cappi-M",
"name": {
"family": "Cappi",
"given": "M."
}
},
{
"id": "De-Marco-B",
"name": {
"family": "De Marco",
"given": "B."
}
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "G."
},
"orcid": "0000-0003-0293-3608"
},
{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
}
},
{
"id": "Petrucci-P-O",
"name": {
"family": "Petrucci",
"given": "P.-O."
}
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Kaastra-J-S",
"name": {
"family": "Kaastra",
"given": "J. S."
},
"orcid": "0000-0001-5540-2822"
},
{
"id": "Kriss-G-A",
"name": {
"family": "Kriss",
"given": "G. A."
}
},
{
"id": "Mehdipour-M",
"name": {
"family": "Mehdipour",
"given": "M."
}
},
{
"id": "Whewell-M",
"name": {
"family": "Whewell",
"given": "M."
}
},
{
"id": "Arav-N",
"name": {
"family": "Arav",
"given": "N."
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{
"id": "Behar-E",
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"family": "Behar",
"given": "E."
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{
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"family": "Boissay",
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{
"id": "Branduardi-Raymont-G",
"name": {
"family": "Branduardi-Raymont",
"given": "G."
}
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{
"id": "Costantini-E",
"name": {
"family": "Costantini",
"given": "E."
}
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{
"id": "Ebrero-J",
"name": {
"family": "Ebrero",
"given": "J."
},
"orcid": "0000-0001-5924-8818"
},
{
"id": "di-Gesu-L",
"name": {
"family": "di Gesu",
"given": "L."
}
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"name": {
"family": "Harrison",
"given": "F. A."
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"orcid": "0000-0003-2992-8024"
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"name": {
"family": "Kaspi",
"given": "S."
}
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"name": {
"family": "Matt",
"given": "G."
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"orcid": "0000-0002-2152-0916"
},
{
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"name": {
"family": "Paltani",
"given": "S."
},
"orcid": "0000-0002-8108-9179"
},
{
"id": "Peterson-B-M",
"name": {
"family": "Peterson",
"given": "B. M."
}
},
{
"id": "Steenbrugge-K-C",
"name": {
"family": "Steenbrugge",
"given": "K. C."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
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},
"title": "Anatomy of the AGN in NGC 5548. VIII. XMM-Newton's EPIC detailed view of an unexpected variable multilayer absorber",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active, X-rays: galaxies, galaxies: individual: NGC 5548",
"note": "\u00a9 ESO, 2016. \n\nReceived: 9 March 2016. Accepted: 5 April 2016. \n\nThis paper is based on observations obtained with the XMM-Newton satellite, an ESA funded mission with contributions by ESA Member States and USA. M.C. and S.B. acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/P1. G.P. acknowledges support via an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2012-IEF- 331095. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA. We thank the International Space Science Institute (ISSI) in Bern for their support and hospitality. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research. M.M. acknowledges support from NWO and the UK STFC. This work was supported by NASA through grants for HST program number 13184 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, incorporated under NASA contract NAS5-26555. M.C. acknowledges financial support from contracts ASI/INAF n.I/037/12/0 and PRIN INAF 2011 and 2012. P.-O.P. acknowledges financial support from the CNES and from the CNRS/PICS. K.C.S. acknowledges financial support from the Fondo Fortalecimiento de la Productividad Cient\u00edfica VRIDT 2013. E.B. received funding from the EU Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 655324, and from the iCORE program of the Planning and Budgeting Committee (grant No. 1937/12). S.B., G.M., and A.D.R. acknowledge INAF/PICS financial support. G.M. and F.U. acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. B.M.P. acknowledges support from the US NSF through grant AST-1008882. G.P. acknowledges support via an EU Marie Curie Intra-European fellowship under contract No. FP-PEOPLE-2012- IEF-331095 and Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408). F.U. acknowledges Ph.D. funding from the VINCI program of the French-Italian University. M.W. acknowledges the support of a Ph.D. studentship awarded by the UK STFC.\n\nPublished - 2016-46.pdf
Submitted - 1604.01777v1.pdf
",
"abstract": "In 2013, we conducted a large multi-wavelength campaign on the archetypical Seyfert 1 galaxy NGC 5548. Unexpectedly, this usually unobscured source appeared strongly absorbed in the soft X-rays during the entire campaign, and signatures of new and strong outflows were present in the almost simultaneous UV HST/COS data. Here we carry out a comprehensive spectral analysis of all available XMM-Newton observations of NGC 5548 (precisely 14 observations from our campaign plus three from the archive, for a total of ~763 ks) in combination with three simultaneous NuSTAR observations. We obtain a best-fit underlying continuum model composed by i) a weakly varying flat (\u0393 ~ 1.5-1.7) power-law component; ii) a constant, cold reflection (FeK + continuum) component; iii) a soft excess, possibly owing to thermal Comptonization; and iv) a constant, ionized scattered emission-line dominated component. Our main findings are that, during the 2013 campaign, the first three of these components appear to be partially covered by a heavy and variable obscurer that is located along the line of sight (LOS), which is consistent with a multilayer of cold and mildly ionized gas. We characterize in detail the short timescale (mostly ~ks-to-days) spectral variability of this new obscurer, and find it is mostly due to a combination of column density and covering factor variations, on top of intrinsic power-law (flux and slope) variations. In addition, our best-fit spectrum is left with several (but marginal) absorption features at rest-frame energies ~6.7-6.9 keV and ~8 keV, aswell as a weak broad emission line feature redwards of the 6.4 keV emission line. These could indicate a more complex underlying model, e.g. a P-Cygni-type emission profile if we allow for a large velocity and wide-angle outflow. These findings are consistent with a picture where the obscurer represents the manifestation along the LOS of a multilayer of gas, which is also in multiphase, and which is likely outflowing at high speed, and simultaneously producing heavy obscuration and scattering in the X-rays, as well as broad absorption features in the UV.",
"date": "2016-08",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "592",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A27",
"id_number": "CaltechAUTHORS:20160810-091225763",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160810-091225763",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI-INAF I/037/12/P1"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "FP-PEOPLE-2012-IEF-331095"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF n.I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN INAF 2011"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN INAF 2012"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)",
"grant_number": "CNRS-PICS"
},
{
"agency": "Fondo Fortalecimiento de la Productividad Cientfica",
"grant_number": "VRIDT 2013"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "655324"
},
{
"agency": "Israeli Committee for Planning and Budgeting",
"grant_number": "1937/12"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/12/0-011/13"
},
{
"agency": "NSF",
"grant_number": "AST-1008882"
},
{
"agency": "French-Italian University VINCI program"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Energie (BMWi)",
"grant_number": "BMWI/DLR, FKZ 50 OR 1408"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "HST 13184"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Le Projet International de Coop\u00e9ration Scientifique (PICS)"
}
]
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"doi": "10.1051/0004-6361/201628464",
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"author_list": "Cappi, M.; De Marco, B.; et el."
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{
"id": "Guainazzi-M",
"name": {
"family": "Guainazzi",
"given": "M."
}
},
{
"id": "Risaliti-G",
"name": {
"family": "Risaliti",
"given": "G."
}
},
{
"id": "Awaki-H",
"name": {
"family": "Awaki",
"given": "H."
}
},
{
"id": "Ar\u00e9valo-P",
"name": {
"family": "Ar\u00e9valo",
"given": "P."
}
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Longinotti-A-L",
"name": {
"family": "Longinotti",
"given": "A."
}
},
{
"id": "Markwardt-C-B",
"name": {
"family": "Markwardt",
"given": "C."
},
"orcid": "0000-0001-9803-3879"
},
{
"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "A."
}
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Svoboda-J",
"name": {
"family": "Svoboda",
"given": "J."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The nature of the torus in the heavily obscured AGN Markarian 3: an X-ray study",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 April 28. Received 2016 April 28. In original form 2016 March 7. First published online May 10, 2016. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). JS acknowledges support from the grant LH14049 and the Project 14-20970P of the Grant Agency of the Czech Republic. FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT Regular 1141218, 'EMBIGGEN' Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. The authors are grateful to an anonymous referee, whose accurate and detailed report greatly improved the clarity of the paper.\n\nPublished - 2016-39.pdf
",
"abstract": "In this paper we report the results of an X-ray monitoring campaign on the heavily obscured Seyfert galaxy Markarian 3 carried out between the fall of 2014 and the spring of 2015 with NuSTAR, Suzaku and XMM-Newton. The hard X-ray spectrum of Markarian 3 is variable on all the time scales probed by our campaign, down to a few days. The observed continuum variability is due to an intrinsically variable primary continuum seen in transmission through a large, but still Compton-thin column density (N_H~0.8-1.1$\\times$10$^{24}$ cm$^{-2}$). If arranged in a spherical-toroidal geometry, the Compton scattering matter has an opening angle ~66 degrees and is seen at a grazing angle through its upper rim (inclination angle ~70 degrees). We report a possible occultation event during the 2014 campaign. If the torus is constituted by a system of clouds sharing the same column density, this event allows us to constrain their number (17$\\pm$5) and individual column density, [~(4.9$\\pm$1.5)$\\times$10$^{22}$ cm$^{-2}$]. The comparison of IR and X-ray spectroscopic results with state-of-the art \"torus\" models suggests that at least two thirds of the X-ray obscuring gas volume might be located within the dust sublimation radius. We report also the discovery of an ionized absorber, characterised by variable resonant absorption lines due to He- and H-like iron. This discovery lends support to the idea that moderate column density absorbers could be due to clouds evaporated at the outer surface of the torus, possibly accelerated by the radiation pressure due to the central AGN emission leaking through the patchy absorber.",
"date": "2016-08",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "460",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1954-1969",
"id_number": "CaltechAUTHORS:20160804-092209395",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160804-092209395",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Grantov\u00e1 agentura \u010cesk\u00e9 republiky",
"grant_number": "LH14049"
},
{
"agency": "Grantov\u00e1 agentura \u010cesk\u00e9 republiky",
"grant_number": "14-20970P"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Basal-CATA PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-39",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw1033",
"primary_object": {
"basename": "2016-39.pdf",
"url": "https://authors.library.caltech.edu/records/b1k9c-gcy38/files/2016-39.pdf"
},
"pub_year": "2016",
"author_list": "Guainazzi, M.; Risaliti, G.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/4jcdj-6bv59",
"eprint_id": 69370,
"eprint_status": "archive",
"datestamp": "2023-08-22 18:21:06",
"lastmod": "2023-10-20 16:50:38",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Chen-Chien-Ting-J",
"name": {
"family": "Chen",
"given": "C.-T. J."
},
"orcid": "0000-0002-4945-5079"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
},
"orcid": "0000-0003-1748-2010"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "A Growth-rate Indicator for Compton-thick Active Galactic Nuclei",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; galaxies: general; galaxies: nuclei; galaxies: Seyfert; masers",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 March 31; revised 2016 May 18; accepted 2016 June 11; published 2016 July 25.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. Furthermore, this research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. A.M. and A.C. acknowledge support from the ASI/INAF grant I/037/12/0-011/13. P.G. acknowledges funding from STFC (ST/J003697/2). M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. \n\nFacility: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission.\n\nPublished - apj_826_1_93.pdf
Submitted - 1606.09265v1.pdf
",
"abstract": "Due to their heavily obscured central engines, the growth rate of Compton-thick (CT) active galactic nuclei (AGNs) is difficult to measure. A statistically significant correlation between the Eddington ratio, \u03bb_(Edd), and the X-ray power-law index, \u0393, observed in unobscured AGNs offers an estimate of their growth rate from X-ray spectroscopy (albeit with large scatter). However, since X-rays undergo reprocessing by Compton scattering and photoelectric absorption when the line of sight to the central engine is heavily obscured, the recovery of the intrinsic \u0393 is challenging. Here we study a sample of local, predominantly CT megamaser AGNs, where the black hole mass, and thus Eddington luminosity, are well known. We compile results of the X-ray spectral fitting of these sources with sensitive high-energy (E > 10 keV) NuSTAR data, where X-ray torus models, which take into account the reprocessing effects have been used to recover the intrinsic \u0393 values and X-ray luminosities, L_X. With a simple bolometric correction to L_X to calculate \u03bb_(Edd), we find a statistically significant correlation between \u0393 and \u03bb_(Edd) (p = 0.007). A linear fit to the data yields \u0393 = (0.41 \u00b1 0.18)log_10 \u03bb_(Edd) + (2.38 \u00b1 0.20), which is statistically consistent with results for unobscured AGNs. This result implies that torus modeling successfully recovers the intrinsic AGN parameters. Since the megamasers have low-mass black holes (M_(BH) \u2248 10^6\u201310^7 M_\u2299) and are highly inclined, our results extend the \u0393\u2013\u03bb Edd relationship to lower masses and argue against strong orientation effects in the corona, in support of AGN unification. Finally this result supports the use of \u0393 as a growth-rate indicator for accreting black holes, even for CT AGNs.",
"date": "2016-07-30",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "826",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 93",
"id_number": "CaltechAUTHORS:20160802-065750850",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160802-065750850",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/2"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-41",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/0004-637X/826/1/93",
"primary_object": {
"basename": "apj_826_1_93.pdf",
"url": "https://authors.library.caltech.edu/records/4jcdj-6bv59/files/apj_826_1_93.pdf"
},
"related_objects": [
{
"basename": "1606.09265v1.pdf",
"url": "https://authors.library.caltech.edu/records/4jcdj-6bv59/files/1606.09265v1.pdf"
}
],
"pub_year": "2016",
"author_list": "Brightman, M.; Masini, A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/00sfm-h9p90",
"eprint_id": 66411,
"eprint_status": "archive",
"datestamp": "2023-08-20 12:56:03",
"lastmod": "2023-10-18 18:03:25",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Malizia-A",
"name": {
"family": "Malizia",
"given": "A."
}
},
{
"id": "Landi-R",
"name": {
"family": "Landi",
"given": "R."
}
},
{
"id": "Molina-M",
"name": {
"family": "Molina",
"given": "M."
}
},
{
"id": "Bassani-L",
"name": {
"family": "Bassani",
"given": "L."
}
},
{
"id": "Bazzano-A",
"name": {
"family": "Bazzano",
"given": "A."
},
"orcid": "0000-0002-2017-4396"
},
{
"id": "Bird-A-J",
"name": {
"family": "Bird",
"given": "A. J."
}
},
{
"id": "Ubertini-P",
"name": {
"family": "Ubertini",
"given": "P."
}
}
]
},
"title": "The INTEGRAL/IBIS AGN catalogue: an update",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "catalogues \u2013 surveys \u2013 galaxies: active",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 April 21. Received 2016 April 19; in original form 2016 February 2. Published: 23 April 2016. \n\nThis research has made use of data obtained from the SIMBAD data base operated at CDS, Strasbourg, France; the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center NASA/IPAC Extragalactic Database (NED). The authors acknowledge the ASI financial support via ASI\u2013INAF grant 2013-025-R.0.\n\nAccepted Version - nustar_4_22.pdf
",
"abstract": "In the most recent IBIS survey based on observations performed during the first 1000 orbits of INTEGRAL, are listed 363 high-energy emitters firmly associated with AGN, 107 of which are reported here for the first time. We have used X-ray data to image the IBIS 90 per cent error circle of all the AGN in the sample of 107, in order to obtain the correct X-ray counterparts, locate them with arcsec accuracy and therefore pinpoint the correct optical counterparts. This procedure has led to the optical and spectral characterization of the entire sample. This new set consists of 34 broad line or type 1 AGN, 47 narrow line or type 2 AGN, 18 blazars and 8 sources of unknown class. These eight sources have been associated with AGN from their positional coincidence with 2MASX/Radio/X-ray sources. Seven high-energy emitters have been included since they are considered to be good AGN candidates. Spectral analysis has been already performed on 55 objects and the results from the most recent and/or best statistical measurements have been collected. For the remaining 52 sources, we report the spectral analysis for the first time in this work. We have been able to obtain the full X-ray coverage of the sample making use of data from Swift/XRT, XMM\u2013Newton and NuSTAR. In addition to the spectral characterization of the entire sample, this analysis has enabled us to identify peculiar sources and by comparing different data sets, highlight flux variability in the 2\u201310 keV and 20\u201340 keV bands.",
"date": "2016-07-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "460",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "19-29",
"id_number": "CaltechAUTHORS:20160422-122726356",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160422-122726356",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "2013-025-R.0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
}
]
},
"doi": "10.1093/mnras/stw972",
"primary_object": {
"basename": "nustar_4_22.pdf",
"url": "https://authors.library.caltech.edu/records/00sfm-h9p90/files/nustar_4_22.pdf"
},
"pub_year": "2016",
"author_list": "Malizia, A.; Landi, R.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/b6mcf-acw53",
"eprint_id": 66163,
"eprint_status": "archive",
"datestamp": "2023-08-20 12:55:55",
"lastmod": "2023-10-18 17:13:15",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman"
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Clavel-M",
"name": {
"family": "Clavel",
"given": "Ma\u00efca"
},
"orcid": "0000-0003-0724-2742"
},
{
"id": "Strader-J",
"name": {
"family": "Strader",
"given": "Jay"
},
"orcid": "0000-0002-1468-9668"
},
{
"id": "Chomiuk-L",
"name": {
"family": "Chomiuk",
"given": "Laura"
},
"orcid": "0000-0002-8400-3705"
}
]
},
"title": "Identifying IGR J14091-6108 as a magnetic CV with a massive white dwarf using X-ray and optical observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: individual: IGR J14091\u22126108 \u2013 novae, cataclysmic variables \u2013 white dwarfs \u2013X-rays: stars",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 April 11. Received 2016 April 11; in original form 2016 February 23. Published: 14 April 2016.\n\nWe would like to thank D. Wik for help with using nuskybgd to produce a background spectrum for NuSTAR. We also thank C. Hailey, J. Hong, and F. Fornasini for useful discussions. FR thanks the ESO staff who performed the service observations. JAT acknowledges partial support from NASA under XMM Guest Observer grant NNX15AW09G. MC acknowledges partial support under NASA Contract NNG08FD60C for work on the NuSTAR mission. This work was partially supported by NASA Fermi grant NNX15AU83G. RK acknowledges support from Russian Science Foundation (grant 14-22-00271). This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist\u00e9rio da Ci\u00eancia, Tecnologia, e Inova\u00e7\u00e3o (MCTI) da Rep\u00fablica Federativa do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS, 143, 23.\n\nSubmitted - 1604.03562v1
",
"abstract": "INTEGRAL Gamma-Ray (IGR) J14091\u22126108 is a Galactic X-ray source known to have an iron emission line, a hard X-ray spectrum, and an optical counterpart. Here, we report on X-ray observations of the source with XMM\u2013Newton and NuSTAR as well as optical spectroscopy with European Southern Obseratory/Very Large Telescope and National Optical Astronomy Observatory/Southern Astrophysical Research Telescope. In the X-rays, this provides data with much better statistical quality than the previous observations, and this is the first report of the optical spectrum. Timing analysis of the XMM data shows a very significant detection of 576.3 \u00b1 0.6 s period. The signal has a pulsed fraction of 30 \u00b1 3 per cent in the 0.3\u201312 keV range and shows a strong drop with energy. The optical spectra show strong emission lines with significant variability in the lines and continuum, indicating that they come from an irradiated accretion disc. Based on these measurements, we identify the source as a magnetic cataclysmic variable of intermediate polar (IP) type where the white dwarf spin period is 576.3 s. The X-ray spectrum is consistent with the continuum emission mechanism being due to thermal bremsstrahlung, but partial covering absorption and reflection are also required. In addition, we use the IP mass model, which suggests that the white dwarf in this system has a high mass, possibly approaching the Chandrasekhar limit.",
"date": "2016-07-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "460",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "513-523",
"id_number": "CaltechAUTHORS:20160414-093817451",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160414-093817451",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AW09G"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX15AU83G"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-22-00271"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw871",
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"title": "NuSTAR Observations of the Black Hole GS 1354\u2013645: Evidence of Rapid Black Hole Spin",
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"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 X-rays: binaries",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 May 18; revised 2016 June 30; accepted 2016 July 1; published 2016 July 19. \n\nWe thank the anonymous referee for comments that improved this manuscript. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA.\n\nPublished - apjl_826_1_L12.pdf
Submitted - 1607.00343v1.pdf
",
"abstract": "We present the results of a NuSTAR study of the dynamically confirmed stellar-mass black hole GS 1354\u2212645. The source was observed during its 2015 \"hard\" state outburst; we concentrate on spectra from two relatively bright phases. In the higher-flux observation, the broadband NuSTAR spectra reveal a clear, strong disk reflection spectrum, blurred by a degree that requires a black hole spin of a = cJ/GM^2 \u2a7e 0.98 (1\u03c3 statistical limits only). The fits also require a high inclination: \u0398 \u2243 75(2)\u00b0. Strong \"dips\" are sometimes observed in the X-ray light curves of sources viewed at such an angle; these are absent, perhaps indicating that dips correspond to flared disk structures that only manifest at higher accretion rates. In the lower flux observation, there is evidence of radial truncation of the thin accretion disk. We discuss these results in the context of spin in stellar-mass black holes, and inner accretion flow geometries at moderate accretion rates.",
"date": "2016-07-20",
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"pagerange": "Art. No. L12",
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"issn": "2041-8205",
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"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
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"agency": "NASA",
"grant_number": "NNG08FD60C"
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"title": "Hard X-Ray Emission from Sh 2-104: A NuSTAR Search for Gamma-Ray Counterparts",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "ISM: individual objects (Sh 2-104, MGRO J2019+37, 3XMM J201744.7+365045, VER J2019+368) \u2013 pulsars: individual (NuSTAR J201744.3+364812) \u2013 stars: neutron",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 2; revised 2016 April 21; accepted 2016 May 8; published 2016 July 18. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software, and calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). E.V.G. acknowledges partial support by the National Aeronautics and Space Administration through XMM-Newton Award Number NNX15AG28G and Chandra Award Number G05-16061X, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.M.P. acknowledges support by the Spanish MINECO under grants AYA2013-47447-C3-1-P, MDM-2014-0369 of ICCUB (Unidad de Excelencia \"Mar\u00eda de Maeztu\"), and the Catalan DEC grant 2014 SGR 86 and ICREA Academia.\n\nPublished - apj_826_1_25.pdf
Submitted - 1605.03641v2.pdf
",
"abstract": "We present NuSTAR hard X-ray observations of Sh 2\u2013104, a compact H II region containing several young massive stellar clusters (YMSCs). We have detected distinct hard X-ray sources coincident with localized VERITAS TeV emission recently resolved from the giant gamma-ray complex MGRO J2019+37 in the Cygnus region. Fainter, diffuse X-rays coincident with the eastern YMSC in Sh2-104 likely result from the colliding winds of a component star. Just outside the radio shell of Sh 2\u2013104 lies 3XMM J201744.7+365045 and a nearby nebula, NuSTAR J201744.3+364812, whose properties are most consistent with extragalactic objects. The combined XMM-Newton and NuSTAR spectrum of 3XMM J201744.7+365045 is well-fit to an absorbed power-law model with N_H = (3.1 \u00b1 1.0) x 10^(22) cm^(\u22122) and a photon index \u0393 = 2.1 \u00b1 0.1. Based on possible long-term flux variation and the lack of detected pulsations (\u226443% modulation), this object is likely a background active galactic nucleus rather than a Galactic pulsar. The spectrum of the NuSTAR nebula shows evidence of an emission line at E = 5.6 keV, suggesting an optically obscured galaxy cluster at z = 0.19 \u00b1 0.02 (d = 800 Mpc) and L X = 1.2 \u00d7 10^(44) erg s^(\u22121). Follow-up Chandra observations of Sh 2\u2013104 will help identify the nature of the X-ray sources and their relation to MGRO J2019+37. We also show that the putative VERITAS excess south of Sh 2\u2013104, is most likely associated with the newly discovered Fermi pulsar PSR J2017+3625 and not the H II region.",
"date": "2016-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "826",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 25",
"id_number": "CaltechAUTHORS:20160801-142718338",
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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{
"agency": "NASA",
"grant_number": "NNX15AG28G"
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{
"agency": "NASA",
"grant_number": "G05-16061X"
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{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)",
"grant_number": "AYA2013-47447-C3-1-P"
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{
"agency": "Unidad de Excelencia \"Mar\u00eda de Maeztu\"",
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},
"title": "The Soft State of Cygnus X-1 Observed with NuSTAR: A Variable Corona and a Stable Inner Disk",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (Cygnus X-1)",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 March 18; revised 2016 April 29; accepted 2016 May 11; published 2016 July 25. \n\nThe authors would like to thank the referee for prompt and useful feedback. DB acknowledges financial support from the French Space Agency (CNES). VG acknowledges financial support provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. This research made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA, and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). Swift BAT transient monitor results are provided by the Swift BAT team. This research has also made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. \n\nFacility: NuSTAR.\n\nPublished - apj_826_1_87.pdf
Submitted - 1605.03966v1.pdf
",
"abstract": "We present a multi-epoch hard X-ray analysis of Cygnus X-1 in its soft state based on four observations with the Nuclear Spectroscopic Telescope Array (NuSTAR). Despite the basic similarity of the observed spectra, there is clear spectral variability between epochs. To investigate this variability, we construct a model incorporating both the standard disk-corona continuum and relativistic reflection from the accretion disk, based on prior work on Cygnus X-1, and apply this model to each epoch independently. We find excellent consistency for the black hole spin and the iron abundance of the accretion disk, which are expected to remain constant on observational timescales. In particular, we confirm that Cygnus X-1 hosts a rapidly rotating black hole, 0.93 \u227e a* \u227e 0.96, in broad agreement with the majority of prior studies of the relativistic disk reflection and constraints on the spin obtained through studies of the thermal accretion disk continuum. Our work also confirms the apparent misalignment between the inner disk and the orbital plane of the binary system reported previously, finding the magnitude of this warp to be ~10\u00b0\u201315\u00b0. This level of misalignment does not significantly change (and may even improve) the agreement between our reflection results and the thermal continuum results regarding the black hole spin. The spectral variability observed by NuSTAR is dominated by the primary continuum, implying variability in the temperature of the scattering electron plasma. Finally, we consistently observe absorption from ionized iron at ~6.7 keV, which varies in strength as a function of orbital phase in a manner consistent with the absorbing material being an ionized phase of the focused stellar wind from the supergiant companion star.",
"date": "2016-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "826",
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"pagerange": "Art. No. 87",
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"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160517-183422492",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
{
"agency": "Smithsonian Astrophysical Observatory (SAO)",
"grant_number": "SV3-73016"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
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"agency": "NASA/JPL/Caltech"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
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"title": "NuSTAR, Swift, and GROND observations of the flaring MeV blazar: PMN J0641\u22120320",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 quasars: general \u2013 quasars: individual (PMN J0641\u20130320) \u2013 X-rays: general",
"note": "\u00a9 2016 The American Astronomical Society. Received 2016 February 20; revised 2016 April 21; accepted 2016 April 22; published 2016 July 22. We thank the anonymous referee for useful comments. M.A. acknowledges generous support from NASA grant NNH09ZDA001N. M.B. acknowledges support from the International Fulbright Science and Technology Award and from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science, and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France. This NuSTAR work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Part of this work is based on archival data, software, or on-line services provided by the ASI Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS). Part of the funding for GROND (both hardware and personnel) was generously granted by the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). Facilities: Fermi/LAT, NuSTAR, Swift, GROND, Keck.\n\nPublished - apj_826_1_76.pdf
Submitted - 1602.06446v1.pdf
",
"abstract": "MeV blazars are a sub-population of the blazar family, exhibiting larger-than-average jet powers, accretion luminosities, and black hole masses. Because of their extremely hard X-ray continua, these objects are best studied in the X-ray domain. Here, we report on the discovery by the Fermi Large Area Telescope and subsequent follow-up observations with NuSTAR, Swift, and GROND of a new member of the MeV blazar family: PMN J0641\u22120320. Our optical spectroscopy provides confirmation that this is a flat-spectrum radio quasar located at a redshift of z = 1.196. Its very hard NuSTAR spectrum (power-law photon index of ~1 up to ~80 keV) indicates that the emission is produced via inverse Compton scattering off of photons coming from outside the jet. The overall spectral energy distribution of PMN J0641\u22120320 is typical of powerful blazars and, using a simple one-zone leptonic emission model, we infer that the emission region is located either inside the broad line region or within the dusty torus.",
"date": "2016-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "826",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 76",
"id_number": "CaltechAUTHORS:20160318-090815693",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160318-090815693",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNH09ZDA001N"
},
{
"agency": "Fulbright Foundation"
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{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Department of Energy (DOE)"
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{
"agency": "Commissariat a l'Energie Atomique (CEA)"
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{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
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{
"agency": "Institut National de Physique Nucleaire et de Physique des Particules (IN2P3)"
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{
"agency": "Agenzia Spaziale Italiana (ASI)"
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{
"agency": "Istituto Nazionale di Fisica Nucleare (INFN)"
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{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)"
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{
"agency": "High Energy Accelerator Research Organization (KEK)"
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{
"agency": "Japan Aerospace Exploration Agency (JAXA)"
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{
"agency": "Knut and Alice Wallenberg Foundation"
},
{
"agency": "Swedish Research Council"
},
{
"agency": "Swedish National Space Board (SNSB)"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "HA 1850/28-1"
}
]
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"pub_year": "2016",
"author_list": "Ajello, M.; Ghisellini, G.; et el."
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},
"title": "The First Focused Hard X-ray Images of the Sun with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "acceleration of particles; methods: data analysis; Sun: X-rays, gamma rays",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 January 27. Accepted 2016 May 20. Published 2016 July 18. \n\nThis work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. Additional funding for this work was also provided under NASA grants NNX12AJ36G and NNX14AG07G. S.K. acknowledges funding from the Swiss National Science Foundation (200021-140308). A.J.M.'s participation was supported by NASA Earth and Space Science Fellowship award NNX13AM41H. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. A.C. was supported by NASA grants NNX15AK26G and NNX14AN84G. I.G.H. is supported by a Royal Society University Research Fellowship. \n\nWe thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research made extensive use of the IDL Astronomy Library (http://idlastro.gsfc.nasa.gov/) and of the SolarSoft IDL distribution (SSW). Additional figures were produced using the Veusz plotting package (\u00a9 2003\u20132015 Jeremy Sanders). \n\nFacility: NuSTAR.\n\nPublished - 2016-43.pdf
",
"abstract": "We present results from the the first campaign of dedicated solar observations undertaken by the Nuclear Spectroscopic Telescope ARray (NuSTAR) hard X-ray (HXR) telescope. Designed as an astrophysics mission, NuSTAR nonetheless has the capability of directly imaging the Sun at HXR energies (>3 keV) with an increase in sensitivity of at least two magnitude compared to current non-focusing telescopes. In this paper we describe the scientific areas where NuSTAR will make major improvements on existing solar measurements. We report on the techniques used to observe the Sun with NuSTAR, their limitations and complications, and the procedures developed to optimize solar data quality derived from our experience with the initial solar observations. These first observations are briefly described, including the measurement of the Fe K-shell lines in a decaying X-class flare, HXR emission from high in the solar corona, and full-disk HXR images of the Sun.",
"date": "2016-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "826",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 20",
"id_number": "CaltechAUTHORS:20160805-091208103",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160805-091208103",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "200021-140308"
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{
"agency": "NASA Earth and Space Science Fellowship",
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{
"agency": "Department of Energy (DOE)",
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{
"agency": "NASA",
"grant_number": "NNX15AK26G"
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{
"agency": "NASA",
"grant_number": "NNX14AN84G"
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{
"agency": "Royal Society"
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},
"title": "NuSTAR Hard X-Ray Survey of the Galactic Center Region. II. X-Ray Point Sources",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center; X-rays: binaries; X-rays: diffuse background; X-rays: general",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 January 29. Accepted 2016 May 12. Published 2016 July 12. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. We thank G. Ponti for careful reading and suggestions of the manuscript. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J. Hong acknowledges support from NASA/APRA grant NNX14AD59G. R. Krivonos acknowledges support from Russian Science Foundation through grant 14-22-00271. F.E. Bauer acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, \"EMBIGGEN\" Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. S. Zhang is supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program\u2014Grant NNX13AM31. D. Barret acknowledges support from the French Space Agency (CNES).\n\nPublished - 2016-44.pdf
",
"abstract": "We present the first survey results of hard X-ray point sources in the Galactic Center (GC) region by NuSTAR. We have discovered 70 hard (3\u201379 keV) X-ray point sources in a 0.6 deg^2 region around Sgr A* with a total exposure of 1.7 Ms, and 7 sources in the Sgr B2 field with 300 ks. We identify clear Chandra counterparts for 58 NuSTAR sources and assign candidate counterparts for the remaining 19. The NuSTAR survey reaches X-ray luminosities of \u223c4\u00d7 and \u223c8 \u00d7 10^(32) erg s^(-1) at the GC (8 kpc) in the 3\u201310 and 10\u201340 keV bands, respectively. The source list includes three persistent luminous X-ray binaries (XBs) and the likely run-away pulsar called the Cannonball. New source-detection significance maps reveal a cluster of hard (> 10 keV) X-ray sources near the Sgr A diffuse complex with no clear soft X-ray counterparts. The severe extinction observed in the Chandra spectra indicates that all the NuSTAR sources are in the central bulge or are of extragalactic origin. Spectral analysis of relatively bright NuSTAR sources suggests that magnetic cataclysmic variables constitute a large fraction (> 40%\u201360%). Both spectral analysis and logN\u2013logS distributions of the NuSTAR sources indicate that the X-ray spectra of the NuSTAR sources should have kT > 20 keV on average for a single temperature thermal plasma model or an average photon index of \u0393 = 1.5\u20132 for a power-law model. These findings suggest that the GC X-ray source population may contain a larger fraction of XBs with high plasma temperatures than the field population.",
"date": "2016-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "825",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 132",
"id_number": "CaltechAUTHORS:20160805-103318852",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160805-103318852",
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"agency": "NASA",
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"agency": "NASA/JPL/Caltech"
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},
{
"agency": "Russian Science Foundation",
"grant_number": "14-22-00271"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
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{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX13AM31"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
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"author_list": "Hong, JaeSub; Mori, Kaya; et el."
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},
"title": "A New Population of Compton-thick AGNs Identified Using the Spectral Curvature above 10 keV",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: Seyfert \u2013 X-rays: galaxies",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 December 1; revised 2016 March 29; accepted 2016 April 18; published 2016 July 6. \n\nWe acknowledge financial support from Ambizione fellowship grant PZ00P2_154799/1 (M.K.), the Swiss National Science Foundation (NSF) grant PP00P2 138979/1 (M.K. and K.S.), the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101 (E.T.), NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.), NSF award AST 1008067 (D.B.), Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G (W.N.B.), and the ASI/INAF grant I/037/12/0 011/13 and the Caltech Kingsley visitor program (A.C.). M.K. also acknowledges that support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number AR3-14010X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research made use of the XRT Data Analysis Software (XRTDAS), archival data, software, and online services provided by the ASDC. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The scientific results reported in this article are based on data obtained from the Chandra Data Archive (Obs ID = 4078, 4868, 12290, 13895). This work is based on observations obtained with XMM-Newton (Obs ID = 0110930201, 0147760101, 0200430201), an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - , XMM - , Sloan - , CXO -\n\nPublished - apj_825_2_85.pdf
Submitted - 1604.07825v1.pdf
",
"abstract": "We present a new metric that uses the spectral curvature (SC) above 10 keV to identify Compton-thick active galactic nuclei (AGNs) in low-quality Swift/Burst Alert Telescope (BAT) X-ray data. Using NuSTAR, we observe nine high SC-selected AGNs. We find that high-sensitivity spectra show that the majority are Compton-thick (78% or 7/9) and the remaining two are nearly Compton-thick (N_H \u2243 (5\u20138) \u00d7 10^(23) cm^(\u22122)). We find that the SC_(BAT) and SC_(NuSTAR) measurements are consistent, suggesting that this technique can be applied to future telescopes. We tested the SC method on well-known Compton-thick AGNs and found that it is much more effective than broadband ratios (e.g., 100% using SC versus 20% using 8\u201324 keV/3\u20138 keV). Our results suggest that using the >10 keV emission may be the only way to identify this population since only two sources show Compton-thick levels of excess in the Balmer decrement corrected [O iii] to observed X-ray emission ratio (F_([O III])/f^(obs)_(2-10 kev) > 1) and WISE colors do not identify most of them as AGNs. Based on this small sample, we find that a higher fraction of these AGNs are in the final merger stage (<10 kpc) than typical BAT AGNs. Additionally, these nine obscured AGNs have, on average, \u22484\u00d7 higher accretion rates than other BAT-detected AGNs (\u3008\u03bb_(Edd)\u3009= 0.068 \u00b1 0.023 compared to \u3008\u03bb_(Edd)\u3009= 0.016 \u00b1 0.004). The robustness of SC at identifying Compton-thick AGNs implies that a higher fraction of nearby AGNs may be Compton-thick (\u224822%) and the sum of black hole growth in Compton-thick AGNs (Eddington ratio times population percentage) is nearly as large as mildly obscured and unobscured AGNs.",
"date": "2016-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "825",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 85",
"id_number": "CaltechAUTHORS:20160729-140218146",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160729-140218146",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PZ00P2_154799/1"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2 138979/1"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "NSF",
"grant_number": "AST 1008067"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0 011/13"
},
{
"agency": "Caltech Kingsley Visitor Program"
},
{
"agency": "NASA",
"grant_number": "AR3-14010X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06"
}
]
},
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"id": "2016-45",
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"doi": "10.3847/0004-637X/825/2/85",
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"pub_year": "2016",
"author_list": "Koss, Michael J.; Assef, R.; et el."
},
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"eprint_id": 66567,
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"datestamp": "2023-08-20 12:45:12",
"lastmod": "2023-10-18 18:35:37",
"type": "article",
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"creators": {
"items": [
{
"id": "Paliya-V-S",
"name": {
"family": "Paliya",
"given": "Vaidehi S."
},
"orcid": "0000-0001-7774-5308"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
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"name": {
"family": "Fabian",
"given": "A. C."
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"orcid": "0000-0002-9378-4072"
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"id": "Stalin-C-S",
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"family": "Stalin",
"given": "C. S."
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},
"title": "Broadband Observations of High Redshift Blazars",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: jets \u2013 gamma rays: galaxies",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 April 12; revised 2016 April 25; accepted 2016 April 28; published 2016 June 29. \n\nWe are grateful to the referee for constructive comments on the manuscript. A.C.F. thanks Greg Madejski for discussions on the curvature of blazar X-ray spectra and acknowledges support from ERC Advanced Grant 340442. This research has made use of data, software, and/or web tools obtained from NASAs High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. \n\nSDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.\n\nSubmitted - 1604.08566v1.pdf
",
"abstract": "We present a multi-wavelength study of four high redshift blazars, S5 0014+81 (z = 3.37), CGRaBS J0225+1846 (z = 2.69), BZQ J1430+4205 (z = 4.72), and 3FGL J1656.2\u22123303 (z = 2.40) using quasi-simultaneous data from the Swift, Nuclear Spectroscopic Telescope Array (NuSTAR) and the Fermi-Large Area Telescope (LAT) and also archival XMM-Newton observations. Other than 3FGL J1656.2\u22123303, none of the sources were known as \u03b3-ray emitters, and our analysis of ~7.5 yr of LAT data reveals the first time detection of statistically significant \u03b3-ray emission from CGRaBS J0225+1846. We generate the broadband spectral energy distributions (SED) of all the objects, centering at the epoch of NuSTAR observations and reproduce them using a one-zone leptonic emission model. The optical\u2212UV emission in all the objects can be explained by radiation from the accretion disk, whereas the X-ray to \u03b3-ray windows of the SEDs are found to be dominated by inverse Compton scattering off the broad line region photons. All of them host black holes that are billions of solar masses. Comparing the accretion disk luminosity and the jet power of these sources with a large sample of blazars, we find them to occupy a high disk luminosity\u2013jet power regime. We also investigate the X-ray spectral properties of the sources in detail with a major focus on studying the causes of soft X-ray deficit, a feature generally seen in high redshift radio-loud quasars. We summarize that this feature could be explained based on the intrinsic curvature in the jet emission rather than being due to the external effects predicted in earlier studies, such as host galaxy and/or warm absorption.",
"date": "2016-07-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "825",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 74",
"id_number": "CaltechAUTHORS:20160501-095905412",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160501-095905412",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Alfred P. Sloan Foundation"
},
{
"agency": "Participating Institutions"
},
{
"agency": "NSF"
},
{
"agency": "Department of Energy (DOE)"
}
]
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"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
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"doi": "10.3847/0004-637X/825/1/74",
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"author_list": "Paliya, Vaidehi S.; Parker, M. L.; et el."
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"datestamp": "2023-08-20 12:31:59",
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"items": [
{
"id": "Suleimanov-V",
"name": {
"family": "Suleimanov",
"given": "V."
}
},
{
"id": "Doroshenko-V",
"name": {
"family": "Doroshenko",
"given": "V."
}
},
{
"id": "Ducci-L",
"name": {
"family": "Ducci",
"given": "L."
}
},
{
"id": "Zhukov-G-V",
"name": {
"family": "Zhukov",
"given": "G. V."
}
},
{
"id": "Werner-K",
"name": {
"family": "Werner",
"given": "K."
}
}
]
},
"title": "GK Persei and EX Hydrae: Intermediate polars with small magnetospheres",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 novae, cataclysmic variables \u2013 X-rays: binaries \u2013 methods: numerical",
"note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 12 February 2016; Accepted 14 April 2016. Published online 07 June 2016.\n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This paper is also based on data from observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Spain, and Switzerland), Czech Republic and Poland, and with the participation of Russia and the USA. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). V.S. thanks Deutsche Forschungsgemeinschaft (DFG) for financial support (grant WE 1312/48-1). V.D. and L.D. acknowledges support by the Bundesministerium f\u00fcr Wirtschaft und Technologie and the Deutsches Zentrum f\u00fcr Luft und Raumfahrt through the grant FKZ 50 OG 1602.\n\nSubmitted - 1604.00232v1.pdf
",
"abstract": "Observed hard X-ray spectra of intermediate polars are determined mainly by the accretion flow velocity at the white dwarf surface, which is normally close to the free-fall velocity. This allows us to estimate the white dwarf masses as the white dwarf mass-radius relation M \u2212 R and the expected free-fall velocities at the surface are well known. This method is widely used. However, derived white dwarf masses M can be systematically underestimated because the accretion flow is stopped at, and re-accelerates from, the magnetospheric boundary R_m and, therefore, its velocity at the surface is lower than free fall. To avoid this problem, we computed a two-parameter set of model hard X-ray spectra, which allows us to constrain a degenerate M \u2013 R_m dependence. Previous works showed that power spectra of accreting X-ray pulsars and intermediate polars exhibit breaks at frequencies corresponding to Keplerian frequencies at the magnetospheric boundary. Therefore, the break frequency \u03bd_b in an intermediate polar power spectrum gives another relation in the M \u2013 R_m plane. The intersection of the two dependences allows us, therefore, to determine the white dwarf mass and magnetospheric radius simultaneously. To verify the method, we analysed the archival Suzaku observation of EX Hya, obtaining M/M\u2299 = 0.73 \u00b1 0.06 and R_m/R = 2.6 \u00b1 0.4, which is consistent with the values determined by other authors. Subsequently, we applied the same method to a recent NuSTAR observation of another intermediate polar GK Per performed during an outburst and found M/M\u2299 = 0.86 \u00b1 0.02 and R_m/R = 2.8 \u00b1 0.2. The long duration observations of GK Per in quiescence performed by Swift/BAT and INTEGRAL observatories indicate increase of magnetosphere radius R_m at lower accretion rates.",
"date": "2016-07",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "591",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A35",
"id_number": "CaltechAUTHORS:20160404-142434779",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160404-142434779",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "WE 1312/48-1"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)"
},
{
"agency": "Deutsche Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "FKZ50OG1602"
}
]
},
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"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201628301",
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},
"pub_year": "2016",
"author_list": "Suleimanov, V.; Doroshenko, V.; et el."
},
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{
"id": "Ludlam-R-M",
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"family": "Ludlam",
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},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
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{
"id": "Cackett-E-M",
"name": {
"family": "Cackett",
"given": "E. M."
},
"orcid": "0000-0002-8294-9281"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "L."
},
"orcid": "0000-0002-6601-9543"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "NuSTAR and XMM-Newton Observations of the Neutron Star X-ray Binary 1RXS J180408.9-34205",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; relativistic processes; stars: neutron; X-rays: binaries",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 November 20; accepted 2016 April 14; published 2016 June 8. \n\nWe thank the referee for the generous and helpful comments. We also thank Javier Garcia for insightful discussion regarding the relxill model. E.M.C. gratefully acknowledges support from the National Science Foundation through CAREER award number AST-1351222. This research makes use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research also made use of data obtained with XMM-Newton, and the ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13.\n\nPublished - apj_824_1_37.pdf
Submitted - 1604.04252v1.pdf
",
"abstract": "We report on observations of the neutron star (NS) residing in the low-mass X-ray binary 1RXS J180408.9-34205 taken 2015 March by NuSTAR and XMM-Newton while the source was in the hard spectral state. We find multiple reflection features (Fe K_\u0251 detected with NuSTAR; N vii, O vii, and O viii detected in the RGS) from different ionization zones. Through joint fits using the self-consistent relativistic reflection model relxill, we determine the inner radius to be \u226411.1 Rg . For a 1.4 M_\u2609 NS with a spin of a_* = 0, this is an inner disk radius of \u2a7d22.2 km. We find the inclination of the system to be between 18\u00b0 and 29\u00b0. If the disk is truncated at a radius greater than the NS radius, it could be truncated by a boundary layer on the NS surface. It is also possible that the disk is truncated at the magnetospheric radius; conservative estimates would then imply B \u2a7d (0.3-1.0) x 10^9 G at the magnetic poles, though coherent pulsations have not been detected and the source is not identified as a pulsar.",
"date": "2016-06-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "824",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 37",
"id_number": "CaltechAUTHORS:20160707-103702416",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160707-103702416",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NSF",
"grant_number": "AST-1351222"
},
{
"agency": "NASA"
},
{
"agency": "ESA Member States"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-53",
"name": "Space Radiation Laboratory"
}
]
},
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"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
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},
"doi": "10.3847/0004-637X/824/1/37",
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}
],
"pub_year": "2016",
"author_list": "Ludlam, R. M.; Miller, J. M.; et el."
},
{
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"datestamp": "2023-08-22 18:06:46",
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"items": [
{
"id": "Bodaghee-A",
"name": {
"family": "Bodaghee",
"given": "Arash"
},
"orcid": "0000-0002-7315-3732"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
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"name": {
"family": "Fornasini",
"given": "Francesca M."
}
},
{
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"name": {
"family": "Krivonos",
"given": "Roman"
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Chirstensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
}
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR discovery of a cyclotron line in the accreting X-ray pulsar IGR J16393-4643",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; gamma-ray burst: general; stars: neutron; X-rays: binaries; X-rays: individual (IGR J16393-4643)",
"note": "\u00a9 2016 The American Astronomical Society. Received 2015 July 7; accepted 2016 March 17; published 2016 June 1.\n\nThe authors are grateful to the anonymous Referee for their\nconstructive criticism that helped improve the quality of the manuscript. A.B. thanks Dr. Konstantin Postnov. FMF acknowledges support from the National Science Foundation\nGraduate Research Fellowship. R.K. acknowledges support\nfrom from Russian Science Foundation (grant 14-22-00271).\nThe scientific results reported in this article are based on data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of: the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology; data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; NASA's Astrophysics Data System Bibliographic Services; and the SIMBAD database operated at CDS, Strasbourg, France.\n\nFacilities: NuSTAR, Swift.\n\nPublished - APJ146.pdf
Submitted - 1603.05580v1.pdf
",
"abstract": "The high-mass X-ray binary and accreting X-ray pulsar IGR J16393-4643 was observed by the Nuclear Spectroscope Telescope Array in the 3\u201379 keV energy band for a net exposure time of 50 ks. We present the results of this observation which enabled the discovery of a cyclotron resonant scattering feature with a centroid energy of 29.3^(+1.3)_(-1.1) keV. This allowed us to measure the magnetic field strength of the neutron star for the first time: B = (2.5 \u00b1 0.1) \u00d7 10^(12) G. The known pulsation period is now observed at 904.0 \u00b1 0.1 s. Since 2006, the neutron star has\nundergone a long-term spin-up trend at a rate of P = -2 x 10^(-8) s s^(\u22121) (\u22120.6 s per year, or a frequency derivative of v = 3 x 10^(-14) Hz s^(\u22121)). In the power density spectrum, a break appears at the pulse frequency which separates the zero slope at low frequency from the steeper slope at high frequency. This addition of angular momentum to the neutron star could be due to the accretion of a quasi-spherical wind, or it could be caused by the transient appearance of a prograde accretion disk that is nearly in corotation with the neutron star whose magnetospheric radius is around 2 \u00d7 10^8 cm.",
"date": "2016-06-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "823",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 146",
"id_number": "CaltechAUTHORS:20160404-144646609",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160404-144646609",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NSF Graduate Research Fellowship"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-22-00271"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-54",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/0004-637X/823/2/146",
"primary_object": {
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"pub_year": "2016",
"author_list": "Bodaghee, Arash; Tomsick, John A.; et el."
},
{
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"eprint_id": 69055,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:52:07",
"lastmod": "2023-10-20 16:29:00",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Staubert-R",
"name": {
"family": "Staubert",
"given": "R."
}
},
{
"id": "Klochkov-D",
"name": {
"family": "Klochkov",
"given": "D."
}
},
{
"id": "Vybornov-V",
"name": {
"family": "Vybornov",
"given": "V."
}
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "Continued decay in the cyclotron line energy in Hercules X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "magnetic fields stars: neutron radiation mechanisms: general radiation mechanisms: non-thermal accretion, accretion disks X-rays: binaries",
"note": "\u00a9 2016 ESO. Received 14 December 2015. Accepted 18 March 2016. Published online 19 May 2016.\n\nThe motivation for this paper are new observational data\ntaken by the NASA satellite NuSTAR. We would like to acknowledge the dedication of all the people who have contributed to the great success of this mission,\nhere especially Karl Forster for his effort with respect to the non-standard scheduling of the observations. Further important data were provided by the equally successful missions RXTE and Swift of NASA and INTEGRAL of ESA. This work was supported by the Deutsche Forschungsgemeinschaft (DFG) through joint grants KL 2734/2-1 and WI 1860/11-1. We thank the anonymous referee for useful comments and suggestions.\n\nPublished - aa27955-15.pdf
Submitted - 1603.07090v2.pdf
",
"abstract": "The centroid energy E_(cyc) of the cyclotron line in the spectrum of the binary X-ray pulsar Her X-1 has been found to decrease with time on a time scale of a few tens of years \u2013 surprisingly short in astrophysical terms. This was found for the pulse phase-averaged line centroid energy using observational data from various X-ray satellites over the time period 1996 to 2012, establishing a reduction of ~4\u2009keV. Here we report on the result of a new observation by NuSTAR performed in August 2015. The earlier results are confirmed and strengthened with respect to both the dependence of E_(cyc) on flux (it is still present after 2006) and the dependence on time: the long-term decay continued with the same rate, corresponding to a reduction of ~5\u2009keV in 20 yr.",
"date": "2016-06",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "590",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A91",
"id_number": "CaltechAUTHORS:20160715-103832678",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160715-103832678",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "KL 2734/2-1"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "WI 1860/11-1"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201527955",
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"pub_year": "2016",
"author_list": "Staubert, R.; Klochkov, D.; et el."
},
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"eprint_status": "archive",
"datestamp": "2023-08-20 11:53:02",
"lastmod": "2023-10-20 16:55:21",
"type": "article",
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"items": [
{
"id": "Yukita-Mihoko",
"name": {
"family": "Yukita",
"given": "M."
},
"orcid": "0000-0001-6366-3459"
},
{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "A. E."
},
"orcid": "0000-0001-8667-2681"
},
{
"id": "Lehmer-B-D",
"name": {
"family": "Lehmer",
"given": "B. D."
},
"orcid": "0000-0003-2192-3296"
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "D. R."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Zezas-A",
"name": {
"family": "Zezas",
"given": "A."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Antoniou-V",
"name": {
"family": "Antoniou",
"given": "V."
},
"orcid": "0000-0001-7539-1593"
},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T. J."
},
"orcid": "0000-0003-0976-4755"
},
{
"id": "Replicon-V",
"name": {
"family": "Replicon",
"given": "V."
}
},
{
"id": "Tyler-J-B",
"name": {
"family": "Tyler",
"given": "J. B."
}
},
{
"id": "Venters-T-M",
"name": {
"family": "Venters",
"given": "T."
}
},
{
"id": "Argo-M-K",
"name": {
"family": "Argo",
"given": "M. K."
}
},
{
"id": "Bechtol-K",
"name": {
"family": "Bechtol",
"given": "K."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "R."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Kuntz-K",
"name": {
"family": "Kuntz",
"given": "K."
}
},
{
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"name": {
"family": "Stern",
"given": "D."
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"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A Hard X-Ray Study of the Normal Star-forming Galaxy M83 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: individual: M83, galaxies: starburst, galaxies: star formation, X-rays: galaxies",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 September 9; accepted 2016 March 25; published 2016 June 20. \n\nWe thank the referee for useful comments and suggests that improved this paper. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We sincerely thank Karl Forster and Brian Grefenstette for their work on the complicated stray light pattern and for assistance in designing the NuSTAR observational setup for minimizing this contamination. We also thank NuSTAR and Chandra mission planners for making the Chandra and NuSTAR observations simultaneous. We also thank P. Tzanavaris and D. Swartz for helpful discussion. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO4-15086Z issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. R.K. acknowledges support from Russian Science Foundation (grant 14-12-01315). \n\nFacilities: Chandra - , NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM-Newton - .\n\nPublished - 2016-49.pdf
",
"abstract": "We present the results from sensitive, multi-epoch NuSTAR observations of the late-type star-forming galaxy M83 (d = 4.6 Mpc). This is the first investigation to spatially resolve the hard (E > 10 keV) X-ray emission of this galaxy. The nuclear region and ~20 off-nuclear point sources, including a previously discovered ultraluminous X-ray source, are detected in our NuSTAR observations. The X-ray hardnesses and luminosities of the majority of the point sources are consistent with hard X-ray sources resolved in the starburst galaxy NGC 253. We infer that the hard X-ray emission is most likely dominated by intermediate accretion state black hole binaries and neutron star low-mass X-ray binaries (Z-sources). We construct the X-ray binary luminosity function (XLF) in the NuSTAR band for an extragalactic environment for the first time. The M83 XLF has a steeper XLF than the X-ray binary XLF in NGC 253, which is consistent with previous measurements by Chandra at softer X-ray energies. The NuSTAR integrated galaxy spectrum of M83 drops quickly above 10 keV, which is also seen in the starburst galaxies NGC 253, NGC 3310, and NGC 3256. The NuSTAR observations constrain any active galactic nucleus (AGN) to be either highly obscured or to have an extremely low luminosity of \u227e 10^(38) erg s^(\u22121) (10\u201330 keV), implying that it is emitting at a very low Eddington ratio. An X-ray point source that is consistent with the location of the nuclear star cluster with an X-ray luminosity of a few times 10^(38) erg s^(\u22121) may be a low-luminosity AGN but is more consistent with being an X-ray binary.",
"date": "2016-06",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "824",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 107",
"id_number": "CaltechAUTHORS:20160804-095528789",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160804-095528789",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "GO4-15086Z"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01315"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-49",
"name": "Space Radiation Laboratory"
}
]
},
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"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.3847/0004-637X/824/2/107",
"primary_object": {
"basename": "2016-49.pdf",
"url": "https://authors.library.caltech.edu/records/0wnk5-3f304/files/2016-49.pdf"
},
"pub_year": "2016",
"author_list": "Yukita, M.; Hornschemeier, A. E.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/96zyw-xdd18",
"eprint_id": 69060,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:52:19",
"lastmod": "2023-10-20 16:29:21",
"type": "article",
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"creators": {
"items": [
{
"id": "Lanzuisi-G",
"name": {
"family": "Lanzuisi",
"given": "G."
},
"orcid": "0000-0001-9094-0984"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
}
]
},
"title": "NuSTAR reveals the extreme properties of the super-Eddington accreting supermassive black hole in PG 1247+267",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 ESO. \n\nReceived 17 February 2016. Accepted 21 March 2016. Published online 13 May 2016.\n\nWe thank the anonymous referee for constructive comments\nthat have helped us to improve the quality of the paper. G.L. thanks F. Gastaldello for useful insights on NuSTAR background issues, E. Dalessandro for advice about HST data, and O. Shemmer for help with the Swift data. G.L. acknowledges financial support from the CIG grant \"eEASY\" No. 321913 and from ASI-INAF 2014-045-R.0 and ASI/INAF I/037/12/0\u2013011/13 grants. A.C.F. acknowledges support from ERC grant 340442. FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT Regular 1141218, \"EMBIGGEN\" Anillo ACT1101), the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS.W.N.B. and B.L. acknowledges support from Caltech NuSTAR subcontract 44A-1092750. This work made use of data from the NuSTAR mission, a project led by the California Institute of\nTechnology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - aa28325-16.pdf
",
"abstract": "PG1247+267 is one of the most luminous known quasars at z ~ 2 and is a strongly super-Eddington accreting supermassive black hole (SMBH) candidate. We obtained NuSTAR data of this intriguing source in December 2014 with the aim of studying its high-energy emission, leveraging the broad band covered by the new NuSTAR and the archival XMM-Newton data. Several measurements are in agreement with the super-Eddington scenario for PG1247+267: the soft power law (\u0393 = 2.3 \u00b1 0.1); the weak ionized Fe emission line; and a hint of the presence of outflowing ionized gas surrounding the SMBH. The presence of an extreme reflection component is instead at odds with the high accretion rate proposed for this quasar. This can be explained with three different scenarios; all of them are in good agreement with the existing data, but imply very different conclusions: i) a variable primary power law observed in a low state, superimposed on a reflection component echoing a past, higher flux state; ii) a power law continuum obscured by an ionized, Compton thick, partial covering absorber; and iii) a relativistic disk reflector in a lamp-post geometry, with low coronal height and high BH spin. The first model is able to explain the high reflection component in terms of variability. The second does not require any reflection to reproduce the hard emission, while a rather low high-energy cutoff of ~100 keV is detected for the first time in such a high redshift source. The third model require a face-on geometry, which may affect the SMBH mass and Eddington ratio measurements. Deeper X-ray broad-band data are required in order to distinguish between these possibilities.",
"date": "2016-06",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "590",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A77",
"id_number": "CaltechAUTHORS:20160715-122452015",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160715-122452015",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "321913 eEasy"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "2014-045-R0"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0\u2013011/13"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "340442"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "Istituto Nazionale di Fisica Nucleare (INFN)"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-57",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201628325",
"primary_object": {
"basename": "aa28325-16.pdf",
"url": "https://authors.library.caltech.edu/records/96zyw-xdd18/files/aa28325-16.pdf"
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"pub_year": "2016",
"author_list": "Lanzuisi, G.; Harrison, F. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/f22ed-kr034",
"eprint_id": 66284,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:42:04",
"lastmod": "2023-10-18 17:19:40",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Wierzcholska-A",
"name": {
"family": "Wierzcholska",
"given": "A."
}
},
{
"id": "Siejkowski-H",
"name": {
"family": "Siejkowski",
"given": "H."
}
}
]
},
"title": "First hard X-ray observations of the blazar S5 0716+714 with NuSTAR during a multiwavelength campaign",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 February 21. Received 2016 February 21. In original form 2015 September 8. First published online February 24, 2016. \n\nThe authors thank anonymous referee for suggestions and remarks provided. This research was supported in part by PLGrid Infrastructure. The plots presented in this paper are rendered using MATPLOTLIB (Hunter 2007).\n\nPublished - 2350.full.pdf+html
",
"abstract": "We report the results of a multifrequency campaign targeting S5 0716+714 in the flaring state of the source observed in 2015 January and February. The observations have been performed using the following instruments: Fermi/Large Area Telescope (LAT), Nuclear Spectroscopic Telescope Array, X-ray Telescope and Ultraviolet/Optical Telescope. The elevated flux level was visible in all frequencies and the outburst consists of five sub-flares. In this paper, we focus on the analysis of the X-ray observations both in the soft and hard regimes for data collected with NuSTAR and Swift/XRT. This is the first time, when hard X-ray observations of the source collected with NuSTAR are reported. The studies reveal both low- and high-energy components clearly visible in the energy band, with the break energy of 8 keV, which is the highest break energy ever reported for S5 0716+714. The second part of this work is concentrated on multifrequency observations collected during the flaring activity period. The variability patterns recorded during the period are characterized using a fractional variability amplitude and description of the flare profiles. The correlation studies reveal strong and significant relation between the optical, ultraviolet and \u03b3-ray observations, and no time lag is found for any of the studied relations.",
"date": "2016-05-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "458",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2350-2359",
"id_number": "CaltechAUTHORS:20160419-142247557",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160419-142247557",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw425",
"primary_object": {
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"pub_year": "2016",
"author_list": "Wierzcholska, A. and Siejkowski, H."
},
{
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"datestamp": "2023-08-22 17:56:14",
"lastmod": "2023-10-18 16:03:29",
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"items": [
{
"id": "Lotti-S",
"name": {
"family": "Lotti",
"given": "Simone"
},
"orcid": "0000-0002-3088-1561"
},
{
"id": "Natalucci-L",
"name": {
"family": "Natalucci",
"given": "Lorenzo"
},
"orcid": "0000-0002-6601-9543"
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Baganoff-F-K",
"name": {
"family": "Baganoff",
"given": "Frederick K."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "Jaesub"
}
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Zhang-Shuo",
"name": {
"family": "Zhang",
"given": "Shuo"
},
"orcid": "0000-0002-2967-790X"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR and XMM-Newton observations of 1E1743.1-2843: indications of a neutron star LMXB nature of the compact object",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; stars: neutron; X-rays: binaries; X-rays: individual (1E1743.1-2843)",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 October 16; accepted 2016 March 4; published 2016 May 5.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The Italian authors acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0. RK acknowledges support from Russian Science Foundation (grant 14-22-00271).\n\nPublished - apj_822_1_57.pdf
Submitted - 1603.02016v2.pdf
",
"abstract": "We report on the results of NuSTAR and XMM-Newton observations of the persistent X-ray source 1E1743.1-2843, located in the Galactic Center region. The source was observed between 2012 September and October by NuSTAR and XMM-Newton, providing almost simultaneous observations in the hard and soft X-ray bands. The high X-ray luminosity points to the presence of an accreting compact object. We analyze the possibilities of this accreting compact object being either a neutron star (NS) or a black hole, and conclude that the joint XMM-Newton and NuSTAR spectrum from 0.3 to 40 keV fits a blackbody spectrum with kT ~ 1.8 keV emitted from a hot spot or an equatorial strip on an NS surface. This spectrum is thermally Comptonized by electrons with kT_e ~ 4.6 keV. Accepting this NS hypothesis, we probe the low-mass X-ray binary (LMXB) or high-mass X-ray binary (HMXB) nature of the source. While the lack of Type-I bursts can be explained in the LMXB scenario, the absence of pulsations in the 2 mHz\u201349 Hz frequency range, the lack of eclipses and of an IR companion, and the lack of a K_\u0251line from neutral or moderately ionized iron strongly disfavor interpreting this source as a HMXB. We therefore conclude that 1E1743.1-2843 is most likely an NS-LMXB located beyond the Galactic Center. There is weak statistical evidence for a soft X-ray excess which may indicate thermal emission from an accretion disk. However, the disk normalization remains unconstrained due to the high hydrogen column density (N_H ~ 1.6 x 10^(23)cm^(-2).",
"date": "2016-05-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "822",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 57",
"id_number": "CaltechAUTHORS:20160318-104326136",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160318-104326136",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-22-00271"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-55",
"name": "Space Radiation Laboratory"
}
]
},
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"items": [
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"id": "NuSTAR"
}
]
},
"doi": "10.3847/0004-637X/822/1/57",
"primary_object": {
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}
],
"pub_year": "2016",
"author_list": "Lotti, Simone; Natalucci, Lorenzo; et el."
},
{
"id": "https://authors.library.caltech.edu/records/6rkhd-asw49",
"eprint_id": 67431,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:26:37",
"lastmod": "2023-10-18 21:10:59",
"type": "article",
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"creators": {
"items": [
{
"id": "Wilkins-D-R",
"name": {
"family": "Wilkins",
"given": "D. R."
}
}
]
},
"title": "Driving extreme variability: Measuring the evolving coronae and evidence for jet launching in AGN",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.",
"abstract": "Relativistically blurred reflection from the accretion disc provides a powerful probe of the extreme environments close to supermassive black holes; the inner regions of the accretion flow and the corona that produces the intense X-ray continuum. Techniques by which the geometry and extent of the corona can be measured through the observed X-ray spectrum are reviewed along with the evolution in the structure of the corona that is seen to accompany variations in the X-ray luminosity both on long and short timescales. Detailed analyses of the narrow line Seyfert 1 galaxies Mrk 335 and 1H 0707-495, over observations with XMM-Newton as well as Suzaku and NuSTAR spanning nearly a decade reveal that increases in the X-ray luminosity coincide with an expansion of the corona to cover a larger area of the inner accretion disc. Underlying this long timescale variability lie more complex patterns of behaviour on short timescales. Flares in the X-ray emission during a low flux state of Mrk 335 observed in 2013 and 2014 are found to mark a reconfiguration of the corona while there is evidence that the flares were caused by a vertical collimation and ejection of coronal material, reminiscent of an aborted jet-launching event. Measurements of the corona and reflecting accretion disc are combined to infer the conditions on the inner disc that lead to the flaring event.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "557-562",
"id_number": "CaltechAUTHORS:20160527-092024172",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-092024172",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
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}
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},
"doi": "10.1002/asna.201612347",
"pub_year": "2016",
"author_list": "Wilkins, D. R."
},
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"items": [
{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
}
},
{
"id": "Petrucci-P-O",
"name": {
"family": "Petrucci",
"given": "P.-O."
}
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Cappi-M",
"name": {
"family": "Cappi",
"given": "M."
}
},
{
"id": "De-Marco-B",
"name": {
"family": "De Marco",
"given": "B."
}
},
{
"id": "De-Rosa-A",
"name": {
"family": "De Rosa",
"given": "A."
},
"orcid": "0000-0001-5668-6863"
},
{
"id": "Malzac-J",
"name": {
"family": "Malzac",
"given": "J."
}
},
{
"id": "Ponti-G",
"name": {
"family": "Ponti",
"given": "G."
},
"orcid": "0000-0003-0293-3608"
}
]
},
"title": "High-energy monitoring of Seyfert galaxies: The case of NGC 4593",
"ispublished": "pub",
"full_text_status": "restricted",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.",
"abstract": "We discuss preliminary results from a joint XMM-Newton and NuSTAR monitoring program on the active galactic nucleus NGC 4593, consisting of 5\u00d720 ks observations, spaced by two days, performed in January 2015. The source is found to be variable, both in flux and spectral shape, on time scales as short as a few ks. The spectrum clearly softens when the source brightens. A simple timing analysis suggests the presence of a variable soft excess that correlates with the primary continuum.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "552-556",
"id_number": "CaltechAUTHORS:20160527-092521863",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-092521863",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612346",
"pub_year": "2016",
"author_list": "Ursini, F.; Petrucci, P.-O.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/c461p-1xq35",
"eprint_id": 67440,
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"datestamp": "2023-08-20 11:27:13",
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"items": [
{
"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "A."
}
},
{
"id": "Tortosa-A",
"name": {
"family": "Tortosa",
"given": "A."
}
}
]
},
"title": "The coronal parameters of local Seyfert galaxies",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. \n\nAM and AT acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n.312789. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nSubmitted - 1511.01332v1.pdf
",
"abstract": "One of the open problems for AGN is the nature of the primary X-ray emission: It is likely due to Comptonization of soft UV photons, but the optical depth and temperature of the emitting corona were largely unknown before the launch of the Nuclear Spectroscopic Telescope Array (NuSTAR). It is the first focusing hard X-ray telescope on orbit, \u223c 100 times more sensitive in the 10-79 keV band compared to previous observatories, enabling the study of AGN at high energies with high precision. We present and discuss the results on the hot corona parameters of active galactic nuclei that have been recently measured with NuSTAR (often in coordination with XMM-Newton, Suzaku, or wift) with unprecedented accuracy, in a number of local Seyfert galaxies.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "490-494",
"id_number": "CaltechAUTHORS:20160527-102828359",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-102828359",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "European Union Seventh Framework Programme (FP7/2007-2013)",
"grant_number": "312789"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"items": [
{
"id": "NuSTAR"
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"doi": "10.1002/asna.201612335",
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"pub_year": "2016",
"author_list": "Marinucci, A. and Tortosa, A."
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"items": [
{
"id": "Hori-T",
"name": {
"family": "Hori",
"given": "T."
}
},
{
"id": "Ueda-Y",
"name": {
"family": "Ueda",
"given": "Y."
}
},
{
"id": "Done-C",
"name": {
"family": "Done",
"given": "C."
}
},
{
"id": "Shidatsu-M",
"name": {
"family": "Shidatsu",
"given": "M."
}
},
{
"id": "Kawamuro-T",
"name": {
"family": "Kawamuro",
"given": "T."
}
},
{
"id": "Kubota-A",
"name": {
"family": "Kubota",
"given": "A."
}
},
{
"id": "Nakahira-S",
"name": {
"family": "Nakahira",
"given": "S."
}
}
]
},
"title": "Broadband X-ray study of the galactic black hole binary 4U 1630-47 with Suzaku",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.",
"abstract": "We present the results from our Suzaku observations of the Galactic black hole binary 4U 1630-47. 4U 1630-47 was observed in the very high state (VHS) during the 2012 September-October outburst. The inner disk appears slightly truncated by comparison with a previous high/soft state (HSS) of this source, even by taking into account energetic coupling between the disk and corona. The spectra do not show the Doppler-shifted emission lines indicating baryonic jets that were seen four days previously in an XMM-Newton observation, despite the source being in a similar state. There are no significant absorption lines from highly ionized iron ions. We also observed 4U 1630-47 in the HSS simultaneously with Suzaku and NuSTAR in an early epoch of the 2015 outburst. All Suzaku spectra in the HSS show variable iron-K absorption line features. We find that the ionization state of the disk wind rapidly increased when the continuum showed significant spectral hardening. This behavior is consistent with that expected from a thermally driven wind.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "467-472",
"id_number": "CaltechAUTHORS:20160527-105327275",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-105327275",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612331",
"pub_year": "2016",
"author_list": "Hori, T.; Ueda, Y.; et el."
},
{
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"eprint_id": 67448,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:27:25",
"lastmod": "2023-10-18 21:11:52",
"type": "article",
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"creators": {
"items": [
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "H. M."
},
"orcid": "0000-0001-5857-5622"
}
]
},
"title": "An intermediate-mass black hole candidate in M51?",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. \n\nWe gratefully acknowledge support from the Science and Technology Facilities Council (HE through grant ST/K501979/1).\n\nSubmitted - 1510.02277v1.pdf
",
"abstract": "We present the current results of an investigation into M51 ULX-7, using archival data from XMM-Newton, Chandra and NuSTAR, and optical and radio data from HST and VLA. The source has a consistently hard power-law X-ray spectrum and high short-term variability. This is unusual variability behaviour for a ULX, as we would expect highly variable ULXs to have soft energy spectra. The power spectrum features a break at \u223c 10^(\u20133) Hz, from low frequency spectral index \u03b1 = 0.1 to high frequency spectral index \u03b1 = 0.8, analogous to the low frequency break found in power spectra of black holes accreting in the low/hard state. We do not observe a corresponding high frequency break, however taking the white noise level as a frequency lower limit of the break, we can calculate a black hole mass upper limit of 9.12\u00d7104 M, assuming that the ULX is in the low/hard state. While there is no radio detection, we find a flux density upper limit of 87 \u00b5Jy/beam. Using the X-ray/radio fundamental plane, we calculate a black hole mass upper limit of 1.95\u00d710^5 M\u00ae. Therefore, this ULX is consistent with being an IMBH accreting in the low/hard state.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "448-453",
"id_number": "CaltechAUTHORS:20160527-110052419",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-110052419",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612328",
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"basename": "1510.02277v1.pdf",
"url": "https://authors.library.caltech.edu/records/zt1n1-12203/files/1510.02277v1.pdf"
},
"pub_year": "2016",
"author_list": "Earnshaw, H. M."
},
{
"id": "https://authors.library.caltech.edu/records/3v1fv-tn056",
"eprint_id": 67443,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:27:17",
"lastmod": "2023-10-18 21:11:41",
"type": "article",
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"creators": {
"items": [
{
"id": "Kobayashi-S",
"name": {
"family": "Kobayashi",
"given": "S."
}
},
{
"id": "Nakazawa-K",
"name": {
"family": "Nakazawa",
"given": "K."
}
},
{
"id": "Makishima-K",
"name": {
"family": "Makishima",
"given": "K."
}
}
]
},
"title": "A new characterization of the Compton process in the ULX spectra",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.\n\nSubmitted - 1511.07975v1.pdf
",
"abstract": "Attempts were made to construct a unified description of the spectra of ULX (Ultra Luminous X-ray source) objects, including their Power-Law (PL) state and Disk-like state. Among spectral models proposed to explain either state, the present work adopts the one which combines multi-color disk (MCD) emission and its thermal Comptonization (THC). This model was applied to several datasets of ULXs obtained by Suzaku, XMM-Newton, and Nustar. The model well explains all the spectra, regardless of the spectral states, in terms of a cool disk (inner radius temperature of 0.2-0.5 keV) and a cool thick (electron temperature of 1-3 keV, and optical thickness ~10) corona. The fit results can be characterized by two new parameters. One is Q (defined as the electron temerature divided by the inner radius temperature) which describes balance between the Compton cooling and gravitational heating of the coronal electrons, while the other is F, namely, the covering fraction of the MCD by the corona. Here, F is calculated from the percentage of the directly-visible disk luminosity in the total radiation. Then, the PL-state spectra have been found to show Q~10 and F~0.5, while those of the Disk-like state Q~3 and F~1. Thus, the two states are clearly separated in terms of Q and F. The obtained results are employed to argue for their interpretation in terms of high-mass (several tens to several hundreds solar masses) black holes.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "479-484",
"id_number": "CaltechAUTHORS:20160527-104705688",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-104705688",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612333",
"primary_object": {
"basename": "1511.07975v1.pdf",
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"pub_year": "2016",
"author_list": "Kobayashi, S.; Nakazawa, K.; et el."
},
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"datestamp": "2023-08-20 11:24:56",
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"type": "article",
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"creators": {
"items": [
{
"id": "Masini-A",
"name": {
"family": "Masini",
"given": "A."
},
"orcid": "0000-0002-7100-9366"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Zaw-I",
"name": {
"family": "Zaw",
"given": "I."
}
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M. J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G."
}
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "E."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR observations of water megamaser AGN",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "masers \u2013 galaxies: active \u2013 galaxies: Seyfert",
"note": "\u00a9 2016 ESO. Article published by EDP Sciences. \n\nReceived 3 November 2015; Accepted 9 February 2016; Published online 13 April 2016. \n\nWe thank the anonymous referee for useful suggestions that helped to improve the paper. This work was supported under NASA Contract NNG08FD60C, and it made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.M., A.C., and S.P. acknowledge support from the ASI/INAF grant I/037/12/0-011/13. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., C.R.), FONDECYT 1141218 (F.E.B., C.R.), \"EMBIGGEN\" Anillo ACT1101 (F.E.B., C.R.), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F. E. B.). W. N. B. acknowledges support from NuSTAR subcontract 44A-1092750.\n\nPublished - aa27689-15.pdf
Submitted - 1602.03185v1.pdf
",
"abstract": "Aims. We study the connection between the masing disk and obscuring torus in Seyfert 2 galaxies. \nMethods. We present a uniform X-ray spectral analysis of the high energy properties of 14 nearby megamaser active galactic nuclei observed by NuSTAR. We use a simple analytical model to localize the maser disk and understand its connection with the torus by combining NuSTAR spectral parameters with the available physical quantities from VLBI mapping.\nResults. Most of the sources that we analyzed are heavily obscured, showing a column density in excess of ~10^(23) cm^(-2); in particular, 79% are Compton-thick (N_H > 1.5 \u00d7 10^(24) cm^(-2)). When using column densities measured by NuSTAR with the assumption that the torus is the extension of the maser disk, and further assuming a reasonable density profile, we can predict the torus dimensions. They are found to be consistent with mid-IR interferometry parsec-scale observations of Circinus and NGC 1068. In this picture, the maser disk is intimately connected to the inner part of the torus. It is probably made of a large number of molecular clouds that connect the torus and the outer part of the accretion disk, giving rise to a thin disk rotating in most cases in Keplerian or sub-Keplerian motion. This toy model explains the established close connection between water megamaser emission and nuclear obscuration as a geometric effect.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "589",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A59",
"id_number": "CaltechAUTHORS:20160318-101742575",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160318-101742575",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NuSTAR",
"grant_number": "44A-1092750"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-19",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1051/0004-6361/201527689",
"primary_object": {
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"basename": "aa27689-15.pdf",
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],
"pub_year": "2016",
"author_list": "Masini, A.; Comastri, A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/4cc4t-mjx47",
"eprint_id": 67449,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:27:29",
"lastmod": "2023-10-18 21:11:55",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
}
]
},
"title": "Unwrapping the X-ray spectra of active galactic nuclei",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. \n\nThe author thanks Laura Brenneman, Andy Fabian, Anne Lohfink, and Francesco Tombesi for insightful discussions that have informed much of the discussion in this paper. The author is grateful for financial support from the Simons Foundation (through a Simons Fellowship in Theoretical Physics), a Sackler Fellowship (hosted by the Institute of Astronomy, Cambridge), and NASA under grant NNX14AF86G.\n\nSubmitted - 1510.07638v1.pdf
",
"abstract": "Active galactic nuclei (AGN) are complex phenomena. At the heart of an AGN is a relativistic accretion disk around a spinning supermassive black hole (SMBH) with an X-ray emitting corona and, sometimes, a relativistic jet. On larger scales, the outer accretion disk and molecular torus act as the reservoirs of gas for the continuing AGN activity. And on all scales from the black hole outwards, powerful winds are seen that probably affect the evolution of the host galaxy as well as regulate the feeding of the AGN itself. In this review article, we discuss how X-ray spectroscopy can be used to study each of these components. We highlight how recent measurements of the high-energy cutoff in the X-ray continuum by NuSTAR are pushing us to conclude that X-ray coronae are radiatively-compact and have electron temperatures regulated by electron-positron pair production. We show that the predominance of rapidly-rotating objects in current surveys of SMBH spin is entirely unsurprising once one accounts for the observational selection bias resulting from the spin-dependence of the radiative efficiency. We review recent progress in our understanding of fast (v\u02dc (0.1-0.3)c, highly-ionized (mainly visible in Fe XXV and Fe XXVI lines), high-column density winds that may dominate quasar-mode galactic feedback. Finally, we end with a brief look forward to the promise of Astro-H and future X-ray spectropolarimeters.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "404-409",
"id_number": "CaltechAUTHORS:20160527-111228804",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-111228804",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Simons Foundation"
},
{
"agency": "Sackler Fellowship Program (Cambridge)"
},
{
"agency": "NASA",
"grant_number": "NNX14AF86G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612321",
"primary_object": {
"basename": "1510.07638v1.pdf",
"url": "https://authors.library.caltech.edu/records/4cc4t-mjx47/files/1510.07638v1.pdf"
},
"pub_year": "2016",
"author_list": "Reynolds, C. S."
},
{
"id": "https://authors.library.caltech.edu/records/jd088-pch67",
"eprint_id": 67456,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:27:32",
"lastmod": "2023-10-18 21:12:21",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "T."
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "J."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J."
},
"orcid": "0000-0003-2065-5410"
}
]
},
"title": "Relativistic reflection: Review and recent developments in modeling",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.",
"abstract": "Measuring relativistic reflection is an important tool to study the innermost regions of the an accreting black hole system. In the following we present a brief review on the different aspects contributing to the relativistic reflection. The combined approach is for the first time incorporated in the new \"relxill\" model. The advantages of this more self-consistent approach are briefly summarized. A special focus is put on the new definition of the intrinsic reflection fraction in the lamp post geometry, which allows to draw conclusions about the primary source of radiation in these system. Additionally the influence of the high energy cutoff of the primary source on the reflection spectrum is motivated, revealing the remarkable capabilities of constraining E_cut by measuring relativistic reflection spectra from NuSTAR, preferably with lower energy coverage.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "362-367",
"id_number": "CaltechAUTHORS:20160527-121830000",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-121830000",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612314",
"pub_year": "2016",
"author_list": "Dauser, T.; Garc\u00eda, J.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/kxab9-abm25",
"eprint_id": 67434,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:26:55",
"lastmod": "2023-10-18 21:11:12",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Roberts-T-P",
"name": {
"family": "Roberts",
"given": "T. P."
},
"orcid": "0000-0001-8252-6337"
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "M. J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Sutton-A-D",
"name": {
"family": "Sutton",
"given": "A. D."
}
},
{
"id": "Mezcua-M",
"name": {
"family": "Mezcua",
"given": "M."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Heil-L-M",
"name": {
"family": "Heil",
"given": "L. M."
}
}
]
},
"title": "ULX behaviour: The ultraluminous state, winds and interesting anomalies",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: binaries \u2013 accretion, accretion disks \u2013 black hole physics",
"note": "\u00a9 2016: WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim. \n\nTPR acknowledges support from STFC as part of the consolidated grant ST/L00075X/1. MM acknowledges financial support from NASA Chandra Grant G05-16099X. All data used is, or will be, public in the relevant mission archives.\n\nSubmitted - 1510.06200v1.pdf
",
"abstract": "Recent evidence - in particular the hard X-ray spectra obtained by {NuSTAR}, and the large amplitude hard X-ray variability observed when ULXs show soft spectra - reveals that common ultraluminous X-ray source (ULX) behaviour is inconsistent with known sub-Eddington accretion modes, as would be expected for an intermediate-mass black hole (IMBH). Instead, it appears that the majority of ULXs are powered by super-Eddington accretion onto stellar-mass black holes. Here, we will review work that delves deeper into ULX spectral-timing behaviour, demonstrating it remains consistent with the expectations of super-Eddington accretion. One critical missing piece from this picture is the direct detection of the massive, radiatively-driven winds expected from ULXs as atomic emission/absorption line features in ULX spectra; we will show it is very likely these have already been detected as residuals in the soft X-ray spectra of ULXs. Finally, we will discuss ULXs that do not appear to conform to the emerging ULX behaviour patterns. In particular we discuss the implications of the identification of a good IMBH candidate as a background QSO; and the confirmation of an IMBH/ULX candidate in the galaxy NGC 2276 via the radio/X-ray fundamental plane.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "534-540",
"id_number": "CaltechAUTHORS:20160527-093054394",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-093054394",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "NASA",
"grant_number": "G05-16099X"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612343",
"primary_object": {
"basename": "1510.06200v1.pdf",
"url": "https://authors.library.caltech.edu/records/kxab9-abm25/files/1510.06200v1.pdf"
},
"pub_year": "2016",
"author_list": "Roberts, T. P.; Middleton, M. J.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/vvekr-tth64",
"eprint_id": 67439,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:27:09",
"lastmod": "2023-10-18 21:11:31",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Risalti-G",
"name": {
"family": "Risaliti",
"given": "G."
}
}
]
},
"title": "Absorption from a multi-layer circumnuclear medium and reflection from the accretion disc in NGC 1365",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.",
"abstract": "NGC 1365 hosts an X-ray obscured AGN known for both its variable absorption and its relativistic features in the reflection component. Recent simultaneous observations performed by XMM-Newton and NuSTAR caught the source in a rare, nearly unobscured state, revealing the presence of a warm absorber and a neutral, but low column density (\u223c 10^(22) cm^-2) absorber, usually not observable due to thicker layers along the line of sight. Here I propose a multi-layer structure of the circumnuclear medium which can explain all the observed absorption states of this source, and their variability properties. Remarkably, despite the spectral complexity due to this multi-component absorber, the relativistic reflection component (and hence the black hole spin) can be unambiguously measured through a time resolved spectroscopic analysis.",
"date": "2016-05",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "337",
"number": "4-5",
"publisher": "Wiley",
"pagerange": "529-533",
"id_number": "CaltechAUTHORS:20160527-102505729",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160527-102505729",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1002/asna.201612342",
"pub_year": "2016",
"author_list": "Risaliti, G."
},
{
"id": "https://authors.library.caltech.edu/records/zzawq-hgg41",
"eprint_id": 59134,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:48:18",
"lastmod": "2023-10-23 20:06:12",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram"
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Loh-Alan",
"name": {
"family": "Loh",
"given": "Alan"
}
},
{
"id": "Corbel-S",
"name": {
"family": "Corbel",
"given": "St\u00e9phane"
}
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "Deepto"
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William"
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles"
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Rahoui-F",
"name": {
"family": "Rahoui",
"given": "Farid"
},
"orcid": "0000-0001-7655-4120"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "Shriharsh P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Characterizing X-ray and Radio emission in the Black Hole X-Ray Binary V404 Cygni during Quiescence",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; stars: black holes; stars: individual (V404 Cyg); X-rays: binaries",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 July 14; accepted 2016 February 10; published 2016 April 19. \n\nWe thank Michael A. Nowak for useful discussion on synchrotron model. This work was supported under NASA contract No. NNG08FD60C,and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operation, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). SC would like to thank James Miller-Jones for excellent help during the preparation of the JVLA observations. SC and AJ acknowledges the financial support from the UnivEarthS Labex programme of Sorbonne Paris Cit\u00b4e (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), and from the CHAOS project ANR-12-BS05-0009 supported by the French Research National Agency. JAT acknowledges partial support from NASA under XMM-Newton Guest Observer grant NNX14AF08G. \n\nFacilities: NuSTAR, XMM-Newton, JVLA.\n\nPublished - apj_821_2_103.pdf
Submitted - 1507.04049v1.pdf
",
"abstract": "We present results from multi-wavelength simultaneous X-ray and radio observations of the black hole X-ray binary V404 Cyg in quiescence. Our coverage with NuSTAR provides the very first opportunity to study the X-ray spectrum of V404 Cyg at energies above 10 keV. The unabsorbed broadband (0.3\u201330 keV) quiescent luminosity of the source is 8.9 \u00d7 10^(32) erg s^(\u22121) for a distance of 2.4 kpc. The source shows clear variability on short timescales (an hour to a couple of hours) in the radio, soft X-ray, and hard X-ray bands in the form of multiple flares. The broadband X-ray spectra obtained from XMM-Newton and NuSTAR can be characterized with a power-law model having a photon index of \u0393 = 2.12 \u00b1 0.07 (90% confidence errors); however, residuals at high energies indicate spectral curvature significant at a 3\u03c3 confidence level with the e-folding energy of the cutoff as 20_(-7)^(+20) keV. Such curvature can be explained using synchrotron emission from the base of a jet outflow. Radio observations using the VLA reveal that the spectral index evolves on very fast timescales (as short as 10 minutes), switching between optically thick and thin synchrotron emission, possibly due to instabilities in the compact jet or stochastic instabilities in the accretion rate. We explore different scenarios to explain this very fast variability.",
"date": "2016-04-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "821",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 103",
"id_number": "CaltechAUTHORS:20150801-085134688",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150801-085134688",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-10-LABX-0023"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-11-IDEX-0005-02"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-12-BS05-0009"
},
{
"agency": "NASA",
"grant_number": "NNX14AF08G"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-58",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/0004-637X/821/2/103",
"primary_object": {
"basename": "1507.04049v1.pdf",
"url": "https://authors.library.caltech.edu/records/zzawq-hgg41/files/1507.04049v1.pdf"
},
"related_objects": [
{
"basename": "apj_821_2_103.pdf",
"url": "https://authors.library.caltech.edu/records/zzawq-hgg41/files/apj_821_2_103.pdf"
}
],
"pub_year": "2016",
"author_list": "Rana, Vikram; Loh, Alan; et el."
},
{
"id": "https://authors.library.caltech.edu/records/yzvwa-c4g12",
"eprint_id": 65482,
"eprint_status": "archive",
"datestamp": "2023-08-20 11:14:50",
"lastmod": "2023-10-18 16:03:32",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Pinto-C",
"name": {
"family": "Pinto",
"given": "C."
},
"orcid": "0000-0003-2532-7379"
},
{
"id": "Alston-W-N",
"name": {
"family": "Alston",
"given": "W."
},
"orcid": "0000-0003-2658-6559"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The rhythm of Fairall 9 - I: Observing the spectral variability with XMM-Newton and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: individual(Fairall 9) \u2013 X-rays: galaxies \u2013 galaxies: nuclei \u2013 galaxies: Seyfert\n\u2013black hole physics",
"note": "\u00a9 2016 The American Astronomical Society. All rights reserved. Received 2015 July 5; accepted 2016 February 17; published 2016 April 4. \n\nWe thank the referee for their comments that have helped to improve the clarity of the paper. AL and ACF acknowledge support from ERC Advanced Grant FEEDBACK. CSR thanks the Simons Foundation Fellows Program (US) and the Sackler Fellowship Program (Cambridge) for support. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA).\n\nPublished - apj_821_1_11.pdf
Submitted - 1602.05589v1.pdf
",
"abstract": "We present a multi-epoch X-ray spectral analysis of the Seyfert 1 galaxy Fairall 9. Our analysis\nshows that Fairall 9 displays unique spectral variability in that its ratio residuals to a simple absorbed\npower law in the 0.5-10 keV band remain constant with time in spite of large variations in flux. This\nbehavior implies an unchanging source geometry and the same emission processes continuously at\nwork at the timescale probed. With the constraints from NuSTAR on the broad-band spectral shape,\nit is clear that the soft excess in this source is a superposition of two different processes, one being\nblurred ionized reflection in the innermost parts of the accretion disk, and the other a continuum\ncomponent such as spatially distinct Comptonizing region. Alternatively, a more complex primary\nComptonization component together with blurred ionized reflection could be responsible.",
"date": "2016-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "821",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 11",
"id_number": "CaltechAUTHORS:20160318-105917798",
"issn": "0004-637X",
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"title": "NuSTAR and Swift observations of the very high state in GX 339-4: Weighing the black hole with X-rays",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 X-rays: binaries \u2013 X-rays: individual (GX 339-4)",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 October 14; accepted 2016 March 10; published 2016 April 7. \n\nWe are grateful to the referee for detailed and thoughtful comments that have significantly improved the paper. M.L.P. acknowledges financial support from the STFC. P.R. acknowledges financial contribution from ASI-INAF I/004/11/0 and ASI-INAF I/037/12/0. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology.\n\nPublished - apjl_821_1_L6.pdf
Submitted - 1603.03777v1.pdf
",
"abstract": "We present results from spectral fitting of the very high state of GX 339-4 with Nuclear Spectroscopic Telescope Array (NuSTAR) and Swift. We use relativistic reflection modeling to measure the spin of the black hole and inclination of the inner disk and find a spin of \u0251 = 0.95^(+0.02)_(-0.08) and inclination of 30\u00b0 \u00b1 1\u00b0 (statistical errors). These values agree well with previous results from reflection modeling. With the exceptional sensitivity of NuSTAR at the high-energy side of the disk spectrum, we are able to constrain multiple physical parameters simultaneously using continuum fitting. By using the constraints from reflection as input for the continuum fitting method, we invert the conventional fitting procedure to estimate the mass and distance of GX 339-4 using just the X-ray spectrum, finding a mass of 9.0^(+1.6)_(-1.2) M_\u2609 and distance of 8.4 \u00b1 0.9 kpc (statistical errors).",
"date": "2016-04-10",
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"pagerange": "Art. No. L6",
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"issn": "2041-8205",
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"agency": "Science and Technology Facilities Council (STFC)"
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{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/004/11/0"
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{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
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{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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{
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"title": "IC 751: a new changing-look AGN discovered by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual:IC 751; galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 November 28; accepted 2016 January 20; published 2016 March 10. \n\nWe thank the anonymous referee for comments that helped us to improve the quality of our manuscript. CR acknowledges Marko Stalevski and Sebastien Guillot for fruitful discussions, and Chin-Shin Chang for her comments on the manuscript. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). We acknowledge financial support from the CONICYT-Chile grants \"EMBIGGEN\" Anillo ACT1101 (CR, ET, FEB, PA), FONDECYT 1141218 (CR, FEB), FONDECYT 1140304 (PA), Basal-CATA PFB-06/2007 (CR, ET, FEB), NuSTAR subcontract 44A-1092750 (WNB), the Swiss National Science Foundation and Ambizione fellowship grant PZ00P2 154799/1 (MK), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center, and of the SIMBAD Astronomical Database which is operated by the Centre de Donn\u00e9es astronomiques de Strasbourg. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, XMM-Newton - .\n\nPublished - Ricci,C.Art.5.pdf
Submitted - 1602.00702v1.pdf
",
"abstract": "We present results of five Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the type 2 active galactic nucleus (AGN) in IC 751, three of which were performed simultaneously with XMM-Newton or Swift/X-Ray Telescope. We find that the nuclear X-ray source underwent a clear transition from a Compton-thick (N_H \u2243 2 x 10^(24)cm^(-2)) to a Compton-thin (N_H \u2243 4 x 10^(23) cm^(-2)) state on timescales of \u227e 3 months, which makes IC 751 the first changing look AGN discovered by NuSTAR. Changes of the line of sight column density at the ~2\u03c3 level are also found on a timescale of ~48 hr (\u0394N_H ~ 10^(23cm^(-2)). From the lack of spectral variability on timescales of ~100 ks, we infer that the varying absorber is located beyond the emission-weighted average radius of the broad-line region (BLR), and could therefore be related either to the external part of the BLR or a clumpy molecular torus. By adopting a physical torus X-ray spectral model, we are able to disentangle the column density of the non-varying absorber (N_H ~ 3.8 x 10^(23)cm^(-2)) from that of the varying clouds [N_H ~ (1-150) x 10^(22 cm^(-2)], and to constrain that of the material responsible for the reprocessed X-ray radiation (N_H ~ 6 x 10^(24) cm^(-2)). We find evidence of significant intrinsic X-ray variability, with the flux varying by a factor of five on timescales of a few months in the 2\u201310 and 10\u201350 keV band.",
"date": "2016-03-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "820",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 5",
"id_number": "CaltechAUTHORS:20160317-141351548",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160317-141351548",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICyT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
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"agency": "Basal-CATA",
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{
"agency": "NuSTAR",
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{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PZ00P2 154799/1"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
}
]
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"family": "Boggs",
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"title": "The first X-ray imaging spectroscopy of quiescent solar active regions with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Sun: X-rays, gamma rays; Sun: activity; Sun: corona",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 8; accepted 2016 March 2; published 2016 March 16. \n\nThis paper made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work is supported by: NASA grants NNX12AJ36G, NNX14AG07G, IGH (Royal Society University Research Fellowship), AM (NASA Earth Space Science Fellowship, NNX13AM41H), SK (Swiss National Science Foundation, 200021-140308), AC (NASA NNX15AK26G, NNX14AN84G). Thanks to Kim Tolbert for OSPEX help.\n\nPublished - apjl_820_1_L14.pdf
Submitted - 1603.01069v1.pdf
",
"abstract": "We present the first observations of quiescent active regions (ARs) using NuSTAR, a focusing hard X-ray telescope capable of studying faint solar emission from high temperature and non-thermal sources. We analyze the first directly imaged and spectrally resolved X-rays above 2~keV from non-flaring ARs, observed near the west limb on 2014 November 1. The NuSTAR X-ray images match bright features seen in extreme ultraviolet and soft X-rays. The NuSTAR imaging spectroscopy is consistent with isothermal emission of temperatures 3.1 \u2212 4.4~MK and emission measures 1 \u2013 8 \u00d7 10^(46)~cm^(\u22123). We do not observe emission above 5~MK but our short effective exposure times restrict the spectral dynamic range. With few counts above 6~keV, we can place constraints on the presence of an additional hotter component between 5 and 12~MK of \u223c 10^(46)cm^(\u22123) and \u223c10^(43) cm^(\u22123), respectively, at least an order of magnitude stricter than previous limits. With longer duration observations and a weakening solar cycle (resulting in an increased livetime), future NuSTAR observations will have sensitivity to a wider range of temperatures as well as possible non-thermal emission.",
"date": "2016-03-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "820",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L14",
"id_number": "CaltechAUTHORS:20160318-095344335",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160318-095344335",
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"agency": "NASA",
"grant_number": "NNX12AJ36G"
},
{
"agency": "NASA",
"grant_number": "NNX14AG07G"
},
{
"agency": "Royal Society"
},
{
"agency": "NASA Earth and Space Science Fellowship"
},
{
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"grant_number": "NNX13AM41H"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
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{
"agency": "NASA",
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"items": [
{
"id": "LaMassa-S-M",
"name": {
"family": "LaMassa",
"given": "Stephanie M."
},
"orcid": "0000-0002-5907-3330"
},
{
"id": "Ricarte-A",
"name": {
"family": "Ricarte",
"given": "Angelo"
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{
"id": "Glikman-E",
"name": {
"family": "Glikman",
"given": "Eilat"
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"id": "Urry-C-M",
"name": {
"family": "Urry",
"given": "C. Megan"
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"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
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"orcid": "0000-0003-2686-9241"
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{
"id": "Yaqoob-T",
"name": {
"family": "Yaqoob",
"given": "Tahir"
}
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{
"id": "Lansbury-G-B",
"name": {
"family": "Lansbury",
"given": "George B."
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Civano-Francesca",
"name": {
"family": "Civano",
"given": "Francesca"
},
"orcid": "0000-0002-2115-1137"
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{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steve E."
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"name": {
"family": "Brandt",
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{
"id": "Chen-Chien-Ting-J",
"name": {
"family": "Chen",
"given": "Chien-Ting J."
},
"orcid": "0000-0002-4945-5079"
},
{
"id": "Christensen-F-E",
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"family": "Christensen",
"given": "Finn E."
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"name": {
"family": "Craig",
"given": "William W."
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"name": {
"family": "Hailey",
"given": "Chuck J."
}
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona"
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "Ryan C."
},
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},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "Michael"
},
"orcid": "0000-0002-7998-9581"
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{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "Claudio"
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{
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"name": {
"family": "Treister",
"given": "Ezequiel"
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
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]
},
"title": "Peering through the Dust: NuSTAR Observations of Two FIRST-2MASS Red Quasars",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; infrared: galaxies; quasars: individual (F2M 0380+3759, F2M 1227+3214); X-rays: individual (F2M 0830+3759, F2M 1227+3214)",
"note": "\u00a9 2016 The American Astronomical Society. Received 2015 November 30; accepted 2016 February 9; published 2016 March 21.\n\nWe thank the referee for a careful reading of this manuscript and helpful comments. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). AR is supported by the Gruber Science Fellowship. EG acknowledges the generous support of the Cottrell College Award through the Research Corporation\nfor Science Advancement. WNB acknowledges support from Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. RCH acknowledges support from NASA through\nADAP award NNX12AE38G, the National Science Foundation through grant nos. 1211096 and 1515364, a Sloan Research Fellowship, and a Dartmouth Class of 1962 Faculty Fellowship. CR acknowledges financial support from the CONICYT-Chile grants \"EMBIGGEN\" Anillo ACT1101, FONDECYT 1141218, Basal-CATA PFB-06/2007. \n\nFacilities: NuSTAR,XMM\n\nPublished - apj_820_1_70.pdf
Submitted - 1602.03532v1.pdf
",
"abstract": "Some reddened quasars appear to be transitional objects in the merger-induced black hole growth/galaxy evolution paradigm, where a heavily obscured nucleus starts to be unveiled by powerful quasar winds evacuating the surrounding cocoon of dust and gas. Hard X-ray observations are able to peer through this gas and dust, revealing the properties of circumnuclear obscuration. Here, we present NuSTAR and XMM-Newton/Chandra observations of FIRST-2MASS selected red quasars F2M 0830+3759 and F2M 1227+3214. We find that though F2M 0830+3759 is moderately obscured (N_(H,Z) = 2.1 \u00b1 0.2 \u00d7 10^(22) cm^(\u22122)) and F2M 1227+3214 is mildly absorbed (N_(H,Z) = 3.4^(+0.8)_(\u22120.7) \u00d7 10^(21) cm^(\u22122)) along the line-of-sight, heavier global obscuration may be present in both sources, with N_(H,S) = 3.7^(+4.1)_(\u22122.6) \u00d7 10^(23) cm^(\u22122) and < 5.5 \u00d7 10^(23) cm^(\u22122), for F2M 0830+3759 and F2M 1227+3214, respectively. F2M 0830+3759 also has an excess of soft X-ray emission below 1 keV which is well accommodated by a model where 7% of the intrinsic AGN X-ray emission is scattered into the line-of-sight. While F2M 1227+3214 has a dust-to-gas ratio (E(B \u2212 V )/N_H) consistent with the Galactic value, the E(B\u2212V )/NH value for F2M 0830+3759 is lower than the Galactic standard, consistent with the paradigm that the dust resides on galactic scales while the X-ray\nreprocessing gas originates within the dust-sublimation zone of the broad-line-region. The X-ray and 6.1\u03bcm luminosities of these red quasars are consistent with the empirical relations derived for high-luminosity, unobscured quasars, extending the parameter space of obscured AGN previously observed by NuSTAR to higher luminosities.",
"date": "2016-03-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "820",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 70",
"id_number": "CaltechAUTHORS:20160318-080750044",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160318-080750044",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Gruber Science Fellowship"
},
{
"agency": "Cottrell Scholar of Research Corporation"
},
{
"agency": "NuSTAR",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "NASA",
"grant_number": "NNX12AE38G"
},
{
"agency": "NSF",
"grant_number": "1211096"
},
{
"agency": "NSF",
"grant_number": "1515364"
},
{
"agency": "Alfred P. Sloan Foundation"
},
{
"agency": "Dartmouth Class of 1962 Faculty Fellowship"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-61",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
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{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/0004-637X/820/1/70",
"primary_object": {
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"pub_year": "2016",
"author_list": "LaMassa, Stephanie M.; Ricarte, Angelo; et el."
},
{
"id": "https://authors.library.caltech.edu/records/qx7hp-mj441",
"eprint_id": 78221,
"eprint_status": "archive",
"datestamp": "2023-08-20 10:57:42",
"lastmod": "2023-10-25 23:53:30",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Ackermann-M",
"name": {
"family": "Ackermann",
"given": "M."
}
}
]
},
"title": "Contemporaneous broadband observations of three high-redshift BL Lac Objects",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "BL Lacertae objects: general \u2013 BL Lacertae objects: individual (3FGL J0022.1\u22121855, 3FGL J0630.9\n\u22122406, 3FGL J0811.2\u22127529) \u2013 galaxies: active \u2013 radiation mechanisms: non-thermal",
"note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2015 November 30; accepted 2016 February 14; published 2016 March 21.\n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nThe Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the High Energy Accelerator Research Organization (KEK), and the Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden.\n\nAdditional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France.\n\nH.A. acknowledges support provided by the NASA-sponsored Fermi Contract NAS5-00147 and by the Kavli Institute for Particle Astrophysics and Cosmology (KIPAC). Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1).\n\nSubmitted - 1602.04510.pdf
",
"abstract": "We have collected broadband spectral energy distributions (SEDs) of three BL Lac objects 3FGL J0022.1\u22121855 (z = 0.689), 3FGL J0630.9\u22122406 (z \u2273 1.239), and 3FGL J0811.2\u22127529 (z = 0.774), detected by Fermi with relatively flat gigaelectronvolt spectra. By observing simultaneously in the near-infrared to hard X-ray band, we can well characterize the high end of the synchrotron component of the SED. Thus, fitting the SEDs to synchro-Compton models of the dominant emission from the relativistic jet, we can constrain the underlying particle properties and predict the shape of the gigaelectronvolt Compton component. Standard extragalactic background light (EBL) models explain the high-energy absorption well, with poorer fits for high-ultraviolet models. The fits show clear evidence for EBL absorption in the Fermi spectrum of our highest-redshift source 3FGL J0630.9\u22122406. While synchrotron self-Compton models adequately describe the SEDs, the situation may be complicated by possible external Compton components. For 3FGL J0811.2\u22127529, we also discover a nearby serendipitous source in the X-ray data, which is almost certainly another lower synchrotron peak frequency (\u03bd^(sy)_(pk)) BL Lac, that may contribute flux in the Fermi band. Since our sources are unusual high-luminosity, moderate \u03bd^(sy)_(pk) BL Lacs, we compare these quantities and the Compton dominance, the ratio of peak inverse Compton to peak synchrotron luminosities (L^(IC)_(pk)/L^(sy)_(pk)), with those of the full Fermi BL Lac population.",
"date": "2016-03-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "820",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 72",
"id_number": "CaltechAUTHORS:20170614-160827182",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170614-160827182",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"corp_creators": {
"items": [
"Fermi LAT Collaboration"
]
},
"doi": "10.3847/0004-637X/820/1/72",
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"pub_year": "2016",
"author_list": "Ackermann, M."
},
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"datestamp": "2023-08-20 10:52:27",
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"items": [
{
"id": "Earnshaw-Hannah-P",
"name": {
"family": "Earnshaw",
"given": "Hannah M."
},
"orcid": "0000-0001-5857-5622"
},
{
"id": "Roberts-Timothy-P",
"name": {
"family": "Roberts",
"given": "Timothy P."
},
"orcid": "0000-0001-8252-6337"
},
{
"id": "Heil-Lucy-M",
"name": {
"family": "Heil",
"given": "Lucy M."
}
},
{
"id": "Mezcua-Mar",
"name": {
"family": "Mezcua",
"given": "Mar"
}
},
{
"id": "Walton-Dominic-J",
"name": {
"family": "Walton",
"given": "Dominic J."
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"orcid": "0000-0001-5819-3552"
},
{
"id": "Done-Christine",
"name": {
"family": "Done",
"given": "Chris"
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Lansbury-George-B",
"name": {
"family": "Lansbury",
"given": "George B."
},
"orcid": "0000-0002-5328-9827"
},
{
"id": "Middleton-Matthew-J",
"name": {
"family": "Middleton",
"given": "Matthew J."
},
"orcid": "0000-0002-8183-2970"
},
{
"id": "Sutton-Andrew-D",
"name": {
"family": "Sutton",
"given": "Andrew D."
}
}
]
},
"title": "A variable ULX and possible IMBH candidate in M51a",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 black hole physics \u2013 galaxies: individual: M51 \u2013 X-rays: binaries \u2013 X-rays: individual: M51 ULX-7",
"note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 December 12. Received 2015 November 17. First published online January 14, 2016.\n\nWe gratefully acknowledge support from the Science and Technology Facilities Council (HE through grant ST/K501979/1 and TR as part of consolidated grant ST/L00075X/1) and from NASA (MM through Chandra Grant G05-16099X). AS is supported by an appointment to the NASA Postdoctoral Program at Marshall Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The scientific results reported in this paper are based on data obtained from the Chandra Data Archive, and on archival observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has also made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech\n(USA). Further results are based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA); and the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - MNRAS-2016-Earnshaw-3840-54.pdf
Submitted - 1512.04825v1.pdf
",
"abstract": "Ultraluminous X-ray source ULX-7, in the northern spiral arm of M51, demonstrates unusual behaviour for an ULX, with a hard X-ray spectrum but very high short-term variability. This suggests that it is not in a typical ultraluminous state. We analyse the source using archival data from XMM-Newton, Chandra and NuSTAR, and by examining optical and radio data from HST and Very Large Array. Our X-ray spectral analysis shows that the source has a hard power-law spectral shape with a photon index \u0393 ~ 1.5, which persists despite the source's X-ray luminosity varying by over an order of magnitude. The power spectrum of the source features a break at 6.5^(+0.5)_(\u22121.1) \u00d7 10^(\u22123) Hz, from a low-frequency spectral index of \u0251_1 = 0.1^(+0.5)_(-0.2) to a high-frequency spectral index of \u0251_2 = 6.5^(+0.05)_(\u22120.14), making it analogous to the low-frequency break found in the power spectra of low/hard state black holes (BHs). We can take a lower frequency limit for a corresponding high-frequency break to calculate a BH mass upper limit of 1.6x10^3 M_\u2609. Using the X-ray/radio fundamental plane we calculate another upper limit to the BH mass of 3.5x10^4 M_\u2609 for a BH in the low/hard state. The hard spectrum, high rms variability and mass limits are consistent with ULX-7 being an intermediate-mass BH; however we cannot exclude other interpretations of this source's interesting behaviour, most notably a neutron star with an extreme accretion rate.",
"date": "2016-03-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "456",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "3840-3854",
"id_number": "CaltechAUTHORS:20160115-064812796",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-064812796",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/L00075X/1"
},
{
"agency": "NASA",
"grant_number": "G05-16099X"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NSF"
},
{
"agency": "ESA Member States"
}
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"name": "Space Radiation Laboratory"
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"doi": "10.1093/mnras/stv2945",
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"pub_year": "2016",
"author_list": "Earnshaw, Hannah M.; Roberts, Timothy P.; et el."
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{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
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"orcid": "0000-0003-0388-0560"
},
{
"id": "M\u00fcller-C",
"name": {
"family": "M\u00fcller",
"given": "C."
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{
"id": "Madsen-K-K",
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"family": "Madsen",
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"orcid": "0000-0003-1252-4891"
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{
"id": "Lanz-L",
"name": {
"family": "Lanz",
"given": "L."
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"orcid": "0000-0002-3249-8224"
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"id": "Rivers-E",
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"family": "Beuchert",
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"orcid": "0000-0001-9567-4224"
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"given": "W. W."
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"id": "Dauser-T",
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"family": "Dauser",
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"family": "Farrah",
"given": "D."
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"title": "NuSTAR and XMM-Newton Observations of the Hard X-Ray Spectrum of Centaurus A",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: individual (Centaurus A) \u2013 X-rays: galaxies",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 November 4; accepted 2016 January 23; published 2016 March 8. \n\nWe thank the anonymous referee for comments that helped\nto improve this work. This work was supported under NASA\nContract No. NNG08FD60C and made use of data from the\nNuSTAR mission, a project led by the California Institute of\nTechnology, managed by the Jet Propulsion Laboratory, and\nfunded by the National Aeronautics and Space Administration.\nWe thank the NuSTAR Operations, Software, and Calibration\nteams for support with the execution and analysis of these\nobservations. This research has made use of the NuSTAR Data\nAnalysis Software (NuSTARDAS), jointly developed by the\nASI Science Data Center (ASDC, Italy) and the California\nInstitute of Technology (USA). Based on observations obtained\nwith XMM-Newton, an ESA science mission with instruments\nand contributions directly funded by ESA Member States and\nNASA. This research has made use of a collection of ISIS\nscripts provided by the Dr. Karl Remeis Observatory,\nBamberg, Germany at http://www.sternwarte.uni-erlangen.\nde/isis/. C.M. acknowledges the support of the Bundesministerium\nf\u00fcr Wirtschaft und Technologie (BMWi) through\nDeutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR) grant\n50OR1404. We acknowledge support of the Deutsche\nForschungsgemeinschaft (DFG) through grant Wi 1860 10-1.\nThis research was funded in part by NASA through Fermi\nGuest Investigator grants NNH09ZDA001N,\nNNH10ZDA001N, NNH12ZDA001N, NNH13ZDA001NFERMI.\nThis research was supported by an appointment to\nthe NASA Postdoctoral Program at the Goddard Space Flight\nCenter, administered by Oak Ridge Associated Universities\nthrough a contract with NASA. M.B. acknowledges support\nfrom NASA Headquarters under the NASA Earth and Space\nScience Fellowship Program, grant NNX14AQ07H. We would\nlike to thank John E. Davis for the slxfig module, which was\nused to produce all figures in this work. \n\nFacilities: NuSTAR, XMM, CXO.\n\nPublished - apj_819_2_150.pdf
Submitted - 1511.01915v1.pdf
",
"abstract": "We present simultaneous XMM-Newton and Nuclear Spectroscopic Telescope Array (NuSTAR) observations spanning 3\u201378 keV of the nearest radio galaxy, Centaurus A (Cen A). The accretion geometry around the central engine in Cen A is still debated, and we investigate possible configurations using detailed X-ray spectral modeling. NuSTAR imaged the central region of Cen A with subarcminute resolution at X-ray energies above 10 keV for the first time, but found no evidence for an extended source or other off-nuclear point sources. The XMM-Newton and NuSTAR spectra agree well and can be described with an absorbed power law with a photon index \u0393 = 1.815 \u00b1 0.005 and a fluorescent Fe K\u0251 line in good agreement with literature values. The spectrum does not require a high-energy exponential rollover, with a constraint of E_(fold) > 1 MeV. A thermal Comptonization continuum describes the data well, with parameters that agree with values measured by INTEGRAL, in particular an electron temperature kTe between \u2248100\u2013300 keV and seed photon input temperatures between 5 and 50 eV. We do not find evidence for reflection or a broad iron line and put stringent upper limits of R < 0.01 on the reflection fraction and accretion disk illumination. We use archival Chandra data to estimate the contribution from diffuse emission, extra-nuclear point sources, and the outer X-ray jet to the observed NuSTAR and XMM-Newton X-ray spectra and find the contribution to be negligible. We discuss different scenarios for the physical origin of the observed hard X-ray spectrum and conclude that the inner disk is replaced by an advection-dominated accretion flow or that the X-rays are dominated by synchrotron self-Compton emission from the inner regions of the radio jet or a combination thereof.",
"date": "2016-03-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "819",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 150",
"id_number": "CaltechAUTHORS:20151117-090958104",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151117-090958104",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "50OR1404"
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{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
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"author_list": "F\u00fcrst, F.; M\u00fcller, C.; et el."
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},
"title": "Measuring A Truncated Disk in Aquila X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; magnetic fields; stars: neutron; X-rays: binaries; X-rays: bursts",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 October 19; accepted 2016 February 22; published 2016 March 7. \n\nThe authors thank the referee for their invaluable comments. A.L.K. would like to thank the support for this work, which was provided by NASA through Einstein Postdoctoral Fellowship grant number PF4-150125 awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. P.R. acknowledges financial contribution from contract ASI-INAF I/004/11/0 and ASI-INAF I/037/12/0. J.C. is grateful for financial support from ESA/PRODEX No. 90057. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - kingaL-L29.pdf
Submitted - 1602.07664v1.pdf
",
"abstract": "We present NuSTAR and Swift observations of the neutron star Aquila X-1 during the peak of its 2014 July outburst. The spectrum is soft with strong evidence for a broad Fe K\u03b1 line. Modeled with a relativistically broadened reflection model, we find that the inner disk is truncated with an inner radius of 15 \u00b1 3R_G. The disk is likely truncated by either the boundary layer and/or a magnetic field. Associating the truncated inner disk with pressure from a magnetic field gives an upper limit of B<5 \u00b1 2 x 10^8 G. Although the radius is truncated far from the stellar surface, material is still reaching the neutron star surface as evidenced by the X-ray burst present in the NuSTAR observation.",
"date": "2016-03-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "819",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L29",
"id_number": "CaltechAUTHORS:20160318-071512595",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160318-071512595",
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"agency": "NASA Einstein Fellowship",
"grant_number": "PF4-150125"
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{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/004/ 11/0"
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{
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"grant_number": "I/037/12/0"
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"grant_number": "90057"
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{
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"author_list": "King, Ashley L.; Tomsick, John A.; et el."
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"title": "Multiwavelength Study of Quiescent States of Mrk 421 with Unprecedented Hard X-Ray Coverage Provided by NuSTAR in 2013",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "BL Lacertae objects: individual (Markarian 421); galaxies: active; gamma rays: general; radiation mechanisms: nonthermal; X-rays: galaxies",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 September 24; accepted 2015 December 5; published 2016 March 9. \n\nWe thank the anonymous referee for constructive suggestions that helped improve and clarify the paper. \n\nM.B. acknowledges support from the International Fulbright Science and Technology Award, and from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. This research was supported in part by the Department of Energy Contract DE-AC02-76SF00515 to the SLAC National Accelerator Center. G.M. and A.F. acknowledge the support via NASA grant NNX13AO97G. D.B. acknowledges support from the French Space Agency (CNES) for financial support. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nVERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. \n\nThe MAGIC Collaboration would like to thank the Instituto de Astrof\u00edsica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. \n\nThe Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France. \n\nThis research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. \n\nThe St. Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015. \n\nThe work of M.B. is supported by the South African Research Chairs Initiative (SARChI) of the Department of Science and Technology and the National Research Foundation of South Africa. Any opinion, finding, and conclusion or recommendation expressed in this material is that of the authors and the NRF does not accept any liability in this regard. \n\nThe IAC team acknowledges the support from the group of support astronomers and telescope operators of the Observatorio del Teide. \n\nG.D. and O.V. gratefully acknowledge the observing grant support from the Institute of Astronomy and Rozhen National Astronomical Observatory, Bulgaria Academy of Sciences. This work is a part of the Projects No. 176011 (Dynamics and kinematics of celestial bodies and systems), No. 176004 (Stellar physics), and No. 176021 (Visible and invisible matter in nearby galaxies: theory and observations) supported by the Ministry of Education, Science, and Technological Development of the Republic of Serbia. \n\nThis research was partially supported by the Scientific Research Fund of the Bulgarian Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09). \n\nThe Abastumani team acknowledges financial support of the project FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under contract 31/77. \n\nT.G. acknowledges support from Istanbul University (Project numbers 49429 and 48285), Bilim Akademisi (BAGEP program), and TUBITAK (project numbers 13AT100-431, 13AT100-466, and 13AT60-430). \n\nThe Boston University effort was supported in part by NASA grants NNX12AO90G and NNX14AQ58G. \n\nData from the Steward Observatory spectropolarimetric monitoring project were used in this paper. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, NNX12AO93G, and NNX15AU81G. \n\nThe OVRO 40 m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G and NSF grants AST-0808050 and AST-1109911. \n\nThe Mets\u00e4hovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). \n\nThis research has made use of NASA's Astrophysics Data System and of Astropy, a community-developed core Python package for astronomy (Astropy Collaboration 2013). \n\nFacilities: NuSTAR, MAGIC, VERITAS, Fermi, Swift.\n\nPublished - Balokovi\u0107_2016_ApJ_819_156.pdf
Submitted - 1512.02235.pdf
",
"abstract": "We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January\u2013March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy (VHE) \u03b3-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3\u201379 keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep \u0393 \u2248 3 power law, with no evidence for an exponential cutoff or additional hard components up to ~80 keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states.",
"date": "2016-03-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "819",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 156",
"id_number": "CaltechAUTHORS:20170815-123455782",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170815-123455782",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Fulbright Foundation"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-AC02-76SF00515"
},
{
"agency": "NASA",
"grant_number": "NNX13AO97G"
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"title": "Demonstrating the likely neutron star nature of five M31 globular cluster sources with Swift-NuSTAR spectroscopy",
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"keywords": "globular clusters: general galaxies: individual: M 31 X-rays: binaries",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 March 1. Received 2016 March 1. In original form 2015 September 21. First published online March 7, 2016. \n\nTJM thanks Christian Knigge for an illuminating talk at 'The Physics of Cataclysmic and Compact Binaries', and Helena Uthas, Joe Patterson, Christian Knigge and Jeno Sokoloski for having organized the meeting. He also thanks Joey Neilsen, Chris Done, and Maria Diaz Trigo for useful discussions about disc winds. AZ acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2103)/ ERC Grant Agreement no. 617001.\n\nPublished - MNRAS-2016-Maccarone-3633-43.pdf
Submitted - 1603.00552v1.pdf
",
"abstract": "We present the results of a joint Swift-NuSTAR spectroscopy campaign on M31. We focus on the five brightest globular cluster X-ray sources in our fields. Two of these had previously been argued to be black hole candidates on the basis of apparent hard-state spectra at luminosities above those for which neutron stars are in hard states. We show that these two sources are likely to be Z-sources (i.e. low magnetic field neutron stars accreting near their Eddington limits), or perhaps bright atoll sources (low magnetic field neutron stars which are just a bit fainter than this level) on the basis of simultaneous Swift and NuSTAR spectra which cover a broader range of energies. These new observations reveal spectral curvature above 6-8 keV that would be hard to detect without the broader energy coverage the NuSTAR data provide relative to Chandra and XMM-Newton. We show that the other three sources are also likely to be bright neutron star X-ray binaries, rather than black hole X-ray binaries. We discuss why it should already have been realized that it was unlikely that these objects were black holes on the basis of their being persistent sources, and we re-examine past work which suggested that tidal capture products would be persistently bright X-ray emitters. We discuss how this problem is likely due to neglecting disk winds in older work that predict which systems will be persistent and which will be transient.",
"date": "2016-03-07",
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"number": "4",
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"pagerange": "3633-3643",
"id_number": "CaltechAUTHORS:20160318-084747231",
"issn": "0035-8711",
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"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "European Research Council (ERC)",
"grant_number": "617001"
}
]
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"title": "A High Braking Index for a Pulsar",
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"keywords": "pulsars: general; pulsars: individual (PSR J1640\u20134631); stars: neutron",
"note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 December 16; accepted 2016 February 17; published 2016 March 1. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. Parkes radio telescope is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We also thank an anonymous referee for helpful comments that improved the manuscript. R.F.A. acknowledges support from an NSERC Alexander Graham Bell Canada Graduate Scholarship. E.V.G. received support from the National Aeronautics and Space Administration through Chandra Award Number GO5-16061X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. V.M.K. receives support from an NSERC Discovery Grant and Accelerator Supplement, Centre de Recherche en Astrophysique du Queb\u00e9c, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344.\n\nPublished - Archibald_2016pL16.pdf
Submitted - 1603.00305v1.pdf
",
"abstract": "We present a phase-coherent timing solution for PSR J1640\u20134631, a young 206 ms pulsar using X-ray timing observations taken with NuSTAR. Over this timing campaign, we have measured the braking index of PSR J1640\u20134631 to be n = 3.15 \u00b1 0.03. Using a series of simulations, we argue that this unusually high braking index is not due to timing noise, but is intrinsic to the pulsar's spin-down. We cannot, however, rule out contamination due to an unseen glitch recovery, although the recovery timescale would have to be longer than most yet observed. If this braking index is eventually proven to be stable, it demonstrates that pulsar braking indices greater than three are allowed in nature; hence, other physical mechanisms such as mass or magnetic quadrupoles are important in pulsar spin-down. We also present a 3\u03c3 upper limit on the pulsed flux at 1.4 GHz of 0.018 mJy.",
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"volume": "819",
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"pagerange": "Art. No. L16",
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"keywords": "accretion, accretion disks; binaries: close; stars: neutron; X-rays: bursts; X-rays: individual (GS 1826\u201324)",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 September 3; accepted 2015 December 24; published 2016 February 17. \n\nJ.C. would like to thank Niels J\u00f8rgen Westergaard for useful discussions. J.C. acknowledges financial support from ESA/PRODEX Nr. 90057. P.R. acknowledges financial contribution from contract ASI-INAF I/004/11/0 and ASI-INAF I/037/12/0. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR and Swift Operations teams for executing the ToO observations and the Software and Calibration teams for analysis support. This research has used the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The MAXI data are provided by RIKEN, JAXA, and the MAXI team. Swift/BAT transient monitor results are provided by the Swift/BAT team. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This paper utilizes preliminary analysis results from the Multi-INstrument Burst ARchive (MINBAR), which is supported under the Australian Academy of Science's Scientific Visits to Europe program, and the Australian Research Council's Discovery Projects and Future Fellowship funding schemes. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, MAXI - JAXA Monitor of All-sky X-ray Image experiment.\n\nPublished - apj_818_2_135.pdf
Submitted - 1509.01248v1.pdf
",
"abstract": "We report on NuSTAR and Swift observations of a soft state of the neutron star low-mass X-ray binary GS 1826\u201324, commonly known as the \"clocked\" burster. The transition to the soft state was recorded in 2014 June through an increase of the 2\u201320 keV source intensity measured by MAXI, simultaneous with a decrease of the 15\u201350 keV intensity measured by Swift/BAT. The episode lasted approximately two months, after which the source returned to its usual hard state. We analyze the broadband spectrum measured by Swift/XRT and NuSTAR and estimate the accretion rate during the soft episode to be \u2248 13% m_(Edd), within the range of previous observations. However, the best-fit spectral model, adopting the double Comptonization used previously, exhibits significantly softer components. We detect seven type-I X-ray bursts, all significantly weaker (and with shorter rise and decay times) than observed previously. The burst profiles and recurrence times vary significantly, ruling out the regular bursts that are typical for this source. One burst exhibited photospheric radius expansion and we estimate the source distance as (5.7 \u00b1 0.2)\u03be_b^(-1/2) kpc, where \u03be_b parameterizes the possible anisotropy of the burst emission. The observed soft state may most likely be interpreted as a change in accretion geometry at about similar bolometric luminosity as in the hard state. The different burst behavior can therefore be attributed to this change in accretion flow geometry, but the fundamental cause and process for this effect remain unclear.",
"date": "2016-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "818",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 135",
"id_number": "CaltechAUTHORS:20151022-140809806",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151022-140809806",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "ESA/PRODEX",
"grant_number": "90057"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/004/11/0"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Australian Research Council"
},
{
"agency": "Australian Academy of Science"
}
]
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"doi": "10.3847/0004-637X/818/2/135",
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"pub_year": "2016",
"author_list": "Chenevez, J.; Galloway, D. K.; et el."
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},
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},
{
"id": "Walton-D-J",
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"family": "McClintock",
"given": "Jeffrey E."
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"name": {
"family": "Laycock",
"given": "Silas G. T."
}
},
{
"id": "Middleton-M-J",
"name": {
"family": "Middleton",
"given": "Matthew J."
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"family": "Barnard",
"given": "Robin"
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"name": {
"family": "Madsen",
"given": "Kristin K."
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},
"title": "On the Spin of the Black Hole in IC 10 X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics; stars: individual (IC 10 X\u20131); X-rays: binaries",
"note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 September 28; accepted 2015 December 14; published 2016 January 28. \n\nThis research has made use of software provided by the Chandra X-ray Center (CXC). This work was made possible by Chandra Grant GO4-15051X. J.F.S. has been supported by the NASA Hubble Fellowship grant HST-HF-51315.01, and the NASA Einstein Fellowship grant PF5-160144. We thank the CXC helpdesk and Larry David for their advice on the Chandra data reductions. J.F.S. thanks R. Remillard and J. Homan for helpful discussions on NS spectral models. We thank the anonymous referee for helpful criticisms which have improved this paper. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and has utilized the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). Chandra ObsId 15803.\n\nPublished - Steiner_2016p154.pdf
Submitted - 1512.03414v1.pdf
",
"abstract": "The compact X-ray source in the eclipsing X-ray binary IC 10 X\u20131 has reigned for years as ostensibly the most massive stellar-mass black hole, with a mass estimated to be about twice that of its closest rival. However, striking results presented recently by Laycock et al. reveal that the mass estimate, based on emission-line velocities, is unreliable and that the mass of the X-ray source is essentially unconstrained. Using Chandra and NuSTAR data, we rule against a neutron-star model and conclude that IC 10 X\u20131 contains a black hole. The eclipse duration of IC 10 X\u20131 is shorter and its depth shallower at higher energies, an effect consistent with the X-ray emission being obscured during eclipse by a Compton-thick core of a dense wind. The spectrum is strongly disk-dominated, which allows us to constrain the spin of the black hole via X-ray continuum fitting. Three other wind-fed black hole systems are known; the masses and spins of their black holes are high: M ~ 10 - 15M_\u2609 and \u0251_* > 0.8. If the mass of IC 10 X-1's black hole is comparable, then its spin is likewise high.",
"date": "2016-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "817",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 154",
"id_number": "CaltechAUTHORS:20160128-120939504",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-120939504",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "GO4-15051X"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF-51315.01"
},
{
"agency": "NASA Einstein Fellowship",
"grant_number": "PF5-160144"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"doi": "10.3847/0004-637X/817/2/154",
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"pub_year": "2016",
"author_list": "Steiner, James F.; Walton, Dominic J.; et el."
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"given": "M."
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"given": "F. E."
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"family": "Gandhi",
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"family": "Guainazzi",
"given": "M."
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"given": "F. A."
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"name": {
"family": "Iwasawa",
"given": "K."
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"family": "Madsen",
"given": "K. K."
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"name": {
"family": "Nicastro",
"given": "F."
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"family": "Puccetti",
"given": "S."
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"name": {
"family": "Ricci",
"given": "C."
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"family": "Stern",
"given": "D."
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},
"title": "NuSTAR catches the unveiling nucleus of NGC 1068",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active galaxies: individual: NGC 1068 galaxies: Seyfert",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 November 10. Received 2015 October 29. In original form 2015 July 16. First published online December 17, 2015. \n\nWe thank the referee for her/his comments. AM, SB and GM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. FEB acknowledges support from CONICYT-Chile (PFB-06/2007, FONDECYT 1141218, ACT1101), and grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. WNB acknowledges Caltech NuSTAR subcontract 44A-1092750. PG thanks STFC for support (grant reference ST/J003697/1). This work was supported under NASA Contracts No. NNG08FD60C, NNX10AC99G, NNX14AQ07H and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - MNRAS-2016-Marinucci-L94-8.pdf
Submitted - 1511.03503v1.pdf
",
"abstract": "We present a NuSTAR and XMM\u2013Newton monitoring campaign in 2014/2015 of the Compton-thick Seyfert 2 galaxy, NGC 1068. During the 2014 August observation, we detect with NuSTAR a flux excess above 20 keV (32 \u00b1 6\u2009per\u2009cent) with respect to the 2012 December observation and to a later observation performed in 2015 February. We do not detect any spectral variation below 10 keV in the XMM\u2013Newton data. The transient excess can be explained by a temporary decrease of the column density of the obscuring material along the line of sight (from N_H \u2243 10^(25) cm^(\u22122) to N_H = 6.7 \u00b1 1.0 \u00d7 10^(24) cm^(\u22122)), which allows us for the first time to unveil the direct nuclear radiation of the buried active galactic nucleus in NGC 1068 and to infer an intrinsic 2\u201310 keV luminosity L_X = 7^(+7)_(\u22124) \u00d7 10^(43) erg s^(\u22121).",
"date": "2016-02-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "456",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L94-L98",
"id_number": "CaltechAUTHORS:20160128-143037685",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-143037685",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "NASA",
"grant_number": "NNX14AQ07H"
},
{
"agency": "NASA/Caltech/JPL"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
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"doi": "10.1093/mnrasl/slv178",
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"pub_year": "2016",
"author_list": "Marinucci, A.; Bianchi, S.; et el."
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"items": [
{
"id": "Chen-Ge",
"name": {
"family": "Chen",
"given": "Ge"
},
"orcid": "0000-0003-2867-4544"
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "Victoria M."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
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"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin"
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},
"title": "NuSTAR observations of the young, energetic radio pulsar PSR B1509-58",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (PSR B1509\u201358) \u2013 stars: neutron \u2013 X-rays: stars",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 July 31; accepted 2015 December 3; published 2016 January 25. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). H.A. acknowledges supports provided by the NASA sponsored Fermi Contract NAS5-00147 and by Kavli Institute for Particle Astrophysics and Cosmology. V.M.K. acknowledges support from an NSERC Discovery Grant and Accelerator Supplement, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology.\n\nPublished - Chen_2016p93.pdf
Submitted - 1507.08977v2.pdf
",
"abstract": "We report on Nuclear Spectroscopic Telescope Array (NuSTAR) hard X-ray observations of the young rotation-powered radio pulsar PSR B1509\u221259 in the supernova remnant MSH 15\u221252. We confirm the previously reported curvature in the hard X-ray spectrum, showing that a log parabolic model provides a statistically superior fit to the spectrum compared with the standard power law. The log parabolic model describes the NuSTAR data, as well as previously published \u03b3-ray data obtained with COMPTEL and AGILE, all together spanning 3 keV through 500 MeV. Our spectral modeling allows us to constrain the peak of the broadband high energy spectrum to be at 2.6 \u00b1 0.8 MeV, an improvement of nearly an order of magnitude in precision over previous measurements. In addition, we calculate NuSTAR spectra in 26 pulse phase bins and confirm previously reported variations of photon indices with phase. Finally, we measure the pulsed fraction of PSR B1509\u221258 in the hard X-ray energy band for the first time. Using the energy resolved pulsed fraction results, we estimate that the pulsar's off-pulse emission has a photon index value between 1.26 and 1.96. Our results support a model in which the pulsar's lack of GeV emission is due to viewing geometry, with the X-rays originating from synchrotron emission from secondary pairs in the magnetosphere.",
"date": "2016-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "817",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 93",
"id_number": "CaltechAUTHORS:20150814-135512925",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150814-135512925",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NAS5-00147"
},
{
"agency": "Kavli Institute for Particle Astrophysics and Cosmology"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Fonds Qu\u00e9b\u00e9cois de la Recherche sur la Nature et les Technologies (FQRNT)"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canada Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
}
]
},
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"doi": "10.3847/0004-637X/817/2/93",
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"author_list": "Chen, Ge; An, Hongjun; et el."
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"id": "Paliya-V-S",
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"family": "Paliya",
"given": "Vaidehi S."
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"orcid": "0000-0001-7774-5308"
},
{
"id": "Diltz-C",
"name": {
"family": "Diltz",
"given": "Chris"
}
},
{
"id": "B\u00f6ttcher-M",
"name": {
"family": "B\u00f6ttcher",
"given": "Markus"
}
},
{
"id": "Stalin-C-S",
"name": {
"family": "Stalin",
"given": "C. S."
},
"orcid": "0000-0002-4998-1861"
},
{
"id": "Buckley-D-A-H",
"name": {
"family": "Buckley",
"given": "David"
},
"orcid": "0000-0002-7004-9956"
}
]
},
"title": "A hard gamma-ray flare from 3C 279 in 2013 December",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 galaxies: jets \u2013 gamma rays: galaxies \u2013 quasars: individual (3C 279)",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 August 4; accepted 2015 November 30; published 2016 January 20. \n\nWe are thankful to the referee for providing a constructive report. This research has made use of data, software, and/or web tools obtained from NASAs High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. This paper has made use of up-to-date SMARTS optical/near-infrared light curves that are available at www.astro.yale.edu/smarts/glast/home.php. Use of the Hydra cluster at the Indian Institute of Astrophysics is acknowledged. The work of M.B. is supported by the South African Research Chair Initiative (SARChI) of the Department of Science and Technology and the National Research Foundation of South Africa.\n\nSubmitted - 1512.00203v1.pdf
",
"abstract": "The blazar 3C 279 exhibited twin \u03b3-ray flares of similar intensity in 2013 December and 2014 April. In this work, we present a detailed multi-wavelength analysis of the 2013 December flaring event. Multi-frequency observations reveal the uncorrelated variability patterns with X-ray and optical\u2013UV fluxes peaking after the \u03b3-ray maximum. The broadband spectral energy distribution (SED) at the peak of the \u03b3-ray activity shows a rising \u03b3-ray spectrum but a declining optical\u2013UV flux. This observation along with the detection of uncorrelated variability behavior rules out the one-zone leptonic emission scenario. We, therefore, adopt two independent methodologies to explain the SED: a time-dependent lepto-hadronic modeling and a two-zone leptonic radiative modeling approach. In the lepto-hadronic modeling, a distribution of electrons and protons subjected to a randomly orientated magnetic field produces synchrotron radiation. Electron synchrotron is used to explain the IR to UV emission while proton synchrotron emission is used to explain the high-energy \u03b3-ray emission. A combination of both electron synchrotron self-Compton emission and proton synchrotron emission is used to explain the X-ray spectral break seen during the later stage of the flare. In the two-zone modeling, we assume a large emission region emitting primarily in IR to X-rays and \u03b3-rays to come primarily from a fast-moving compact emission region. We conclude by noting that within a span of four months, 3C 279 has shown the dominance of a variety of radiative processes over each other and this reflects the complexity involved in understanding the physical properties of blazar jets in general.",
"date": "2016-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "817",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 61",
"id_number": "CaltechAUTHORS:20160131-143450702",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160131-143450702",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX08AW56G"
},
{
"agency": "NASA",
"grant_number": "NNX09AU10G"
},
{
"agency": "NASA",
"grant_number": "NNX12AO93G"
},
{
"agency": "Department of Science and Technology (South Africa)"
},
{
"agency": "National Research Foundation (South Africa)"
}
]
},
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"doi": "10.3847/0004-637X/817/1/61",
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"pub_year": "2016",
"author_list": "Paliya, Vaidehi S.; Diltz, Chris; et el."
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"id": "Hamaguchi-Kenji",
"name": {
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},
{
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"given": "Michael F."
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"orcid": "0000-0002-7762-3172"
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{
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"name": {
"family": "Gull",
"given": "Theodore R."
},
"orcid": "0000-0002-6851-5380"
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{
"id": "Takahashi-Hiromitsu",
"name": {
"family": "Takahashi",
"given": "Hiromitsu"
},
"orcid": "0000-0001-6314-5897"
},
{
"id": "Grefenstette-Brian-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
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"orcid": "0000-0002-1984-2932"
},
{
"id": "Yuasa-Takayuki",
"name": {
"family": "Yuasa",
"given": "Takayuki"
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{
"id": "Stuhlinger-Martin",
"name": {
"family": "Stuhlinger",
"given": "Martin"
}
},
{
"id": "Russell-Christopher-M-P",
"name": {
"family": "Russell",
"given": "Christopher M. P."
}
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{
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"name": {
"family": "Moffat",
"given": "Anthony F. J."
},
"orcid": "0000-0002-4333-9755"
},
{
"id": "Sharma-Neetika",
"name": {
"family": "Sharma",
"given": "Neetika"
}
},
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"id": "Madura-Thomas-I",
"name": {
"family": "Madura",
"given": "Thomas I."
}
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{
"id": "Richardson-Noel-D",
"name": {
"family": "Richardson",
"given": "Noel D."
},
"orcid": "0000-0002-2806-9339"
},
{
"id": "Groh-Jose-H",
"name": {
"family": "Groh",
"given": "Jose"
}
},
{
"id": "Pittard-Julian-M",
"name": {
"family": "Pittard",
"given": "Julian M."
},
"orcid": "0000-0003-2244-5070"
},
{
"id": "Owocki-Stanley-P",
"name": {
"family": "Owocki",
"given": "Stanley"
}
}
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},
"title": "Eta Carinae's Thermal X-Ray Tail Measured with XMM-Newton and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: general; stars: early-type; stars: individual (etacar); stars: winds, outflows; X-rays: stars",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 September 18; accepted 2015 November 11; published 2016 January 19. \n\nThis research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. This research has made use of NASA's Astrophysics Data System Bibliographic Services. We appreciate the XMM-Newton help desk and calibration team on helping resolve the XMM-Newton EPIC gain issue. K.H. is supported by the Chandra grant GO4-15019A, the XMM-Newton grant NNX15AK62G, and the ADAP grant NNX15AM96G. CMPR is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. \n\nFacilities: XMM (EPIC) - , NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission\n\nPublished - Hamaguchi_2016p23.pdf
Accepted Version - nihms-908267.pdf
",
"abstract": "The evolved, massive highly eccentric binary system, \u03b7 Car, underwent a periastron passage in the summer of 2014. We obtained two coordinated X-ray observations with XMM-Newton and NuSTAR during the elevated X-ray flux state and just before the X-ray minimum flux state around this passage. These NuSTAR observations clearly detected X-ray emission associated with \u03b7 Car extending up to \u02dc50 keV for the first time. The NuSTAR spectrum above 10 keV can be fit with the bremsstrahlung tail from a kT \u02dc 6 keV plasma. This temperature is \u0394kT \u02dc 2 keV higher than those measured from the iron K emission line complex, if the shocked gas is in collisional ionization equilibrium. This result may suggest that the companion star's pre-shock wind velocity is underestimated. The NuSTAR observation near the X-ray minimum state showed a gradual decline in the X-ray emission by 40% at energies above 5 keV in a day, the largest rate of change of the X-ray flux yet observed in individual \u03b7 Car observations. The column density to the hardest emission component, NH \u02dc 1024 H cm^(-2), marked one of the highest values ever observed for \u03b7 Car, strongly suggesting increased obscuration of the wind-wind colliding X-ray emission by the thick primary stellar wind prior to superior conjunction. Neither observation detected the power-law component in the extremely hard band that INTEGRAL and Suzaku observed prior to 2011. If the non-detection by NuSTAR is caused by absorption, the power-law source must be small and located very near the wind-wind collision apex. Alternatively, it may be that the power-law source is not related to either \u03b7 Car or the GeV \u03b3-ray source.",
"date": "2016-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "817",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 23",
"id_number": "CaltechAUTHORS:20160204-090402539",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160204-090402539",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "GO4-15019A"
},
{
"agency": "NASA",
"grant_number": "NNX15AK62G"
},
{
"agency": "NASA",
"grant_number": "NNX15AM96G"
}
]
},
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"doi": "10.3847/0004-637X/817/1/23",
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"pub_year": "2016",
"author_list": "Hamaguchi, Kenji; Corcoran, Michael F.; et el."
},
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"id": "D'Ammando-F",
"name": {
"family": "D'Ammando",
"given": "F."
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"family": "Orienti",
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},
"title": "High-energy properties of the high-redshift flat spectrum radio quasar PKS 2149\u2212306",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 October 20. Received 2015 October 14. In original form 2015 August 10. First published online November 19, 2015. \n\nThe Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France. \n\nPart of this work was done with the contribution of the Italian Ministry of Foreign Affairs and Research for the collaboration project between Italy and Japan. We thank the Swift team for making these observations possible, the duty scientists, and science planners. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We thank Eugenio Bottacini, Luca Baldini, and Jeremy Perkins for useful comments and suggestions.\n\nPublished - MNRAS-2016-D'Ammando-1881-91.pdf
Published - MNRAS-2016-D=0027Ammando-1881-91.pdf
",
"abstract": "We investigate the \u03b3-ray and X-ray properties of the flat spectrum radio quasar PKS 2149\u2212306 at redshift z = 2.345. A strong \u03b3-ray flare from this source was detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope satellite in 2013 January, reaching on January 20 a daily peak flux of (301 \u00b1 36) \u00d7 10^(\u22128) ph cm^(\u22122) s^(\u22121) in the 0.1\u2013100 GeV energy range. This flux corresponds to an apparent isotropic luminosity of (1.5 \u00b1 0.2) \u00d7 10^(50) erg s^(\u22121), comparable to the highest values observed by a blazar so far. During the flare the increase of flux was accompanied by a significant change of the spectral properties. Moreover significant flux variations on a 6-h time-scale were observed, compatible with the light crossing time of the event horizon of the central black hole. The broad-band X-ray spectra of PKS 2149\u2212306 observed by Swift-XRT and NuSTAR are well described by a broken power-law model, with a very hard spectrum (\u0393_1 \u223c 1) below the break energy, at E_(break) = 2.5\u20133.0 keV, and \u0393_2 \u223c 1.4\u20131.5 above the break energy. The steepening of the spectrum below \u223c3 keV may indicate that the soft X-ray emission is produced by the low-energy relativistic electrons. This is in agreement with the small variability amplitude and the lack of spectral changes in that part of the X-ray spectrum observed between the two NuSTAR and Swift joint observations. As for the other high-redshift FSRQ detected by both Fermi-LAT and Swift-BAT, the photon index of PKS 2149\u2212306 in hard X-ray is 1.6 or lower and the average \u03b3-ray luminosity higher than 2 \u00d7 10^(48) erg s^(\u22121).",
"date": "2016-01-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "455",
"number": "2",
"publisher": "Oxford",
"pagerange": "1881-1891",
"id_number": "CaltechAUTHORS:20160204-183823009",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160204-183823009",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA"
},
{
"agency": "Department of Energy (DOE)"
},
{
"agency": "Commissariat \u00e0 l'Energie Atomique (CEA)"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)"
},
{
"agency": "High Energy Accelerator Research Organization (KEK)"
},
{
"agency": "Japan Aerospace Exploration Agency (JAXA)"
},
{
"agency": "K. A. Wallenberg Foundation"
},
{
"agency": "Swedish Research Council"
},
{
"agency": "Swedish National Space Board (SNSB)"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
},
{
"agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)"
},
{
"agency": "Istituto Nazionale di Fisica Nucleare (INFN)"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Italian Ministry of Foreign Affairs and Research"
}
]
},
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"doi": "10.1093/mnras/stv2452",
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"pub_year": "2016",
"author_list": "D'Ammando, F. and Orienti, M."
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"items": [
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "Ann E."
},
"orcid": "0000-0001-8667-2681"
},
{
"id": "Zezas-A",
"name": {
"family": "Zezas",
"given": "Andreas"
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "Andrew F."
},
"orcid": "0000-0001-5655-1440"
},
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "Shriharsh P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "Yukita-Mihoko",
"name": {
"family": "Yukita",
"given": "Mihoko"
},
"orcid": "0000-0001-6366-3459"
}
]
},
"title": "Spectral and Temporal Properties of the Ultraluminous X-Ray Pulsar in M82 from 15 years of Chandra Observations and Analysis of the Pulsed Emission Using NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: individual (M82) \u2013 stars: neutron \u2013 X-rays: binaries",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 July 21; accepted 2015 November 18; published 2016 January 5. \n\nThis work made significant use of archival observations made by the Chandra X-ray observatory, for which we thank the builders and operators, as well as the software package ciao. The data were obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This work also made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.Z. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007\u20132013)/ERC grant agreement No. 617001. \n\nFacilities: CXO (ACIS), NuSTAR - Chandra X-ray Observatory satellite\n\nPublished - Brightman_2015p60.pdf
Submitted - 1507.06014v1.pdf
",
"abstract": "The recent discovery by Bachetti et al. of a pulsar in M82 that can reach luminosities of up to 10^(40) erg s^(\u22121), a factor of ~100 times the Eddington luminosity for a 1.4 M\u2299 compact object, poses a challenge for accretion physics. In order to better understand the nature of this source and its duty cycle, and in light of several physical models that have been subsequently published, we conduct a spectral and temporal analysis of the 0.5\u20138 keV X-ray emission from this source from 15 years of Chandra observations. We analyze 19 ACIS observations where the point-spread function (PSF) of the pulsar is not contaminated by nearby sources. We fit the Chandra spectra of the pulsar with a power-law model and a disk blackbody model, subjected to interstellar absorption in M82. We carefully assess for the effect of pile-up in our observations, where four observations have a pile-up fraction of >10%, which we account for during spectral modeling with a convolution model. When fitted with a power-law model, the average photon index when the source is at high luminosity (L_X > 10^(39) erg s^(\u22121)) is \u0393 = 1.33 \u00b1 0.15. For the disk blackbody model, the average temperature is T_(in) = 3.24 \u00b1 0.65 keV, the spectral shape being consistent with other luminous X-ray pulsars. We also investigated the inclusion of a soft excess component and spectral break, finding that the spectra are also consistent with these features common to luminous X-ray pulsars. In addition, we present spectral analysis from NuSTAR over the 3\u201350 keV range where we have isolated the pulsed component. We find that the pulsed emission in this band is best fit by a power-law with a high-energy cutoff, where \u0393 = 0.6 \u00b1 0.3 and E_C = 14^(+5)_(-3) keV. While the pulsar has previously been identified as a transient, we find from our longer-baseline study that it has been remarkably active over the 15-year period, where for 9/19 (47%) observations that we analyzed, the pulsar appears to be emitting at a luminosity in excess of 10^(39) erg s^(\u22121), greater than 10 times its Eddington limit.",
"date": "2016-01-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "816",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 60",
"id_number": "CaltechAUTHORS:20150801-082902636",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150801-082902636",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "617001"
}
]
},
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"items": [
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"id": "2016-12",
"name": "Space Radiation Laboratory"
}
]
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"doi": "10.3847/0004-637X/816/2/60",
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"pub_year": "2016",
"author_list": "Brightman, Murray; Harrison, Fiona A.; et el."
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{
"id": "Wehrle-A-E",
"name": {
"family": "Wehrle",
"given": "Ann E."
}
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{
"id": "Grupe-D",
"name": {
"family": "Grupe",
"given": "Dirk"
},
"orcid": "0000-0002-9961-3661"
},
{
"id": "Jorstad-S-G",
"name": {
"family": "Jorstad",
"given": "Svetlana G."
}
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"name": {
"family": "Marscher",
"given": "Alan P."
}
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"given": "Mark"
},
"orcid": "0000-0003-0685-3621"
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{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
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},
{
"id": "Hovatta-T",
"name": {
"family": "Hovatta",
"given": "Talvikki"
},
"orcid": "0000-0002-2024-8199"
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "Grzegorz M."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona H."
},
"orcid": "0000-0003-2992-8024"
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{
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"name": {
"family": "Stern",
"given": "Daniel"
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]
},
"title": "Erratic Flaring of BL Lac in 2012-2013: Multiwavelength Observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "BL Lacertae objects: individual (BL Lacertae); galaxies: active; galaxies: individual (BL Lacertae); galaxies: jets",
"note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 February 26; accepted 2015 August 28; published 2016 January 5. \n\nWe thank the anonymous reviewer for comments that improved the paper. We thank Paul Smith (Steward Observatory) and Claudia Raiteri (Osservatorio Astrofisico di Torino) for helpful discussions. We are grateful to G\u00f6ran Pilbratt (Herschel) and Neil Gehrels (Swift) for allocation of Target of Opportunity time. We thank Mark Kidger and Rosario Lorente (Herschel Science Centre) for advice in observing with Herschel, David Shupe (NASA Herschel Science Center) for assistance with data reduction, and the Swift schedulers (Swift Operations Center at Pennsylvania State University) for responsive scheduling. A. Wehrle is grateful to Penny Milbouer (Houston, TX) for helpful discussions.\n\nA. Wehrle acknowledges Guest Investigator support from NASA via Herschel RSA 1427799. The Boston University group acknowledges support by NASA under Fermi Guest Investigator grants NNX11AQ03G, NNX12AO79G, NNX13AP06G, and NNX14AQ58G, and Swift Guest Investigator grants NNX14AC59G. S. G. Jorstad acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The VLBA is an instrument of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy.\n\nSwift at PSU is supported by NASA contract NAS5-00136.\n\nM. Balokovi\u0107 acknowledges support from the International Fulbright Science and Technology Award and from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.\n\nPart of this work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nT. Hovatta acknowledges support from the Jenny and Antti Wihuri foundation and Academy of Finland project number 267324. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities.\n\nThe Fermi LAT Collaboration acknowledges generous on-going support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat lEnergie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nuclaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National dtudes Spatiales in France.\n\nThis research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nFacilities: Herschel - European Space Agency's Herschel space observatory, Fermi - Fermi Gamma-Ray Space Telescope (formerly GLAST), Swift - Swift Gamma-Ray Burst Mission, SMA - SubMillimeter Array, CARMA - Combined Array for Research in Millimeter-Wave Astronomy, NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, VLBA - Very Long Baseline Array.\n\nPublished - Wehrle_2016p53.pdf
",
"abstract": "BL Lac, the eponymous blazar, flared to historically high levels at millimeter, infrared, X-ray, and gamma-ray wavelengths in 2012. We present observations made with Herschel, Swift, NuSTAR, Fermi, the Submillimeter Array, CARMA, and the VLBA in 2012\u20132013, including three months with nearly daily sampling at several wavebands. We have also conducted an intensive campaign of 30 hr with every-orbit observations by Swift and NuSTAR, accompanied by Herschel, and Fermi observations. The source was highly variable at all bands. Time lags, correlations between bands, and the changing shapes of the spectral energy distributions can be explained by synchrotron radiation and inverse Compton emission from nonthermal seed photons originating from within the jet. The passage of four new superluminal very long baseline interferometry knots through the core and two stationary knots about 4 pc downstream accompanied the high flaring in 2012\u20132013. The seed photons for inverse Compton scattering may arise from the stationary knots and from a Mach disk near the core where relatively slow-moving plasma generates intense nonthermal radiation. The 95 spectral energy distributions obtained on consecutive days form the most densely sampled, broad wavelength coverage for any blazar. The observed spectral energy distributions and multi-waveband light curves are similar to simulated spectral energy distributions and light curves generated with a model in which turbulent plasma crosses a conical shock with a Mach disk.",
"date": "2016-01-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "816",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 53",
"id_number": "CaltechAUTHORS:20160204-144237295",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160204-144237295",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "RSA 1427799"
},
{
"agency": "NASA",
"grant_number": "NNX11AQ03G"
},
{
"agency": "NASA",
"grant_number": "NNX12AO79G"
},
{
"agency": "NASA",
"grant_number": "NNX13AP06G"
},
{
"agency": "NASA",
"grant_number": "NNX14AQ58G"
},
{
"agency": "NASA",
"grant_number": "NNX14AC59G"
},
{
"agency": "Russian Foundation for Basic Research",
"grant_number": "15-02-00949"
},
{
"agency": "St. Petersburg University",
"grant_number": "6.38.335.2015"
},
{
"agency": "Smithsonian Institution"
},
{
"agency": "Academia Sinica"
},
{
"agency": "NSF"
},
{
"agency": "NASA",
"grant_number": "NAS5-00136"
},
{
"agency": "Fulbright Commission"
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{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
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{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Jenny and Antti Wihuri Foundation"
},
{
"agency": "Academy of Finland",
"grant_number": "267324"
},
{
"agency": "Gordon and Betty Moore Foundation"
},
{
"agency": "Kenneth T. and Eileen L. Norris Foundation"
},
{
"agency": "James S. McDonnell Foundation"
},
{
"agency": "Associates of the California Institute of Technology"
},
{
"agency": "University of Chicago"
},
{
"agency": "states of California, Illinois, and Maryland"
},
{
"agency": "Department of Energy (DOE)"
},
{
"agency": "Commissariat \u00e0 l'Energie Atomique (CEA)"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
},
{
"agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)"
},
{
"agency": "Istituto Nazionale di Fisica Nucleare (INFN)"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)"
},
{
"agency": "High Energy Accelerator Research Organization (KEK)"
},
{
"agency": "Japan Aerospace Exploration Agency (JAXA)"
},
{
"agency": "K. A. Wallenberg Foundation"
},
{
"agency": "Swedish Research Council"
},
{
"agency": "Swedish National Space Board (SNSB)"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-25",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.3847/0004-637X/816/2/53",
"primary_object": {
"basename": "Wehrle_2016p53.pdf",
"url": "https://authors.library.caltech.edu/records/fx690-d2h97/files/Wehrle_2016p53.pdf"
},
"pub_year": "2016",
"author_list": "Wehrle, Ann E.; Grupe, Dirk; et el."
},
{
"id": "https://authors.library.caltech.edu/records/whge2-q5p63",
"eprint_id": 64254,
"eprint_status": "archive",
"datestamp": "2023-08-20 09:50:21",
"lastmod": "2023-10-17 19:38:10",
"type": "article",
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"creators": {
"items": [
{
"id": "Xu-Weiwei",
"name": {
"family": "Xu",
"given": "Weiwei"
}
},
{
"id": "Liu-Zhu",
"name": {
"family": "Liu",
"given": "Zhu"
},
"orcid": "0000-0002-8968-7050"
},
{
"id": "Gou-Lijun",
"name": {
"family": "Gou",
"given": "Lijun"
}
},
{
"id": "Liu-Jiren",
"name": {
"family": "Liu",
"given": "Jiren"
}
}
]
},
"title": "X-ray fluorescent lines from the Compton-thick AGN in M51",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "atomic processes \u2013 galaxies: individual: M51 (NGC 5194) \u2013 galaxies: Seyfert \u2013 X-rays: galaxies",
"note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \nAccepted 2015 September 29. Received 2015 September 28. In original form 2015 August 3. First published online October 20, 2015. \n\nWe thank our referee for valuable comments. JL is supported by NSFC grant 11203032, and LG is supported by the Strategic Priority Research Program 'The Emergence of Cosmological Structures' of CAS grant XDB09000000, NSFC grant 11333005, and NAOC grant Y234031001. This research is based on data obtained from the Chandra Data Archive and uses data from NuSTAR mission.\n\nPublished - MNRAS-2016-Xu-L26-30.pdf
",
"abstract": "The cold disc/torus gas surrounding active galactic nuclei (AGN) emits fluorescent lines when irradiated by hard X-ray photons. The fluorescent lines of elements other than Fe and Ni are rarely detected due to their relative faintness. We report the detection of K\u03b1 lines of neutral Si, S, Ar, Ca, Cr, and Mn, along with the prominent Fe K\u03b1, Fe K\u03b2, and Ni K\u03b1 lines, from the deep Chandra observation of the low-luminosity Compton-thick AGN in M51. The Si K\u03b1 line at 1.74 keV is detected at \u223c3\u03c3, the other fluorescent lines have a significance between 2 and 2.5 \u03c3, while the Cr line has a significance of \u223c1.5\u03c3. These faint fluorescent lines are made observable due to the heavy obscuration of the intrinsic spectrum of M51, which is revealed by NuSTAR observation above 10 keV. The hard X-ray continuum of M51 from Chandra and NuSTAR can be fitted with a power-law spectrum with an index of 1.8, reprocessed by a torus with an equatorial column density of NH \u223c 7 \u00d7 10^(24) cm^(\u22122) and an inclination angle of 74\u00b0. This confirms the Compton-thick nature of the nucleus of M51. The relative element abundances inferred from the fluxes of the fluorescent lines are similar to their solar values, except for Mn, which is about 10 times overabundant. It indicates that Mn is likely enhanced by the nuclear spallation of Fe.",
"date": "2016-01-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society: Letters",
"volume": "455",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L26-L30",
"id_number": "CaltechAUTHORS:20160204-181822135",
"issn": "1745-3925",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160204-181822135",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "National Science Foundation of China",
"grant_number": "11203032"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDB09000000"
},
{
"agency": "National Science Foundation of China",
"grant_number": "11333005"
},
{
"agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)",
"grant_number": "Y234031001"
}
]
},
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"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnrasl/slv14",
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},
"pub_year": "2016",
"author_list": "Xu, Weiwei; Liu, Zhu; et el."
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{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
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{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
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{
"id": "Bauer-F-E",
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"family": "Bauer",
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"id": "Fiore-F",
"name": {
"family": "Fiore",
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"family": "Luo",
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"family": "Stern",
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"name": {
"family": "Urry",
"given": "C. M."
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"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
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"name": {
"family": "Annuar",
"given": "A."
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"id": "Ar\u00e9valo-P",
"name": {
"family": "Ar\u00e9valo",
"given": "P."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
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{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
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"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
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"family": "Christensen",
"given": "F. E."
},
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"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
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"family": "Gandhi",
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"family": "Hailey",
"given": "C. J."
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"family": "Koss",
"given": "M. J."
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{
"id": "La-Massa-S",
"name": {
"family": "La Massa",
"given": "S."
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"name": {
"family": "Marinucci",
"given": "A."
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"family": "Zappacosta",
"given": "L."
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"name": {
"family": "Zhang",
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},
"title": "Hard X-ray emission of the luminous infrared galaxy NGC 6240 as observed by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 ESO, 2016. \n\nReceived 14 August 2015 / Accepted 14 October 2015. \n\nThis work was supported under NASA Contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.C., A.M., F.F. and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 \u2212 011/13. W.N.B. acknowledges support from Caltech NuSTAR sub-contract 44A-1092750. F.E.B. and C.R. acknowledge support from CONICYT\u2212Chile grants Basal\u2212CATA PFB\u221206/2007 and FONDECYT 1141218. F.E.B., C.R. and P.A. acknowledge support from \"EMBIGGEN\" Anillo ACT1101. FEB acknowledges support from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.\n\nPublished - aa27189-15.pdf
",
"abstract": "We present a broadband (~0.3\u221270 keV) spectral and temporal analysis of NuSTAR observations of the luminous infrared galaxy NGC 6240 combined with archival Chandra, XMM-Newton, and BeppoSAX data. NGC 6240 is a galaxy in a relatively early merger state with two distinct nuclei separated by ~1.\u030b5. Previous Chandra observations resolved the two nuclei and showed that they are both active and obscured by Compton-thick material. Although they cannot be resolved by NuSTAR, we were able to clearly detect, for the first time, both the primary and the reflection continuum components thanks to the unprecedented quality of the NuSTAR data at energies >10 keV. The NuSTAR hard X-ray spectrum is dominated by the primary continuum piercing through an absorbing column density which is mildly optically thick to Compton scattering (\u03c4 \u2243 1.2, N_H ~ 1.5 \u00d7 10^(24) cm^(-2)). We detect moderately hard X-ray (>10 keV) flux variability up to 20% on short (15\u221220 ks) timescales. The amplitude of the variability is largest at ~30 keV and is likely to originate from the primary continuum of the southern nucleus. Nevertheless, the mean hard X-ray flux on longer timescales (years) is relatively constant. Moreover, the two nuclei remain Compton-thick, although we find evidence of variability in the material along the line of sight with column densities N_H \u2264 2 \u00d7 10^(23) cm^(-2) over long (~3\u221215 yr) timescales. The observed X-ray emission in the NuSTAR energy range is fully consistent with the sum of the best-fit models of the spatially resolved Chandra spectra of the two nuclei.",
"date": "2016-01",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "585",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A157",
"id_number": "CaltechAUTHORS:20160204-180325331",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160204-180325331",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "t I/037/12/0 \u2212 011/13"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "t 44A-1092750"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NASA",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2016-27",
"name": "Space Radiation Laboratory"
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},
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{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
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"doi": "10.1051/0004-6361/201527189",
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"title": "Hard X-ray Morphological and Spectral Studies of The Galactic Center Molecular Cloud Sgr B2: Constraining Past Sgr A* Flaring Activity",
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"keywords": "Galaxy: center; ISM: clouds; X-rays: individual (Sgr B2); X-rays: ISM",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 July 24; accepted 2015 November 7; published 2015 December 21. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contribution directly funded by ESA Member States and NASA. S.Z. is supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program\u2014Grant \"NNX13AM31.\" F.E.B. acknowledges support from CONICYT-Chile and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative. G.P. acknowledges support via an EU Marie Curie Intra European fellowship under contract no. FP-PEOPLE-2012-IEF-331095 and Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft-und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. M.C., A.G., R.T., and S.S. acknowledge support by CNES.\n\nPublished - Zhang_2015.pdf
Submitted - 1507.08740v1.pdf
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"abstract": "In 2013, NuSTAR observed the Sgr B2 region and for the first time resolved its hard X-ray emission on subarcminute scales. Two prominent features are detected above 10 keV: a newly emerging cloud, G0.66\u22120.13, and the central 90\" radius region containing two compact cores, Sgr B2(M) and Sgr B2(N), surrounded by diffuse emission. It is inconclusive whether the remaining level of Sgr B2 emission is still decreasing or has reached a constant background level. A decreasing X-ray emission can be best explained by the X-ray reflection nebula scenario, where the cloud reprocesses a past giant outburst from Sgr A^*. In the X-ray reflection nebula (XRN) scenario, the 3\u201379 keV Sgr B2 spectrum allows us to self-consistently test the XRN model using both the Fe K\u03b1 line and the continuum emission. The peak luminosity of the past Sgr A^* outburst is constrained to L_(3-79keV) ~ 5 x 10^(38); erg s^(-1). A newly discovered cloud feature, G0.66\u22120.13, shows different timing variability. We suggest that it could be a molecular clump located in the Sgr B2 envelope reflecting the same Sgr A^* outburst. In contrast, if the Sgr B2 X-ray emission has reached a constant background level, it would imply an origin of low-energy cosmic-ray (CR) proton bombardment. In this scenario, from the NuSTAR measurements we infer a CR ion power of dW/dt=(1-4) x 10^(39) erg s^(-1) and a CR ionization rate of \u03b6_H =(6-10) x 10^(-15) H^(-1) s^(-1. These measurements can become powerful tools to constrain the GC CR population.",
"date": "2015-12-20",
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"pagerange": "Art. No. 132",
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"title": "Very-high-energy gamma-rays from the Universe's middle age: detection of the z=0.940 blazar PKS 1441+25 with MAGIC",
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"keywords": "cosmic background radiation; galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (PKS 1441+25)",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 August 11; accepted 2015 November 22; published 2015 December 15. \n\nWe would like to thank the Instituto de Astrof\u00edsica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2012-39502) and MECD (FPU13/00618), and the Japanese JSPS, and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. \n\nThe Fermi-LAT Collaboration acknowledges support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. \n\nWe thank the Swift team duty scientists and science planners. L.P. acknowledges the PRIN-INAF 2014 financial support.\n\nPublished - Ahnen_2016pL23.pdf
Submitted - 1512.04435v1.pdf
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"abstract": "The flat-spectrum radio quasar PKS 1441+25 at a redshift of z = 0.940 is detected between 40 and 250 GeV with a significance of 25.5 {\\sigma} using the MAGIC telescopes. Together with the gravitationally lensed blazar QSO B0218+357 (z = 0.944), PKS 1441+25 is the most distant very high energy (VHE) blazar detected to date. The observations were triggered by an outburst in 2015 April seen at GeV energies with the Large Area Telescope on board Fermi. Multi-wavelength observations suggest a subdivision of the high state into two distinct flux states. In the band covered by MAGIC, the variability time scale is estimated to be 6.4 +/- 1.9 days. Modeling the broadband spectral energy distribution with an external Compton model, the location of the emitting region is understood as originating in the jet outside the broad line region (BLR) during the period of high activity, while being partially within the BLR during the period of low (typical) activity. The observed VHE spectrum during the highest activity is used to probe the extragalactic background light at an unprecedented distance scale for ground-based gamma-ray astronomy.",
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"title": "Gamma rays from the quasar PKS 1441+25: story of an escape",
"ispublished": "pub",
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"keywords": "cosmology: observations; diffuse radiation; gamma rays: galaxies; quasars: individual (PKS 1441+25&VER J1443+250); radiation mechanisms: non-thermal",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 August 10; accepted 2015 November 17; published 2015 December 15. \n\nThis research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, and by NSERC in Canada, with additional support from NASA Swift GI grant NNX15AR38G. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. \n\nASAS-SN thanks LCOGT, NSF, Mt. Cuba Astronomical Foundation, OSU/CCAPP and MAS/Chile for their support. \n\nThe observations at Steward Observatory are funded through NASA Fermi GI grant NNX12AO93G. \n\nCRTS is supported by the NSF grants AST-1313422 and AST-1413600. \n\nThe OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. \n\nThe National Radio Astronomy Observatory is a facility of NSF operated under cooperative agreement by Associated Universities, Inc. \n\nThis research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009).\n\nPublished - Abeysekara_2015pL22.pdf
Submitted - 1512.04434v1.pdf
",
"abstract": "Outbursts from gamma-ray quasars provide insights on the relativistic jets of active galactic nuclei and constraints on the diffuse radiation fields that fill the Universe. The detection of significant emission above 100 GeV from a distant quasar would show that some of the radiated gamma rays escape pair-production interactions with low-energy photons, be it the extragalactic background light (EBL), or the radiation near the supermassive black hole lying at the jet's base. VERITAS detected gamma-ray emission up to 200 GeV from PKS 1441+25 (z=0.939) during April 2015, a period of high activity across all wavelengths. This observation of PKS 1441+25 suggests that the emission region is located thousands of Schwarzschild radii away from the black hole. The gamma-ray detection also sets a stringent upper limit on the near-ultraviolet to near-infrared EBL intensity, suggesting that galaxy surveys have resolved most, if not all, of the sources of the EBL at these wavelengths.",
"date": "2015-12-15",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
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"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L22",
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{
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"grant_number": "NNX11A043G"
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{
"agency": "NASA",
"grant_number": "AST-1109911"
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{
"agency": "Associated Universities, Inc"
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{
"agency": "Las Cumbres Observatory Global Telescope Network"
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{
"agency": "Mt. Cuba Astronomical Foundation"
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{
"agency": "Ohio State University"
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{
"agency": "Instituto Milenio de Astrof\u00edsica (MAS)"
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"doi": "10.1088/2041-8205/815/2/L22",
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},
"title": "The NuSTAR view of reflection and absorption in NGC 7582",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 7582); X-rays: galaxies",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 July 21; accepted 2015 November 5; published 2015 December 9. \n\nWe would like to thank the anonymous referee for helpful and constructive comments contributing to this work. This work was supported under NASA Contract No. NNG08FD60C and sub-contract No. 44A-1092750. We have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work has made use of also made use of RXTE and Swift archival data and HEASARC online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic Database, operated by JPL/California Institute of Technology under contract with NASA. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. P.A. acknowledges financial support form Fondecyt grant 1140304. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, \"EMBIGGEN\" Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. M.K. acknowledges support from the Swiss National Science Foundation and Ambizione fellowship grant PZ00P2 154799/1. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, RXTE - Rossi X-ray Timing Explorer.\n\nPublished - Rivers_2015.pdf
Submitted - 1511.01951v1.pdf
",
"abstract": "NGC 7582 is a well-studied X-ray bright Seyfert 2 with moderately heavy N_H ~ 10^(23)-10^(24) cm^(\u22122), highly variable absorption and strong reflection spectral features. The spectral shape changed around the year 2000, dropping in observed flux and becoming much more highly absorbed. Two scenarios have been put forth to explain this spectral change: (1) the central X-ray source partially \"shut off\" around this time, decreasing in intrinsic luminosity, with a delayed decrease in reflection features due to the light-crossing time of the Compton-thick material or (2) the source became more heavily obscured, with only a portion of the power law continuum leaking through. NuSTAR observed NGC 7582 twice in 2012, two weeks apart, in order to quantify the reflection using high-quality data above 10 keV. We find that the most plausible scenario is that NGC 7582 has recently become more heavily absorbed by a patchy torus with a covering fraction of ~80%\u201390% and an equatorial column density of ~ 3 x 10^(24) cm^(\u22122). We find the need for an additional highly variable full-covering absorber with N_H = (4\u20136) \u00d7 10^(23) cm^(\u22122) in the line of sight, possibly associated with a hidden broad line region.",
"date": "2015-12-10",
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"given": "R. C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Ricci-C",
"name": {
"family": "Ricci",
"given": "C."
},
"orcid": "0000-0001-5231-2645"
},
{
"id": "Rigby-J-R",
"name": {
"family": "Rigby",
"given": "J. R."
},
"orcid": "0000-0002-7627-6551"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zappacosta-L",
"name": {
"family": "Zappacosta",
"given": "L."
},
"orcid": "0000-0002-4205-6884"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Observations of the Compton-thick Active Galactic Nucleus and Ultraluminous X-ray Source Candidate in NGC 5643",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: nuclei; techniques: spectroscopic; X-rays: galaxies; X-rays: individual (NGC 5643, NGC 5643 X\u20131)",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 June 2; accepted 2015 October 4; published 2015 December 4. \n\nThe authors thank the anonymous referee for useful comments that have helped to improve the paper. We thank Chris Done for some discussions on the residuals around the iron line complex. A.A. thanks Wasutep Luangtip for useful discussion on NGC 5643 X\u20131 and help with the MARX simulation. We also thank Neil Gehrels and the Swift team for the simultaneous Swift-XRT observation. We acknowledge financial support from Majlis Amanah Rakyat (MARA) Malaysia (A.A.), the Science and Technology Facilities Council (STFC) grants ST/J003697/1 (P.G.), ST/I0015731/1 (D.M.A. and A.D.M.), and ST/K501979/1 (G.B.L.), the Leverhulme Trust (D.M.A.), NASA Headquarters under the NASA Earth and Space Science Fellowship Program grant NNX14AQ07H (M.B.), CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B.), FONDECYT 1141218 (F.E.B.), and \"EMBIGGEN\" Anillo ACT1101 (F.E.B.); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.). \n\nNuSTAR is a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). We thank the NuSTAR Operations, Software and Calibrations teams for support with these observations. This research has made use of the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA), and the XRT Data Analysis Software (xrt-das). This research also made use of the data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) Online Service, provided by the NASA/Goddard Space Flight Center, and the NASA/IPAC extragalactic Database (NED) operated by JPL, Caltech under contract with NASA. \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM - Newton X-Ray Multimirror Mission satellite, CXO - , Swift - Swift Gamma-Ray Burst Mission.\n\nPublished - Annuar_2015.pdf
Submitted - 1509.03322v1.pdf
",
"abstract": "We present two Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the local Seyfert 2 active galactic nucleus (AGN) and an ultraluminous X-ray source (ULX) candidate in NGC 5643. Together with archival data from Chandra, XMM-Newton, and Swift-BAT, we perform a high-quality broadband spectral analysis of the AGN over two decades in energy (~0.5\u2013100 keV). Previous X-ray observations suggested that the AGN is obscured by a Compton-thick (CT) column of obscuring gas along our line of sight. However, the lack of high-quality \u227310 keV observations, together with the presence of a nearby X-ray luminous source, NGC 5643 X\u20131, have left significant uncertainties in the characterization of the nuclear spectrum. NuSTAR now enables the AGN and NGC 5643 X\u20131 to be separately resolved above 10 keV for the first time and allows a direct measurement of the absorbing column density toward the nucleus. The new data show that the nucleus is indeed obscured by a CT column of N_H \u2273 5 \u00d7 10^(24) cm^(\u22122). The range of 2\u201310 keV absorption-corrected luminosity inferred from the best-fitting models is L_(2\u201310,int) = (0.8\u20131.7) \u00d7 10^(42) erg s^(\u22121), consistent with that predicted from multiwavelength intrinsic luminosity indicators. In addition, we also study the NuSTAR data for NGC 5643 X\u20131 and show that it exhibits evidence of a spectral cutoff at energy E ~ 10 keV, similar to that seen in other ULXs observed by NuSTAR. Along with the evidence for significant X-ray luminosity variations in the 3\u20138 keV band from 2003 to 2014, our results further strengthen the ULX classification of NGC 5643 X\u20131.",
"date": "2015-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "815",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 36",
"id_number": "CaltechAUTHORS:20160115-121320570",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-121320570",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I0015731/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-17",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/815/1/36",
"primary_object": {
"basename": "1509.03322v1.pdf",
"url": "https://authors.library.caltech.edu/records/15er2-31c39/files/1509.03322v1.pdf"
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"basename": "Annuar_2015.pdf",
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],
"pub_year": "2015",
"author_list": "Annuar, A.; Gandhi, P.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/0aka3-x7m79",
"eprint_id": 64195,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:02:43",
"lastmod": "2023-10-17 19:35:23",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Weng-Shan-Shan",
"name": {
"family": "Weng",
"given": "Shan-Shan"
}
},
{
"id": "G\u00f6\u011f\u00fc\u015f-E",
"name": {
"family": "G\u00f6\u011f\u00fc\u015f",
"given": "Ersin"
},
"orcid": "0000-0002-5274-6790"
}
]
},
"title": "Broadband X-ray Spectral Investigations of Magnetars, 4U 0142+61, 1E 1841-045, 1E 2259+586, and 1E 1048.1-5937",
"ispublished": "pub",
"full_text_status": "restricted",
"keywords": "magnetic fields; pulsars: individual (4U 0142+61, 1E 1841\u2013045); radiation mechanisms: non-thermal; stars: neutron; X-rays: stars",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 June 22; accepted 2015 October 21; published 2015 December 2. \n\nWe thank the referee for helpful suggestions and comments. We thank Feryal \u00d6zel for providing the highly magnetized NS surface emission code. S.S.W. is supported by the Scientific and Technological Research Council of Turkey (T\u00dcB\u0130TAK) and EC-FP7 Marie Curie Actions-People-COFUND Brain Circulation Scheme (2236).",
"abstract": "We have generated an extended version of rather simplified but physically oriented three-dimensional magnetar emission model, STEMS3D, to allow spectral investigations up to 100 keV. We have then applied it to the broadband spectral spectra of four magnetars: 4U 0142+61, 1E 1841-045, 1E 2259+586 and 1E 1048.1-5937, using data collected with Swift/XRT or XMM-Newton in soft X-rays, and Nuclear Spectroscopic Telescope Array in the hard X-ray band. We found that the hard X-ray emission of 4U 0142+61 was spectrally hard compared to the earlier detections, indicating that the source was likely in a transition to or from a harder state. We find that the surface properties of the four magnetars are consistent with what we have obtained using only the soft X-ray data with STEMS3D, implying that our physically motivated magnetar emission model is a robust tool. Based on our broadband spectral investigations, we conclude that resonant scattering of the surface photons in the magnetosphere alone cannot account for the hard X-ray emission in magnetars; therefore, an additional non-thermal process, or a population of relativistic electrons is required. We also discuss the implication of the non-detection of persistent hard X-ray emission in 1E 1048.1-5937.",
"date": "2015-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "815",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 15",
"id_number": "CaltechAUTHORS:20160203-100844301",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160203-100844301",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "T\u00dcB\u0130TAK"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "2236"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/815/1/15",
"pub_year": "2015",
"author_list": "Weng, Shan-Shan and G\u00f6\u011f\u00fc\u015f, Ersin"
},
{
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"eprint_id": 63703,
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"datestamp": "2023-08-22 17:02:08",
"lastmod": "2023-10-17 15:28:44",
"type": "article",
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"creators": {
"items": [
{
"id": "Aird-J-A",
"name": {
"family": "Aird",
"given": "J."
},
"orcid": "0000-0003-1908-8463"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
}
]
},
"title": "The NuSTAR Extragalactic Surveys: First Direct Measurements of the > 10 keV X-Ray Luminosity Function for Active Galactic Nuclei at z > 0.1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: evolution; X-rays: galaxies",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 July 31; accepted 2015 October 8; published 2015 December 10. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge financial support from: ERC Advanced Grant FEEDBACK at the University of Cambridge (J.A., A.C.F.); a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University (J.A.); the Science and Technology Facilities Council (STFC) grants ST/I001573/1 (D.M.A. and A.D.M.), ST/K501979/1 (G.B.L.), and ST/J003697/1 (P.G.); the Leverhulme Trust (D.M.A.); the Caltech Kingsley Visitor Program (D.M.A., A.C.); NSF award AST 1008067 (D.R.B.); NASA grants 11-ADAP11-0218 and GO3-14150C (F.C.); an Alfred P. Sloan Research Fellowship and a Dartmouth Class of 1962 Faculty Fellowship (R.C.H.); CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., E.T.); FONDECYT 1141218 (F.E.B.) and 1120061 (E.T.); \"EMBIGGEN\" Anillo ACT1101 (F.E.B., E.T.); the Ministry of Economy, Development, and Tourisms Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.); NASA NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G (W.N.B., B.L.); ASI/INAF grant I/037/12/0011/13 (A.C., L.Z.); and NASA Earth and Space Science Fellowship Program grant NNX14AQ07H (M.B.).\n\nPublished - Aird_2015.pdf
Submitted - 1511.04184v1.pdf
",
"abstract": "We present the first direct measurements of the rest-frame 10\u201340 keV X-ray luminosity function (XLF) of active galactic nuclei (AGNs) based on a sample of 94 sources at 0.1 < z < 3, selected at 8\u201324 keV energies from sources in the Nuclear Spectroscopic Telescope Array (NuSTAR) extragalactic survey program. Our results are consistent with the strong evolution of the AGN population seen in prior, lower-energy studies of the XLF. However, different models of the intrinsic distribution of absorption, which are used to correct for selection biases, give significantly different predictions for the total number of sources in our sample, leading to small, systematic differences in our binned estimates of the XLF. Adopting a model with a lower intrinsic fraction of Compton-thick sources and a larger population of sources with column densities N_H ~ 10^(23-24) cm^(\u22122) or a model with stronger Compton reflection component (with a relative normalization of R ~ 2 at all luminosities) can bring extrapolations of the XLF from 2\u201310 keV into agreement with our NuSTAR sample. Ultimately, X-ray spectral analysis of the NuSTAR sources is required to break this degeneracy between the distribution of absorbing column densities and the strength of the Compton reflection component and thus refine our measurements of the XLF. Furthermore, the models that successfully describe the high-redshift population seen by NuSTAR tend to over-predict previous, high-energy measurements of the local XLF, indicating that there is evolution of the AGN population that is not fully captured by the current models.",
"date": "2015-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "815",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 66",
"id_number": "CaltechAUTHORS:20160115-101313300",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160115-101313300",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "FEEDBACK"
},
{
"agency": "Durham University"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Caltech Kingsley Visitor Program"
},
{
"agency": "NSF",
"grant_number": "AST-1008067"
},
{
"agency": "NASA",
"grant_number": "GO3-14150C"
},
{
"agency": "Alfred P. Sloan Foundation"
},
{
"agency": "Dartmouth College"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-16",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
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},
{
"id": "Space-Radiation-Laboratory"
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]
},
"doi": "10.1088/0004-637X/815/1/66",
"primary_object": {
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"basename": "Aird_2015.pdf",
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"pub_year": "2015",
"author_list": "Aird, J.; Harrison, F. A.; et el."
},
{
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"eprint_id": 63162,
"eprint_status": "archive",
"datestamp": "2023-08-22 17:00:25",
"lastmod": "2023-10-25 23:36:24",
"type": "article",
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"creators": {
"items": [
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mao-Peter-H",
"name": {
"family": "Mao",
"given": "Peter H."
}
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram"
},
"orcid": "0000-0003-1703-8796"
}
]
},
"title": "NuSTAR Hard X-ray Survey of the Galactic Center Region I: Hard X-ray Morphology and Spectroscopy of the Diffuse Emission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center; radiation mechanisms: non-thermal; X-rays: general; X-rays: ISM",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 June 8; accepted 2015 October 14; published 2015 November 19. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). R. Krivonos acknowledges support from Russian Science Foundation through grant 14\u201322-00271. G. Ponti acknowledges support via an EU Marie Curie IntraEuropean fellowship under contract no. FP-PEOPLE-2012-IEF-331095, the Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. F.E. Bauer acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, \"EMBIGGEN\" Anillo ACT1101), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. S. Zhang is supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program\u2014Grant \"NNX13AM31.\" D. Barret acknowledges support from the French Space Agency (CNES). We thank Tahir Yaqoob for useful discussions on the MYTorus model.\n\nPublished - Mori_2015.pdf
Submitted - 1510.04631v1.pdf
",
"abstract": "We present the first sub-arcminute images of the Galactic Center above 10 keV, obtained with NuSTAR. NuSTAR resolves the hard X-ray source IGR J17456\u20132901 into non-thermal X-ray filaments, molecular clouds, point sources, and a previously unknown central component of hard X-ray emission (CHXE). NuSTAR detects four non-thermal X-ray filaments, extending the detection of their power-law spectra with \u0393 ~ 1.3\u20132.3 up to ~50 keV. A morphological and spectral study of the filaments suggests that their origin may be heterogeneous, where previous studies suggested a common origin in young pulsar wind nebulae (PWNe). NuSTAR detects non-thermal X-ray continuum emission spatially correlated with the 6.4 keV Fe K\u03b1 fluorescence line emission associated with two Sgr A molecular clouds: MC1 and the Bridge. Broadband X-ray spectral analysis with a Monte-Carlo based X-ray reflection model self-consistently determined their intrinsic column density (~10^(23) cm^(\u22122)), primary X-ray spectra (power-laws with \u0393 ~ 2) and set a lower limit of the X-ray luminosity of Sgr A* flare illuminating the Sgr A clouds to L_X \u2273 10^(38) erg s^(\u22121). Above ~20 keV, hard X-ray emission in the central 10 pc region around Sgr A* consists of the candidate PWN G359.95\u20130.04 and the CHXE, possibly resulting from an unresolved population of massive CVs with white dwarf masses M_(WD) ~ 0.9 M_\u2299. Spectral energy distribution analysis suggests that G359.95\u20130.04 is likely the hard X-ray counterpart of the ultra-high gamma-ray source HESS J1745\u2013290, strongly favoring a leptonic origin of the GC TeV emission.",
"date": "2015-12-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "814",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 94",
"id_number": "CaltechAUTHORS:20151223-064848832",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151223-064848832",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-22-00271"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "FP-PEOPLE-2012-IEF-331095"
},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)",
"grant_number": "BMWI/DLR, FKZ 50 OR 1408"
},
{
"agency": "Max Planck Society"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y TurismoMinistry for the Economy, Development, and Tourism's Millennium Science Initiative",
"grant_number": "IC120009"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX13AM31"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-19",
"name": "Space Radiation Laboratory"
}
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},
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{
"id": "Space-Radiation-Laboratory"
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},
"doi": "10.1088/0004-637X/814/2/94",
"primary_object": {
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"basename": "Mori_2015.pdf",
"url": "https://authors.library.caltech.edu/records/tpt82-syd77/files/Mori_2015.pdf"
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"pub_year": "2015",
"author_list": "Mori, Kaya; Forster, Karl; et el."
},
{
"id": "https://authors.library.caltech.edu/records/p1jtm-x1q74",
"eprint_id": 64111,
"eprint_status": "archive",
"datestamp": "2023-08-20 09:24:59",
"lastmod": "2023-10-17 19:30:54",
"type": "article",
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"creators": {
"items": [
{
"id": "Yan-Dahai",
"name": {
"family": "Yan",
"given": "Dahai"
}
},
{
"id": "Zhang-Li",
"name": {
"family": "Zhang",
"given": "Li"
}
},
{
"id": "Zhang-Shuang-Nan",
"name": {
"family": "Zhang",
"given": "Shuang-Nan"
}
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]
},
"title": "Parameter constraints in a near-equipartition model with multifrequency NuSTAR, Swift, and Fermi-LAT data from 3C 279",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 September 7. Received 2015 September 4; in original form 2015 June 23. First published online October 1, 2015. \n\nWe would like to give special thanks to Charles Dermer, who carefully edited the manuscript and gave us many valuable suggestions and comments. We thank Charles Dermer, J. Finke, Kinwah Wu for discussions, and the anonymous referee for very helpful and constructive questions. We are grateful to Krzysztof Nalewajko for providing us the data of 3C 279. This work is partially supported by the National Natural Science Foundation of China (NSFC 11433004) and Top Talents Program of Yunnan Province, China. DHY acknowledges partial funding support by China Postdoctoral Science Foundation under grant no. 2015M570152. SNZ acknowledges partial funding support by 973 Program of China under grant 2014CB845802, by the National Natural Science Foundation of China (NSFC) under grant nos. 11133002 and 11373036, by the Qianren start-up grant 292012312D1117210, and by the Strategic Priority Research Program 'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences (CAS) under grant no. XDB09000000. We acknowledge the use of the ASDC web tools (SED Builder, http://tools.asdc.asi.it).\n\nPublished - MNRAS-2015-Yan-1310-9.pdf
",
"abstract": "Precise spectra of 3C 279 in the 0.5\u201370 keV range, obtained during two epochs of Swift and NuSTAR observations, are analysed using a near-equipartition model. We apply a one-zone leptonic model with a three-parameter log-parabola electron energy distribution to fit the Swift and NuSTAR X-ray data, as well as simultaneous optical and Fermi-LAT gamma-ray data. The Markov chain Monte Carlo technique is used to search the high-dimensional parameter space and evaluate the uncertainties on model parameters. We show that the two spectra can be successfully fitted in near-equipartition conditions, defined by the ratio of the energy density of relativistic electrons to magnetic field \u03b6e being close to unity. In both spectra, the observed X-rays are dominated by synchrotron self-Compton photons, and the observed gamma-rays are dominated by Compton scattering of external infrared photons from a surrounding dusty torus. Model parameters are well constrained. From the low state to the high state, both the curvature of the log-parabola width parameter and the synchrotron peak frequency significantly increase. The derived magnetic fields in the two states are nearly identical (\u223c1 G), but the Doppler factor in the high state is larger than that in the low state (\u223c28 versus \u223c18). We derive that the gamma-ray emission site takes place outside the broad-line region, at \u22730.1 pc from the black hole, but within the dusty torus. Implications for 3C 279 as a source of high-energy cosmic rays are discussed.",
"date": "2015-12-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "454",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1310-1319",
"id_number": "CaltechAUTHORS:20160131-145440789",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160131-145440789",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "National Natural Science Foundation of China (NSFC)",
"grant_number": "11433004"
},
{
"agency": "973 Program of China",
"grant_number": "2014CB845802"
},
{
"agency": "National Natural Science Foundation of China (NSFC)",
"grant_number": "11133002"
},
{
"agency": "National Natural Science Foundation of China (NSFC)",
"grant_number": "11373036"
},
{
"agency": "Qianren",
"grant_number": "292012312D1117210"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDB09000000"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stv2091",
"primary_object": {
"basename": "MNRAS-2015-Yan-1310-9.pdf",
"url": "https://authors.library.caltech.edu/records/p1jtm-x1q74/files/MNRAS-2015-Yan-1310-9.pdf"
},
"pub_year": "2015",
"author_list": "Yan, Dahai; Zhang, Li; et el."
},
{
"id": "https://authors.library.caltech.edu/records/pm89c-yr556",
"eprint_id": 64110,
"eprint_status": "archive",
"datestamp": "2023-08-20 09:24:54",
"lastmod": "2023-10-17 19:30:51",
"type": "article",
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"creators": {
"items": [
{
"id": "Sazonov-S",
"name": {
"family": "Sazonov",
"given": "S."
}
},
{
"id": "Churazov-E",
"name": {
"family": "Churazov",
"given": "E."
}
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "R."
},
"orcid": "0000-0003-2737-5673"
}
]
},
"title": "Does the obscured AGN fraction really depend on luminosity?",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 September 2. Received 2015 September 2; in original form 2015 July 14. \n\nThis research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This study was supported by the Russian Foundation for Basic Research (grant 13-02-01365). We thank the referee for useful comments.\n\nPublished - MNRAS-2015-Sazonov-1202-20__1_.pdf
",
"abstract": "We use a sample of 151 local non-blazar active galactic nuclei (AGN) selected from the INTEGRAL all-sky hard X-ray survey to investigate if the observed declining trend of the fraction of obscured (i.e. showing X-ray absorption) AGN with increasing luminosity is mostly an intrinsic or selection effect. Using a torus-obscuration model, we demonstrate that in addition to negative bias, due to absorption in the torus, in finding obscured AGN in hard X-ray flux-limited surveys, there is also positive bias in finding unobscured AGN, due to Compton reflection in the torus. These biases can be even stronger taking into account plausible intrinsic collimation of hard X-ray emission along the axis of the obscuring torus. Given the AGN luminosity function, which steepens at high luminosities, these observational biases lead to a decreasing observed fraction of obscured AGN with increasing luminosity even if this fraction has no intrinsic luminosity dependence. We find that if the central hard X-ray source in AGN is isotropic, the intrinsic (i.e. corrected for biases) obscured AGN fraction still shows a declining trend with luminosity, although the intrinsic obscured fraction is significantly larger than the observed one: the actual fraction is larger than \u223c85\u2009per\u2009cent at L \u2272 10^(42.5)\u2009erg s^(\u22121) (17\u201360 keV), and decreases to \u227260\u2009per\u2009cent at L \u2273 1044 erg s\u22121. In terms of the half-opening angle \u03b8 of an obscuring torus, this implies that \u03b8 \u2272 30\u00b0 in lower luminosity AGN, and \u03b8 \u2273 45\u00b0 in higher luminosity ones. If, however, the emission from the central supermassive black hole is collimated as dL/d\u03a9\u2009\u221d\u2009cos\u2009\u03b1, the intrinsic dependence of the obscured AGN fraction is consistent with a luminosity-independent torus half-opening angle \u03b8 \u223c 30\u00b0.",
"date": "2015-12-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "454",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1202-1220",
"id_number": "CaltechAUTHORS:20160131-144240325",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160131-144240325",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Russian Foundation for Basic Research",
"grant_number": "13-02-01365"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stv2069",
"primary_object": {
"basename": "MNRAS-2015-Sazonov-1202-20__1_.pdf",
"url": "https://authors.library.caltech.edu/records/pm89c-yr556/files/MNRAS-2015-Sazonov-1202-20__1_.pdf"
},
"pub_year": "2015",
"author_list": "Sazonov, S.; Churazov, E.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/q6vjs-1rk92",
"eprint_id": 64194,
"eprint_status": "archive",
"datestamp": "2023-08-20 09:25:06",
"lastmod": "2023-10-17 19:35:18",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Pahari-M",
"name": {
"family": "Pahari",
"given": "Mayukh"
}
},
{
"id": "Misra-R",
"name": {
"family": "Misra",
"given": "Ranjeev"
}
},
{
"id": "Dewangan-G-C",
"name": {
"family": "Dewangan",
"given": "Gulab C"
}
},
{
"id": "Pawar-P",
"name": {
"family": "Pawar",
"given": "Pramod"
}
}
]
},
"title": "Constraining distance and inclination angle of V4641 Sgr using SWIFT and NuSTAR observations during low soft spectral state",
"ispublished": "pub",
"full_text_status": "restricted",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 April 25; accepted 2015 October 19; published 2015 December 1.\n\nWe thank the referee for useful discussions and comments.\nWe are thankful to the NuSTAR team for making data publicly\navailable. This research has made use of the NuSTAR Data\nAnalysis Software (NuSTARDAS) jointly developed by the\nASI Science Data Center (ASDC, Italy) and the California\nInstitute of Technology (USA). RXTE/PCA data obtained\nthrough the High Energy Astrophysics Science Archive\nResearch Center online service, provided by the NASA/\nGoddard Space Flight Center and the Swift data center. MAXI\ndata are obtained from the MAXI team, RIKEN, JAXA.",
"abstract": "We present results from NuSTAR and Swift/XRT joint spectral analysis of V4641 Sgr during a disk dominated or soft state, as well as a power law dominated or hard state. The soft state spectrum is well modeled by a relativistically blurred disk emission, a power law, a broad iron line, two narrow emission lines, and two edges. The Markov Chain Monte Carlo simulation technique and the relativistic effects seen in the disk and broad iron line allow us to self-consistently constrain the inner disk radius, disk inclination angle, and distance to the source at ${2.43}_{-0.17}^{+0.39}$Rg (GM/c2), ${69.5}_{-4.2}^{+12.8}$ degrees and ${10.8}_{-2.5}^{+1.6}$ kpc respectively. For the hard state, the spectrum is a power law with a weakly broad iron line and an edge. The distance estimate gives a measure of the Eddington fraction, ${L}_{2.0-80.0\\;\\mathrm{keV}}/{L}_{\\mathrm{Edd}},$ to be ~1.3 \u00d7 10\u22122 and ~1.9 \u00d7 10\u22123 for the soft and hard states, respectively. Unlike many other typical black hole systems, which are always in a hard state at such a low Eddington fraction, V4641 Sgr shows a soft, disk dominated state. The soft state spectrum shows narrow emission lines at ~6.95 and ~8.31 keV which can be identified as being due to emission from highly ionized iron and nickel in an X-ray irradiated wind respectively. If this is not due to instrumental effect or calibration error, this would be the first detection of a Ni fluorescent line in a black hole X-ray binary.",
"date": "2015-12-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "814",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art No 158",
"id_number": "CaltechAUTHORS:20160203-100150948",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160203-100150948",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/814/2/158",
"pub_year": "2015",
"author_list": "Pahari, Mayukh; Misra, Ranjeev; et el."
},
{
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"eprint_id": 64192,
"eprint_status": "archive",
"datestamp": "2023-08-22 16:54:21",
"lastmod": "2023-10-17 19:35:08",
"type": "article",
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"creators": {
"items": [
{
"id": "Lopez-L-A",
"name": {
"family": "Lopez",
"given": "Laura A."
},
"orcid": "0000-0002-1790-3148"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Reynolds-S-P",
"name": {
"family": "Reynolds",
"given": "Stephen P."
}
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Eriksen-K-A",
"name": {
"family": "Eriksen",
"given": "Kristoffer A."
}
},
{
"id": "Fryer-C-L",
"name": {
"family": "Fryer",
"given": "Chris L."
},
"orcid": "0000-0003-2624-0056"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel K."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
},
{
"id": "Zoglauer-A-C",
"name": {
"family": "Zoglauer",
"given": "Andreas"
}
}
]
},
"title": "A Spatially Resolved Study of the Synchrotron Emission and Titanium in Tycho's Supernova Remnant with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "ISM: individual objects:Tycho's SNR; ISM: supernova remnants; X-rays: ISM",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 April 26; accepted 2015 October 11; published 2015 November 30. \n\nWe acknowledge helpful discussions with Drs. Marco Miceli, Lorenzo Sironi, and Patrick Slane. L.A.L. received support for this work from NASA through Hubble Fellowship grant number HST-HF2-51342.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Additionally, the work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: NuSTAR, CXO, VLA.\n\nPublished - pdf
",
"abstract": "We report results from deep observations (~750 ks) of Tycho's supernova remnant (SNR) with NuSTAR. Using these data, we produce narrow-band images over several energy bands to identify the regions producing the hardest X-rays and to search for radioactive decay line emission from ^(44)Ti. We find that the hardest (>10 keV) X-rays are concentrated in the southwest of Tycho, where recent Chandra observations have revealed high emissivity \"stripes\" associated with particles accelerated to the knee of the cosmic-ray spectrum. We do not find evidence of ^(44)Ti, and we set limits on its presence and distribution within the SNR. These limits correspond to a upper-limit 44Ti mass of M44 < 2.4x10^(-4) M_sun for a distance of 2.3 kpc. We perform spatially resolved spectroscopic analysis of sixty-six regions across Tycho. We map the best-fit rolloff frequency of the hard X-ray spectra, and we compare these results to measurements of the shock expansion and ambient density. We find that the highest energy electrons are accelerated at the lowest densities and in the fastest shocks, with a steep dependence of the roll-off frequency with shock velocity. Such a dependence is predicted by models where the maximum energy of accelerated electrons is limited by the age of the SNR rather than by synchrotron losses, but this scenario requires far lower magnetic field strengths than those derived from observations in Tycho. One way to reconcile these discrepant findings is through shock obliquity effects, and future observational work is necessary to explore the role of obliquity in the particle acceleration process.",
"date": "2015-11-30",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "814",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 132",
"id_number": "CaltechAUTHORS:20160203-095010885",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160203-095010885",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF2-51342.001"
},
{
"agency": "NASA",
"grant_number": "NAS 5-26555"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-20",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/814/2/132",
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"basename": "pdf",
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},
"pub_year": "2015",
"author_list": "Lopez, Laura A.; Grefenstette, Brian W.; et el."
},
{
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"eprint_id": 61450,
"eprint_status": "archive",
"datestamp": "2023-08-22 16:52:42",
"lastmod": "2023-10-25 14:54:11",
"type": "article",
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"creators": {
"items": [
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Ogle-P-M",
"name": {
"family": "Ogle",
"given": "P."
},
"orcid": "0000-0002-3471-981X"
},
{
"id": "Tombesi-F",
"name": {
"family": "Tombesi",
"given": "F."
},
"orcid": "0000-0002-6562-8654"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
}
},
{
"id": "Zoghbi-A",
"name": {
"family": "Zoghbi",
"given": "A."
},
"orcid": "0000-0002-0572-9613"
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "A. L."
}
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G."
}
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Ursini-F",
"name": {
"family": "Ursini",
"given": "F."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Corona of the Broad-Line Radio Galaxy 3C 390.3",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; X-rays: individual (3C 390.3)",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 July 3; accepted 2015 October 5; published 2015 November 13. \n\nWe thank the anonymous referee for helpful comments. A.L. thanks Julien Malzac for helpful discussions and acknowledges support from the ERC Advanced Grant FEEDBACK. F.T. would like to thank M. Coleman Miller and Brian Morsony for useful comments. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA).\n\nPublished - Lohfink_2015.pdf
Submitted - 1510.01333v1.pdf
",
"abstract": "We present the results from a joint Suzaku/NuSTAR broadband spectral analysis of 3C 390.3. The high quality data enables us to clearly separate the primary continuum from the reprocessed components allowing us to detect a high energy spectral cut-off (E_(cut) = 117 ^(+18)_(\u221214) keV), and to place constraints on the Comptonization parameters of the primary continuum for the first time. The hard over soft compactness is 69 ^(+124)_(\u221224) and the optical depth is 4.1 ^(+0.5)_(\u22123.6), his leads to an electron temperature of 30 ^(+32)_(\u22128) keV. Expanding our study of the Comptonization spectrum to the optical/UV by studying the simultaneous Swift-UVOT data, we find indications that the compactness of the corona allows only a small fraction of the total UV/optical flux to be Comptonized. Our analysis of the reprocessed emission show that 3C 390.3 only has a small amount of reflection (R \u223c 0.3), and of that the vast majority is from distant neutral matter. However, we also discover a soft-X-ray excess in the source, which can be described by a weak ionized reflection component from the inner parts of the accretion disk. In addition to the backscattered emission, we also detect the highly ionized iron emission lines Fe xxv and Fe xxvi.",
"date": "2015-11-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "814",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 24",
"id_number": "CaltechAUTHORS:20151022-144502050",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151022-144502050",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "FEEDBACK"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-21",
"name": "Space Radiation Laboratory"
}
]
},
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"doi": "10.1088/0004-637X/814/1/24",
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"pub_year": "2015",
"author_list": "Lohfink, A. M.; Ogle, P.; et el."
},
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"items": [
{
"id": "Teng-Stacy-H",
"name": {
"family": "Teng",
"given": "Stacy H."
}
},
{
"id": "Rigby-J-R",
"name": {
"family": "Rigby",
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},
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},
{
"id": "Stern-D",
"name": {
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"orcid": "0000-0003-2686-9241"
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{
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{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
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},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "Franz E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Stephen E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
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},
"orcid": "0000-0002-0167-2453"
},
{
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"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "Andrea"
},
"orcid": "0000-0003-3451-9970"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "Duncan"
},
"orcid": "0000-0003-1748-2010"
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{
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"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "Ryan C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "Michael"
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Luo-Bin",
"name": {
"family": "Luo",
"given": "Bin"
},
"orcid": "0000-0002-9036-0063"
},
{
"id": "Treister-E",
"name": {
"family": "Treister",
"given": "Ezequiel"
},
"orcid": "0000-0001-7568-6412"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A NuSTAR Survey of Nearby Ultraluminous Infrared Galaxies",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; X-rays: galaxies",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 March 30; accepted 2015 October 9; published 2015 November 17. \n\nWe thank Lee Armus who provided useful comments in the early planning phase of the NuSTAR ULIRG program. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory and data obtained from the Chandra Data Archive published previously in cited articles. This work, in part, made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). We made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. S.H.T. was supported by a NASA Postdoctoral Program Fellowship. Partial funding for this research was provided by a NASA XMM-Newton AO-12 Grant award associated with proposal number 72261. Support for the work of E.T. was provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101. \n\nFacilities: NuSTAR, Chandra, XMM-Newton - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission.\n\nPublished - Teng_2015.pdf
Submitted - 1510.04453v1.pdf
",
"abstract": "We present a Nuclear Spectroscopic Telescope Array (NuSTAR), Chandra, and XMM-Newton survey of nine of the nearest ultraluminous infrared galaxies (ULIRGs). The unprecedented sensitivity of NuSTAR at energies above 10 keV enables spectral modeling with far better precision than was previously possible. Six of the nine sources observed were detected sufficiently well by NuSTAR to model in detail their broadband X-ray spectra, and recover the levels of obscuration and intrinsic X-ray luminosities. Only one source (IRAS 13120\u20135453) has a spectrum consistent with a Compton-thick active galactic nucleus (AGN), but we cannot rule out that a second source (Arp 220) harbors an extremely highly obscured AGN as well. Variability in column density (reduction by a factor of a few compared to older observations) is seen in IRAS 05189\u20132524 and Mrk 273, altering the classification of these borderline sources from Compton-thick to Compton-thin. The ULIRGs in our sample have surprisingly low observed fluxes in high-energy (>10 keV) X-rays, especially compared to their bolometric luminosities. They have lower ratios of unabsorbed 2\u201310 keV to bolometric luminosity, and unabsorbed 2\u201310 keV to mid-IR [O iv] line luminosity than do Seyfert 1 galaxies. We identify IRAS 08572+3915 as another candidate intrinsically X-ray weak source, similar to Mrk 231. We speculate that the X-ray weakness of IRAS 08572+3915 is related to its powerful outflow observed at other wavelengths.",
"date": "2015-11-17",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "814",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 56",
"id_number": "CaltechAUTHORS:20151022-145255616",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151022-145255616",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "72261"
},
{
"agency": "Center for Astrophysics and Associated Technologies (CATA)",
"grant_number": "PFB 06"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Postdoctoral Program"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-22",
"name": "Space Radiation Laboratory"
}
]
},
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"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
}
]
},
"doi": "10.1088/0004-637X/814/1/56",
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"author_list": "Teng, Stacy H.; Rigby, Jane R.; et el."
},
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{
"id": "Ponti-G",
"name": {
"family": "Ponti",
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{
"id": "Bianchi-S",
"name": {
"family": "Bianchi",
"given": "S."
},
"orcid": "0000-0002-4622-4240"
},
{
"id": "Mu\u00f1oz-Darias-T",
"name": {
"family": "Mu\u00f1oz-Darias",
"given": "T."
}
},
{
"id": "De-Marco-B",
"name": {
"family": "De Marco",
"given": "B."
}
},
{
"id": "Dwelly-T",
"name": {
"family": "Dwelly",
"given": "T."
}
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{
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"given": "R. P."
}
},
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"family": "Nandra",
"given": "K."
},
"orcid": "0000-0002-7150-9192"
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"orcid": "0000-0003-2177-6388"
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"name": {
"family": "Mori",
"given": "K."
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"orcid": "0000-0002-9709-5389"
},
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"name": {
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"given": "D."
},
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"given": "C. O."
},
"orcid": "0000-0003-3944-6109"
},
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"family": "Degenaar",
"given": "N."
}
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{
"id": "Aramaki-Tsuguo",
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"family": "Aramaki",
"given": "T."
}
},
{
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"name": {
"family": "Clavel",
"given": "M."
},
"orcid": "0000-0003-0724-2742"
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"id": "Goldwurm-A",
"name": {
"family": "Goldwurm",
"given": "A."
}
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{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Israel-G-L",
"name": {
"family": "Israel",
"given": "G. L."
}
},
{
"id": "Morris-M-R",
"name": {
"family": "Morris",
"given": "M. R."
},
"orcid": "0000-0002-6753-2066"
},
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"id": "Rushton-A-P",
"name": {
"family": "Rushton",
"given": "A."
}
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"name": {
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},
"title": "On the Fe K absorption - accretion state connection in the Galactic Centre neutron star X-ray binary AX J1745.6-2901",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 September 4. Received 2014 September 4. In original form 2014 July 10. First published online November 21, 2014.\n\nThe authors wish to thank Jan-Uwe Ness, Ignacio de la Calle and the rest of the XMM\u2013Newton scheduling team for the enormous support that made the new XMM\u2013Newton observations possible. GP and TMD acknowledge support via an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2012-IEF-331095 and FP-PEOPLE-2011-IEF-301355, respectively. The GC XMM\u2013Newton monitoring project is partially supported by the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. This project was funded in part by European Research Council Advanced Grant 267697 '4\u03c0sky:Extreme Astrophysics with Revolutionary Radio Telescopes'. DH acknowledges support from Chandra X-ray Observatory (CXO) Award Number GO3-14121X, operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and also by NASA Swift grant NNX14AC30G. CH is supported by an NSERC Discovery Grant, and an Ingenuity New Faculty Award. ND is supported by NASA through Hubble Postdoctoral Fellowship grant number HST-HF-51287.01-A from the Space Telescope Science Institute. The scientific results reported in this article are based on observations obtained with XMM\u2013Newton, Swift and NuSTAR.\n\nPublished - MNRAS-2015-Ponti-1536-50.pdf
",
"abstract": "AX J1745.6-2901 is a high-inclination (eclipsing) neutron star low-mass X-ray binary (LMXB) located less than \u223c1.5 arcmin from Sgr A\u22c6. Ongoing monitoring campaigns have targeted Sgr A\u22c6 frequently and these observations also cover AX J1745.6-2901. We present here an X-ray analysis of AX J1745.6-2901 using a large data set of 38 XMM\u2013Newton observations, including 11 which caught AX J1745.6-2901 in outburst. Fe K absorption is clearly seen when AX J1745.6-2901 is in the soft state, but disappears during the hard state. The variability of these absorption features does not appear to be due to changes in the ionizing continuum. The small K\u03b1/K\u03b2 ratio of the equivalent widths of the Fe xxv and Fe xxvi lines suggests that the column densities and turbulent velocities of the absorbing ionized plasma are in excess of NH \u2243 10^(23) cm^(\u22122) and vturb \u2273 500 km s^(\u22121). These findings strongly support a connection between the wind (Fe K absorber) and the accretion state of the binary. These results reveal strong similarities between AX J1745.6-2901 and the eclipsing neutron star LMXB, EXO 0748-676, as well as with high-inclination black hole binaries, where winds (traced by the same Fe K absorption features) are observed only during the accretion-disc-dominated soft states, and disappear during the hard states characterized by jet emission.",
"date": "2015-11-14",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "446",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1536-1550",
"id_number": "CaltechAUTHORS:20150824-162639408",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150824-162639408",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Marie Curie Fellowship",
"grant_number": "FP-PEOPLE-2012-IEF-331095"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "FP-PEOPLE-2011-IEF-301355"
},
{
"agency": "Bundesministerium fur Wirtschaft und Technologie (BMWI)",
"grant_number": "FKZ 50"
},
{
"agency": "Bundesministerium fur Wirtschaft und Technologie (BMWI)",
"grant_number": "FKZ 1408"
},
{
"agency": "Max Planck Society"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "267697"
},
{
"agency": "NASA",
"grant_number": "GO3-14121X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "NASA",
"grant_number": "NNX14AC30G"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "NASA",
"grant_number": "HST-HF-51287.01-A"
},
{
"agency": "Deutsches Zentrum fur Luft-und Raumfahrt"
}
]
},
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"doi": "10.1093/mnras/stu1853",
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"pub_year": "2015",
"author_list": "Ponti, G.; Bianchi, S.; et el."
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{
"id": "Feruglio-C",
"name": {
"family": "Feruglio",
"given": "C."
}
},
{
"id": "Fiore-F",
"name": {
"family": "Fiore",
"given": "F."
}
},
{
"id": "Carniani-S",
"name": {
"family": "Carniani",
"given": "S."
}
},
{
"id": "Piconcelli-E",
"name": {
"family": "Piconcelli",
"given": "E."
},
"orcid": "0000-0001-9095-2782"
},
{
"id": "Zappacosta-L",
"name": {
"family": "Zappacosta",
"given": "L."
},
"orcid": "0000-0002-4205-6884"
},
{
"id": "Bongiorno-A",
"name": {
"family": "Bongiorno",
"given": "A."
}
},
{
"id": "Cicone-C",
"name": {
"family": "Cicone",
"given": "C."
},
"orcid": "0000-0003-0522-6941"
},
{
"id": "Maiolino-R",
"name": {
"family": "Maiolino",
"given": "R."
}
},
{
"id": "Marconi-A",
"name": {
"family": "Marconi",
"given": "A."
}
},
{
"id": "Menci-N",
"name": {
"family": "Menci",
"given": "N."
}
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Veilleux-S",
"name": {
"family": "Veilleux",
"given": "S."
},
"orcid": "0000-0002-3158-6820"
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]
},
"title": "The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 ESO, 2015. \n\nReceived: 4 March 2015. Accepted: 25 August 2015. Published: November 2015. \n\nC.F. thanks the IRAM staff for support in observations and data analysis, particularly Dennis Downes, Roberto Neri, Sergio Martin-Ruiz, Jan Martin Winters, Melanie Krips, and Sabine Koenig. We thank Susanne Aalto, Santiago Garcia-Burillo, and Andrea Ferrara for stimulating discussions. C.F. gratefully acknowledges financial support from PRIN MIUR 2010-2011, project \"The Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies\", prot. 2010LY5N2T. C.F. and F.F. acknowledge financial support from INAF under the contract PRIN-INAF-2011. E.P. and A.B. acknowledge financial support from INAF under the contract PRIN-INAF-2012. S.V. acknowledges financial support from NASA grant G02-13129X. Data used in this work will be made available from http://cdsweb.u-strasbg.fr\n\nPublished - aa26020-15.pdf
",
"abstract": "Mrk 231 is a nearby ultra-luminous IR galaxy exhibiting a kpc-scale, multi-phase AGN-driven outflow. This galaxy represents the best target to investigate in detail the morphology and energetics of powerful outflows, as well as their still poorly-understood expansion mechanism and impact on the host galaxy. In this work, we present the best sensitivity and angular resolution maps of the molecular disk and outflow of Mrk 231, as traced by CO(2\u22121) and (3\u22122) observations obtained with the IRAM/PdBI. In addition, we analyze archival deep Chandra and NuSTAR X-ray observations. We use this unprecedented combination of multi-wavelength data sets to constrain the physical properties of both the molecular disk and outflow, the presence of a highly-ionized ultra-fast nuclear wind, and their connection. The molecular CO(2\u22121) outflow has a size of ~1 kpc, and extends in all directions around the nucleus, being more prominent along the south-west to north-east direction, suggesting a wide-angle biconical geometry. The maximum projected velocity of the outflow is nearly constant out to ~1 kpc, thus implying that the density of the outflowing material must decrease from the nucleus outwards as ~r-2. This suggests that either a large part of the gas leaves the flow during its expansion or that the bulk of the outflow has not yet reached out to ~1 kpc, thus implying a limit on its age of ~1 Myr. Mapping the mass and energy rates of the molecular outflow yields OF = [500\u22121000] M\u2299 yr-1 and \u0116kin,OF = [7\u221210] \u00d7 10^(43) erg\u2009s^(-1). The total kinetic energy of the outflow is Ekin,OF is of the same order of the total energy of the molecular disk, Edisk. Remarkably, our analysis of the X-ray data reveals a nuclear ultra-fast outflow (UFO) with velocity \u221220 000 km\u2009s^(-1), UFO = [0.3\u22122.1] M_\u2299 yr^(-1), and momentum load UFO/ rad = [0.2\u22121.6]. We find \u0116kin,UFO ~ \u0116kin,OF as predicted for outflows undergoing an energy conserving expansion. This suggests that most of the UFO kinetic energy is transferred to mechanical energy of the kpc-scale outflow, strongly supporting that the energy released during accretion of matter onto super-massive black holes is the ultimate driver of giant massive outflows. The momentum flux OF derived for the large scale outflows in Mrk 231 enables us to estimate a momentum boost OF/ UFO \u2248 [30\u221260]. The ratios \u0116kin,UFO/Lbol,AGN = [1\u22125] % and \u0116kin,OF/Lbol,AGN = [1\u22123] % agree with the requirements of the most popular models of AGN feedback.",
"date": "2015-11",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "583",
"publisher": "EDP Sciences",
"pagerange": "A99",
"id_number": "CaltechAUTHORS:20160201-105807048",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160201-105807048",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN-INAF-2011"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN-INAF-2012"
},
{
"agency": "NASA",
"grant_number": "G02-13129X"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201526020",
"primary_object": {
"basename": "aa26020-15.pdf",
"url": "https://authors.library.caltech.edu/records/7zfss-t4s78/files/aa26020-15.pdf"
},
"pub_year": "2015",
"author_list": "Feruglio, C.; Fiore, F.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/khaj8-r9p18",
"eprint_id": 64054,
"eprint_status": "archive",
"datestamp": "2023-08-20 08:49:20",
"lastmod": "2023-10-17 18:36:30",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Wilkins-D-R",
"name": {
"family": "Wilkins",
"given": "D. R."
}
},
{
"id": "Gallo-L-C",
"name": {
"family": "Gallo",
"given": "L. C."
}
},
{
"id": "Grupe-D",
"name": {
"family": "Grupe",
"given": "D."
},
"orcid": "0000-0002-9961-3661"
},
{
"id": "Bonson-K",
"name": {
"family": "Bonson",
"given": "K."
}
},
{
"id": "Komossa-S",
"name": {
"family": "Komossa",
"given": "S."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
}
]
},
"title": "Flaring from the supermassive black hole in Mrk 335 studied with Swift and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 September 10. Received 2015 September 10. In original form 2015 April 13. First published online October 30, 2015. \n\nDRW is supported by a CITA National Fellowship. This work is based on observations made by the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA.\n\nPublished - MNRAS-2015-Wilkins-4440-51.pdf
",
"abstract": "Monitoring of the narrow line Seyfert 1 galaxy Markarian 335 (Mrk 335) with the Swift satellite discovered an X-ray flare beginning 2014 August 29. At the peak, the 0.5\u20135 keV count rate had increased from that in the low-flux state by a factor of 10. A target of opportunity observation was triggered with NuSTAR, catching the decline of the flare on 2014 September 20. We present a joint analysis of Swift and NuSTAR observations to understand the cause of this flare. The X-ray spectrum shows an increase in directly observed continuum flux and the softening of the continuum spectrum to a photon index of 2.49 +0.08/\u22120.072.49\u22120.07+0.08 compared to the previous low-flux observations. The X-ray spectrum remains well described by the relativistically blurred reflection of the continuum from the accretion disc whose emissivity profile suggests that it is illuminated by a compact X-ray source, extending at most 5.2 rg over the disc. A very low reflection fraction of 0.41+0.15\u22120.150.41\u22120.15+0.15 is measured, unexpected for such a compact corona. The X-ray flare is, hence, interpreted as arising from the vertical collimation and ejection of the X-ray emitting corona at a mildly relativistic velocity, causing the continuum emission to be beamed away from the disc. As the flare subsides, the base of this jet-like structure collapses into a compact X-ray source that provides the majority of the radiation that illuminates the disc while continuum emission is still detected from energetic particles further out, maintaining the low reflection fraction.",
"date": "2015-10-30",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "454",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4440-4451",
"id_number": "CaltechAUTHORS:20160128-132716870",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-132716870",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stv2130",
"primary_object": {
"basename": "MNRAS-2015-Wilkins-4440-51.pdf",
"url": "https://authors.library.caltech.edu/records/khaj8-r9p18/files/MNRAS-2015-Wilkins-4440-51.pdf"
},
"pub_year": "2015",
"author_list": "Wilkins, D. R.; Gallo, L. C.; et el."
},
{
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"eprint_id": 52317,
"eprint_status": "archive",
"datestamp": "2023-08-20 08:41:31",
"lastmod": "2023-10-18 19:45:46",
"type": "article",
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"creators": {
"items": [
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "Franz E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "Murray"
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "Elizabeth"
}
}
]
},
"title": "NuSTAR Spectroscopy of Multi-Component X-ray Reflection from NGC 1068",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxies: active, galaxies: individual (NGC 1068), X-rays: galaxies",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 November 3; accepted 2015 September 8; published 2015 October 14.\n\nWe thank the anonymous referee for useful comments, which improved the clarity of the paper. We acknowledge financial support from the following: CONICYT-Chile Basal-CATA PFB-06/2007 (FEB, ET), FONDECYT grants 1141218 (FEB), 1140304 (PA), 1120061 (ET), and Anillo grant ACT1101 (FEB, PA, ET); Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" funded by the Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo (FEB); Swiss National Science Foundation through the Ambizione fellowship grant PZ00P2_154799/1 (MK); NuSTAR subcontract 44A-1092750 NASA ADP grant NNX10AC99G (WNB, BL); ASI/INAF grant I/037/12/0\u2013011/13 (SP, AC, AM and GM); and STFC grant ST/J003697/1 (PG). This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) Online Service, provided by the NASA/Goddard Space Flight Center. \n\nFacilities: CXO (ACIS, HETG), XMM (pn, MOS), NuSTAR (FPMA, FPMB), Swift (XRT, BAT), BeppoSAX (MECS, PDS), Suzaku (XIS, PIN),\n\nPublished - Bauer_2015p116.pdf
Submitted - 1411.0670v1.pdf
",
"abstract": "We report on observations of NGC1068 with NuSTAR, which provide the best constraints to date on its > 10 keV spectral shape. The NuSTAR data are consistent with past instruments, with no strong continuum or line variability over the past two decades, consistent with its classification as a Compton-thick AGN. The combined NuSTAR, Chandra, XMM-Newton, and Swift BAT spectral dataset offers new insights into the complex secondary emission seen instead of the completely obscured transmitted nuclear continuum. The critical combination of the high signal-to-noise NuSTAR data and the decomposition of the nuclear and extranuclear emission with Chandra allow us to break several model degeneracies and greatly aid physical interpretation. When modeled as a monolithic (i.e., a single N_H) reflector, none of the common Compton-reflection models are able to match the neutral fluorescence lines and broad spectral shape of the Compton reflection without requiring unrealistic physical parameters (e.g., large Fe overabundances, inconsistent viewing angles, poor fits to the spatially resolved spectra). A multi-component reflector with three distinct column densities (e.g., with best-fit values of N_H = 1.5\u00d710^(23), 5\u00d710^(24), and 10^(25) cm^(-2)) provides a more reasonable fit to the spectral lines and Compton hump, with near-solar Fe abundances. In this model, the higher N_H component provides the bulk of the flux to the Compton hump while the lower N_H component produces much of the line emission, effectively decoupling two key features of Compton reflection. We also find that \u2248 30% of the neutral Fe K\u0251 line flux arises from >2\" (\u2248140 pc) and is clearly extended, implying that a significant fraction of the <10 keV reflected component arises from regions well outside of a parsec-scale torus. These results likely have ramifications for the interpretation of Compton-thick spectra from observations with poorer signal-to-noise and/or\nmore distant objects.",
"date": "2015-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "812",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 116",
"id_number": "CaltechAUTHORS:20141203-100546034",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141203-100546034",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1140304"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "Project IC120009 \"Millennium Institute of Astrophysics (MAS)\""
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PZ00P2_154799/1"
},
{
"agency": "NuSTAR",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0\u2013011/13"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-26",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/812/2/116",
"primary_object": {
"basename": "Bauer_2015p116.pdf",
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],
"pub_year": "2015",
"author_list": "Bauer, Franz E.; Walton, Dominic J.; et el."
},
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"items": [
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
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"orcid": "0000-0001-5819-3552"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Nalewajko-K",
"name": {
"family": "Nalewajko",
"given": "Krzysztof"
}
},
{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "David R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steve E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Brenneman-L-W",
"name": {
"family": "Brenneman",
"given": "Laura W."
}
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Guainazzi-M",
"name": {
"family": "Guainazzi",
"given": "Matteo"
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "Greg M."
}
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "Giorgio"
},
"orcid": "0000-0002-2152-0916"
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
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"id": "Walter-Roland",
"name": {
"family": "Walter",
"given": "Roland"
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "3C 273 with NuSTAR: Unveiling the Active Galactic Nucleus",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "quasars: individual (3C 273) - X-rays: individual (3C 273)",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 June 16; accepted 2015 August 26; published 2015 October 5. \n\nWe thank Chris Done for bringing to our attention the alternative interpretation of the jet as a two-component inverse Compton model, and the anonymous referee, whose remarks and corrections helped improve the quality of this paper. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: Fermi - Fermi Gamma-Ray Space Telescope (formerly GLAST), Chandra (CXO) - , INTEGRAL - International Gamma-Ray Astrophysics Laboratory satellite, NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Suzaku - Suzaku (ASTRO-EII), Swift - Swift Gamma-Ray Burst Mission, and XMM - Newton X-Ray Multimirror Mission satellite.\n\nPublished - Craig_2015p14.pdf
Submitted - 1506.06182v2.pdf
",
"abstract": "We present results from a 244 ks NuSTAR observation of 3C 273 obtained during a cross-calibration campaign with the Chandra, INTEGRAL, Suzaku, Swift, and XMM-Newton observatories. We show that the spectrum, when fit with a power-law model using data from all observatories except INTEGRAL over the 1\u201378 keV band, leaves significant residuals in the NuSTAR data between 30 and 78 keV. The NuSTAR 3\u201378 keV spectrum is well described by an exponentially cutoff power law (\u0393 = 1.646 \u00b1 0.006, E_(cutoff) = 202_(-34)^(+51) keV) with a weak reflection component from cold, dense material. There is also evidence for a weak (EW = 23 \u00b1 11 eV) neutral iron line. We interpret these features as arising from coronal emission plus reflection off an accretion disk or distant material. Beyond 80 keV INTEGRAL data show clear excess flux relative to an extrapolation of the active galactic nucleus model fit to NuSTAR. This high-energy power law is consistent with the presence of a beamed jet, which begins to dominate over emission from the inner accretion flow at 30\u201340 keV. Modeling the jet locally (in the NuSTAR + INTEGRAL band) as a power law, we find that the coronal component is fit by \u0393_(AGN) = 1.638 \u00b1 0.045, E_(cutoff) = 47 \u00b1 15 keV, and jet photon index by \u0393_(jet) = 1.05 \u00b1 0.4. We also consider Fermi/LAT observations of 3C 273, and here the broadband spectrum of the jet can be described by a log-parabolic model, peaking at ~2 MeV. Finally, we investigate the spectral variability in the NuSTAR band and find an inverse correlation between flux and \u0393.",
"date": "2015-10-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "812",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 14",
"id_number": "CaltechAUTHORS:20151015-090448563",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151015-090448563",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-27",
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"doi": "10.1088/0004-637X/812/1/14",
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],
"pub_year": "2015",
"author_list": "Madsen, Kristin K.; F\u00fcrst, Felix; et el."
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{
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"eprint_id": 61449,
"eprint_status": "archive",
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"title": "First NuSTAR Observations of Mrk 501 within a Radio to TeV Multi-Instrument Campaign",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "BL Lacertae objects: general; galaxies: individual (Markarian 501); X-rays: galaxies",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 April 22; accepted 2015 September 5; published 2015 October 8. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nThe MAGIC Collaboration would like to thank the Instituto de Astrof\u00edsica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.\n\nThis research is also supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the VERITAS instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible.\n\nThe Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.\n\nAdditional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France.\n\nWe thank the Swift team duty scientists and science planners and we acknowledge the use of public data from the Swift data archive. This research has made use of the Swift XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy.\n\nThis research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut f\u00fcr Radioastronomie) at Effelsberg and with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). V. Karamanavis and I. Myserlis are funded by the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne.\n\nThe OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911.\n\nT.G. acknowledges support from Istanbul University (Project numbers 49429 and 48285), Bilim Akademisi (BAGEP program) and TUBITAK (project numbers 13AT100-431, 13AT100-466, and 13AT60-430).\n\nSt. Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015.\n\nThe research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grant NNX14AQ58G and Swift Guest Investigator grant NNX14AI96G. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory.\n\nThis research was partially supported by Scientific Research Fund of the Bulgarian Ministry of Education and Sciences under grant DO 02-137 (BIn-13/09). The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology\u2014Hellas, and the Max-Planck-Institut f\u00fcr Extraterrestrische Physik.\n\nThe Abastumani Observatory team acknowledges financial support by the by Shota Rustaveli National Science Foundation under contract FR/577/6-320/13.\n\nWe are grateful to the American Association of Variable Star Observers (AAVSO) for assisting us with some of the optical data acquisition.\n\nG. Damljanovic and O. Vince gratefully acknowledge the observing grant support from the Institute of Astronomy and Rozhen National Astronomical Observatory, Bulgarian Academy of Sciences. This work is in accordance with the Projects No 176011 (\"Dynamics and kinematics of celestial bodies and systems\"), No 176004 (\"Stellar physics\") and No 176021 (\"Visible and invisible matter in nearby galaxies: theory and observations\") supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia.\n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, MAGIC - Major Atmospheric Gamma Imaging Cherenkov Telescope, VERITAS - Very Energetic Radiation Imaging Telescope Array System, Fermi LAT - , Swift XRT/UVOT - , AAVSOnet - , FLWO - , WEBT, CrAO: 1.25m, Perkins - Lowell Observatory's 72in Perkins Telescope, Rozhen - , Skinakas - , OVRO - , Metsahovi - .\n\nPublished - Furniss_2015p65.pdf
Submitted - 1509.04936v2.pdf
",
"abstract": "We report on simultaneous broadband observations of the TeV-emitting blazar Markarian 501 between 1 April and 10 August 2013, including the first detailed characterization of the synchrotron peak with Swift and NuSTAR. During the campaign, the nearby BL Lac object was observed in both a quiescent and an elevated state. The broadband campaign includes observations with NuSTAR, MAGIC, VERITAS, the Fermi Large Area Telescope (LAT), Swift X-ray Telescope and UV Optical Telescope, various ground-based optical instruments, including the GASP-WEBT program, as well as radio observations by OVRO, Mets\u00e4hovi and the F-Gamma consortium. Some of the MAGIC observations were affected by a sand layer from the Saharan desert, and had to be corrected using event-by-event corrections derived with a LIDAR (LIght Detection And Ranging) facility. This is the first time that LIDAR information is used to produce a physics result with Cherenkov Telescope data taken during adverse atmospheric conditions, and hence sets a precedent for the current and future ground-based gamma-ray instruments. The NuSTAR instrument provides unprecedented sensitivity in hard X-rays, showing the source to display a spectral energy distribution between 3 and 79 keV consistent with a log-parabolic spectrum and hard X-ray variability on hour timescales. None (of the four extended NuSTAR observations) shows evidence of the onset of inverse-Compton emission at hard X-ray energies. We apply a single-zone equilibrium synchrotron self-Compton model to five simultaneous broadband spectral energy distributions. We find that the synchrotron self-Compton model can reproduce the observed broadband states through a decrease in the magnetic field strength coinciding with an increase in the luminosity and hardness of the relativistic leptons responsible for the high-energy emission.",
"date": "2015-10-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "812",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 65",
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"issn": "0004-637X",
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"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "Department of Energy (DOE)"
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"agency": "Centre National de la Recherche Scientifique (CNRS)"
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"agency": "Science Foundation, Ireland",
"grant_number": "SFI 10/ RFP/AST2748"
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{
"agency": "Institut national des sciences de l'Univers (INSU)"
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{
"agency": "Max-Planck-Gesellschaft"
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{
"agency": "Instituto Geogr\u00e1fico Nacional (IGN)"
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{
"agency": "International Max Planck Research School (IMPRS) for Astronomy and Astrophysics"
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{
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"grant_number": "NNX08AW31G"
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{
"agency": "NASA",
"grant_number": "NNX11A043G"
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"agency": "NSF",
"grant_number": "AST-0808050"
},
{
"agency": "NSF",
"grant_number": "AST-1109911"
},
{
"agency": "Istanbul University",
"grant_number": "49429"
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{
"agency": "Istanbul University",
"grant_number": "48285"
},
{
"agency": "Bilim Akademisi"
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"agency": "TUBITAK",
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"agency": "Russian Foundation for Basic Research",
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"agency": "Boston University"
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{
"agency": "Scientific Research Fund of the Bulgarian Ministry of Education and Sciences",
"grant_number": "DO 02-137 (BIn-13/09)"
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"agency": "Shota Rustaveli National Science Foundation",
"grant_number": "FR/577/6-320/13"
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"agency": "Astronomy and Rozhen National Astronomical Observatory"
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"agency": "Bulgarian Academy of Sciences"
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"agency": "Ministry of Education, Science and Technological Development (Serbia)",
"grant_number": "176011"
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"agency": "Ministry of Education, Science and Technological Development (Serbia)",
"grant_number": "176004"
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"agency": "Ministry of Education, Science and Technological Development (Serbia)",
"grant_number": "176021"
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"agency": "Istituto Nazionale di Astrofisica (INAF)"
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"author_list": "Furniss, A. K.; Noda, K.; et el."
},
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{
"id": "Paliya-V-S",
"name": {
"family": "Paliya",
"given": "Vaidehi S."
},
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},
{
"id": "B\u00f6ttcher-M",
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"family": "B\u00f6ttcher",
"given": "Markus"
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"given": "C. S."
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"name": {
"family": "Sahayanathan",
"given": "S."
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},
"title": "The Violent Hard X-Ray Variability of Mrk 421 Observed by NuSTAR in 2013 April",
"ispublished": "pub",
"full_text_status": "restricted",
"keywords": "galaxies: active; galaxies: jets; quasars: individual (Mrk 421); X-rays: galaxies",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 July 3; accepted 2015 August 25; published 2015 September 30. \n\nWe are thankful to the referee for a constructive review of the manuscript. This research has made use of data, software, and/or web tools obtained from NASAs High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). This work has made use of light curves provided by the University of California, San Diego Center for Astrophysics and Space Sciences, X-ray Group (R.E. Rothschild, A.G. Markowitz, E.S. Rivers, and B.A. McKim), obtained at http://cass.ucsd.edu/~rxteagn/. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The work of M.B. is supported by the South African Research Chair Initiative (SARChI) of the Department of Science and Technology and the National Research Foundation9 of South Africa.",
"abstract": "The well-studied blazar Markarian 421 (Mrk 421, z = 0.031) was the subject of an intensive multi-wavelength campaign when it flared in 2013 April. The recorded X-ray and very high-energy (E > 100 GeV) \u03b3-ray fluxes are the highest ever measured from this object. At the peak of the activity, it was monitored by the hard X-ray focusing telescope Nuclear Spectroscopic Telescope Array (NuSTAR) and the Swift X-Ray Telescope (XRT). In this work, we present a detailed variability analysis of NuSTAR and Swift-XRT observations of Mrk 421 during this flaring episode. We obtained the shortest flux doubling time of 14.01 \u00b1 5.03 minutes, which is the shortest hard X-ray (3-79 keV) variability ever recorded from Mrk 421, and is on the order of the light-crossing time of the black hole's event horizon. A pattern of extremely fast variability events superposed on slowly varying flares is found in most of the NuSTAR observations. We suggest that these peculiar variability patterns may be explained by magnetic energy dissipation and reconnection in a fast-moving compact emission region within the jet. Based on the fast variability, we derive a lower limit on the magnetic field strength of B \u2265 0.73{\u03b4 }_1^(-2/3) {\u03bd }_(19)^(1/3) G, where \u03b4_1 is the Doppler factor in units of 10, and \u03bd_(19) is the characteristic X-ray synchrotron frequency in units of 10^(19) Hz.",
"date": "2015-10-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "811",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 143",
"id_number": "CaltechAUTHORS:20160131-142700185",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160131-142700185",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"doi": "10.1088/0004-637X/811/2/143",
"pub_year": "2015",
"author_list": "Paliya, Vaidehi S.; B\u00f6ttcher, Markus; et el."
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"datestamp": "2023-08-20 08:26:47",
"lastmod": "2023-10-17 19:31:33",
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{
"id": "Chernyakova-Maria",
"name": {
"family": "Chernyakova",
"given": "M."
},
"orcid": "0000-0002-9735-3608"
},
{
"id": "Neronov-A",
"name": {
"family": "Neronov",
"given": "A."
}
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"id": "van-Soelen-Brian",
"name": {
"family": "van Soelen",
"given": "B."
},
"orcid": "0000-0003-1873-7855"
},
{
"id": "Callanan-P-J",
"name": {
"family": "Callanan",
"given": "P."
}
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"id": "O'Shaughnessy-L",
"name": {
"family": "O'Shaughnessy",
"given": "L."
}
},
{
"id": "Babyk-L",
"name": {
"family": "Babyk",
"given": "L."
}
},
{
"id": "Tsygankov-Sergey-S",
"name": {
"family": "Tsygankov",
"given": "S."
},
"orcid": "0000-0002-9679-0793"
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"id": "Vovk-L",
"name": {
"family": "Vovk",
"given": "L."
}
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"family": "Krivonos",
"given": "R."
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"orcid": "0000-0003-2737-5673"
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"id": "Tomsick-John-A",
"name": {
"family": "Tomsick",
"given": "J. A."
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"orcid": "0000-0001-5506-9855"
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{
"id": "Malyshev-D",
"name": {
"family": "Malyshev",
"given": "D."
}
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{
"id": "Li-J",
"name": {
"family": "Li",
"given": "J."
}
},
{
"id": "Wood-Kent-S",
"name": {
"family": "Wood",
"given": "K."
},
"orcid": "0000-0002-7376-3151"
},
{
"id": "Torres-Diego-F",
"name": {
"family": "Torres",
"given": "D."
},
"orcid": "0000-0002-1522-9065"
},
{
"id": "Zhang-S",
"name": {
"family": "Zhang",
"given": "S."
}
},
{
"id": "Kretschmar-Peter",
"name": {
"family": "Kretschmar",
"given": "P."
},
"orcid": "0000-0001-9840-2048"
},
{
"id": "McSwain-M-Virginia",
"name": {
"family": "McSwain",
"given": "M.V."
},
"orcid": "0000-0002-4775-2803"
},
{
"id": "Buckley-David-A-H",
"name": {
"family": "Buckley",
"given": "D. A. H."
},
"orcid": "0000-0002-7004-9956"
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{
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"family": "Koen",
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"title": "Multi-wavelength observations of the binary system PSR B1259\u221263/LS 2883 around the 2014 periastron passage",
"ispublished": "pub",
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"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 August 21. Received 2015 August 21. In original form 2015 July 17. First published online October 1, 2015. \n\nThis work was partially supported by the EU COST Action MP1304 'NewCompStar'. The authors thank the International Space Science Institute (ISSI, Bern) for support within the ISSI team 'Study of Gamma-ray Loud Binary Systems' and SFI/HEA Irish Centre for\nHigh-End Computing (ICHEC) for the provision of computational facilities and support. SZh acknowledges support from the Chinese NSFC 11473027, 11133002, XTP project XDA 04060604; Strategic Priority Research Program 'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences, Grant No. XDB09000000 and Strategic Priority Research Program on Space Science, Chinese Academy of Sciences, Grant No.XDA04010300. ST thanks Russian Scientific Foundation for the support (grant 14-12-01287). MVM is grateful for support from the National Science Foundation through the grant AST-1109247. Some of the observations reported in this paper were obtained with the SALT. Authors acknowledge the allocation of telescope time by the South African Astronomical Observatory. CK acknowledges funding from the South African Research Foundation. The work of IuB was partially supported by the Stipendium of the President of Ukraine (2014-2016). JL and DFT acknowledge support from the grants AYA2012-39303, SGR 2014-1073 and support from the National Natural Science Foundation of China via NSFC-11473027. JL acknowledges support by the Faculty of the European Space Astronomy Centre. DFT acknowledges the Chinese Academy of Sciences visiting professorship programme 2013T2J0007.\n\nPublished - MNRAS-2015-Chernyakova-1358-70.pdf
",
"abstract": "We report on the results of the extensive multi-wavelength campaign from optical to GeV \u03b3-rays of the 2014 periastron passage of PSR B1259\u221263, which is a unique high-mass \u03b3-ray emitting binary system with a young pulsar companion. Observations demonstrate the stable nature of the post-periastron GeV flare and prove the coincidence of the flare with the start of rapid decay of the H\u03b1 equivalent width, usually interpreted as a disruption of the Be stellar disc. Intensive X-ray observations reveal changes in the X-ray spectral behaviour happening at the moment of the GeV flare. We demonstrate that these changes can be naturally explained as a result of synchrotron cooling of monoenergetic relativistic electrons injected into the system during the GeV flare.",
"date": "2015-10",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "454",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1358-1370",
"id_number": "CaltechAUTHORS:20160201-111521546",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160201-111521546",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11473027"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11133002"
},
{
"agency": "XTP project XDA",
"grant_number": "04060604"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDB09000000"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDA04010300"
},
{
"agency": "Russian Scientific Foundation",
"grant_number": "14- 12-01287"
},
{
"agency": "NSF",
"grant_number": "AST-1109247"
},
{
"agency": "National Research Foundation (South Africa)"
},
{
"agency": "Stipendium of the President of Ukraine"
},
{
"agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)",
"grant_number": "AYA2012-39303"
},
{
"agency": "National Natural Science Foundation of China",
"grant_number": "11473027"
},
{
"agency": "European Space Astronomy Centre"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "2013T2J0007"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stv1988",
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"url": "https://authors.library.caltech.edu/records/nfvq1-wb791/files/MNRAS-2015-Chernyakova-1358-70.pdf"
},
"pub_year": "2015",
"author_list": "Chernyakova, M.; Neronov, A.; et el."
},
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{
"id": "Tao-Lian",
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"name": {
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{
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{
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"family": "F\u00fcrst",
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},
{
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"name": {
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},
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"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "Poshak"
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
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"name": {
"family": "Krimm",
"given": "Hans A."
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"orcid": "0000-0003-4348-6058"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
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{
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"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "Shriharsh P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR and Swift observations of the black hole candidate XTE J1908+094 during its 2013 outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 stars: individual (XTE J1908+094) \u2013 X-rays: binaries",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 June 5; accepted 2015 August 5; published 2015 September 18.\n\nThis work was supported under NASA contract No.\nNNG08FD60C and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software, and Calibration teams for\nsupport with the execution and analysis of these observations.\nThis research has made use of the NuSTAR Data Analysis\nSoftware (NuSTARDAS), jointly developed by the ASI\nScience Data Center (ASDC, Italy) and the California Institute\nof Technology (USA).\nFacilities: NuSTAR, Swift.\n\nPublished - Tao_2015p51.pdf
Submitted - 1506.02001v1.pdf
",
"abstract": "The black hole candidate XTE J1908+094 went into outburst for the first time\nsince 2003 in October 2013. We report on an observation with the Nuclear\nSpectroscopic Telescope Array (NuSTAR) and monitoring observations with Swift\nduring the outburst. NuSTAR caught the source in the soft state: the spectra\nshow a broad relativistic iron line, and the light curves reveal a ~40 ks flare\nwith the count rate peaking about 40% above the non-flare level and with\nsignificant spectral variation. A model combining a multi-temperature thermal\ncomponent, a power-law, and a reflection component with an iron line provides a\ngood description of the NuSTAR spectrum. Although relativistic broadening of\nthe iron line is observed, it is not possible to constrain the black hole spin\nwith these data. The variability of the power-law component, which can also be\nmodeled as a Comptonization component, is responsible for the flux and spectral\nchange during the flare, suggesting that changes in the corona (or possibly\ncontinued jet activity) are the likely cause of the flare.",
"date": "2015-09-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "811",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 51",
"id_number": "CaltechAUTHORS:20150802-092031817",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-092031817",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-11",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/811/1/51",
"primary_object": {
"basename": "1506.02001v1.pdf",
"url": "https://authors.library.caltech.edu/records/vyrqz-2f181/files/1506.02001v1.pdf"
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}
],
"pub_year": "2015",
"author_list": "Tao, Lian; Tomsick, John A.; et el."
},
{
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"eprint_id": 59136,
"eprint_status": "archive",
"datestamp": "2023-08-20 08:04:43",
"lastmod": "2023-10-23 20:06:19",
"type": "article",
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"creators": {
"items": [
{
"id": "Riemer-S\u00f8rensen-S",
"name": {
"family": "Riemer-S\u00f8rensen",
"given": "S."
}
},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "D."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G."
}
},
{
"id": "Molendi-S",
"name": {
"family": "Molendi",
"given": "S."
}
},
{
"id": "Gastaldello-F",
"name": {
"family": "Gastaldello",
"given": "F."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
},
{
"id": "Hornstrup-A",
"name": {
"family": "Hornstrup",
"given": "A."
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}
]
},
"title": "Dark matter line emission constraints from NuSTAR observations of the Bullet Cluster",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "dark matter \u2013 line: identification \u2013 X-rays: galaxies: clusters",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 July 6; accepted 2015 July 28; published 2015 August 27. \n\nThis research made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA, and it also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacility: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission\n\nPublished - Riemer-S\u00f8rensen_2015.pdf
Submitted - 1507.01378v1.pdf
",
"abstract": "Line emission from dark matter is well motivated for some candidates e.g. sterile neutrinos. We present the first search for dark matter line emission in the 3-80keV range in a pointed observation of the Bullet Cluster with NuSTAR.\nWe do not detect any significant line emission and instead we derive upper\nlimits (95% CL) on the flux, and interpret these constraints in the context of\nsterile neutrinos and more generic dark matter candidates. NuSTAR does not have the sensitivity to constrain the recently claimed line detection at 3.5keV, but improves on the constraints for energies of 10-25keV.",
"date": "2015-09-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "810",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 48",
"id_number": "CaltechAUTHORS:20150801-092701193",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150801-092701193",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/810/1/48",
"primary_object": {
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}
],
"pub_year": "2015",
"author_list": "Riemer-S\u00f8rensen, S.; Wik, D.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/fwq4x-9pf09",
"eprint_id": 64107,
"eprint_status": "archive",
"datestamp": "2023-08-22 16:18:37",
"lastmod": "2023-10-17 19:30:36",
"type": "article",
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"creators": {
"items": [
{
"id": "Chandra-P",
"name": {
"family": "Chandra",
"given": "Poonam"
}
},
{
"id": "Chevalier-R-A",
"name": {
"family": "Chevalier",
"given": "Roger A."
}
},
{
"id": "Chugai-N",
"name": {
"family": "Chugai",
"given": "Nikolai"
}
},
{
"id": "Fransson-C",
"name": {
"family": "Fransson",
"given": "Claes"
},
"orcid": "0000-0001-8532-3594"
},
{
"id": "Soderberg-A-M",
"name": {
"family": "Soderberg",
"given": "Alicia M."
}
}
]
},
"title": "X-Ray and Radio Emission from Type IIn Supernova SN 2010jl",
"ispublished": "pub",
"full_text_status": "restricted",
"keywords": "circumstellar matter; radiation mechanisms: non-thermal; radio continuum: general; stars: mass-loss; supernovae: individual (SN 2010jl); X-rays: general",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2014 December 10; accepted 2015 July 20; published 2015 August 26. \n\nP.C. thanks Jayaram Chengalur, Nissim Kanekar, and Gulabchand Dewangan for useful discussions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Awards GO0-211080X, GO2-13082X, and GO4-15065X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. The research by C.F. is supported by the Swedish Research Council and Swedish National Space Board. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. \n\nFacilities: EVLA - Expanded Very Large Array, XMM-CXO - Newton X-Ray Multimirror Mission satellite, Swift - Swift Gamma-Ray Burst Mission, NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission.",
"abstract": "We present all X-ray and radio observations of the Type IIn supernova SN 2010jl. The X-ray observations cover a period up to day 1500 with Chandra, XMM-Newton, NuSTAR, and Swift-X-ray Telescope (XRT). The Chandra observations after 2012 June, the XMM-Newton observation in 2013 November, and most of the Swift-XRT observations until 2014 December are presented for the first time. All the spectra can be fitted by an absorbed hot thermal model except for Chandra spectra on 2011 October and 2012 June when an additional component is needed. Although the origin of this component is uncertain, it is spatially coincident with the supernova and occurs when there are changes to the supernova spectrum in the energy range close to that of the extra component, indicating that the emission is related to the supernova. The X-ray light curve shows an initial plateau followed by a steep drop starting at day \u02dc300. We attribute the drop to a decrease in the circumstellar density. The column density to the X-ray emission drops rapidly with time, showing that the absorption is in the vicinity of the supernova. We also present Very Large Array radio observations of SN 2010jl. Radio emission was detected from SN 2010jl from day 570 onwards. The radio light curves and spectra suggest that the radio luminosity was close to its maximum at the first detection. The velocity of the shocked ejecta derived assuming synchrotron self-absorption is much less than that estimated from the optical and X-ray observations, suggesting that free-free absorption dominates.",
"date": "2015-09-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "810",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 32",
"id_number": "CaltechAUTHORS:20160131-141702244",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160131-141702244",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "GO0-211080X"
},
{
"agency": "NASA",
"grant_number": "GO2-13082X"
},
{
"agency": "NASA",
"grant_number": "GO4-15065X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/810/1/32",
"pub_year": "2015",
"author_list": "Chandra, Poonam; Chevalier, Roger A.; et el."
},
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"datestamp": "2023-08-20 08:01:48",
"lastmod": "2023-10-25 17:14:47",
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"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
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},
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"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Markwardt-C-B",
"name": {
"family": "Markwardt",
"given": "Craig B."
},
"orcid": "0000-0001-9803-3879"
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
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"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
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"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "Takao"
}
},
{
"id": "Bhalerao-V-B",
"name": {
"family": "Bhalerao",
"given": "Varun"
},
"orcid": "0000-0002-6112-7609"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steve E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
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"name": {
"family": "Craig",
"given": "William W."
}
},
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"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
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},
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},
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},
"orcid": "0000-0002-2734-7835"
},
{
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"name": {
"family": "Rana",
"given": "Vikram"
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Westergaard-N-J",
"name": {
"family": "Westergaard",
"given": "Niels J\u00f8rgen"
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
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"title": "Calibration of the NuSTAR High-energy Focusing X-ray Telescope",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "instrumentation: detectors \u2013 space vehicles: instruments \u2013 telescopes",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 April 7; accepted 2015 August 4; published 2015 September 1. \n\nWe would like to thank the referee for helpful comments and suggestions which helped improve the paper. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: CXO, NuSTAR, Swift, Suzaku, and XMM.\n\nPublished - Madsen_2015p8.pdf
Submitted - 1504.01672v2.pdf
",
"abstract": "We present the calibration of the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray satellite. We used the Crab as the primary effective area calibrator and constructed a piece-wise linear spline function to modify the vignetting response. The achieved residuals for all off-axis angles and energies, compared to the assumed spectrum, are typically better than \u00b12% up to 40 keV and 5%\u201310% above due to limited counting statistics. An empirical adjustment to the theoretical two-dimensional point-spread function (PSF) was found using several strong point sources, and no increase of the PSF half-power diameter has been observed since the beginning of the mission. We report on the detector gain calibration, good to 60 eV for all grades, and discuss the timing capabilities of the observatory, which has an absolute timing of \u00b13 ms. Finally, we present cross-calibration results from two campaigns between all the major concurrent X-ray observatories (Chandra, Swift, Suzaku, and XMM-Newton), conducted in 2012 and 2013 on the sources 3C 273 and PKS 2155-304, and show that the differences in measured flux is within ~10% for all instruments with respect to NuSTAR.",
"date": "2015-09",
"date_type": "published",
"publication": "Astrophysical Journal Supplement Series",
"volume": "220",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 8",
"id_number": "CaltechAUTHORS:20151202-143838895",
"issn": "0067-0049",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151202-143838895",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"author_list": "Madsen, Kristin K.; Harrison, Fiona A.; et el."
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},
"title": "NuSTAR Reveals Extreme Absorption in z < 0.5 Type 2 Quasars",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active \u2013 X-rays: galaxies",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 February 12; accepted 2015 June 12; published 2015 August 14. \n\nWe thank the referee for a careful review, which has improved this work. We acknowledge financial support from: the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/J003697/1 (P.G.), ST/I001573/1 (D.M.A. and A.D.M.); the Leverhulme Trust (D.M.A.); Gemini-CONICYT grant 32120009 (R.J.A.); the ERC Advanced Grant FEEDBACK at the University of Cambridge (J.A.); NSF AST award 1008067 (D.R.B.); the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.); CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B.), FONDECYT 1141218 (F.E.B.), and \"EMBIGGEN\" Anillo ACT1101 (F.E.B.); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.); Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.); NASA ADP grant NNX10AC99G (W.N.B. and B.L.); the Caltech Kingsley visitor program (A.C.); ASI/INAF grant I/037/12/0011/13 (A.C., S.P., C.V.); NASA ADAP award NNX12AE38G (R.C.H.); National Science Foundation grant 1211096 (R.C.H.); and Swiss National Science Foundation grant PP00P2_138979/1 (M.K.). We thank Andrew Ptak and Jianjun Jia for the useful correspondence. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: Chandra, IRAS, NuSTAR, Sloan, Spitzer, Swift, WISE, XMM-Newton.\n\nPublished - Lansbury_2015.pdf
Submitted - 1506.05120v1.pdf
",
"abstract": "The intrinsic column density (N_H) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z < 1, the X-ray spectra can only be reliably characterized using broad-band measurements that extend to energies above 10 keV. Using the hard X-ray observatory NuSTAR, along with archival Chandra and XMM-Newton data, we study the broad-band X-ray spectra of nine optically selected (from the SDSS), candidate Compton-thick (N_H > 1.5 \u00d7 10^(24) cm^(\u22122)) type 2 quasars (CTQSO2s); five new NuSTAR observations are reported herein, and four have been previously published. The candidate CTQSO2s lie at z < 0.5, have observed [O III] luminosities in the range 8.4 < log(L_([O III])/L\u2299) < 9.6, and show evidence for extreme, Compton-thick absorption when indirect absorption diagnostics are considered. Among the nine candidate CTQSO2s, five are detected by NuSTAR in the high-energy (8\u201324 keV) band: two are weakly detected at the \u22483\u03c3 confidence level and three are strongly detected with sufficient counts for spectral modeling (\u227390 net source counts at 8\u201324 keV). For these NuSTAR-detected sources direct (i.e., X-ray spectral) constraints on the intrinsic active galactic nucleus properties are feasible, and we measure column densities \u22482.5\u20131600 times higher and intrinsic (unabsorbed) X-ray luminosities \u224810\u201370 times higher than pre-NuSTAR constraints from Chandra and XMM-Newton. Assuming the NuSTAR-detected type 2 quasars are representative of other Compton-thick candidates, we make a correction to the N_H distribution for optically selected type 2 quasars as measured by Chandra and XMM-Newton for 39 objects. With this approach, we predict a Compton-thick fraction of f_(CT) = 36^(+14)_(-12)%, although higher fractions (up to 76%) are possible if indirect absorption diagnostics are assumed to be reliable.",
"date": "2015-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "809",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 115",
"id_number": "CaltechAUTHORS:20150708-124636254",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150708-124636254",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "32120009"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "FEEDBACK"
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},
{
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{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
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{
"agency": "NASA",
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},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
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{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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{
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"grant_number": "1211096"
},
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"agency": "Swiss National Science Foundation (SNSF)",
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{
"agency": "NASA",
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"agency": "Caltech Kingsley Foundation Fellowship"
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"author_list": "Lansbury, G. B.; Gandhi, P.; et el."
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},
"title": "NuSTAR discovery of an unusually steady long-term spin-up of the Be binary 2RXP J130159.6-635806",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (2RXP J130159.6\u2013635806) \u2013 stars: emission-line, Be \u2013 X-rays: binaries",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 May 27; accepted 2015 July 16; published 2015 August 18. \n\nThis research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States. A.L. and S.T. acknowledge support from Russian Science Foundation (grant 14-12-01287). \n\nFacilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM-Newton - Newton X-Ray Multimirror Mission satellite.\n\nPublished - Krivonos_2015.pdf
Submitted - 1507.04534v1.pdf
",
"abstract": "We present spectral and timing analyses of Nuclear Spectroscopic Telescope Array (NuSTAR) observations of the accreting X-ray pulsar 2RXP J130159.6\u2013635806. The source was serendipitously observed during a campaign focused on the gamma-ray binary PSR B1259\u201363 and was later targeted for a dedicated observation. The spectrum has a typical shape for accreting X-ray pulsars, consisting of a simple power law with an exponential cutoff starting at ~7 keV with a folding energy of E_(fold) \u2243 18 keV. There is also an indication of the presence of a 6.4 keV iron line in the spectrum at the ~3\u03c3 significance level. NuSTAR measurements of the pulsation period reveal that the pulsar has undergone a strong and steady spin-up for the last 20 years. The pulsed fraction is estimated to be ~80%, and is constant with energy up to 40 keV. The power density spectrum shows a break toward higher frequencies relative to the current spin period. This, together with steady persistent luminosity, points to a long-term mass accretion rate high enough to bring the pulsar out of spin equilibrium.",
"date": "2015-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "809",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 140",
"id_number": "CaltechAUTHORS:20150801-084010223",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150801-084010223",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "Russian Science Foundation",
"grant_number": "14-12-01287"
}
]
},
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"doi": "10.1088/0004-637X/809/2/140",
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"author_list": "Krivonos, Roman A.; Tsygankov, Sergey S.; et el."
},
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},
"orcid": "0000-0002-7122-3549"
},
{
"id": "Shukla-A",
"name": {
"family": "Shukla",
"given": "A."
}
},
{
"id": "Misra-R",
"name": {
"family": "Misra",
"given": "R."
}
},
{
"id": "Chitnis-V-R",
"name": {
"family": "Chitnis",
"given": "V. R."
}
},
{
"id": "Rao-A-R",
"name": {
"family": "Rao",
"given": "A. R."
}
},
{
"id": "Acharya-B-S",
"name": {
"family": "Acharya",
"given": "B. S."
}
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},
"title": "Underlying particle spectrum of Mkn 421 during the huge X-ray flare in April 2013",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 ESO, 2015. \n\nReceived: 6 April 2015. Accepted: 9 June 2015. Published: 7 Aug 2015. \n\nA. Sinha would like to thank Sunder Sahayanathan from the Bhabha Atomic Research Center, Mumbai, for helpful discussions and comments. This research has made use of data, software and/or web tools obtained from NASAs High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility the ASI Science Data Center (ASDC), Italy, and the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). Data from the Steward Observatory spectropolarimetric monitoring project were used. This program is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G.\n\nPublished - aa26264-15.pdf
",
"abstract": "Context. In April 2013, the nearby TeV blazar, Mkn 421, showed one of the largest flares in X-rays in the past decade.\nAims. We study all multiwavelength data available during MJD 56\u2009392 to 56\u2009403, with special emphasis on X-ray data to understand the underlying particle energy distribution.\nMethods. We studied the correlations between the UV and gamma-ray bands with the X-ray band using the z-transformed discrete correlation function. We modelled the underlying particle energy spectrum with a single population of electrons emitting synchrotron radiation, and statistically fitted the simultaneous time-resolved data from Swift-XRT and NuSTAR.\nResults. The flux varied rapidly in the X-ray band, with a minimum doubling timescale of 1.69 \u00b1 0.13 h. There were no corresponding flares in UV and gamma-ray bands. The variability in UV and gamma rays was relatively modest with ~8% and ~16%, respectively, and no significant correlation was found with the X-ray light curve. The observed X-ray spectrum shows a clear curvature that can be fit by a log parabolic spectral form. This is best explained as originating from a log parabolic electron spectrum. However, a broken power law or a power law with an exponentially falling electron distribution cannot be ruled out either. Moreover, the excellent broadband spectrum from 0.3\u201379 keV allows us to make predictions of the UV flux. We find that this prediction is compatible with the observed flux during the low state in X-rays. However, during the X-ray flares, depending on the adopted model, the predicted flux is a factor of 2\u201350 lower than the observed one. This suggests that the X-ray flares are probably caused by a separate population that does not contribute significantly to the radiation at lower energies. Alternatively, the underlying particle spectrum can be much more complex than those explored in this work.",
"date": "2015-08-07",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "580",
"publisher": "EDP Sciences",
"pagerange": "Art No.100",
"id_number": "CaltechAUTHORS:20160128-203947016",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-203947016",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX08AW56G"
},
{
"agency": "NASA",
"grant_number": "NNX09AU10G"
},
{
"agency": "NASA",
"grant_number": "NNX12AO93G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1051/0004-6361/201526264",
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"author_list": "Sinha, A.; Shukla, A.; et el."
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"name": {
"family": "Ursini",
"given": "F."
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"name": {
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"given": "A."
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"name": {
"family": "Bianchi",
"given": "S."
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"orcid": "0000-0002-4622-4240"
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"family": "Tortosa",
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"family": "Arevalo",
"given": "P."
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"given": "D. R."
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"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
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},
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"family": "Lohfink",
"given": "A. M."
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"name": {
"family": "Reynolds",
"given": "C. S."
}
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"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
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},
"title": "The NuSTAR X-ray spectrum of the low-luminosity active galactic nucleus in NGC 7213",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual: NGC 7213; galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 July 7. Received 2015 May 27. In original form 2015 April 17. First published online August 3, 2015. \n\nWe thank the anonymous referee for his/her helpful comments, which improved the manuscript. FU thanks Pierre-Olivier Petrucci for useful discussions and comments. This work is based on observations obtained with the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA. This research has made use of data, software and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. FU, GM and SB acknowledge support from the French-Italian International Project of Scientific Collaboration: PICS-INAF project number 181542. FU acknowledges support from CNES and Universit\u00e9 Franco-Italienne (Vinci PhD fellowship). FU, AM and GM acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. SB acknowledges financial support from the Italian Space Agency under grant ASI-INAF I/037/12/P1. PA acknowledges support from FONDECYT 1140304. FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, 'EMBIGGEN' Anillo ACT1101) and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS.\n\nPublished - MNRAS-2015-Ursini-3266-72.pdf
Submitted - 1507.01775v1.pdf
",
"abstract": "We present an analysis of the 3\u201379 keV NuSTAR spectrum of the low-luminosity active galactic nucleus NGC 7213. In agreement with past observations, we find a lower limit to the high-energy cut-off of E_c > 140 keV, no evidence for a Compton-reflected continuum and the presence of an iron K \u03b1 complex, possibly produced in the broad-line region. From the application of the MYTORUS model, we find that the line-emitting material is consistent with the absence of a significant Compton reflection if arising from a Compton-thin torus of gas with a column density of 5.0^(+2.0)_(\u22121.6) \u00d7 10^(23) cm^(\u22122). We report variability of the equivalent width of the iron lines on the time-scale of years using archival observations from XMM\u2013Newton, Chandra and Suzaku. This analysis suggests a possible contribution from dusty gas. A fit with a Comptonization model indicates the presence of a hot corona with a temperature kT_e > 40 keV and an optical depth \u03c4 \u2272 1, assuming a spherical geometry.",
"date": "2015-08-06",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "452",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3266-3272",
"id_number": "CaltechAUTHORS:20150801-091143342",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150801-091143342",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "181542"
},
{
"agency": "Universite Franco-Italienne"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/P1"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1140304"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio (ICM) del Ministerio de Econom\u00eda",
"grant_number": "IC120009"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
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"doi": "10.1093/mnras/stv1527",
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"pub_year": "2015",
"author_list": "Ursini, F.; Marinucci, A.; et el."
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{
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"name": {
"family": "Nowak",
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{
"id": "Bachetti-M",
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"given": "D."
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"family": "Walton",
"given": "D. J."
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"name": {
"family": "Wilms",
"given": "J."
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"family": "Zhang",
"given": "W. W."
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},
"title": "The complex accretion geometry of GX 339-4 as seen by NuSTAR and Swift",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 stars: black holes \u2013 X-rays: binaries \u2013 X-rays: individual (GX 339\u20134)",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 January 23; accepted 2015 June 4; published 2015 July 27.\n\nWe thank the anonymous referee for very constructive and\nhelpful comments. This work was supported under NASA\nContract No. NNG08FD60C and made use of data from the\nNuSTAR mission, a project led by the California Institute of\nTechnology, managed by the Jet Propulsion Laboratory, and\nfunded by the National Aeronautics and Space Administration.\nWe thank the NuSTAR Operations, Software, and Calibration\nteams for support with the execution and analysis of these\nobservations. This research has made use of the NuSTAR Data\nAnalysis Software (NuSTARDAS), jointly developed by the\nASI Science Data Center (ASDC, Italy) and the California\nInstitute of Technology (USA). J.A.T. acknowledges partial\nsupport from NASA Swift Guest Investigator grants\nNNX13AJ81G and NNX14AC56G. S.C. acknowledges funding\nsupport from the ANR \"CHAOS\" (ANR-12-BS05-0009).\nWe would like to thank John E. Davis for the\nslxfig module, which was used to produce all figures in\nthis work.\n\nPublished - F\u00fcrst_2015p122.pdf
Submitted - 1506.01381v1.pdf
",
"abstract": "We present spectral analyses of five Nuclear Spectroscopic Telescope Array and Swift observations of GX 339\u20134 taken during a failed outburst during the summer of 2013. These observations cover Eddington luminosity fractions in the range \u22480.9%\u20136%. Throughout this outburst GX 339\u20134 stayed in the hard state and all five observations show similar X-ray spectra, with a hard power law with a photon index near 1.6, and significant contribution from reflection. Using simple reflection models we find unrealistically high iron abundances. Allowing for different photon indices for the continuum incident on the reflector relative to the underlying observed continuum results in a statistically better fit and reduced iron abundances. With a photon index around 1.3, the input power law on the reflector is significantly harder than that which is directly observed. We study the influence of different emissivity profiles and geometries and consistently find an improvement when using separate photon indices. The inferred inner accretion disk radius is strongly model dependent, but we do not find evidence for a truncation radius larger than 100 r_g in any model. The data do not allow independent spin constraints, but the results are consistent with the literature (i.e., a > 0). Our best-fit models indicate an inclination angle in the range 40\u00b0\u201360\u00b0, consistent with limits on the orbital inclination but higher than reported in the literature using standard reflection models. The iron line around 6.4 keV is clearly broadened, and we detect a superimposed narrow core as well. This core originates from a fluorescent region outside the influence of the strong gravity of the black hole. Additionally, we discuss possible geometries.",
"date": "2015-08-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 122",
"id_number": "CaltechAUTHORS:20150802-092749093",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-092749093",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX13AJ81G"
},
{
"agency": "NASA",
"grant_number": "NNX14AC56G"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-12-BS05-0009"
},
{
"agency": "NASA/JPL/Caltech"
}
]
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"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
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},
"title": "NuSTAR observations of the powerful radio-galaxy Cygnus A",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 galaxies: clusters: intracluster medium \u2013 galaxies: jets \u2013 X-rays: individual (Cygnus A)",
"note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 March 18; accepted 2015 June 17; published 2015 July 29. \n\nWe thank the anonymous referee for their thorough and constructive comments that improved the quality of the manuscript. The authors also thank Francesco Tombesi for stimulating conversations throughout the course of this work. C.S.R. thanks NASA for support under grant NNX14AF86G. Our analysis makes use of the XSPEC_EMCEE package developed and distributed by Jeremy Sanders. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities:NuSTAR, XMM-Newton, Chandra\n\nPublished - Reynolds_2015p154.pdf
Submitted - 1506.07175v1.pdf
",
"abstract": "We present NuSTAR observations of the powerful radio galaxy Cygnus A, focusing on the central absorbed active galactic nucleus (AGN). Cygnus A is embedded in a cool-core galaxy cluster, and hence we also examine archival XMM-Newton data to facilitate the decomposition of the spectrum into the AGN and intracluster medium components. NuSTAR gives a source-dominated spectrum of the AGN out to >70 keV. In gross terms, the NuSTAR spectrum of the AGN has the form of a power law (\u0393 ~ 1.6-1.7) absorbed by a neutral column density of N_H ~ 1.6 x 10^(23) cm^(-2). However, we also detect curvature in the hard (>10 keV) spectrum resulting from reflection by Compton-thick matter out of our line of sight to the X-ray source. Compton reflection, possibly from the outer accretion disk or obscuring torus, is required even permitting a high-energy cut off in the continuum source; the limit on the cut-off energy is E_(cut) > 111 keV(90% confidence). Interestingly, the absorbed power law plus reflection model leaves residuals suggesting the absorption/emission from a fast (15,000-26,000 km s^(-1)), high column-density (N_W > 3 x 10^(23) cm^(-2)), highly ionized (\u03b6 \u2013 2500 erg cm s^(-1)) wind. A second, even faster ionized wind component is also suggested by these data. We show that the ionized wind likely carries a significant mass and momentum flux, and may carry sufficient kinetic energy to exercise feedback on the host galaxy. If confirmed, the simultaneous presence of a strong wind and powerful jets in Cygnus A demonstrates that feedback from radio-jets and sub-relativistic winds are not mutually exclusive phases of AGN activity but can occur simultaneously.",
"date": "2015-08-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 154",
"id_number": "CaltechAUTHORS:20150802-074905579",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-074905579",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX14AF86G"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
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"author_list": "Reynolds, Christopher S.; Lohfink, Anne M.; et el."
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},
"title": "The NuSTAR Extragalactic Surveys: Overview and catalog from the COSMOS field",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 February 27; accepted 2015 June 17; published 2015 August 3.\n\nWe thank the anonymous referee for interesting comments and A. Goulding and M. Rose for useful discussions. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge support from the NASA grants 11-ADAP11-0218 and GO3-14150C (FC); from the Science and Technology Facilities Council ST/I001573/1 (ADM, DMA); NSF award AST 1008067 (DRB); NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V.M. Willaman Endowment (WNB, BL); CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), and \"EMBIGGEN\" Anillo ACT1101 (FEB, ET); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and by the FONDECYT regular grant 1120061 (ET); financial support under ASI/INAF contract I/037/12/0 (LZ).\n\nPublished - pdf__1_
Submitted - 1511.04185v1.pdf
",
"abstract": "To provide the census of the sources contributing to the X-ray background peak above 10 keV, Nuclear Spectroscopic Telescope Array (NuSTAR) is performing extragalactic surveys using a three-tier \"wedding cake\"\napproach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity, and medium area tier,\ncovering 1.7 deg^2 and overlapping with both Chandra and XMM-Newton data. This survey consists of 121\nobservations for a total exposure of \u223c3 Ms. To fully exploit these data, we developed a new detection strategy,\ncarefully tested through extensive simulations. The survey sensitivity at 20% completeness is 5.9, 2.9, and 6.4 \u00d7\n10^(\u221214) erg cm^(-2) s^(-1) in the 3\u201324, 3\u20138, and 8\u201324 keV bands, respectively. By combining detections in 3 bands, we\nhave a sample of 91 NuSTAR sources with 1042\u20131045.5 erg s^(-1) luminosities and redshift z = 0.04\u20132.5. Thirty-two\nsources are detected in the 8\u201324 keV band with fluxes \u223c100 times fainter than sources detected by Swift-BAT. Of\nthe 91 detections, all but 4 are associated with a Chandra and/or XMM-Newton point-like counterpart. One source\nis associated with an extended lower energy X-ray source. We present the X-ray (hardness ratio and luminosity)\nand optical-to-X-ray properties. The observed fraction of candidate Compton-thick active galactic nuclei measured\nfrom the hardness ratio is between 13%\u201320%. We discuss the spectral properties of NuSTAR J100259+0220.6\n(ID 330) at z = 0.044, with the highest hardness ratio in the entire sample. The measured column density exceeds\n1024 cm^(\u22122), implying the source is Compton-thick. This source was not previously recognized as such without the\n>10 keV data.",
"date": "2015-08-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 185",
"id_number": "CaltechAUTHORS:20150907-154658360",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150907-154658360",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "11-ADAP11-0218"
},
{
"agency": "NASA",
"grant_number": "GO3-14150C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "NASA",
"grant_number": "AST 1008067"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "V. M. Willaman Endowment"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0 011/13"
}
]
},
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"id": "2015-43",
"name": "Space Radiation Laboratory"
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"doi": "10.1088/0004-637X/808/2/185",
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"author_list": "Civano, F.; Hickox, R. C.; et el."
},
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"datestamp": "2023-08-20 07:23:31",
"lastmod": "2023-10-23 22:47:13",
"type": "article",
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"items": [
{
"id": "Garc\u00eda-Javier-A",
"name": {
"family": "Garc\u00eda",
"given": "Javier A."
},
"orcid": "0000-0003-3828-2448"
},
{
"id": "Dauser-T",
"name": {
"family": "Dauser",
"given": "Thomas"
},
"orcid": "0000-0003-4583-9048"
},
{
"id": "Steiner-J-F",
"name": {
"family": "Steiner",
"given": "James F."
},
"orcid": "0000-0002-5872-6061"
},
{
"id": "McClintock-J-E",
"name": {
"family": "McClintock",
"given": "Jeffrey E."
}
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{
"id": "Keck-M-L",
"name": {
"family": "Keck",
"given": "Mason L."
}
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
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},
"title": "On Estimating the High-Energy Cutoff in the X-Ray Spectra of Black Holes via Reflection Spectroscopy",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 March 1, accepted for publication 2015 July 2, Published 2015 July 27. \n\nJ.G. and J.E.M. acknowledge the support of NASA grant NNX11AD08G. J.F.S. has been supported by NASA Hubble Fellowship HST-HF-51315.01.\n\nPublished - 2041-8205_808_2_L37.pdf
",
"abstract": "The fundamental parameters describing the coronal spectrum of an accreting black hole are the slope \u0393 of the power-law continuum and the energy E_(cut) at which it rolls over. Remarkably, this latter parameter can be accurately measured for values as high as 1 MeV by modeling the spectrum of X-rays reflected from a black hole accretion disk at energies below 100 keV. This is possible because the details in the reflection spectrum, rich in fluorescent lines and other atomic features, are very sensitive to the spectral shape of the hardest coronal radiation illuminating the disk. We show that by fitting simultaneous NuSTAR (3\u201379 keV) and low-energy (e.g., Suzaku) data with the most recent version of our reflection model relxill one can obtain reasonable constraints on E_(cut) at energies from tens of keV up to 1 MeV, for a source as faint as 1 mCrab in a 100 ks observation.",
"date": "2015-07-27",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "L37-L42",
"id_number": "CaltechAUTHORS:20150824-150947187",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150824-150947187",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX11AD08G"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HST-HF-51315.01"
}
]
},
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"pub_year": "2015",
"author_list": "Garc\u00eda, Javier A.; Dauser, Thomas; et el."
},
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"items": [
{
"id": "Degenaar-N",
"name": {
"family": "Degenaar",
"given": "N."
}
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "D."
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
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},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
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"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
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},
"title": "A NuSTAR observation of disc reflection from close to the neutron star in 4U 1608\u201352",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs \u2013 stars: individual: 4U 1608\u201352 \u2013 stars: neutron \u2013\nX-rays: binaries",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2015 May 8. Received 2015 May 8. In original form 2015 April 2. First published online June 10, 2015. \n\n\nWe thank the referee, Craig Heinke, for thoughtful comments. ND acknowledges support via an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2013-IEF-627148. This work is based on data from the NuSTAR mission, a project led by California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank Neil Gehrels and the Swift team for rapid scheduling of observations.\n\nPublished - MNRAS-2015-Degenaar-L85-9.pdf
Submitted - 1505.07112v1.pdf
",
"abstract": "Studying the reflection of X-rays off the inner edge of the accretion disc in a neutron star low-mass X-ray binary allows us to investigate the accretion geometry and to constrain the radius of the neutron star. We report on a NuSTAR observation of 4U 1608\u201352 obtained during a faint outburst in 2014 when the neutron star, which has a known spin frequency of \u03bd = 620 Hz, was accreting at \u22431\u20132\u2009per\u2009cent of the Eddington limit. The 3\u201379 keV continuum emission was dominated by a \u0393 \u2243 2 power law, with an \u22431\u20132\u2009per\u2009cent contribution from a kT_(bb) \u2243 0.3\u20130.6 keV blackbody component. The high-quality NuSTAR spectrum reveals the hallmarks of disc reflection; a broad iron-line peaking near 7 keV and a Compton back-scattering hump around \u224320\u201330 keV. Modelling the disc reflection spectrum points to a binary inclination of i \u224330\u00b0\u201340\u00b0 and a small 'coronal' height of h \u22728.5GM/c^2. Furthermore, our spectral analysis suggests that the inner disc radius extended to R_(in) \u2243 7\u201310GM/c^2, close to the innermost stable circular orbit. This constrains the neutron star radius to R \u227221\u2009km and the redshift from the stellar surface to z \u22730.12, for a mass of M = 1.5\u2009M\u2299 and a spin parameter of a = 0.29.",
"date": "2015-07-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "451",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L85-L89",
"id_number": "CaltechAUTHORS:20150802-162212946",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-162212946",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Marie Curie Fellowship",
"grant_number": "FP-PEOPLE-2013-IEF-627148"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
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"doi": "10.1093/mnrasl/slv072",
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"title": "NuSTAR and Suzaku observations of the hard state in Cygnus X-1: locating the inner accretion disk",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 X-rays: binaries \u2013 X-rays: individual (Cygnus X-1)",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 April 7; accepted 2015 May 28; published 2015 July 14.\n\nM.L.P. acknowledges financial support from the Science and\nTechnology Facilities Council (STFC)\uf0a0and is grateful to Simon\nGibbons for helpful discussions. J.A.T. acknowledges partial\nsupport from NASA ADAP grant NNX13AE98G. W.N.A.,\nE.K., and A.C.F. acknowledge support from the European\nUnion Seventh Framework Programme (FP7/2013\u20132017)\nunder grant agreement no. 312789, StrongGravity. J.W.\nacknowledges support from Deutsches Zentrum f\u00fcr Luft- und\nRaumfahrt grant 50 OR 1411. This work made use of data from\nthe NuSTAR mission, a project led by the California Institute of\nTechnology, managed by the Jet Propulsion Laboratory, and\nfunded by the National Aeronautics and Space Administration.\nThis research has made use of the NuSTAR Data Analysis\nSoftware (NuSTARDAS) jointly developed by the ASI\nScience Data Center (ASDC, Italy) and the California Institute\nof Technology (USA). This research has made use of data\nobtained from the Suzaku satellite, a collaborative mission\nbetween the space agencies of Japan (JAXA) and the\nUSA (NASA).\n\nPublished - Parker_2015p9.pdf
Submitted - 1506.00007v1.pdf
",
"abstract": "We present simultaneous Nuclear Spectroscopic Telescope Array (NuSTAR ) and Suzaku observations of the X-ray binary Cygnus X-1 in the hard state. This is the first time this state has been observed in Cyg X-1 with NuSTAR, which enables us to study the reflection and broadband spectra in unprecedented detail. We confirm that the iron line cannot be fit with a combination of narrow lines and absorption features, instead requiring a relativistically blurred profile in combination with a narrow line and absorption from the companion wind. We use the reflection models of Garc\u00eda et al. to simultaneously measure the black hole spin, disk inner radius, and coronal height in a self-consistent manner. Detailed fits to the iron line profile indicate a high level of relativistic blurring, indicative of reflection from the inner accretion disk. We find a high spin, a small inner disk radius, and a low source height and rule out truncation to greater than three gravitational radii at the 3\u03c3 confidence level. In addition, we find that the line profile has not changed greatly in the switch from soft to hard states, and that the differences are consistent with changes in the underlying reflection spectrum rather than the relativistic blurring. We find that the blurring parameters are consistent when fitting either just the iron line or the entire broadband spectrum, which is well modeled with a Comptonized continuum plus reflection model.",
"date": "2015-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 9",
"id_number": "CaltechAUTHORS:20150802-155802162",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-155802162",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "NASA",
"grant_number": "NNX13AE98G"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Deutsches Zentrum fur Luft- und Raumfahrt (DLR)",
"grant_number": "50 OR 1411"
},
{
"agency": "NASA/JPL/Caltech"
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"name": {
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"family": "Moritani",
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"name": {
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"title": "The Accreting Black Hole Swift J1753.5-0127 from Radio to Hard X-Ray",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 stars: individual (Swift J1753.5\u20130127) \u2013 X-rays:\ngeneral \u2013 X-rays: stars",
"note": "\u00a9 2015 American Astronomical Society. Received 2015 April 29; accepted 2015 June 15; published 2015 July 22.\n\nWe thank the referee for useful comments that helped to improve the manuscript. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The PS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating\ninstitutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the\nNational Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. JAT acknowledges partial support from NASA under Swift Guest\nObserver grants NNX13AJ81G and NNX14AC56G. SC acknowledges the financial support from the UnivEarthS Labex programme of Sorbonne Paris Cit\u00e9 (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), and from the CHAOS project\nANR-12-BS05-0009 supported by the French Research National Agency. JMJ is supported by an Australian Research\nCouncil (ARC) Future Fellowship (FT140101082) and also acknowledges support from an ARC Discovery Grant. EK\nacknowledges support from TUBITAK BIDEB 2219 program. This work was supported by the Spanish Ministerio de Econom\u00e1 y Competitividad (MINECO) under grant AYA2013-47447-C3-1-P (SM).\n\nPublished - 0004-637X_808_1_85.pdf
Submitted - 1506.06780v1.pdf
",
"abstract": "We report on multi-wavelength measurements of the accreting black hole Swift J1753.5\u20130127 in the hard\nstate at low luminosity (L \u223c 2.7\u00d710^(36) erg s^(\u22121) assuming a distance of d = 3 kpc) in 2014 April. The radio emission\nis optically thick synchrotron, presumably from a compact jet. We take advantage of the low extinction (E(B\u2212V) = 0.45 from earlier work) and model the near-IR to UV emission with a multi-temperature disk model. Assuming a black hole mass of MBH = 5M\u2299 and a system inclination of i = 40^\u25e6, the fits imply an inner radius for the disk of R_(in)/R_g > 212 d3 (MBH/5M_\u2299)^\u22121, where R_g is the gravitational radius of the black hole, and d_3 is the distance to the source in units of 3 kpc. The outer radius is R_(out)/R_g = 90,000 d_3 (MBH/5M_\u2299)^(\u22121), which corresponds to 6.6\u00d710^(10) d_3 cm, consistent with the expected size of the disk given previous measurements of the size of the companion's Roche lobe. The 0.5\u2013240 keV energy spectrum measured by Swift/XRT, Suzaku (XIS, PIN, and GSO), and NuSTAR is relatively well characterized by an absorbed power-law with a photon index of \u0393 = 1.722\u00b10.003 (90% confidence error), but a significant improvement is seen when a second continuum component is added. Reflection is a possibility, but no iron line is detected, implying a low iron abundance. We are able to fit the entire (radio to 240 keV) spectral energy distribution (SED) with a multi-temperature disk component, a Comptonization component, and a broken power-law, representing the emission from the compact jet. The broken power-law cannot significantly contribute to the soft X-ray emission, and this may be related to why Swift J1753.5\u20130127 is an outlier in the radio/X-ray correlation. The broken power-law (i.e., the jet) might dominate above 20 keV, which would constrain the break frequency to be between 2.4\u00d710^(10) Hz and 3.6\u00d710^(12) Hz. Although the fits to the full SED do not include significant thermal emission in the X-ray band, previous observations have consistently seen such a component, and we find that there is evidence at the 3.1-\u03c3 level for a disk-blackbody component with a temperature of kTin = 150 +30/\u221220 eV and an inner radius of 5\u201314R_g.\nIf this component is real, it might imply the presence of an inner optically thick accretion disk in addition to the strongly truncated (R_(in) > 212R_g) disk. We also perform X-ray timing analysis, and the power spectrum is dominated by a Lorentzian component with \u03bdmax = 0.110\u00b10.003Hz and \u03bdmax = 0.16\u00b10.04 Hz as measured by XIS and XRT, respectively.",
"date": "2015-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 85",
"id_number": "CaltechAUTHORS:20150802-075928230",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-075928230",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX08AR22G"
},
{
"agency": "NASA",
"grant_number": "NNX13AJ81G"
},
{
"agency": "NASA",
"grant_number": "NNX14AC56G"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-10-LABX-0023"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-11-IDEX-0005-02"
},
{
"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-12-BS05-0009"
},
{
"agency": "Australian Research Council (ARC)",
"grant_number": "FT140101082"
},
{
"agency": "T\u00fcrkiye Bilimsel ve Teknolojik Ara\u015ft\u0131rma Kurumu (T\u00dcB\u0130TAK)",
"grant_number": "BIDEB 2219"
},
{
"agency": "Ministerio de Econom\u00e1 y Competitividad (MINECO)",
"grant_number": "AYA2013-47447-C3-1-P"
},
{
"agency": "NASA/JPL/Caltech"
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"name": {
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"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
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{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
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"name": {
"family": "Madsen",
"given": "K. K."
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"family": "Middleton",
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"title": "A Hard X-Ray Study of the Ultraluminous X-Ray Source NGC 5204 X-1 with NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; X-rays: binaries; X-rays: individual (NGC 5204 X-1)",
"note": "\u00a9 2015 American Astronomical Society. Received 2015 February 5; accepted 2015 June 9; published 2015 July 17.\n\nThe authors thank the referee for useful feedback which\nhelped improve the final manuscript. This research has made\nuse of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analsis of these observations. This research has made use of the NuSTAR Data Analysis Software ( NUSTARDAS), jointly\ndeveloped by the ASI Science Data Center (ASDC, Italy)\nand Caltech (USA).\n\nPublished - 0004-637X_808_1_64.pdf
Submitted - 1502.01764v2.pdf
",
"abstract": "We present the results from coordinated X-ray observations of the ultraluminous X-ray source NGC 5204 X-1 performed by the Nuclear Spectroscopic Telescope Array and XMM-Newton in early 2013. These observations provide the first detection of NGC 5204 X-1 above 10 keV, extending the broadband coverage to 0.3-20 keV. The observations were carried out in two epochs separated by approximately 10 days, and showed little spectral variation with an observed luminosity of L_X =(4.95 \u00b1 0.11) x 10^(39) erg s^(\u22121). The broadband spectrum robustly confirms the presence of a clear spectral downturn above 10 keV seen in some previous observations. This cutoff is inconsistent with the standard low/hard state seen in Galactic black hole binaries, as would be expected from an intermediate-mass black hole accreting at significantly sub-Eddington rates given the observed luminosity. The continuum is apparently dominated by two optically thick thermal-like components, potentially accompanied by a faint high-energy tail. The broadband spectrum is likely associated with an accretion disk that differs from a standard Shakura & Sunyaev thin disk.",
"date": "2015-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 64",
"id_number": "CaltechAUTHORS:20150831-100926591",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150831-100926591",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA"
},
{
"agency": "ESA Member States"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-50",
"name": "Space Radiation Laboratory"
}
]
},
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"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/808/1/64",
"primary_object": {
"basename": "1502.01764v2.pdf",
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}
],
"pub_year": "2015",
"author_list": "Mukherjee, E. S.; Walton, D. J.; et el."
},
{
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"datestamp": "2023-08-20 07:21:14",
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"type": "article",
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"creators": {
"items": [
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "Shriharsh P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "Hasco\u00ebt-R",
"name": {
"family": "Hasco\u00ebt",
"given": "Romain"
}
},
{
"id": "Yang-Chengwei",
"name": {
"family": "Yang",
"given": "Chengwei"
}
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "Victoria M."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Beloborodov-A-M",
"name": {
"family": "Beloborodov",
"given": "Andrei M."
}
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Guillot-S",
"name": {
"family": "Guillot",
"given": "Sebastien"
},
"orcid": "0000-0002-6449-106X"
},
{
"id": "Hailey-C-A",
"name": {
"family": "Hailey",
"given": "Charles A."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Phase-resolved NuSTAR and Swift-XRT Observations of Magnetar 4U 0142+61",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 American Astronomical Society. Received 2015 April 24; accepted 2015 June 8; published 2015 July 16.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V.M.K. acknowledges support from an NSERC Discovery Grant and Accelerator Supplement, the FQRNT Centre de Recherche Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology.\n\nPublished - 0004-637X_808_1_32.pdf
Submitted - 1506.03098v1.pdf
",
"abstract": "We present temporal and spectral analysis of simultaneous 0.5-79 keV Swift-XRT and NuSTAR observations of the magnetar 4U 0142+61. The pulse profile changes significantly with photon energy between 3 and 35 keV. The pulse fraction increases with energy, reaching a value of ~20%, similar to that observed in 1E 1841-045 and much lower than the ~80% pulse fraction observed in 1E 2259+586. We do not detect the 55-ks phase modulation reported in previous Suzaku-HXD observations. The phase-averaged spectrum of 4U 0142+61 above 20 keV is dominated by a hard power law with a photon index, \u0393 ~ 0.65, and the spectrum below 20 keV can be described by two blackbodies, a blackbody plus a soft power law, or by a Comptonized blackbody model. We study the full phase-resolved spectra using the electron-positron outflow model of Beloborodov (2013). Our results are consistent with the parameters of the active j-bundle derived from INTEGRAL data by Hascoet et al. (2014). We find that a significant degeneracy appears in the inferred parameters if the footprint of the j-bundle is allowed to be a thin ring instead of a polar cap. The degeneracy is reduced when the footprint is required to be the hot spot inferred from the soft X-ray data.",
"date": "2015-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 32",
"id_number": "CaltechAUTHORS:20150615-051918365",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150615-051918365",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Fonds Qu\u00e9b\u00e9cois de la Recherche sur la Nature et les Technologies (FQRNT)"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canadian Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-51",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/808/1/32",
"primary_object": {
"basename": "0004-637X_808_1_32.pdf",
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},
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"basename": "1506.03098v1.pdf",
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],
"pub_year": "2015",
"author_list": "Tendulkar, Shriharsh P.; Hasco\u00ebt, Romain; et el."
},
{
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"datestamp": "2023-08-20 07:17:39",
"lastmod": "2023-10-20 23:31:48",
"type": "article",
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"creators": {
"items": [
{
"id": "Tagliaferri-G",
"name": {
"family": "Tagliaferri",
"given": "G."
}
},
{
"id": "Ghisellini-G",
"name": {
"family": "Ghisellini",
"given": "G."
}
},
{
"id": "Perri-M",
"name": {
"family": "Perri",
"given": "M."
}
},
{
"id": "Hayashida-M",
"name": {
"family": "Hayashida",
"given": "M."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
}
},
{
"id": "Covino-S",
"name": {
"family": "Covino",
"given": "S."
}
},
{
"id": "Giommi-P",
"name": {
"family": "Giommi",
"given": "P."
}
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G. M."
}
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Sbarrato-T",
"name": {
"family": "Sbarrato",
"given": "T."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Chiang-J",
"name": {
"family": "Chiang",
"given": "J."
}
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR and multifrequency study of the two high-redshift blazars S5 0836+710 and PKS 2149-306",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 American Astronomical Society. Received 2015 March 4; accepted 2015 May 18; published 2015 July 9.\n\nWe acknowledge financial support from the ASI-INAF grant I/037/12/0. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. We also thank the Swift team for quickly approving and executing the requested ToO observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. Part of this work is based on archival data, software or on-line services provided by the ASI Data Center (ASDC).\n\nPublished - 0004-637X_807_2_167.pdf
Submitted - nustar.pdf
",
"abstract": "Powerful blazars are flat-spectrum radio quasars whose emission is dominated by a Compton component peaking between a few hundred keV and a few hundred MeV. We observed two bright blazars, PKS 2149\u2013306 at redshift z = 2.345 and S5 0836+710 at z = 2.172, in the hard X-ray band with the Nuclear Spectroscopic Telescope Array satellite. Simultaneous soft-X-rays and UV\u2013optical observations were performed with the Swift satellite, while near-infrared (near-IR) data were obtained with the Rapid Eye Mount telescope. To study their variability, we repeated these observations for both sources on a timescale of a few months. While no fast variability was detected during a single observation, both sources were variable in the X-ray band, up to 50%, between the two observations, with larger variability at higher energies. No variability was detected in the optical/NIR band. These data, together with Fermi-Large Area Telescope, Wide-field Infrared Survey Explorer, and other literature data, are then used to study the overall spectral energy distributions (SEDs) of these blazars. Although the jet nonthermal emission dominates the SED, it leaves the UV band unhidden, allowing us to detect the thermal emission of the disk and to estimate the black hole mass. The nonthermal emission is well reproduced by a one-zone leptonic model by the synchrotron, self-Compton, and external Compton processes. Our data are better reproduced if we assume that the location of the dissipation region of the jet, R_(diss), is in between the torus and the broad-line region. The observed variability is explained by changing a minimum number of model parameters by a very small amount.",
"date": "2015-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "807",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 167",
"id_number": "CaltechAUTHORS:20150323-163935434",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150323-163935434",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Department of Energy (DOE)"
},
{
"agency": "Commissariat \u00e0 l'Energie Atomique (CEA)"
},
{
"agency": "Institut National de Physique Nucleaire et de Physique des Particules"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)"
},
{
"agency": "High Energy Accelerator Research Organization (KEK)"
},
{
"agency": "Japan Aerospace Exploration Agency (JAXA)"
},
{
"agency": "K. A. Wallenberg Foundation"
},
{
"agency": "Swedish Research Council"
},
{
"agency": "Swedish National Space Board (SNSB)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-53",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/807/2/167",
"primary_object": {
"basename": "0004-637X_807_2_167.pdf",
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"basename": "nustar.pdf",
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"pub_year": "2015",
"author_list": "Tagliaferri, G.; Ghisellini, G.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/3k6tc-1mp70",
"eprint_id": 59370,
"eprint_status": "archive",
"datestamp": "2023-08-20 07:17:46",
"lastmod": "2023-10-23 20:31:16",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Mukai-K",
"name": {
"family": "Mukai",
"given": "K."
}
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Bernardini-Federico",
"name": {
"family": "Bernardini",
"given": "F."
}
},
{
"id": "de-Martino-D",
"name": {
"family": "de Martino",
"given": "D."
}
}
]
},
"title": "Unambiguous Detection of Reflection in Magnetic Cataclysmic Variables: Joint NuSTAR\u2013XMM-Newton Observations of Three Intermediate Polars",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "novae, cataclysmic variables \u2013 X-rays: binaries",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 20 May 2015, accepted for publication 23 June 2015, Published 10 July 2015. \n\nThis research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA. We acknowledge financial support from NASA under XMM-Newton grant NNX15AK63G and from ASI/INAF contract I/037/12/0.\n\nPublished - 2041-8205_807_2_L30.pdf
Submitted - 1506.07213v1.pdf
",
"abstract": "In magnetic cataclysmic variables (CVs), X-ray emission regions are located close to the white dwarf surface, which is expected to reflect a significant fraction of intrinsic X-rays above 10 keV, producing a Compton reflection hump. However, up to now, a secure detection of this effect in magnetic CVs has largely proved elusive because of the limited sensitivity of non-imaging X-ray detectors. Here we report our analysis of joint NuSTAR\u2013XMM-Newton observations of three magnetic CVs, V709 Cas, NY Lup, and V1223 Sgr. The improved hard X-ray sensitivity of the imaging NuSTAR data has resulted in the first robust detection of Compton hump in all three objects, with amplitudes of ~1 or greater in NY Lup, and likely <1.0 in the other two. We also confirm earlier reports of a strong spin modulation above 10 keV in V709 Cas, and we report the first detection of small spin amplitudes in the others. We interpret this as due to different height of the X-ray emitting region among these objects. A height of ~0.2 white dwarf radii provides a plausible explanation for the low reflection amplitude of V709 Cas. Since emission regions above both poles are visible at certain spin phases, this can also explain the strong hard X-ray spin modulation. A shock height of ~0.05 white dwarf radii can explain our results on V1223 Sgr, while the shock height in NY Lup appears negligible.",
"date": "2015-07-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "807",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L30",
"id_number": "CaltechAUTHORS:20150810-154140351",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150810-154140351",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX15AK63G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/2041-8205/807/2/L30",
"primary_object": {
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}
],
"pub_year": "2015",
"author_list": "Mukai, K.; Rana, V.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/v9cww-jz136",
"eprint_id": 59144,
"eprint_status": "archive",
"datestamp": "2023-08-20 07:17:18",
"lastmod": "2023-10-23 20:06:46",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "Michael J."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Romero-Ca\u00f1izales-C",
"name": {
"family": "Romero-Ca\u00f1izales",
"given": "C."
}
},
{
"id": "Baronchelli-L",
"name": {
"family": "Baronchelli",
"given": "L."
}
},
{
"id": "Teng-Stacy-H",
"name": {
"family": "Teng",
"given": "S. H."
}
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Ar\u00e9valo-P",
"name": {
"family": "Ar\u00e9valo",
"given": "P."
}
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"name": {
"family": "Stern",
"given": "D."
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"name": {
"family": "Treister",
"given": "E."
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},
"title": "Broadband Observations of the Compton-thick Nucleus of NGC 3393",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 January 29, accepted for publication 2015 May 5\nPublished 2015 July 9. \n\nWe thank Jim Condon, Fred Lo, and Antxon Alberdi for their useful discussion of radio data and astrometry. We thank Harvey Tananbaum and Diab Jerius for useful discussions on the Chandra PSF and using the MARX software. We thank Pepi Fabbiano and Alessandro Paggi for useful discussions of previous NGC 3393 papers. M. K. acknowledges support from the Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant PZ00P2 154799/1. M.K. and K. S. acknowledge support from Swiss National Science Foundation (NSF) grant PP00P2 138979/1. M.K. also acknowledges support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number AR3-14010X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. C.R.C. acknowledges financial support from the ALMA-CONICYT FUND Project 31100004. We also acknowledge support from CONICYT through FONDECYT grant 3150238 (C.R.C.) and from project IC120009 \"Millennium Institute of Astrophysics (MAS) funded by the Iniciativa Cient\u00edfica Milenio del Ministerio Econom\u00eda, Fomento y Turismo de Chile (C.R.C, F.E.B.). A.C. acknowledges support from the ASI/INAF grant I/037/12/0 011/13 and the Caltech Kingsley visitor program. ST acknowledges support from the NASA postdoctoral fellowship program. Support for the work of ET was provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101. M. B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. R.J.A. was supported by GeminiCONICYT grant number 32120009. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science DataCenter (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. \n\nThe scientific results reported in this article are based on data obtained from the Chandra Data Archive. This research made use of the XRT Data Analysis Software (XRTDAS), archival data, software and on-line services provided by the ASDC. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. The Cornell Atlas of Spitzer IRS Sources (CASSIS) is a product of the Infrared Science Center at Cornell University, supported by NASA and JPL. We used observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). \n\nThis research made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu). This paper is based on observations made with the Very Large Array (VLA) and the Very Long Baseline Array (VLBA) of the National Radio Astronomy Observatory (NRAO); the NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. \n\nFacilities: NuSTAR, Swift, CXO, HST (NICMOS, UVIS, WFC3), Keck:II (NIRC2), Spitzer, VLBA, VLA, UH:2.2m, PS1, XMM, Suzaku, BeppoSAX\n\nPublished - 0004-637X_807_2_149.pdf
Submitted - 1505.03524v1.pdf
",
"abstract": "We present new Nuclear Spectroscopic Telescope Array (NuSTAR ) and Chandra observations of NGC 3393, a galaxy reported to host the smallest separation dual active galactic nuclei (AGN) resolved in the X-rays. While past results suggested a 150 pc separation dual AGN, three times deeper Chandra imaging, combined with adaptive optics and radio imaging suggest a single, heavily obscured, radio-bright AGN. Using Very Large Array and Very Long Baseline Array data, we find an AGN with a two-sided jet rather than a dual AGN and that the hard X-ray, UV, optical, near-infrared, and radio emission are all from a single point source with a radius <\"0.2. We find that the previously reported dual AGN is most likely a spurious detection resulting from the low number of X-ray counts (<160) at 6\u20137 keV and Gaussian smoothing of the data on scales much smaller than the point-spread function (PSF) (0\".25 versus 0\u2033.80 FWHM). We show that statistical noise in a single Chandra PSF generates spurious dual peaks of the same separation (0.\" 55 \u00b10 .\"07 versus 0.\"6) and flux ratio (39% \u00b1 9% versus 32% counts) as the\npurported dual AGN. With NuSTAR, we measure a Compton-thick source (NH 2.2 0.4 10 \u00b1 24 cm^(-2)) with a large torus half-opening angle, 0_(tor) 79 +1/_19\u00b0 which we postulate results from feedback from strong radio jets. This AGN shows a 2\u201310 keV intrinsic-to-observed flux ratio of \u00bb150 (L_(-10 keV int) 2.6 \u00b1 0.3 10^(erg) s^(-1)- versus L_(2-10 keV int) observed 1.7 \u00b1 0.2 X 10^(41) erg s^(-1). Using simulations, we find that even the deepest Chandra observations would severely underestimate the intrinsic luminosity of NGC 3393 above z > 0.2, but would detect an unobscured AGN of this luminosity out to high redshift (z \u00bb 5).",
"date": "2015-07-09",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "807",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 149",
"id_number": "CaltechAUTHORS:20150802-194947106",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-194947106",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PZ00P2 154799/1"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2 138979/1"
},
{
"agency": "NASA",
"grant_number": "AR3-14010X"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "31100004"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "3150238"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0 011/13"
},
{
"agency": "Center of Excellence in Astrophysics and Associated Technologies",
"grant_number": "PFB 06"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "NASA",
"grant_number": "NNX14AQ07H"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "32120009"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
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"pub_year": "2015",
"author_list": "Koss, Michael J.; Romero-Ca\u00f1izales, C.; et el."
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"name": {
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"orcid": "0000-0002-4017-8837"
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"orcid": "0000-0001-9345-0307"
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},
"title": "Deep NuSTAR and Swift Monitoring Observations of the Magnetar 1E 1841-045",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 January 28, accepted for publication 2015 May 13\nPublished 2015 July 2. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). H.A. acknowledges supports provided by the NASA sponsored Fermi Contract NAS5-00147 and by Kavli Institute for Particle Astrophysics and Cosmology. V.M.K. acknowledges support from an NSERC Discovery Grant and Accelerator Supplement, the FQRNT Centre de Recherche Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. acknowledges the support by NASA grant NNX13AI34G.\n\nPublished - 0004-637X_807_1_93.pdf
Submitted - 1505.03570v2.pdf
",
"abstract": "We report on a 350 ks NuSTAR observation of the magnetar 1E 1841\u2013045 taken in 2013 September. During the observation, NuSTAR detected six bursts of short duration, with T90 \u2264 1 s. An elevated level of emission tail is detected after the brightest burst, persisting for \u223c1 ks. The emission showed a power-law decay with a temporal index of 0.5 before returning to the persistent emission level. The long observation also provided detailed phaseresolved spectra of the persistent X-ray emission of the source. By comparing the persistent spectrum with that previously reported, we find that the source hard-band emission has been stable for over approximately 10 yr. The persistent hard-X-ray emission is well fitted by a coronal outflow model, where e^\u00b1 pairs in the magnetosphere\nupscatter thermal X-rays. Our fit of phase-resolved spectra allowed us to estimate the angle between the rotational and magnetic dipole axes of the magnetar, amag = 0.25, the twisted magnetic flux, 2.5 \u00d7 10^(26) G cm^2, and the power released in the twisted magnetosphere, L_j = 6 \u00d7 10^(36) erg s^(\u22121). Assuming this model for the hard-X-ray\nspectrum, the soft-X-ray component is well fit by a two-blackbody model, with the hotter blackbody consistent with the footprint of the twisted magnetic field lines on the star. We also report on the 3 yr Swift monitoring observations obtained since 2011 July. The soft-X-ray spectrum remained stable during this period, and the timing\nbehavior was noisy, with large timing residuals.",
"date": "2015-07-02",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "807",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 93",
"id_number": "CaltechAUTHORS:20150802-163958438",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150802-163958438",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NAS5-00147"
},
{
"agency": "Kavli Institute for Particle Astrophysics and Cosmology"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Fonds Qu\u00e9b\u00e9cois de la Recherche sur la Nature et les Technologies (FQRNT)"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canadian Research Chairs Program"
},
{
"agency": "NASA",
"grant_number": "NNX13AI34G"
}
]
},
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"items": [
{
"id": "2015-06",
"name": "Space Radiation Laboratory"
}
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{
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"doi": "10.1088/0004-637X/807/1/93",
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"pub_year": "2015",
"author_list": "An, Hongjun; Archibald, Robert F.; et el."
},
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"items": [
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Lohfink-A",
"name": {
"family": "Lohfink",
"given": "A."
}
},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
},
"orcid": "0000-0003-0172-0854"
},
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"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
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"id": "Vasudevan-R",
"name": {
"family": "Vasudevan",
"given": "R."
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},
"title": "Properties of AGN coronae in the NuSTAR era",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 May 27. Received 2015 May 26. In original form 2015 April 27. First published online July 1, 2015. \n\nWe thank Julien Malzac for a discussion and the referee for helpful comments. ACF and AL acknowledge support from ERC Advanced Grant FEEDBACK. CSR thanks the Simons Foundation Fellows\nProgram (US) and the Sackler Fellowship Program (Cambridge) for support, and is grateful to the Institute of Astronomy (Cambridge) for its hospitality during a six month visit in which this work was conducted.\n\nPublished - MNRAS-2015-Fabian-4375-83.pdf
",
"abstract": "The focusing optics of NuSTAR have enabled high signal-to-noise ratio spectra to be obtained from many X-ray bright active galactic nuclei (AGN) and galactic black hole binaries (BHB). Spectral modelling then allows robust characterization of the spectral index and upper energy cutoff of the coronal power-law continuum, after accounting for reflection and absorption effects. Spectral-timing studies, such as reverberation and broad iron line fitting, of these sources yield coronal sizes, often showing them to be small and in the range of 3 to 10 gravitational radii in size. Our results indicate that coronae are hot and radiatively compact, lying close to the boundary of the region in the compactness\u2013temperature (\u0398 \u2212 \u2113) diagram which is forbidden due to runaway pair production. The coincidence suggests that pair production and annihilation are essential ingredients in the coronae of AGN and BHB and that they control the shape of the observed spectra.",
"date": "2015-07-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "451",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "4375-4383",
"id_number": "CaltechAUTHORS:20160128-135737582",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-135737582",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "FEEDBACK"
},
{
"agency": "Simons Foundation"
},
{
"agency": "Sackler Fellowship Program (Cambridge)"
}
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"title": "Rapid Variability of Blazar 3C 279 During Flaring States in 2013-2014 with Joint Fermi-LAT, NuSTAR, Swift, and Ground-Based Multi-Wavelength Observations",
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"note": "\u00a9 2015 IOP Publishing. \n\nReceived 2015 February 14; Accepted 2015 March 31; Published 2015 July 2. \n\nThe Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States; the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France; the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan; and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France. \n\nThis work was partially supported under the NASA contract no. NNG08FD60C, and made use of observations from the NuSTAR mission, a project led by California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support of the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. \n\nK.N. was supported by NASA through Einstein Postdoctoral Fellowship grant number PF3\u2013140130 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8\u201303060. M.B. acknowledges support from NASA Headquarters under the NASA earth and Space Science Fellowship Program, grant NNX14AQ07H. \n\nFacilities: Fermi (LAT) - Fermi Gamma-Ray Space Telescope (formerly GLAST), NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - Swift Gamma-Ray Burst Mission, CTIO: 0.9m - , CTIO: 1.0m - , CTIO: 1.3m - , CTIO: 1.5m - , SMA - SubMillimeter Array\n\nPublished - pdf
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"abstract": "We report the results of a multiband observing campaign on the famous blazar 3C 279 conducted during a phase of increased activity from 2013 December to 2014 April, including first observations of it with NuSTAR. The gamma-ray emission of the source measured by Fermi-LAT showed multiple distinct flares reaching the highest flux level measured in this object since the beginning of the Fermi mission, with F(E > 100 MeV) of 10^(-5) photons cm^(-2) s^(-1), and with a flux-doubling time scale as short as 2 hr. The gamma-ray spectrum during one of the flares was very hard, with an index of Gamma(gamma) = 1.7 +/- 0.1, which is rarely seen in flat-spectrum radio quasars. The lack of concurrent optical variability implies a very high Compton dominance parameter L-gamma/L-syn > 300. Two 1 day NuSTAR observations with accompanying Swift pointings were separated by 2 weeks, probing different levels of source activity. While the 0.5 - 70 keV X-ray spectrum obtained during the first pointing, and fitted jointly with Swift-XRT is well-described by a simple power law, the second joint observation showed an unusual spectral structure: the spectrum softens by Delta Gamma(X) similar or equal to 0.4 at similar to 4 keV. Modeling the broadband spectral energy distribution during this flare with the standard synchrotron plus inverse-Compton model requires: (1) the location of the gamma-ray emitting region is comparable with the broad-line region radius, (2) a very hard electron energy distribution index p similar or equal to 1, (3) total jet power significantly exceeding the accretion-disk luminosity L-j/L-d greater than or similar to 10, and (4) extremely low jet magnetization with L-B/L-j less than or similar to 10^(-4). We also find that single-zone models that match the observed gamma-ray and optical spectra cannot satisfactorily explain the production of X-ray emission.",
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"title": "The NuSTAR Extragalactic Surveys: Initial Results and Catalog from the Extended Chandra Deep Field South",
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"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 March 2; accepted 2015 June 19; published 2015 August 3. \n\nWe thank the anonymous referee for their careful reading of the manuscript and comments that improved the clarity of the text. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). A.D.M. and D.M.A. gratefully acknowledge financial support from the Science and Technology Facilities Council (ST/I001573/1). J.A. acknowledges support from a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University, and ERC Advanced Grant FEEDBACK at the University of Cambridge. F.M.C. acknowledges support from NASA grants 11-ADAP11-0218 and GO3-14150C. D.R.B. is supported in part by NSF award AST 1008067. W.N.B. and B.L. thank NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment. We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB) and 1120061 (ET), and \"EMBIGGEN\" Anillo ACT1101 (FEB, ET); and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). Support for the work of E.T. was also provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). A.C., S.P., and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 011/13. A.C. acknowledges the Caltech Kingsley visitor program. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.\n\nPublished - document.pdf
Submitted - 1511.04186v1.pdf
",
"abstract": "We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)\u2014currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full \u224830' \u00d7 30' area of this field to a maximum depth of \u2248360 ks (\u2248 220 ks when corrected for vignetting at 3\u201324 keV), reaching sensitivity limits of \u2248 1.3 X 10^(-14) erg s^(-1) cm^(-2) (3\u20138 keV), \u2248 3.4 X 10^ s^(-1)}, cm^(-2) (8\u201324 keV), and ~3 X 10^(-14) erg, s^(-1) cm^(-2) (3\u201324 keV). A total of 54 sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8\u201324 keV band. The 8\u201324 to 3\u20138 keV band ratios of the 12 sources that are detected in both bands span the range 0.39\u20131.7, corresponding to a photon index range of \u0393 \u2248 0.5-2.3, with a median photon index of \u0393[bar]} = 1.70 \u00b1 0.52. The redshifts of the 49 sources in our main sample span the range z = 0.21-2.7, and their rest-frame 10\u201340 keV luminosities (derived from the observed 8\u201324 keV fluxes) span the range L_(10-40 keV) \u2248 (0.7-300) X 10^(43) erg s^(-1), sampling below the \"knee\" of the X-ray luminosity function out to sim 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS.",
"date": "2015-07-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "808",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 184",
"id_number": "CaltechAUTHORS:20150907-151739240",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150907-151739240",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "NASA/JPL/Caltech"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Durham University"
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{
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"title": "Thermal Emissions Spanning the Prompt and the Afterglow Phases of the Ultra-long GRB 130925A",
"ispublished": "pub",
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"keywords": "gamma-ray burst: general; gamma-ray burst: individual (130925A); methods: data analysis; methods: observational; radiation mechanisms: thermal",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2014 September 17; accepted 2015 May 10; published 2015 June 26. \n\nThis research has made use of data obtained through the HEASARC Online Service, provided by the NASA/GSFC, in support of NASA High Energy Astrophysics Programs. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank the referee for valuable comments that made the presentation more rigorous.",
"abstract": "GRB 130925A is an ultra-long gamma-ray burst (GRB), and it shows clear evidence for thermal emission in the soft X-ray data of the Swift/X-ray Telescope (XRT; ~0.5 keV), lasting until the X-ray afterglow phase. Due to the long duration of the GRB, the burst could be studied in hard X-rays with high-resolution focusing detectors (NuSTAR). The blackbody temperature, as measured by the Swift/XRT, shows a decreasing trend until the late phase (Piro et al.) whereas the high-energy data reveal a significant blackbody component during the late epochs at an order of magnitude higher temperature (~5 keV) compared to contemporaneous low energy data (Bellm et al.). We resolve this apparent contradiction by demonstrating that a model with two black bodies and a power law (2BBPL) is consistent with the data right from the late prompt emission to the afterglow phase. Both blackbodies show a similar cooling behavior up to late times. We invoke a structured jet, having a fast spine and a slower sheath layer, to identify the location of these blackbodies. Independent of the physical interpretation, we propose that the 2BBPL model is a generic feature of the prompt emission of all long GRBs, and the thermal emission found in the afterglow phase of different GRBs reflects the lingering thermal component of the prompt emission with different timescales. We strengthen this proposal by pointing out a close similarity between the spectral evolutions of this GRB and GRB 090618, a source with significant wide band data during the early afterglow phase.",
"date": "2015-06-26",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "807",
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"doi": "10.1088/0004-637X/807/1/34",
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"title": "NuSTAR and Suzaku X-Ray Spectroscopy of NGC 4151: Evidence for Reflection from the Inner Accretion Disk",
"ispublished": "pub",
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"keywords": "accretion, accretion disks; black hole physics; galaxies: active; galaxies: individual (NGC 4151); galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 September 30; accepted 2015 April 27; published 2015 June 15. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). M.L.K. gratefully acknowledges support through NASA grant #NNX13AE90G. G.M. and A.M. acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0\u2013011/13 and from the European Union Seventh Framework Programme (FP7/2007\u20132013) under grant agreement n.312789. C.S.R. acknowledges support from the NASA-ADAP program under grants NNX14AF86G and NNX14AF89G. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, Anillo ACT1101) and ICM grant\nIC120009, awarded to The Millennium Institute of Astrophysics, MAS. We thank Alan Marscher for helpful discussions. We thank the anonymous referee for comments, which have improved this manuscript. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Matplotlib (Hunter 2007). \n\nFacilities:NuSTAR (FPMA, FPMB), Suzaku (XIS, HXD)\n\nPublished - 0004-637X_806_2_149.pdf
Submitted - 1504.07950v1.pdf
",
"abstract": "We present X-ray timing and spectral analyses of simultaneous 150 ks Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku X-ray observations of the Seyfert 1.5 galaxy NGC 4151. We disentangle the continuum emission, absorption, and reflection properties of the active galactic nucleus (AGN) by applying inner accretion disk reflection and absorption-dominated models. With a time-averaged spectral analysis, we find strong evidence for relativistic reflection from the inner accretion disk. We find that relativistic emission arises from a highly ionized inner accretion disk with a steep emissivity profile, which suggests an intense, compact illuminating source. We find a preliminary, near-maximal black hole spin_(\u0251 > 0.9) accounting for statistical and systematic modeling errors. We find a relatively moderate reflection fraction with respect to predictions for the lamp post geometry, in which the illuminating corona is modeled as a point source. Through a time-resolved spectral analysis, we find that modest coronal and inner disk reflection (IDR) flux variation drives the spectral variability during the observations. We discuss various physical scenarios for the IDR model and we find that a compact corona is consistent with the observed features.",
"date": "2015-06-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "806",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 149",
"id_number": "CaltechAUTHORS:20150803-105900589",
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"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"grant_number": "NNG08FD60C"
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{
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"grant_number": "NNX13AE90G"
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{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0\u2013011/13"
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{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
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{
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"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
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"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
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{
"agency": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio (ICM) del Ministerio de Econom\u00eda",
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{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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"id": "Tomsick-J-A",
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"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
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},
"title": "Broadband X-Ray Properties of the Gamma-Ray Binary 1FGL J1018.6\u20135856",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: close; gamma rays: stars; stars: individual (1FGL J1018.6\u20135856); X-rays: binaries",
"note": "\u00a9 2015 American Astronomical Society. Received 2015 March 9; accepted 2015 May 7; published 2015 June 17.\n\nWe thank R. W. Romani for useful discussions. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. H.A. acknowledges supports provided by the NASA sponsored Fermi Contract NAS5-00147 and by Kavli Institute for Particle Astrophysics and Cosmology (KIPAC). LN wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13.\n\nPublished - 0004-637X_806_2_166.pdf
Submitted - 1505.02096v2.pdf
",
"abstract": "We report on NuSTAR, XMM-Newton, and Swift observations of the gamma-ray binary 1FGL J1018.6\u20135856. We measure the orbital period to be 16.544 \u00b1 0.008 days using Swift data spanning 1900 days. The orbital period is different from the 2011 gamma-ray measurement which was used in the previous X-ray study of An et al. using ~400 days of Swift data, but is consistent with a new gamma-ray solution reported in 2014. The light curve folded on the new period is qualitatively similar to that reported previously, having a spike at phase 0 and broad sinusoidal modulation. The X-ray flux enhancement at phase 0 occurs more regularly in time than was previously suggested. A spiky structure at this phase seems to be a persistent feature, although there is some variability. Furthermore, we find that the source flux clearly correlates with the spectral hardness throughout all orbital phases, and that the broadband X-ray spectra measured with NuSTAR, XMM-Newton, and Swift are well fit with an unbroken power-law model. This spectrum suggests that the system may not be accretion-powered.",
"date": "2015-06-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "806",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 166",
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"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150803-144537922",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
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"agency": "NASA/Caltech/JPL"
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"grant_number": "NAS5-00147"
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{
"agency": "Kavli Institute for Particle Astrophysics and Cosmology"
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"agency": "Agenzia Spaziale Italiana (ASI)",
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},
"title": "Distorted cyclotron line profile in Cep X-4 as observed by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 April 22; accepted 2015 May 9; published 2015 June 15.\n\nWe thank the anonymous referee for valuable comments. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 2041-8205_806_2_L24.pdf
Submitted - 1505.02788v1.pdf
",
"abstract": "We present spectral analysis of Nuclear Spectroscopic Telescope Array and Swift observations of Cep X-4 during its outburst in 2014. We observed the source once during the peak of the outburst and once during the decay, finding good agreement in the spectral shape between the observations. We describe the continuum using a power law with a Fermi\u2013Dirac cutoff at high energies. Cep X-4 has a very strong cyclotron resonant scattering feature (CRSF) around 30 keV. A simple absorption-like line with a Gaussian optical depth or a pseudo-Lorentzian profile both fail to describe the shape of the CRSF accurately, leaving significant deviations at the red side of the line. We characterize this asymmetry with a second absorption feature around 19 keV. The line energy of the CRSF, which is not influenced by the addition of this feature, shows a small but significant positive luminosity dependence. With luminosities between (1\u20136) \u00d7 10^(36) erg s^(\u22121), Cep X-4 is below the theoretical limit where such a correlation is expected. This behavior is similar to Vela X-1 and we discuss parallels between the two systems.",
"date": "2015-06-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "806",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L24",
"id_number": "CaltechAUTHORS:20150615-060247495",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150615-060247495",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-06",
"name": "Space Radiation Laboratory"
}
]
},
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"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
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},
"doi": "10.1088/2041-8205/806/2/L24",
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"pub_year": "2015",
"author_list": "F\u00fcrst, F.; Pottschmidt, K.; et el."
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{
"id": "Lehmer-B-D",
"name": {
"family": "Lehmer",
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{
"id": "Tyler-J-B",
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},
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},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "D. R."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Yukita-Mihoko",
"name": {
"family": "Yukita",
"given": "M."
},
"orcid": "0000-0001-6366-3459"
},
{
"id": "Antoniou-V",
"name": {
"family": "Antoniou",
"given": "V."
},
"orcid": "0000-0001-7539-1593"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
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},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T. J."
},
"orcid": "0000-0003-0976-4755"
},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
},
"orcid": "0000-0001-5655-1440"
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
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{
"id": "Zezas-A",
"name": {
"family": "Zezas",
"given": "A."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
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"orcid": "0000-0002-1426-9698"
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},
"title": "The 0.3-30 keV Spectra of Powerful Starburst Galaxies: NuSTAR and Chandra Observations of NGC 3256 and NGC 3310",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 3256 and NGC 3310); galaxies: starburst; galaxies: star formation; X-rays: galaxies",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 December 22; accepted 2015 May 3; published 2015 June 12.\n\nWe thank the anonymous referee for helpful comments, which have improved the quality of this paper. We gratefully acknowledge financial support from Chandra X-ray Center grant GO4-15086 Z (B.D.L., J.B.T.) and NASA ADAP grant NNX13AI48G (B.D.L.). A.Z. acknowledges funding from the European Research Council under the European Union\u02bcs Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 617001. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (Italy) and the California Institute of Technology (USA).\nFacilities: Chandra, NuSTAR\n\nPublished - 0004-637X_806_1_126.pdf
Submitted - 1505.00789v1.pdf
",
"abstract": "We present nearly simultaneous Chandra and NuSTAR observations of two actively star-forming galaxies within 50 Mpc: NGC 3256 and NGC 3310. Both galaxies are significantly detected by both Chandra and NuSTAR, which together provide the first-ever spectra of these two galaxies spanning 0.3\u201330 keV. The X-ray emission from both galaxies is spatially resolved by Chandra; we find that hot gas dominates the E < 1\u20133 keV emission while ultraluminous X-ray sources (ULXs) provide majority contributions to the emission at E > 1\u20133 keV. The NuSTAR galaxy-wide spectra of both galaxies follow steep power-law distributions with \u0393 \u2248 2.6 at E > 5\u20137 keV. Using new and archival Chandra data, we search for signatures of heavily obscured or low luminosity active galactic nuclei (AGNs). We find that both NGC 3256 and NGC 3310 have X-ray detected sources coincident with nuclear regions; however, the steep NuSTAR spectra of both galaxies restricts these sources to be either low luminosity AGNs (L_(2\u221210 keV)/L_(Edd) 10^(\u22125)) or non-AGNs in nature (e.g., ULXs or crowded X-ray sources that reach L_(2\u221210 keV) ~ 10^(40) erg s^(\u22121) cannot be ruled out). Combining our constraints on the 0.3\u201330 keV spectra of NGC 3256 and NGC 3310 with equivalent measurements for nearby star-forming galaxies M83 and NGC 253, we analyze the star formation rate (SFR) normalized spectra of these starburst galaxies. The spectra of all four galaxies show sharply declining power-law slopes at energies above 3\u20136 keV primarily due to ULX populations. Our observations therefore constrain the average spectral shape of galaxy-wide populations of luminous accreting binaries (i.e., ULXs). Interestingly, despite a completely different galaxy sample selection, emphasizing here a range of SFRs and stellar masses, these properties are similar to those of super-Eddington accreting ULXs that have been studied individually in a targeted NuSTAR ULX program. We also find that NGC 3310 exhibits a factor of \u22483\u201310 elevation of X-ray emission over the other star-forming galaxies due to a corresponding overabundance of ULXs. We argue that the excess of ULXs in NGC 3310 is most likely explained by the relatively low metallicity of the young stellar population in this galaxy, a property that is expected to produce an excess of luminous X-ray binaries for a given SFR.",
"date": "2015-06-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "806",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 126",
"id_number": "CaltechAUTHORS:20150722-123446121",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150722-123446121",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Chandra X-ray Center",
"grant_number": "GO4-15086 Z"
},
{
"agency": "NASA",
"grant_number": "NNX13AI48G"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "617001"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
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"items": [
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"id": "2015-57",
"name": "Space Radiation Laboratory"
}
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"doi": "10.1088/0004-637X/806/1/126",
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"author_list": "Lehmer, B. D.; Tyler, J. B.; et el."
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"id": "Walton-D-J",
"name": {
"family": "Walton",
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{
"id": "Middleton-M-J",
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"given": "M. J."
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},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
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},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
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"name": {
"family": "Boggs",
"given": "S. E."
},
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},
{
"id": "Christensen-F-E",
"name": {
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"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
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"name": {
"family": "Craig",
"given": "W. W."
}
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"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
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},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W."
},
"orcid": "0000-0002-1426-9698"
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]
},
"title": "NuSTAR, XMM-Newton, and Suzaku Observations of the Ultraluminous X-Ray Source Holmberg II X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; X-rays: binaries; X-rays: individual (Holmberg II X-1)",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 March 30; accepted 2015 April 24; published 2015 June 9. \n\nThe authors would like to thank the referee for the positive feedback, which helped improve the clarity of the final manuscript. M.B. and D.B. acknowledge financial support from the French Space Agency (CNES). This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States, and with Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). \n\nFacilites: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, XMM - Newton X-Ray Multimirror Mission satellite, Suzaku - Suzaku (ASTRO-EII).\n\nPublished - pdf__1_.pdf
",
"abstract": "We present the first broadband 0.3\u201325.0 keV X-ray observations of the bright ultraluminous X-ray source (ULX)\nHolmberg II X^(-1), performed by NuSTAR, XMM-Newton, and Suzaku in 2013 September. The NuSTAR data\nprovide the first observations of Holmberg II X^(-1) above 10 keV and reveal a very steep high-energy spectrum,\nsimilar to other ULXs observed by NuSTAR to date. These observations further demonstrate that ULXs exhibit\nspectral states that are not typically seen in Galactic black hole binaries. Comparison with other sources implies\nthat Holmberg II X^(-1) accretes at a high fraction of its Eddington accretion rate and possibly exceeds it. The soft Xray\nspectrum (E < 10 keV) appears to be dominated by two blackbody-like emission components, the hotter of\nwhich may be associated with an accretion disk. However, all simple disk models under-predict the NuSTAR data\nabove \u223c10 keV and require an additional emission component at the highest energies probed, implying the\nNuSTAR data does not fall away with a Wien spectrum. We investigate physical origins for such an additional\nhigh-energy emission component and favor a scenario in which the excess arises from Compton scattering in a hot\ncorona of electrons with some properties similar to the very high state seen in Galactic binaries. The observed\nbroadband 0.3\u201325.0 keV luminosity inferred from these epochs is L_X (8.1 0.1) 1039 =\u00b1\u00d7 erg s^(\u22121), typical for\nHolmberg II X^(-1), with the majority of this flux (\u223c90%) emitted below 10 keV.",
"date": "2015-06-09",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "806",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art No. 65",
"id_number": "CaltechAUTHORS:20160128-201524771",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-201524771",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "Japan Aerospace Exploration Agency (JAXA)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-58",
"name": "Space Radiation Laboratory"
}
]
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"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
}
]
},
"doi": "10.1088/0004-637X/806/1/65",
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"pub_year": "2015",
"author_list": "Walton, D. J.; Middleton, M. J.; et el."
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},
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"id": "Balokovi\u0107-M",
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"given": "M."
},
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"family": "Stern",
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},
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"id": "Ar\u00e9valo-P",
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"family": "Ar\u00e9valo",
"given": "P."
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"given": "F. E."
},
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"family": "Comastri",
"given": "A."
},
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"family": "LaMassa",
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"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
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"name": {
"family": "Rivers",
"given": "E."
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"family": "Vasudevan",
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"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
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},
"title": "Determining the Covering Factor of Compton-thick Active Galactic Nuclei with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 424, NGC 1068, NGC 4945, Circinus); X-rays: galaxies",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 November 7; accepted 2015 February 24; published 2015 May 19.\n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The work presented here was also based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has also made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. Furthermore, this research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. M. Balokovi\u0107 acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. D.R.B. acknowledges support from NSF award AST 1008067; P.G. acknowledges support from STFC (grant reference ST/J003697/1), M.K. acknowledges support from the Swiss National Science Foundation (SNSF) through the Ambizione fellowship grant PZ00P2 154799/1. We also acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), \"EMBIGGEN\" Anillo ACT1101 (FEB), Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" of the Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo (FEB).\n\nFacilities: NuSTAR, XMM (EPIC)\n\nPublished - 0004-637X_805_1_41.pdf
Submitted - 1502.07353v1.pdf
",
"abstract": "The covering factor of Compton-thick (CT) obscuring material associated with the torus in active galactic nuclei (AGNs) is at present best understood through the fraction of sources exhibiting CT absorption along the line of sight (N_H > 1.5 \u00d7 10^(24) cm^(\u22122)) in the X-ray band, which reveals the average covering factor. Determining this CT fraction is difficult, however, due to the extreme obscuration. With its spectral coverage at hard X-rays (>10 keV), Nuclear Spectroscopic Telescope Array (NuSTAR) is sensitive to the AGNs covering factor since Compton scattering of X-rays off optically thick material dominates at these energies. We present a spectral analysis of 10 AGNs observed with NuSTAR where the obscuring medium is optically thick to Compton scattering, so-called CT AGNs. We use the torus models of Brightman & Nandra that predict the X-ray spectrum from reprocessing in a torus and include the torus opening angle as a free parameter and aim to determine the covering factor of the CT gas in these sources individually. Across the sample we find mild to heavy CT columns, with N_H measured from 10^(24) to 10^(26) cm^(\u22122), and a wide range of covering factors, where individual measurements range from 0.2 to 0.9. We find that the covering factor, f_c, is a strongly decreasing function of the intrinsic 2\u201310 keV luminosity, L_X, where f_c = (\u22120.41 \u00b1 0.13)log_(10)(L_X/erg s^(\u22121))+18.31 \u00b1 5.33, across more than two orders of magnitude in L_X (10^(41.5)\u201310^(44) erg s^(\u22121)). The covering factors measured here agree well with the obscured fraction as a function of L_X as determined by studies of local AGNs with L_X > 10^(42.5) erg s^(\u22121).",
"date": "2015-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "805",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 41",
"id_number": "CaltechAUTHORS:20150619-091157800",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150619-091157800",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA Earth and Space Science Fellowship",
"grant_number": "NNX14AQ07H"
},
{
"agency": "NSF",
"grant_number": "AST1008067"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PZ00P2 154799/1"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Basal-CATA PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-62",
"name": "Space Radiation Laboratory"
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]
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"doi": "10.1088/0004-637X/805/1/41",
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],
"pub_year": "2015",
"author_list": "Brightman, M.; Balokovi\u0107, M.; et el."
},
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"items": [
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "E."
}
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{
"id": "Risaliti-G",
"name": {
"family": "Risaliti",
"given": "G."
}
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{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Ar\u00e9valo-P",
"name": {
"family": "Ar\u00e9valo",
"given": "P."
}
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Brenneman-L-W",
"name": {
"family": "Brenneman",
"given": "L. W."
}
},
{
"id": "Brightman-M",
"name": {
"family": "Brightman",
"given": "M."
},
"orcid": "0000-0002-8147-2602"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Hickox-R-C",
"name": {
"family": "Hickox",
"given": "R. C."
},
"orcid": "0000-0003-1468-9526"
},
{
"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "A."
}
},
{
"id": "Reeves-J",
"name": {
"family": "Reeves",
"given": "J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Multi-layer Variable Absorbers in NGC 1365 Revealed by XMM-Newton and NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 1365); X-rays: galaxies",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 November 7; accepted 2015 March 6; published 2015 May 7.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work has also made use of HEASARC online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic Database, operated by JPL/California Institute of Technology under contract with NASA. This work also made use of data from the XMM-Newton observatory.\nFacilities: NuSTAR, XMM\n\nPublished - 0004-637X_804_2_107.pdf
Submitted - 1503.03109v1.pdf
",
"abstract": "Between 2012 July and 2013 February, NuSTAR and XMM-Newton performed four long-look joint observations of the type 1.8 Seyfert, NGC 1365. We have analyzed the variable absorption seen in these observations in order to characterize the geometry of the absorbing material. Two of the observations caught NGC 1365 in an unusually low absorption state, revealing complexity in the multi-layer absorber that had previously been hidden. We find the need for three distinct zones of neutral absorption in addition to the two zones of ionized absorption and the Compton-thick torus previously seen in this source. The most prominent absorber is likely associated with broad-line region clouds with column densities of around ~10^(23) cm^(\u22122) and a highly clumpy nature as evidenced by an occultation event in 2013 February. We also find evidence of a patchy absorber with a variable column around ~10^(22) cm^(\u22122) and a line-of-sight covering fraction of 0.3\u20130.9, which responds directly to the intrinsic source flux, possibly due to a wind geometry. A full-covering, constant absorber with a low column density of ~1 \u00d7 10^(22) cm^(\u22122) is also present, though the location of this low density haze is unknown.",
"date": "2015-05-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "804",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 107",
"id_number": "CaltechAUTHORS:20150619-084553247",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150619-084553247",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-63",
"name": "Space Radiation Laboratory"
}
]
},
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"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/804/2/107",
"primary_object": {
"basename": "0004-637X_804_2_107.pdf",
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},
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],
"pub_year": "2015",
"author_list": "Rivers, E.; Risaliti, G.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/6mm5v-vd778",
"eprint_id": 57542,
"eprint_status": "archive",
"datestamp": "2023-08-20 06:13:38",
"lastmod": "2023-10-23 17:31:15",
"type": "article",
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"creators": {
"items": [
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "H."
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mao-Peter-H",
"name": {
"family": "Mao",
"given": "P. H."
}
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
}
]
},
"title": "^(44)Ti gamma-ray emission lines from SN1987A reveal an asymmetric explosion",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 American Association for the Advancement of Science.\n\nReceived 3 November 2014; accepted 8 April 2015.\n\nThis work was supported under NASA Contract no. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). D.B. acknowledges funding from the French Space Agency (CNES). T.K. was supported by Japan Society for the Promotion of Science Grant-in-Aid for Young Scientists (B) (no. 24740185). N.J.W. acknowledges funding from the Technical University of Denmark. NuSTAR data are accessible from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC, http://heasarc.gsfc.nasa.gov/).\n\nSupplemental Material - Boggs.SM.pdf
",
"abstract": "In core-collapse supernovae, titanium-44 (^(44)Ti) is produced in the innermost ejecta, in the layer of material directly on top of the newly formed compact object. As such, it provides a direct probe of the supernova engine. Observations of supernova 1987A (SN1987A) have resolved the 67.87- and 78.32\u2013kilo\u2013electron volt emission lines from decay of ^(44)Ti produced in the supernova explosion. These lines are narrow and redshifted with a Doppler velocity of ~700 kilometers per second, direct evidence of large-scale asymmetry in the explosion.",
"date": "2015-05-08",
"date_type": "published",
"publication": "Science",
"volume": "348",
"number": "6235",
"publisher": "American Association for the Advancement of Science",
"pagerange": "670-671",
"id_number": "CaltechAUTHORS:20150514-152641080",
"issn": "0036-8075",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150514-152641080",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "24740185"
},
{
"agency": "Technical University of Denmark"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-60",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1126/science.aaa2259",
"primary_object": {
"basename": "Boggs.SM.pdf",
"url": "https://authors.library.caltech.edu/records/6mm5v-vd778/files/Boggs.SM.pdf"
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"pub_year": "2015",
"author_list": "Boggs, S. E.; Harrison, F. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/zrynx-bpa69",
"eprint_id": 64051,
"eprint_status": "archive",
"datestamp": "2023-08-20 06:11:17",
"lastmod": "2023-10-17 18:36:22",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Paliya-V-S",
"name": {
"family": "Paliya",
"given": "Vaidehi S."
},
"orcid": "0000-0001-7774-5308"
}
]
},
"title": "The High Redshift Blazar S5 0836+71: A Broadband Study",
"ispublished": "pub",
"full_text_status": "restricted",
"note": "\u00a9 Copyright 2015 IOP Publishing. \n\nReceived 2015 January 19; accepted 2015 February 25; published 2015 May 4. \n\nThe author thanks the referee for constructive comments and C.S. Stalin and Sunder Sahayanathan for useful discussions. Substantial help in NuSTAR data analysis received from Michael Parker is also acknowledged. This research has made use of data, software, and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). Use of the Hydra cluster at the Indian Institute of Astrophysics is acknowledged.",
"abstract": "A broadband study of the high redshift blazar S5 0836+71 (z = 2.172) is presented. Multi-frequency light curves show multiple episodes of X-ray and \u03b3-ray flares, while optical-UV fluxes show little variations. During the GeV outburst, the highest \u03b3-ray flux measured is (5.22 \u00b1 1.10) \u00d7 10\u22126 ph cm^(\u22122) s^\u22121 in the range of 0.1-300 GeV, which corresponds to an isotropic \u03b3-ray luminosity of (1.62 \u00b1 0.44) \u00d7 1050 erg s^\u22121, thereby making this as one of the most luminous \u03b3-ray flare ever observed from any blazar. A fast \u03b3-ray flux rising time of \u223c3 hours is also noticed which is probably the first measurement of hour scale variability detected from a high redshift (z > 2) blazar. The various activity states of S5 0836+71 are reproduced under the assumption of single zone leptonic emission model. In all the states, the emission region is located inside the broad line region, and the optical-UV radiation is dominated by the accretion disk emission. The modeling parameters suggests the enhancement in bulk Lorentz factor as a primary cause of the \u03b3-ray flare. The high X-ray activity with less variable \u03b3-ray counterpart can be due to emission region to be located relatively closer to the black hole where the dominating energy density of the disk emission results in higher X-ray flux due to inverse-Compton scattering of disk photons.",
"date": "2015-05-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "804",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art No. 74",
"id_number": "CaltechAUTHORS:20160128-132317989",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-132317989",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/804/1/74",
"pub_year": "2015",
"author_list": "Paliya, Vaidehi S."
},
{
"id": "https://authors.library.caltech.edu/records/956hy-mes83",
"eprint_id": 56360,
"eprint_status": "archive",
"datestamp": "2023-08-20 06:10:02",
"lastmod": "2023-10-23 15:20:50",
"type": "article",
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"creators": {
"items": [
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
},
"orcid": "0000-0003-0172-0854"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Lohfink-A-M",
"name": {
"family": "Lohfink",
"given": "A. M."
}
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Matt-G",
"name": {
"family": "Matt",
"given": "G."
},
"orcid": "0000-0002-2152-0916"
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Compton hump and variable blue wing in the extreme low-flux NuSTAR observations of 1H0707\u2212495",
"ispublished": "pub",
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"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2015 February 11. Received 2015 February 10. In original form 2014 November 12. First published online March 17, 2015.\n\nEK thanks Javier Garcia and Thomas Dauser for interesting discussions on the RELXILLLP modelling. EK is supported by the Gates Cambridge Scholarship. ACF thanks the Royal Society. EK, ACF, AML, and GM acknowledge support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789, StrongGravity. AML and GM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. This work was supported under National Aeronautics and Space Administration (NASA) contract no. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.\n\nPublished - MNRAS-2015-Kara-234-42.pdf
Submitted - 1501.06849v2.pdf
",
"abstract": "The narrow-line Seyfert I galaxy, 1H0707\u2212495, has been well observed in the 0.3\u201310 keV band, revealing a dramatic drop in flux in the iron K\u03b1 band, a strong soft excess, and short time-scale reverberation lags associated with these spectral features. In this paper, we present the first results of a deep 250-ks NuSTAR (Nuclear Spectroscopic Telescope Array) observation of 1H0707\u2212495, which includes the first sensitive observations above 10 keV. Even though the NuSTAR observations caught the source in an extreme low-flux state, the Compton hump is still significantly detected. NuSTAR, with its high effective area above 7 keV, clearly detects the drop in flux in the iron K\u03b1 band, and by comparing these observations with archival XMM\u2013Newton observations, we find that the energy of this drop increases with increasing flux. We discuss possible explanations for this, the most likely of which is that the drop in flux is the blue wing of the relativistically broadened iron K\u03b1 emission line. When the flux is low, the coronal source height is low, thus enhancing the most gravitationally redshifted emission.",
"date": "2015-05-01",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "449",
"number": "1",
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"pagerange": "232-242",
"id_number": "CaltechAUTHORS:20150405-152254064",
"issn": "0035-8711",
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"agency": "Gates Cambridge Scholarship"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
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{
"agency": "Agenzia Spaziale Italiana (ASI)",
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{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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"author_list": "Kara, E.; Fabian, A. C.; et el."
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"title": "Anatomy of the AGN in NGC 5548. III. The high-energy view with NuSTAR and INTEGRAL",
"ispublished": "pub",
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"keywords": "galaxies: active \u2013 galaxies: Seyfert \u2013 X-rays: galaxies",
"note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 25 November 2014; Accepted 12 January 2015; Published online 28 April 2015. \n\nWe are grateful to the anonymous referee for his/her helpful comments, which have improved the manuscript. This work is based on observations obtained with: the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by NASA; INTEGRAL, an ESA project with instrument and science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic, and Poland and with the participation of Russia and the USA; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). The data used in this research are stored in the public archives of the international space observatories involved. This research has made use of data, software and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. F.U., P.O.P., G.M., and S.B. acknowledge support from the French-Italian International Project of Scientific Collaboration: PICS-INAF project number 181542. F.U., P.O.P. acknowledge support from CNES. F.U. acknowledges support from Universit\u00e9 Franco-Italienne (Vinci Ph.D. fellowship). F.U., G.M. acknowledges financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. G.A.K. was supported by NASA through grants for HST program number 13184 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. B.M.P. acknowledges support from the US NSF through grant AST-1008882. G.P. acknowledges support via an E.U. Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2012-IEF- 331095. K.C.S. acknowledges financial support from the Fondo Fortalecimiento de la Productividad Cient\u00edfica VRIDT 2013. We acknowledge support by ISSI in Bern; The Netherlands Organization for Scientific Research; the UK STFC; the French CNES, CNRS/PICS and CNRS/PNHE; the Swiss SNSF; the Italian INAF/PICS; the German Bundesministerium f\u00fcr Wirtschaft und Technologie/Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408); we acknowledge support from the Italian Space Agency under grants ASI-INAF I/037/12/P1 and ASI/INAF NuSTAR I/037/12/0.\n\nPublished - aa25401-14.pdf
Submitted - 1501.03426v1.pdf
",
"abstract": "We describe the analysis of the seven broad-band X-ray continuum observations of the archetypal Seyfert 1 galaxy NGC 5548 that were obtained with XMM-Newton or Chandra, simultaneously with high-energy (>10 keV) observations with NuSTAR and INTEGRAL. These data were obtained as part of a multiwavelength campaign undertaken from the summer of 2013 till early 2014. We find evidence of a high-energy cut-off in at least one observation, which we attribute to thermal Comptonization, and a constant reflected component that is likely due to neutral material at least a few light months away from the continuum source. We confirm the presence of strong, partial covering X-ray absorption as the explanation for the sharp decrease in flux through the soft X-ray band. The obscurers appear to be variable in column density and covering fraction on time scales as short as weeks. A fit of the average spectrum over the range 0.3\u2013400 keV with a realistic Comptonization model indicates the presence of a hot corona with a temperature of 40^(+40)_(-10) keV and an optical depth of 2.7^(+0.7)_(-1.2) if a spherical geometry is assumed.",
"date": "2015-05",
"date_type": "published",
"publication": "Astronomy and Astrophysics",
"volume": "577",
"publisher": "EDP Sciences",
"pagerange": "Art. No. A38",
"id_number": "CaltechAUTHORS:20150126-090538888",
"issn": "0004-6361",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150126-090538888",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
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},
{
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},
{
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},
{
"agency": "Science and Technology Facilities Council (STFC)"
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{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
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{
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},
{
"agency": "Bundesministerium f\u00fcr Wirtschaft und Technologie (BMWi)"
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"title": "Extended hard-X-ray emission in the inner few parsecs of the Galaxy",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 Macmillan Publishers Limited.\n\nReceived 15 December 2014 Accepted 24 February 2015, Published 30 April 2015.\n\nThis work was supported by NASA contract no. NNG08FD60C,\nand made use of data from the NuSTAR mission, a project led by the California Institute\nof Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We\nthank the NuSTAR Operations, Software and Calibration teams for support with the\nexecution and analysis of these observations. This research has made use of the\nNuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science\nData Center (ASDC, Italy) and the California Institute of Technology (USA). We also\nthank A. Canipe, J. Dodaro, D. Hong and T. V. T. Luu for assistance with data preparation\nand analysis. F.E.B. acknowledges support from Basal-CATA PFB-06/2007,\nCONICYT-Chile (FONDECYT 1141218 and EMBIGGEN Anillo ACT1101), and Project\nIC120009 ''Millennium Institute of Astrophysics (MAS)'' funded by the Iniciativa\nCient\u0131\u00b4fica Milenio del Ministerio de Econom\u0131\u00b4a, Fomento y Turismo.\n\nSupplemental Material - nature14353-pf1.ppt
Supplemental Material - nature14353-pf2.ppt
Supplemental Material - nature14353-pf3.ppt
Supplemental Material - nature14353-sf1.jpg
Supplemental Material - nature14353-sf2.jpg
Supplemental Material - nature14353-sf3.jpg
Supplemental Material - nature14353-sf4.jpg
Supplemental Material - nature14353-sf5.jpg
Supplemental Material - nature14353-sf6.jpg
Supplemental Material - nature14353-st1.jpg
Supplemental Material - nature14353-st2.jpg
Supplemental Material - nature14353-st3.jpg
",
"abstract": "The Galactic Centre hosts a puzzling stellar population in its inner\nfew parsecs, with a high abundance of surprisingly young, relatively\nmassive stars bound within the deep potential well of the\ncentral supermassive black hole, Sagittarius A*. Previous\nstudies suggest that the population of objects emitting soft X-rays\n(less than 10 kiloelectronvolts) within the surrounding hundreds\nof parsecs, as well as the population responsible for unresolved\nX-ray emission extending along the Galactic plane, is dominated\nby accreting white dwarf systems. Observations of diffuse hard X-ray\n(more than 10 kiloelectronvolts) emission in the inner 10\nparsecs, however, have been hampered by the limited spatial resolution\nof previous instruments. Here we report the presence of a\ndistinct hard-X-ray component within the central 4 X 8 parsecs, as\nrevealed by subarcminute-resolution images in the 20\u201340 kiloelectronvolt\nrange. This emission is more sharply peaked towards the\nGalactic Centre than is the surface brightness of the soft-X-ray\npopulation. This could indicate a significantly more massive\npopulation of accreting white dwarfs, large populations of lowmass\nX-ray binaries or millisecond pulsars, or particle outflows\ninteracting with the surrounding radiation field, dense molecular\nmaterial or magnetic fields. However, all these interpretations pose\nsignificant challenges to our understanding of stellar evolution,\nbinary formation, and cosmic-ray production in the Galactic\nCentre.",
"date": "2015-04-30",
"date_type": "published",
"publication": "Nature",
"volume": "520",
"number": "7549",
"publisher": "Nature Publishing Group",
"pagerange": "646-649",
"id_number": "CaltechAUTHORS:20150209-221241720",
"issn": "0028-0836",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150209-221241720",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "EMBIGGEN Anillo ACT1101"
},
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"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
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"doi": "10.1038/nature14353",
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"id": "Paliya-V-S",
"name": {
"family": "Paliya",
"given": "Vaidehi S."
},
"orcid": "0000-0001-7774-5308"
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Stalin-C-S",
"name": {
"family": "Stalin",
"given": "C. S."
},
"orcid": "0000-0002-4998-1861"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Ramya-S",
"name": {
"family": "Ramya",
"given": "S."
}
},
{
"id": "Covino-S",
"name": {
"family": "Covino",
"given": "S."
}
},
{
"id": "Tagliaferri-G",
"name": {
"family": "Tagliaferri",
"given": "G."
}
},
{
"id": "Sahayanathan-S",
"name": {
"family": "Sahayanathan",
"given": "S."
}
},
{
"id": "Ravikumar-C-D",
"name": {
"family": "Ravikumar",
"given": "C. D."
}
}
]
},
"title": "Awakening of the High-Redshift Blazar CGRaBS J0809+5341",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2014 October 14, accepted for publication 2015 February 19 Published 2015 April 22. \n\nWe thank the referee for a constructive report that improved the manuscript significantly. We are thankful to the Swift PI for accepting the ToO request and the Swift operation duty scientist for quickly scheduling the observations. We also thank the NuSTAR PI for approving the request of observation. V.S.P. is grateful to the MASTER-Tunka team for providing optical images of the source. This research has made use of the data obtained from HEASARC provided by NASA's Goddard Space Flight Center. Part of this work is based on archival data, software, or online services provided by the ASI Science Data\nCenter (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. This research has also made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly\ndeveloped by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). \n\nFunding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Use of the Hydra cluster at the Indian Institute of Astrophysics is acknowledged. S.R. acknowledges the support of National Natural Science Foundation of China grant No. 11450110401.\n\nPublished - 0004-637X_803_2_112.pdf
",
"abstract": "CGRaBS J0809+5341, a high-redshift blazar at z = 2.144, underwent a giant optical outburst on 2014 April 19 when it brightened by ~5 mag and reached an unfiltered apparent magnitude of 15.7 mag. This implies an absolute magnitude of \u221230.5 mag, making it one of the brightest quasars in the universe. This optical flaring triggered us to carry out observations during the decaying part of the flare covering a wide energy range using the Nuclear Spectroscopic Telescope Array, Swift, and ground-based optical facilities. For the first time, the source is detected in \u03b3-rays by the Large Area Telescope on board the Fermi Gamma-Ray Space Telescope. A high optical polarization of ~10% is also observed. Using the Sloan Digital Sky Survey spectrum, the accretion disk luminosity and black hole mass are estimated as 1.5 \u00d7 10^(45) erg s^(\u22121) and 10^(8.4) M_\u2299, respectively. Using a single zone leptonic emission model, we reproduce the spectral energy distribution of the source during the flaring activity. This analysis suggests that the emission region is probably located outside the broad-line region, and the jet becomes radiatively efficient. We also show that the overall properties of CGRaBS J0809+5341 seem to not be in agreement with the general properties observed in high-redshift blazars up to now.",
"date": "2015-04-22",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "803",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 112",
"id_number": "CaltechAUTHORS:20150824-194557019",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150824-194557019",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Alfred P. Sloan Foundation"
},
{
"agency": "NSF"
},
{
"agency": "Department of Energy (DOE)"
},
{
"agency": "National Natural Science Foundation China",
"grant_number": "11450110401"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/803/2/112",
"primary_object": {
"basename": "0004-637X_803_2_112.pdf",
"url": "https://authors.library.caltech.edu/records/hvb5c-dzt46/files/0004-637X_803_2_112.pdf"
},
"pub_year": "2015",
"author_list": "Paliya, Vaidehi S.; Parker, M. L.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/0dj99-st166",
"eprint_id": 59864,
"eprint_status": "archive",
"datestamp": "2023-08-20 05:45:41",
"lastmod": "2023-10-23 22:47:19",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "D'Angelo-C-R",
"name": {
"family": "D'Angelo",
"given": "C. R."
}
},
{
"id": "Fridriksson-J-K",
"name": {
"family": "Fridriksson",
"given": "J. K."
}
},
{
"id": "Messenger-C",
"name": {
"family": "Messenger",
"given": "C."
}
},
{
"id": "Patruno-A",
"name": {
"family": "Patruno",
"given": "A."
}
}
]
},
"title": "The radiative efficiency of a radiatively inefficient accretion flow",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 February 27. Received 2015 February 26. In original form 2014 October 14. First published online April 4, 2015. \n\nCRD'A and AP are financially supported by an NWO Vidi grant (PI: Patruno). We are grateful to Daniel Wik for sharing his nuskybgd background analysis tools for NuSTAR. AP acknowledges very useful conversations with Anne Archibald. CRD'A acknowledges very useful conversations with Deepto Chakrabarty, Marat Gilfanov, Craig Heinke, Andrew King, John Raymond, and Rudy Wijnands.\n\nPublished - MNRAS-2015-D'Angelo-2803-17.pdf
Published - MNRAS-2015-D=0027Angelo-2803-17.pdf
",
"abstract": "A recent joint XMM\u2013Newton/Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the accreting neutron star Cen X-4 (LX \u223c 10^(33)\u2009erg\u2009s^(\u22121)) revealed a hard power-law component (\u0393 \u223c 1\u20131.5) with a relatively low cut-off energy (\u223c10 keV), suggesting bremsstrahlung emission. The physical requirements for bremsstrahlung combined with other observed properties of Cen X-4 suggest the emission comes from a boundary layer rather than the accretion flow. The accretion flow itself is thus undetected (with an upper limit of L_(flow) \u2272 0.3LX). A deep search for coherent pulsations (which would indicate a strong magnetic field) places a 6\u2009per\u2009cent upper limit on the fractional amplitude of pulsations, suggesting the flow is not magnetically regulated. Considering the expected energy balance between the accretion flow and the boundary layer for different values of the neutron star parameters (size, magnetic field, and spin) we use the upper limit on L_(flow) to set an upper limit of \u03b5 \u2272 0.3 for the intrinsic radiative efficiency of the accretion flow for the most likely model of a fast-spinning, non-magnetic neutron star. The non-detection of the accretion flow provides the first direct evidence that this flow is indeed 'radiatively inefficient', i.e. most of the gravitational potential energy lost by the flow before it hits the star is not emitted as radiation.",
"date": "2015-04-04",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "449",
"number": "3",
"publisher": "Oxford University Press",
"pagerange": "2803-2817",
"id_number": "CaltechAUTHORS:20150824-152453139",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150824-152453139",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stv465",
"primary_object": {
"basename": "MNRAS-2015-D=0027Angelo-2803-17.pdf",
"url": "https://authors.library.caltech.edu/records/0dj99-st166/files/MNRAS-2015-D=0027Angelo-2803-17.pdf"
},
"pub_year": "2015",
"author_list": "D'Angelo, C. R.; Fridriksson, J. K.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/8bj5p-f2h37",
"eprint_id": 57975,
"eprint_status": "archive",
"datestamp": "2023-08-20 05:30:42",
"lastmod": "2023-10-23 17:57:41",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Orio-M",
"name": {
"family": "Orio",
"given": "M."
}
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Page-K-L",
"name": {
"family": "Page",
"given": "K. L."
},
"orcid": "0000-0001-5624-2613"
},
{
"id": "Sokoloski-J-L",
"name": {
"family": "Sokoloski",
"given": "J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F."
},
"orcid": "0000-0003-2992-8024"
}
]
},
"title": "A NuSTAR observation of the fast symbiotic nova V745 Sco in outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: close \u2013white dwarfs \u2013X-rays: stars",
"note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 December 3. Received 2014 November 26; in original form 2014 October 17. First published online January 9, 2015. \n\nWe wish to acknowledge the support of the following awards and funding agencies: MO of ASI (Italian Space Agency) through an INAF-ASI grant, JLS of the NSF award AST-1211778, and KLP of the UK Space Agency funding the UK Swift Science Data Centre.\n\nPublished - MNRAS-2015-Orio-L35-9.pdf
",
"abstract": "The fast recurrent nova V745 Sco was observed in the 3\u201379 keV X-rays band with NuSTAR 10 d after the optical discovery. The measured X-ray emission is consistent with a collisionally ionized optically thin plasma at temperature of about 2.7 keV. A prominent iron line observed at 6.7 keV does not require enhanced iron in the ejecta. We attribute the X-ray flux to shocked circumstellar material. No X-ray emission was observed at energies above 20 keV, and the flux in the 3\u201320 keV range was about 1.6 \u00d7 10^(\u221211) erg cm^(\u22122) s^(\u22121). The emission measure indicates an average electron density of the order of 10^7 cm^(\u22122). The X-ray flux in the 0.3\u201310 keV band almost simultaneously measured with Swift was about 40 times larger, mainly due to the luminous central supersoft source emitting at energy below 1 keV. The fact that the NuSTAR spectrum cannot be fitted with a power law, and the lack of hard X-ray emission, allow us to rule out Comptonized gamma-rays, and to place an upper limit of the order of 10^(\u221211) erg cm^(\u22122) s^(\u22121) on the gamma-ray flux of the nova on the tenth day of the outburst.",
"date": "2015-03-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "448",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "L35-L39",
"id_number": "CaltechAUTHORS:20150603-103349166",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150603-103349166",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)"
},
{
"agency": "NSF",
"grant_number": "AST-1211778"
},
{
"agency": "United Kingdom Space Agency (UKSA)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-68",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1093/mnrasl/slu195",
"primary_object": {
"basename": "MNRAS-2015-Orio-L35-9.pdf",
"url": "https://authors.library.caltech.edu/records/8bj5p-f2h37/files/MNRAS-2015-Orio-L35-9.pdf"
},
"pub_year": "2015",
"author_list": "Orio, M.; Rana, V.; et el."
},
{
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"eprint_id": 56965,
"eprint_status": "archive",
"datestamp": "2023-08-22 15:12:04",
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"items": [
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Reynolds-S-P",
"name": {
"family": "Reynolds",
"given": "Stephen P."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Humensky-T-B",
"name": {
"family": "Humensky",
"given": "T. Brian"
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Fryer-C-L",
"name": {
"family": "Fryer",
"given": "Chris L."
},
"orcid": "0000-0003-2624-0056"
},
{
"id": "Delaney-T",
"name": {
"family": "Delaney",
"given": "Tracey"
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "Daniel R."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Zoglauer-A-C",
"name": {
"family": "Zoglauer",
"given": "Andreas"
}
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "Karl"
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "Takao"
}
},
{
"id": "Lopez-L-A",
"name": {
"family": "Lopez",
"given": "Laura"
},
"orcid": "0000-0002-1790-3148"
},
{
"id": "Nynka-M",
"name": {
"family": "Nynka",
"given": "Melania"
},
"orcid": "0000-0002-3310-1946"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Locating the Most Energetic Electrons in Cassiopeia A",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "acceleration of particles; ISM: individual objects (Cassiopeia A); ISM: supernova remnants; radiation mechanisms: non-thermal; X-rays: ISM",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 September 16; accepted 2015 January 14; published 2015 March 16. \n\nB.G. thanks Una Hwang for the Chandra 4\u20136 keV band image. This work was supported under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacilities: Chandra, Fermi, HESS, NuSTAR, VERITAS, VLA\n\nPublished - 0004-637X_802_1_15.pdf
Submitted - 1502.03024v1.pdf
",
"abstract": "We present deep (>2.4 Ms) observations of the Cassiopeia A supernova remnant with NuSTAR, which operates in the 3\u201379 keV bandpass and is the first instrument capable of spatially resolving the remnant above 15 keV. We find that the emission is not entirely dominated by the forward shock nor by a smooth \"bright ring\" at the reverse shock. Instead we find that the >15 keV emission is dominated by knots near the center of the remnant and dimmer filaments near the remnant's outer rim. These regions are fit with unbroken power laws in the 15\u201350 keV bandpass, though the central knots have a steeper (\u0393 ~ \u22123.35) spectrum than the outer filaments (\u0393 ~ \u22123.06). We argue this difference implies that the central knots are located in the 3-D interior of the remnant rather than at the outer rim of the remnant and seen in the center due to projection effects. The morphology of >15 keV emission does not follow that of the radio emission nor that of the low energy (<12 keV) X-rays, leaving the origin of the >15 keV emission an open mystery. Even at the forward shock front we find less steepening of the spectrum than expected from an exponentially cut off electron distribution with a single cutoff energy. Finally, we find that the GeV emission is not associated with the bright features in the NuSTAR band while the TeV emission may be, suggesting that both hadronic and leptonic emission mechanisms may be at work.",
"date": "2015-03-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "802",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 15",
"id_number": "CaltechAUTHORS:20150424-140813411",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150424-140813411",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/802/1/15",
"primary_object": {
"basename": "0004-637X_802_1_15.pdf",
"url": "https://authors.library.caltech.edu/records/sn14w-hgk17/files/0004-637X_802_1_15.pdf"
},
"related_objects": [
{
"basename": "1502.03024v1.pdf",
"url": "https://authors.library.caltech.edu/records/sn14w-hgk17/files/1502.03024v1.pdf"
}
],
"pub_year": "2015",
"author_list": "Grefenstette, Brian W.; Reynolds, Stephen P.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/5134r-tpe84",
"eprint_id": 64053,
"eprint_status": "archive",
"datestamp": "2023-08-20 05:27:43",
"lastmod": "2023-10-17 18:36:27",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Wilkins-D-R",
"name": {
"family": "Wilkins",
"given": "D. R."
}
},
{
"id": "Gallo-L-C",
"name": {
"family": "Gallo",
"given": "L. C."
}
}
]
},
"title": "Driving extreme variability: the evolving corona and evidence for jet launching in Markarian 335",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2015 January 21.\nReceived 2015 January 21.\nIn original form 2014 September 23.\nFirst published online March 17, 2015.\n\nDRW is supported by a CITA National Fellowship. This work is\nbased on observations obtained with XMM\u2013Newton, an ESA science\nmission with instruments and contributions directly funded by ESA\nMember States and NASA and has also made use of data obtained\nfrom the Suzaku satellite, a collaborative mission between the space\nagencies of Japan (JAXA) and the USA (NASA). This work also\nuses observations made by the NuSTAR mission, a project led by the\nCalifornia Institute of Astronomy, managed by the Jet Propulsion\nLaboratory, and funded by NASA. We thank the anonymous referees\nfor their constructive feedback on the original manuscript.\n\nPublished - MNRAS-2015-Wilkins-129-46.pdf
",
"abstract": "Variations in the X-ray emission from the narrow-line Seyfert 1 galaxy, Markarian 335, are studied on both long and short time-scales through observations made between 2006 and 2013 with XMM\u2013Newton, Suzaku and NuSTAR. Changes in the geometry and energetics of the corona that give rise to this variability are inferred through measurements of the relativistically blurred reflection seen from the accretion disc. On long time-scales, we find that during the high-flux epochs the corona has expanded, covering the inner regions of the accretion disc out to a radius of 26 +10/\u2212726\u22127+10 rg. The corona contracts to within 12r_g and 5r_g in the intermediate- and low-flux epochs, respectively. While the earlier high-flux observation made in 2006 is consistent with a corona extending over the inner part of the accretion disc, a later high-flux observation that year revealed that the X-ray source had become collimated into a vertically extended jet-like corona and suggested relativistic motion of material upwards. On short time-scales, we find that an X-ray flare during a low-flux epoch in 2013 corresponded to a reconfiguration from a slightly extended corona to one much more compact, within just 2 \u223c 3r_g of the black hole. There is evidence that during the flare itself, the spectrum softened and the corona became collimated and slightly extended vertically as if a jet-launching event was aborted. Understanding the evolution of the X-ray emitting corona may reveal the underlying mechanism by which the luminous X-ray sources in AGN are powered.",
"date": "2015-03-17",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "449",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "129-146",
"id_number": "CaltechAUTHORS:20160128-132426857",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-132426857",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Canadian Institute for Theoretical Astrophysics"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "NASA"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stv162",
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"title": "Broadband x-ray imaging and spectroscopy of the Crab nebula and pulsar with NuSTAR",
"ispublished": "pub",
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"note": "\u00a9 2015. The American Astronomical Society.\n\nReceived 26 June 2014, accepted for publication 23 December 2014. Published 4 March 2015. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_801_1_66.pdf
",
"abstract": "We present broadband (3-78 keV) NuSTAR X-ray imaging and spectroscopy of the Crab nebula and pulsar. We show that while the phase-averaged and spatially integrated nebula + pulsar spectrum is a power law in this energy band, spatially resolved spectroscopy of the nebula finds a break at ~9 keV in the spectral photon index of the torus structure with a steepening characterized by \u0394\u0393 ~ 0.25. We also confirm a previously reported steepening in the pulsed spectrum, and quantify it with a broken power law with break energy at ~12 keV and \u0394\u0393 ~ 0.27. We present spectral maps of the inner 100'' of the remnant and measure the size of the nebula as a function of energy in seven bands. These results find that the rate of shrinkage with energy of the torus size can be fitted by a power law with an index of \u03b3 = 0.094 \u00b1 0.018, consistent with the predictions of Kennel and Coroniti. The change in size is more rapid in the NW direction, coinciding with the counter-jet where we find the index to be a factor of two larger. NuSTAR observed the Crab during the latter part of a \u03b3-ray flare, but found no increase in flux in the 3-78 keV energy band.",
"date": "2015-03-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "801",
"number": "1",
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"pagerange": "Art. No. 66",
"id_number": "CaltechAUTHORS:20150404-114619633",
"issn": "0004-637X",
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"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
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"agency": "NASA",
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},
{
"agency": "NASA/JPL/Caltech"
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"pub_year": "2015",
"author_list": "Madsen, Kristin K.; Reynolds, Stephen; et el."
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},
"title": "NuSTAR detection of a cyclotron line in the supergiant fast X-ray transient IGR J17544\u22122619",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: individual (IGR J17544-2619) \u2013 X-rays: binaries",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 November 22. Received 2014 September 12. In original form 2014 June 30. First published online January 7, 2015. \n\nThis work was supported in part under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams as well as the Swift team for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). PR acknowledges contract ASI-INAF I/004/11/0. LN wishes to acknowledge the Italian Space Agency (ASI) for Financial support by ASI/INAF grant I/037/12/0-011/13. VB thanks Dipankar Bhattacharya for helpful discussions. \n\nFacilities: NuSTAR, Swift\n\nPublished - 2274.full.pdf
Submitted - 1407.0112v1.pdf
",
"abstract": "We present NuSTAR spectral and timing studies of the Supergiant Fast X-ray Transient (SFXT) IGR J17544-2619. The spectrum is well-described by a ~ 1 keV blackbody and a hard continuum component, as expected from an accreting X-ray pulsar. We detect a cyclotron line at 17 keV, confirming that the compact object in IGR J17544-2619 is indeed a neutron star. This is the first measurement of the magnetic field in a SFXT. The inferred magnetic field strength, B = (1.45 \u00b1 0.03) x 10^(12)G \u2022 (1 + z) is typical of neutron stars in X-ray binaries, and rules out a magnetar nature for the compact object. We do not find any significant pulsations in the source on time scales of 1\u20132000 s.",
"date": "2015-03",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "447",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2274-2281",
"id_number": "CaltechAUTHORS:20141211-083525123",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141211-083525123",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/004/11/0"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
}
]
},
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"doi": "10.1093/mnras/stu2495",
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"author_list": "Bhalerao, Varun; Romano, Patrizia; et el."
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"id": "Hailey-C-J",
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"given": "Finn E."
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"family": "Harrison",
"given": "Fiona A."
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"name": {
"family": "Mori",
"given": "Kaya"
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"id": "Perez-K-M",
"name": {
"family": "Perez",
"given": "Kerstin M."
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"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
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"family": "Zhang",
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"title": "G359.97-0.038: A Hard X-Ray Filament Associated with a Supernova Shell-Molecular Cloud Interaction",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 September 29; accepted 2014 December 9; published 2015 February 18. \n\nThis work was supported under NASA contract No.NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, \"EMBIGGEN\" Anillo ACT1101), and Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" funded by the Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_800_2_119.pdf
",
"abstract": "We present the first high-energy X-ray (>10 keV) observations of the non-thermal filament G359.97-0.038 using the Nuclear Spectroscopic Telescope Array (NuSTAR). This filament is one of approximately 20 X-ray filaments of unknown origin located in the central 20 pc region in the Galactic Center near Sgr A^*. Its NuSTAR and Chandra broadband spectrum is characterized by a single power law with \u0393 = 1.3 \u00b1 0.3 that extends from 2 to 50 keV, with an unabsorbed luminosity of 1.3 \u00d7 10^(33) erg s^(\u20131) (d/8 kpc)^2 in the 2-8 keV band. Despite possessing a cometary X-ray morphology that is typical of a pulsar wind nebula (PWN) in high-resolution Chandra imaging, our spatially resolved Chandra spectral analysis found no significant spectral softening along the filament as would be expected from particle synchrotron cooling. Coincident radio emission is detected using the Very Large Array at 5.5 and 8.3 GHz. We examine and subsequently discard a PWN or magnetic flux tube as the origin of G359.97-0.038. We use broadband spectral characteristics and a morphological analysis to show that G359.97-0.038 is likely an interaction site between the shell of Sgr A East and an adjacent molecular cloud. This is supported by CS molecular line spectroscopy and the presence of an OH maser.",
"date": "2015-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "800",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 119",
"id_number": "CaltechAUTHORS:20150323-152801857",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150323-152801857",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "EMBIGGEN Anillo ACT1101"
},
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"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "Project IC120009 \"Millennium Institute of Astrophysics (MAS)\""
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"given": "T. J."
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"orcid": "0000-0003-2971-1722"
},
{
"id": "Ward-M-J",
"name": {
"family": "Ward",
"given": "M. J."
}
}
]
},
"title": "Black hole feedback in the luminous quasar PDS 456",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 American Association for the Advancement of Science.\n\nReceived for publication 25 July 2014. Accepted for publication 20 January 2015.\n\nThis research was supported under the U.K. Science and Technology Facilities Council grant ST/J001384/1 and is based on x-ray observations obtained with the XMM-Newton and NuSTAR satellites. XMM-Newton is a European Space Agency (ESA) science mission with instruments and contributions directly funded by ESA member states and the National Aeronautics and Space Administration. The NuSTAR mission is a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with execution and analysis of these observations. We also acknowledge financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0 (G.R. and G.M.); the Italian National Institute for Astrophysics under grant PRIN-INAF 2012 (G.R.); the I-CORE program of the Planning and Budgeting Committee, the Israel Science Foundation under grants 1937/12 and 1163/10, Israel's Ministry of Science and Technology (E.B.); and NASA under grants NNX11AJ57G and NNG08FD60C (T.J.T.). The data are stored in the science archives of the two x-ray observatories involved and will become publicly available on 25 March 2015 (XMM-Newton) and with the upcoming DR6 data release (NuSTAR).\n\nSupplemental Material - Nardini-SM.pdf
",
"abstract": "The evolution of galaxies is connected to the growth of supermassive black holes in their centers. During the quasar phase, a huge luminosity is released as matter falls onto the black hole, and radiation-driven winds can transfer most of this energy back to the host galaxy. Over five different epochs, we detected the signatures of a nearly spherical stream of highly ionized gas in the broadband x-ray spectra of the luminous quasar PDS 456. This persistent wind is expelled at relativistic speeds from the inner accretion disk, and its wide aperture suggests an effective coupling with the ambient gas. The outflow's kinetic power larger than 1046 ergs per second is enough to provide the feedback required by models of black hole and host galaxy coevolution.",
"date": "2015-02-20",
"date_type": "published",
"publication": "Science",
"volume": "347",
"number": "6224",
"publisher": "American Association for the Advancement of Science",
"pagerange": "860-863",
"id_number": "CaltechAUTHORS:20150221-084649758",
"issn": "0036-8075",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150221-084649758",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J001384/1"
},
{
"agency": "European Space Agency (ESA)"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "ASI-INAF I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)",
"grant_number": "PRIN-INAF 2012"
},
{
"agency": "Israel Science Foundation",
"grant_number": "1937/12"
},
{
"agency": "Israel Science Foundation",
"grant_number": "1163/10"
},
{
"agency": "NASA",
"grant_number": "NNX11AJ57G"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
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"items": [
{
"id": "2015-75",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
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{
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{
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},
"doi": "10.1126/science.1259202",
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"url": "https://authors.library.caltech.edu/records/efsjh-s8433/files/Nardini-SM.pdf"
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"pub_year": "2015",
"author_list": "Nardini, E.; Reeves, J. N.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/w8xpr-et711",
"eprint_id": 52576,
"eprint_status": "archive",
"datestamp": "2023-08-20 05:00:39",
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"items": [
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Cook-R-J",
"name": {
"family": "Cook",
"given": "Rick"
}
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John"
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Schmid-C",
"name": {
"family": "Schmid",
"given": "Christian"
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "Andrew C."
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"orcid": "0000-0002-9378-4072"
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"name": {
"family": "F\u00fcrst",
"given": "Felix"
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"orcid": "0000-0003-0388-0560"
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"name": {
"family": "Gandhi",
"given": "Poshak"
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"orcid": "0000-0003-3105-2615"
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{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
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"name": {
"family": "Kara",
"given": "Erin"
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"orcid": "0000-0003-0172-0854"
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"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "Thomas J."
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"orcid": "0000-0003-0976-4755"
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{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
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"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
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"orcid": "0000-0002-4656-6881"
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"name": {
"family": "Stern",
"given": "Daniel"
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"orcid": "0000-0003-2686-9241"
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{
"id": "Uttley-P",
"name": {
"family": "Uttley",
"given": "Phil"
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "No Time for Dead Time: Timing analysis of bright black hole binaries with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: stars, accretion, accretion disks, black hole physics",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 September 9; accepted 2014 December 22; published 2015 February 18.\n\nMB and DB wish to acknowledge the support from the Centre National d'\u00c9tudes Spatiales (CNES) and the Centre National de la Recherche Scientifique (CNRS). CS acknowledges funding by the German BMWi under DLR grant numbers 50 QR 0801, 50 QR 0903, and 50 OO 1111. P.G. thanks STFC for support (grant reference ST/J003697/1). This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The timing analysis was executed with Matteo Bachetti's Libraries and Tools in Python for NuSTAR Timing (MaLTPyNT). This code is available upon request. Most of the plots were produced with the Veusz software by Jeremy Sanders. The authors wish to thank Chris Done, Denis\nLeahy and Tomaso Belloni for very insightful discussions.\n\nPublished - 0004-637X_800_2_109.pdf
Submitted - 1409.3248v1.pdf
",
"abstract": "Timing of high-count rate sources with the NuSTAR Small Explorer Mission requires specialized analysis techniques. NuSTAR was primarily designed for spectroscopic observations of sources with relatively low count-rates rather than for timing analysis of bright objects. The instrumental dead time per event is relatively long (\u223c2.5 msec), and varies by a few percent event-to-event. The most\nobvious effect is a distortion of the white noise level in the power density spectrum (PDS) that cannot be modeled easily with the standard techniques due to the variable nature of the dead time. In this paper, we show that it is possible to exploit the presence of two completely independent focal planes and use the cross power density spectrum to obtain a good proxy of the white noise-subtracted PDS. Thereafter, one can use a Monte Carlo approach to estimate the remaining effects of dead time,\nnamely a frequency-dependent modulation of the variance and a frequency-independent drop of the sensitivity to variability. In this way, most of the standard timing analysis can be performed, albeit with a sacrifice in signal to noise relative to what would be achieved using more standard techniques. We apply this technique to NuSTAR observations of the black hole binaries GX339\u22124, CygX-1 and\nGRS 1915+105.",
"date": "2015-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "800",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 109",
"id_number": "CaltechAUTHORS:20141211-085027843",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141211-085027843",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "50 QR 0801"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "50 QR 0903"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)",
"grant_number": "50 OO 1111"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
}
]
},
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"doi": "10.1088/0004-637X/800/2/109",
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"pub_year": "2015",
"author_list": "Bachetti, Matteo; Harrison, Fiona A.; et el."
},
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"id": "Gastaldello-F",
"name": {
"family": "Gastaldello",
"given": "Fabio"
}
},
{
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"name": {
"family": "Wik",
"given": "Daniel R."
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"orcid": "0000-0001-8952-676X"
},
{
"id": "Molendi-S",
"name": {
"family": "Molendi",
"given": "S."
}
},
{
"id": "Westergaard-N-J",
"name": {
"family": "Westergaard",
"given": "N. J."
}
},
{
"id": "Hornstrup-A",
"name": {
"family": "Hornstrup",
"given": "A."
}
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G."
}
},
{
"id": "Ferreira-D-D-M",
"name": {
"family": "Ferreira",
"given": "D. D. M."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
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{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A NuSTAR Observation of the Center of the Coma Cluster",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: clusters: general; galaxies: clusters: individual (Coma); X-rays: galaxies: clusters",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 November 4; accepted 2014 December 28; published 2015 February 20.\n\nThis research made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\nFacility: NuSTAR\n\nPublished - 0004-637X_800_2_139.pdf
Submitted - 1411.1573v2.pdf
",
"abstract": "We present the results of a 55 ks NuSTAR observation of the core of the Coma Cluster. The global spectrum can be explained by thermal gas emission, with a conservative 90% upper limit to non-thermal inverse Compton (IC) emission of 5.1 \u00d7 10^(\u201312) erg cm^(\u20132) s^(\u20131) in a 12' \u00d7 12' field of view. The brightness of the thermal component in this central region does not allow more stringent upper limits on the IC component when compared with non-imaging instruments with much larger fields of view where claims of detections have been made. Future mosaic NuSTAR observations of Coma will further address this issue. The temperature map shows a relatively uniform temperature distribution with a gradient from the hot northwest side to the cooler southeast, in agreement with previous measurements. The temperature determination is robust given the flat effective area and low background in the 3-20 keV band, making NuSTAR an ideal instrument to measure high temperatures in the intracluster medium.",
"date": "2015-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "800",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 139",
"id_number": "CaltechAUTHORS:20150324-113734112",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150324-113734112",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/Caltech/JPL"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-77",
"name": "Space Radiation Laboratory"
}
]
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"doi": "10.1088/0004-637X/800/2/139",
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],
"pub_year": "2015",
"author_list": "Gastaldello, Fabio; Wik, Daniel R.; et el."
},
{
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"eprint_id": 55984,
"eprint_status": "archive",
"datestamp": "2023-08-22 14:59:33",
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},
{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "A."
},
"orcid": "0000-0001-8667-2681"
},
{
"id": "Zezas-A",
"name": {
"family": "Zezas",
"given": "A."
},
"orcid": "0000-0001-8952-676X"
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{
"id": "Lehmer-B-D",
"name": {
"family": "Lehmer",
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"id": "Yukita-Mihoko",
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"family": "Yukita",
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"family": "Wik",
"given": "D."
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"id": "Antoniou-V",
"name": {
"family": "Antoniou",
"given": "V."
},
"orcid": "0000-0001-7539-1593"
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{
"id": "Argo-M-K",
"name": {
"family": "Argo",
"given": "M. K."
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},
{
"id": "Ballo-L",
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"family": "Ballo",
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{
"id": "Bechtol-K",
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"given": "C. J."
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
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{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T. J."
},
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
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{
"id": "Tatum-M",
"name": {
"family": "Tatum",
"given": "M."
}
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{
"id": "Venters-T-M",
"name": {
"family": "Venters",
"given": "T."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
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},
"title": "A Focused, Hard X-Ray Look at Arp 299 with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (Arp 299); galaxies: starburst; X-rays: galaxies",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 May 22; accepted 2014 December 3; published 2015 February 18. \n\nThis research has made use of data obtained with the NuSTAR\nmission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). We also made use of the NASA/IPAC Extragalactic Database (NED) and NASA's Astrophysics Data System. L.B. received financial supports from the European Commission Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 \"Astronomy Fellowships in Italy\" (AstroFIt). A.Z. acknowledges partial support by NASA grant NNX12AN05G and Chandra grant GO3-14124X. We thank the anonymous referee for suggestions that improved this paper.\n\nPublished - 0004-637X_800_2_104.pdf
Submitted - 1412.3120v1.pdf
",
"abstract": "We report on simultaneous observations of the local starburst system Arp 299 with NuSTAR and Chandra, which provides the first resolved images of this galaxy up to energies of ~45 keV. Fitting the 3-40 keV spectrum reveals a column density of N_H ~ 4 \u00d7 10^(24) cm^(\u20132), characteristic of a Compton-thick active galactic nucleus (AGN), and a 10-30 keV luminosity of 1.2 \u00d7 10^(43) erg s^(\u20131). The hard X-rays detected by NuSTAR above 10 keV are centered on the western nucleus, Arp 299-B, which previous X-ray observations have shown to be the primary source of neutral Fe-K emission. Other X-ray sources, including Arp 299-A, the eastern nucleus also thought to harbor an AGN, as well as X-ray binaries, contribute \u227e 10% to the 10-20 keV emission from the Arp 299 system. The lack of significant emission above 10 keV other than that attributed to Arp 299-B suggests that: (1) any AGN in Arp 299-A must be heavily obscured (N_H > 10^(24) cm^(\u20132)) or have a much lower luminosity than Arp 299-B and (2) the extranuclear X-ray binaries have spectra that cut-off above ~10 keV. Such soft spectra are characteristic of ultraluminous X-ray sources observed to date by NuSTAR.",
"date": "2015-02-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "800",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 104",
"id_number": "CaltechAUTHORS:20150323-142831946",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150323-142831946",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "267251"
},
{
"agency": "NASA",
"grant_number": "NNX12AN05G"
},
{
"agency": "NASA",
"grant_number": "GO3-14124X"
}
]
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"doi": "10.1088/0004-637X/800/2/104",
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"author_list": "Ptak, A.; Hornschemeier, A.; et el."
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},
"title": "The Seyfert 2 galaxy NGC 2110: hard X-ray emission observed by NuSTAR and variability of the iron K\u03b1 line",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual: NGC 2110; galaxies: Seyfert",
"note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 November 15. Received 2014 October 29; in original form 2014 September 15. First published online December 12, 2014.\n\nAM and GM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n.312789. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). MB acknowledges support from the International Fulbright Science and Technology Award.\n\nPublished - MNRAS-2015-Marinucci-160-7.pdf
Submitted - 1411.5151v1.pdf
",
"abstract": "We present NuSTAR observations of the bright Seyfert 2 galaxy NGC 2110 obtained in 2012, when the source was at the highest flux level ever observed, and in 2013, when the source was at a more typical flux level. We include archival observations from other X-ray satellites, namely XMM\u2013Newton, Suzaku, BeppoSAX, Chandra and Swift. Simultaneous NuSTAR and Swift broad-band spectra (in the 3\u201380 keV range) indicate a cutoff energy E_c > 210 keV, with no detectable contribution from Compton reflection. NGC 2110 is one of the very few sources where no evidence for distant Compton-thick scattering is found and, by using temporal information collected over more than a decade, we investigate variations of the iron K\u03b1 line on time-scales of years. The Fe K\u03b1 line is likely the sum of two components: one constant (originating from distant Compton-thick material) and the other one variable and linearly correlated with the source flux (possibly arising from Compton-thin material much closer to the black hole).",
"date": "2015-02-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "447",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "160-167",
"id_number": "CaltechAUTHORS:20150403-083343981",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150403-083343981",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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"doi": "10.1093/mnras/stu2439",
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"name": {
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},
"title": "Coronal Properties of the Seyfert 1.9 Galaxy MCG-05-23-016 Determined from Hard X-Ray Spectroscopy with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (MCG-5-23-016); galaxies: nuclei; galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 16 July 2014; accepted for publication 17 December 2014; Published 9 February 2015.\n\nM.B. acknowledges support from the International Fulbright Science and Technology Award. A.M. and G.M. acknowledge financial support from the Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 312789. C.S.R. thanks NASA for support under ADAP grant NNX14AF86G. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of NASA's Astrophysics Data System.\n\nPublished - 0004-637X_800_1_62.pdf
Submitted - 1412.5978v1.pdf
",
"abstract": "Measurements of the high-energy cut-off in the coronal continuum of active galactic nuclei have long been elusive for all but a small number of the brightest examples. We present a direct measurement of the cut-off energy in the nuclear continuum of the nearby Seyfert 1.9 galaxy MCG\u201305-23-016 with unprecedented precision. The high sensitivity of NuSTAR up to 79\u2009keV allows us to clearly disentangle the spectral curvature of the primary continuum from that of its reflection component. Using a simple phenomenological model for the hard X-ray spectrum, we constrain the cut-off energy to 116^(+6)_(-5)\u2009keV with 90% confidence. Testing for more complex models and nuisance parameters that could potentially influence the measurement, we find that the cut-off is detected robustly. We further use simple Comptonized plasma models to provide independent constraints for both the kinetic temperature of the electrons in the corona and its optical depth. At the 90% confidence level, we find kT_e = 29\u2009 \u00b1 \u20092\u2009keV and \u03c4_e = 1.23 \u00b1 0.08 assuming a slab (disk-like) geometry, and kT_e = 25 \u00b1 2\u2009keV and \u03c4e = 3.5 \u00b1 0.2 assuming a spherical geometry. Both geometries are found to fit the data equally well and their two principal physical parameters are correlated in both cases. With the optical depth in the \u03c4_e \u2273 1 regime, the data are pushing the currently available theoretical models of the Comptonized plasma to the limits of their validity. Since the spectral features and variability arising from the inner accretion disk have been observed previously in MCG\u201305-23-016, the inferred high optical depth implies that a spherical or disk-like corona cannot be homogeneous.",
"date": "2015-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "800",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 62",
"id_number": "CaltechAUTHORS:20150316-084932916",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150316-084932916",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/12/0-011/13"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "NASA",
"grant_number": "NNX14AF86G"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
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"doi": "10.1088/0004-637X/800/1/62",
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"family": "Webb",
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},
"title": "The Broadband XMM-Newton and NuSTAR X-ray Spectra of Two Ultraluminous X-ray Sources in the Galaxy IC 342",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks, black hole physics, X-rays: binaries { X-rays: individual (IC 342 X-1, IC 342 X-2)",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 January 20; accepted 2014 November 14; published 2015 January 21. \n\nThis work was supported under NASA No. NNG08FD60C, and made use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration, and XMM-Newton, an ESA mission. We would like to thank the anonymous referee for his positive comments to improve quality of this paper. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). D. Barret and M. Bachetti are grateful to the Centre National d'Etudes Spatiales (CNES) for funding their activities.\n\nPublished - 0004-637X_799_2_121.pdf
Submitted - 1401.4637v2.pdf
",
"abstract": "We present results for two Ultraluminous X-ray Sources (ULXs), IC 342 X-1 and IC 342 X-2, using two epochs of XMM-Newton and NuSTAR observations separated by ~ 7 days. We observe little spectral or ux variability above 1 keV between epochs, with unabsorbed 0.3-30 keV luminosities\nbeing 1.04^(+0.08)_(-0.06) x 10^(40) erg s^(-1) for IC 342 X-1 and 7.40 \u00b1 0.20 x 10^(39) erg s^(-1) for IC 342 X-2, so that both were observed in a similar, luminous state. Both sources have a high absorbing column in excess of the Galactic value. Neither source has a spectrum consistent with a black hole binary in low/hard state, and both ULXs exhibit strong curvature in their broadband X-ray spectra. This curvature rules out models that invoke a simple reflection-dominated spectrum with a broadened iron line and\nno cutoff in the illuminating power-law continuum. X-ray spectrum of IC 342 X-1 can be characterized by a soft disk-like black body component at low energies and a cool, optically thick Comptonization continuum at high energies, but unique physical interpretation of the spectral components remains challenging. The broadband spectrum of IC 342 X-2 can be fit by either a hot (3.8 keV) accretion\ndisk, or a Comptonized continuum with no indication of a seed photon population. Although the seed photon component may be masked by soft excess emission unlikely to be associated with the binary system, combined with the high absorption column, it is more plausible that the broadband X-ray emission arises from a simple thin blackbody disk component. Secure identification of the origin of the spectral components in these sources will likely require broadband spectral variability studies.",
"date": "2015-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "799",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 121",
"id_number": "CaltechAUTHORS:20141210-150832641",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141210-150832641",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
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"agency": "Centre National d'Etudes Spatiales (CNES)"
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"doi": "10.1088/0004-637X/799/2/121",
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"pub_year": "2015",
"author_list": "Rana, Vikram R.; Harrison, Fiona A.; et el."
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"name": {
"family": "Rana",
"given": "V."
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"id": "Roberts-T-P",
"name": {
"family": "Roberts",
"given": "T. P."
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"name": {
"family": "Stern",
"given": "D."
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"id": "Sutton-A-D",
"name": {
"family": "Sutton",
"given": "A. D."
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"id": "Webb-N-A",
"name": {
"family": "Webb",
"given": "N."
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},
"title": "NuSTAR and XMM-Newton Observations of the Extreme Ultraluminous X-Ray Source NGC 5907 ULX1: A Vanishing Act",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; X-rays: binaries; X-rays: individual (NGC 5907 ULX1)",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 August 19; accepted 2014 November 21; published 2015 January 21. \n\nThe authors would like to thank the reviewer for positive and useful feedback, which helped improve the manuscript, as well as Diego Altamarino for useful discussions. M.B. and D.B. acknowledge financial support from the French Space Agency (CNES). This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and has utilized the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). This research has also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and NASA's Chandra and Swift satellites. \n\nFacilites: NuSTAR, XMM, Chandra, Swift\n\nPublished - 0004-637X_799_2_122.pdf
Submitted - 1411.5974v1.pdf
",
"abstract": "We present results obtained from two broadband X-ray observations of the extreme ultraluminous X-ray source (ULX) NGC 5907 ULX1, known to have a peak X-ray luminosity of ~5 \u00d7 10^(40) erg s^(\u20131). These XMM-Newton and NuSTAR observations, separated by only ~4 days, revealed an extreme level of short-term flux variability. In the first epoch, NGC 5907 ULX1 was undetected by NuSTAR, and only weakly detected (if at all) with XMM-Newton, while in the second NGC 5907 ULX1 was clearly detected at high luminosity by both missions. This implies an increase in flux of ~2 orders of magnitude or more during this ~4 day window. We argue that this is likely due to a rapid rise in the mass accretion rate, rather than to a transition from an extremely obscured to an unobscured state. During the second epoch we observed the broadband 0.3-20.0 keV X-ray luminosity to be (1.55 \u00b1 0.06) \u00d7 10^(40) erg s^(\u20131), similar to the majority of the archival X-ray observations. The broadband X-ray spectrum obtained from the second epoch is inconsistent with the low/hard accretion state observed in Galactic black hole binaries, but is well modeled with a simple accretion disk model incorporating the effects of photon advection. This strongly suggests that when bright, NGC 5907 ULX1 is a high-Eddington accretor.",
"date": "2015-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "799",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 122",
"id_number": "CaltechAUTHORS:20150306-121109629",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150306-121109629",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA/Caltech/JPL"
},
{
"agency": "ESA Member States"
}
]
},
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"items": [
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"id": "2015-83",
"name": "Space Radiation Laboratory"
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"author_list": "Walton, D. J.; Harrison, F. A.; et el."
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"id": "Barri\u00e8re-N-M",
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"family": "Bachetti",
"given": "Matteo"
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"orcid": "0000-0002-4576-9337"
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{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
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"orcid": "0000-0001-9567-4224"
},
{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "Deepto"
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"orcid": "0000-0001-8804-8946"
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"name": {
"family": "Christensen",
"given": "Finn E."
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"orcid": "0000-0001-5679-1946"
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"name": {
"family": "Craig",
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{
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"name": {
"family": "Hailey",
"given": "Charles J."
}
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"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "Jaesub"
}
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"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
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},
"title": "NuSTAR Observation of a Type I X-Ray Burst from GRS 1741.9-2853",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; nuclear reactions, nucleosynthesis, abundances; stars: neutron; X-rays: binaries; X-rays: bursts; X-rays: individual (GRS 1741.9-2853)",
"note": "\u00a9 2015 American Astronomical Society. Received 2014 May 20; accepted 2014 November 21; published 2015 January 21.\n\nThis work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors thank Nevin Weinberg for useful discussions, and the anonymous referee for constructive comments. \n\nFacility: NuSTAR\n\nPublished - 0004-637X_799_2_123.pdf
Submitted - 1411.4745v1.pdf
",
"abstract": "We report on two NuSTAR observations of GRS 1741.9-2853, a faint neutron star (NS) low-mass X-ray binary burster located 10' away from the Galactic center. NuSTAR detected the source serendipitously as it was emerging from quiescence: its luminosity was 6 \u00d7 10^(34) erg s^(\u20131) on 2013 July 31 and 5 \u00d7 10^(35) erg s^(\u20131) in a second observation on 2013 August 3. A bright, 800 s long, H-triggered mixed H/He thermonuclear Type I burst with mild photospheric radius expansion (PRE) was present during the second observation. Assuming that the luminosity during the PRE was at the Eddington level, an H mass fraction X = 0.7 in the atmosphere, and an NS mass M = 1.4 M_\u2609, we determine a new lower limit on the distance for this source of 6.3 \u00b1 0.5 kpc. Combining with previous upper limits, this places GRS 1741.9-2853 at a distance of 7 kpc. Energy independent (achromatic) variability is observed during the cooling of the NS, which could result from the disturbance of the inner accretion disk by the burst. The large dynamic range of this burst reveals a long power-law decay tail. We also detect, at a 95.6% confidence level (1.7\u03c3), a narrow absorption line at 5.46 \u00b1 0.10 keV during the PRE phase of the burst, reminiscent of the detection by Waki et al. We propose that the line, if real, is formed in the wind above the photosphere of the NS by a resonant K\u03b1 transition from H-like Cr gravitationally redshifted by a factor 1 + z = 1.09, corresponding to a radius range of 29.0-41.4 km for a mass range of 1.4-2.0 M_\u2609.",
"date": "2015-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "799",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 123",
"id_number": "CaltechAUTHORS:20150306-124238863",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150306-124238863",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
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"id": "Space-Radiation-Laboratory"
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"doi": "10.1088/0004-637X/799/2/123",
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"pub_year": "2015",
"author_list": "Barri\u00e8re, Nicolas M.; Krivonos, Roman; et el."
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"datestamp": "2023-08-22 14:48:35",
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"items": [
{
"id": "Zoghbi-A",
"name": {
"family": "Zoghbi",
"given": "A."
},
"orcid": "0000-0002-0572-9613"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
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{
"id": "Walton-D-J",
"name": {
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"given": "D. J."
},
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
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},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Reynolds-C-S",
"name": {
"family": "Reynolds",
"given": "C. S."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W",
"name": {
"family": "Craig",
"given": "W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Reveals Relativistic Reflection But No Ultra-Fast Outflow In The Quasar PG 1211+143",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars: absorption lines; quasars: individual (PG 1211+143)",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 December 22; accepted 2015 January 6; published 2015 January 29. \n\nThis work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration.\n\nPublished - 2041-8205_799_2_L24.pdf
Submitted - 1501.01663v1.pdf
",
"abstract": "We report on four epochs of observations of the quasar PG 1211+143 using NuSTAR. The net exposure time is 300 ks. Prior work on this source found suggestive evidence of an ultra-fast outflow (UFO) in the Fe K band with a velocity of approximately 0.1c. The putative flow would carry away a high-mass flux and kinetic power, with broad implications for feedback and black hole--galaxy co-evolution. NuSTAR detects PG 1211+143 out to 30 keV, meaning that the continuum is well-defined both through and above the Fe K band. A characteristic relativistic disk reflection spectrum is clearly revealed via a broad Fe K emission line and Compton back-scattering curvature. The data offer only weak constraints on the spin of the black hole. A careful search for UFOs shows no significant absorption feature above 90% confidence. The limits are particularly tight when relativistic reflection is included. We discuss the statistics and the implications of these results in terms of connections between accretion onto quasars, Seyferts, and stellar-mass black holes, and feedback into their host environments.",
"date": "2015-01-30",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "799",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L24",
"id_number": "CaltechAUTHORS:20150126-085830836",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150126-085830836",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-86",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/2041-8205/799/2/L24",
"primary_object": {
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}
],
"pub_year": "2015",
"author_list": "Zoghbi, A.; Miller, J. M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/tqhxt-taf72",
"eprint_id": 59867,
"eprint_status": "archive",
"datestamp": "2023-08-20 04:42:28",
"lastmod": "2023-10-23 22:47:26",
"type": "article",
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"creators": {
"items": [
{
"id": "Zhang-Liang",
"name": {
"family": "Zhang",
"given": "Liang"
},
"orcid": "0000-0003-3115-1752"
},
{
"id": "Chen-Li",
"name": {
"family": "Chen",
"given": "Li"
}
},
{
"id": "Qu-Jin-lu",
"name": {
"family": "Qu",
"given": "Jin-lu"
}
},
{
"id": "Bu-Qing-cui",
"name": {
"family": "Bu",
"given": "Qing-cui"
}
}
]
},
"title": "The NuSTAR view of a QPO Evolution of GRS 1915+105",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015. The American Astronomical Society.\n\nReceived 2014 October 16, accepted for publication 2014 December 26. Published 2015 January 30.\n\nWe thank H. Q. Gao and Z. Zhang for theory suggestions. This research has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work is supported by the National Basic Research program of China 973 Program 2009CB824800, the National Natural Science Foundation of China (11173024), and the Fundamental Research Funds for the Central Universities, the Strategic Priority Research Program on Space Science, the\nChinese Academy of Sciences, Grant No. XDA04010300.\n\nPublished - 1538-3881_149_2_82.pdf
",
"abstract": "We report a timing analysis of the black hole binary GRS 1915+105 with the Nuclear Spectroscopic Telescope Array Observatory. A strong type-C quasi-periodic oscillation (QPO) below 2 Hz appears in the power density spectrum during the whole observation, whose frequency is correlated with the 3\u201325 keV count rate. The QPO shows a sudden increase in frequency along with an increase in flux and a softening of the spectrum. We discuss the possible origin of the QPO and the reasons that lead to the QPO frequency variation. It is suggested that the reflection component has little influence on QPO frequency and the increase in QPO frequency could be associated with the inward motion of the outer part of the disk.",
"date": "2015-01-30",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "149",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "82-88",
"id_number": "CaltechAUTHORS:20150824-183949369",
"issn": "0004-6256",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150824-183949369",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "National Basic Research Program of China, Program 973",
"grant_number": "2009CB824800"
},
{
"agency": "Natural Science Foundation China",
"grant_number": "11173024"
},
{
"agency": "Chinese Academy of Sciences",
"grant_number": "XDA04010300"
},
{
"agency": "NASA"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-6256/149/2/82",
"primary_object": {
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},
"pub_year": "2015",
"author_list": "Zhang, Liang; Chen, Li; et el."
},
{
"id": "https://authors.library.caltech.edu/records/ppz2b-3xc61",
"eprint_id": 54996,
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},
"orcid": "0000-0002-9378-4072"
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{
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"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
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{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kara-E",
"name": {
"family": "Kara",
"given": "E."
},
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{
"id": "King-A-L",
"name": {
"family": "King",
"given": "A. L."
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{
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"name": {
"family": "Stern",
"given": "D. K."
},
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "New Constraints on the Black Hole Low/Hard State Inner Accretion Flow with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics",
"note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 September 2; accepted 2014 November 5; published 2015 January 19. \n\nJ.M.M. thanks Javier Garcia and Thomas Dauser for helpful\nconversations. This work was supported under NASA Contract\nNo. NNG08FD60C, and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA.\n\nPublished - 2041-8205_799_1_L6.pdf
Submitted - 1411.1921v1.pdf
",
"abstract": "We report on an observation of the Galactic black hole candidate GRS 1739\u2013278 during its 2014 outburst, obtained with NuSTAR. The source was captured at the peak of a rising \"low/hard\" state, at a flux of ~0.3 Crab. A broad, skewed iron line and disk reflection spectrum are revealed. Fits to the sensitive NuSTAR spectra with a number of relativistically blurred disk reflection models yield strong geometrical constraints on the disk and hard X-ray \"corona.\" Two models that explicitly assume a \"lamp post\" corona find its base to have a vertical height above the black hole of h = 5^(+7)_(-2) (GM)/c^(2) and h = 18 \u00b1 4 GM/c ^2(90% confidence errors); models that do not assume a \"lamp post\" return emissivity profiles that are broadly consistent with coronae of this size. Given that X-ray microlensing studies of quasars and reverberation lags in Seyferts find similarly compact coronae, observations may now signal that compact coronae are fundamental across the black hole mass scale. All of the models fit to GRS 1739\u2013278 find that the accretion disk extends very close to the black hole\u2014the least stringent constraint is r_(in) = 5^(+3)_(-4) GM/c^(2). Only two of the models deliver meaningful spin constraints, but a = 0.8 \u00b1 0.2 is consistent with all of the fits. Overall, the data provide especially compelling evidence of an association between compact hard X-ray coronae and the base of relativistic radio jets in black holes.",
"date": "2015-01-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "799",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L6",
"id_number": "CaltechAUTHORS:20150219-092157983",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150219-092157983",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-87",
"name": "Space Radiation Laboratory"
}
]
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"doi": "10.1088/2041-8205/799/1/L6",
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"pub_year": "2015",
"author_list": "Miller, J. M.; Tomsick, J. A.; et el."
},
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"datestamp": "2023-08-22 14:42:57",
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"id": "Zoglauer-A-C",
"name": {
"family": "Zoglauer",
"given": "Andreas"
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{
"id": "Reynolds-S-P",
"name": {
"family": "Reynolds",
"given": "Stephen P."
}
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
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{
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"name": {
"family": "Craig",
"given": "William W."
}
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{
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"name": {
"family": "Fryer",
"given": "Chris L."
},
"orcid": "0000-0003-2624-0056"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
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},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
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},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
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{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Hard X-Ray View of the Young Supernova Remnant G1.9+0.3",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "ISM: supernova remnants; X-rays: individual (G1.9+0.3)",
"note": "\u00a9 2015 American Astronomical Society.\n\nReceived 2014 September 29; accepted 2014 October 29; published 2014 December 31. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology\n(Caltech, USA). \n \nFacilities: NuSTAR, CXO\n\nPublished - 0004-637X_798_2_98.pdf
Submitted - 1411.6752v1.pdf
",
"abstract": "NuSTAR observed G1.9+0.3, the youngest known supernova remnant in the Milky Way, for 350 ks and detected emission up to ~30 keV. The remnant's X-ray morphology does not change significantly across the energy range from 3 to 20 keV. A combined fit between NuSTAR and Chandra shows that the spectrum steepens with energy. The spectral shape can be well fitted with synchrotron emission from a power-law electron energy distribution with an exponential cutoff with no additional features. It can also be described by a purely phenomenological model such as a broken power law or a power law with an exponential cutoff, though these descriptions lack physical motivation. Using a fixed radio flux at 1 GHz of 1.17 Jy for the synchrotron model, we get a column density of N_H = (7.23 \u00b1 0.07) \u00d7 10^(22) cm^(\u20132), a spectral index of \u03b1 = 0.633 \u00b1 0.003, and a roll-off frequency of \u03bd_(rolloff) = (3.07 \u00b1 0.18) \u00d7 10^(17) Hz. This can be explained by particle acceleration, to a maximum energy set by the finite remnant age, in a magnetic field of about 10 \u03bcG, for which our roll-off implies a maximum energy of about 100 TeV for both electrons and ions. Much higher magnetic-field strengths would produce an electron spectrum that was cut off by radiative losses, giving a much higher roll-off frequency that is independent of magnetic-field strength. In this case, ions could be accelerated to much higher energies. A search for ^(44)Ti emission in the 67.9 keV line results in an upper limit of 1.5 \u00d7 10^(\u20135) photons cm^(\u20132) s^(\u20131) assuming a line width of 4.0 keV (1 sigma).",
"date": "2015-01-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "798",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 98",
"id_number": "CaltechAUTHORS:20150409-102019403",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150409-102019403",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-88",
"name": "Space Radiation Laboratory"
}
]
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"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/798/2/98",
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],
"pub_year": "2015",
"author_list": "Zoglauer, Andreas; Reynolds, Stephen P.; et el."
},
{
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"eprint_id": 59866,
"eprint_status": "archive",
"datestamp": "2023-08-20 04:30:21",
"lastmod": "2023-10-23 22:47:24",
"type": "article",
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"creators": {
"items": [
{
"id": "Tam-Pak-Hin-Thomas",
"name": {
"family": "Tam",
"given": "P. H. T."
},
"orcid": "0000-0002-1262-7375"
},
{
"id": "Li-Kwan-Lok",
"name": {
"family": "Li",
"given": "K. L."
},
"orcid": "0000-0001-8229-2024"
},
{
"id": "Takata-Jumpei",
"name": {
"family": "Takata",
"given": "J."
},
"orcid": "0000-0002-8731-0129"
},
{
"id": "Okazaki-A-T",
"name": {
"family": "Okazaki",
"given": "A. T."
}
},
{
"id": "Hui-David-C-Y",
"name": {
"family": "Hui",
"given": "C. Y."
},
"orcid": "0000-0003-1753-1660"
},
{
"id": "Kong-Albert-K-H",
"name": {
"family": "Kong",
"given": "A. K. H."
},
"orcid": "0000-0002-5105-344X"
}
]
},
"title": "High-Energy Observations of PSR B1259-63/LS 2883 Through the 2014 Periastron Passage: Connecting X-Rays to the GeV Flare",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2014 October 7, accepted for publication 2014 December 5. Published 2014 December 19. \n\nWe acknowledge the use of data and software facilities from the FSSC, managed by the HEASARC at the Goddard Space Flight Center. P.H.T. and K.L.L. are supported by the Ministry of Science and Technology (MOST) of the Republic of China (Taiwan) through grant 101-2112-M-007-022-MY3. A.K.H.K. is supported by MOST through grants 100-2628-M-007-002-MY3, 100-2923-M-007-001-MY3, and 103-2628-M-007-003-MY3. J.T. is supported by a 2014 GRF grant of Hong Kong Government under HKU 17300814P. C.Y.H. is supported by the National Research Foundation of Korea through grant 2014R1A1A2058590.\n\nPublished - 2041-8205_798_1_L26.pdf
",
"abstract": "The binary system PSR B1259\u201363/LS 2883 is well sampled in radio, X-rays, and TeV \u03b3-rays, and shows orbital-phase-dependent variability in these frequencies. The first detection of GeV \u03b3-rays from the system was made around the 2010 periastron passage. In this Letter, we present an analysis of X-ray and \u03b3-ray data obtained by the Swift/XRT, NuSTAR/FPM, and Fermi/LAT, through the recent periastron passage which occurred on 2014 May 4. While PSR B1259\u201363/LS 2883 was not detected by the Large Area Telescope before and during this passage, we show that the GeV flares occurred at a similar orbital phase as in early 2011, thus establishing the repetitive nature of the post-periastron GeV flares. Multiple flares each lasting for a few days have been observed and short-term variability is seen as well. We also found X-ray flux variation contemporaneous with the GeV flare for the first time. Strong evidence of the keV-to-GeV connection came from the broadband high-energy spectra, which we interpret as synchrotron radiation from the shocked pulsar wind.",
"date": "2015-01-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "798",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "L26-L31",
"id_number": "CaltechAUTHORS:20150824-164910021",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150824-164910021",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "101-2112-M-007-022-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "100-2628- M-007-002-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "100-2923-M-007-001-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "100-2628- M-007-002-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "100-2923-M-007-001-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "103-2628- M-007-003-MY3"
},
{
"agency": "General Research Fund (Hong Kong)",
"grant_number": "HKU 17300814P"
},
{
"agency": "National Research Foundation of Korea",
"grant_number": "2014R1A1A2058590"
}
]
},
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}
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},
"doi": "10.1088/2041-8205/798/1/L26",
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"pub_year": "2015",
"author_list": "Tam, P. H. T.; Li, K. L.; et el."
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{
"id": "Wik-D-R",
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"family": "Wik",
"given": "D. R."
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},
{
"id": "Lehmer-B-D",
"name": {
"family": "Lehmer",
"given": "B. D."
},
"orcid": "0000-0003-2192-3296"
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{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "A. E."
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{
"id": "Yukita-Mihoko",
"name": {
"family": "Yukita",
"given": "M."
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},
{
"id": "Ptak-A",
"name": {
"family": "Ptak",
"given": "A."
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"name": {
"family": "Zezas",
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"name": {
"family": "Antoniou",
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"orcid": "0000-0001-7539-1593"
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{
"id": "Argo-M-K",
"name": {
"family": "Argo",
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}
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"id": "Bechtol-K",
"name": {
"family": "Bechtol",
"given": "K."
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{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S."
},
"orcid": "0000-0001-9567-4224"
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{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F."
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"orcid": "0000-0001-5679-1946"
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{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W."
}
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"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C."
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "R."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T. J."
},
"orcid": "0000-0003-0976-4755"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
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{
"id": "Venters-T-M",
"name": {
"family": "Venters",
"given": "T."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
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},
"title": "Spatially resolving a starburst galaxy at hard x-ray energies: NuSTAR, CHANDRA and VLBA observations of NGC 253",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2014 June 27, accepted for publication 2014 October 8. Published 2014 December 1.\n\nWe thank the referee for insightful suggestions that improved the paper. This research was supported by an appointment (DRW) to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with the National Aeronautics and Space Administration (NASA) and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work was also funded by a Chandra grant for Program #13620679 (PI: Hornschemeier). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator, developed as part of the Australian Major National Research Facilities Programme and operated under license.\n\nPublished - 0004-637X_797_2_79.pdf
",
"abstract": "Prior to the launch of NuSTAR, it was not feasible to spatially resolve the hard (E > 10 keV) emission from galaxies beyond the Local Group. The combined NuSTAR data set, comprised of three similar to 165 ks observations, allows spatial characterization of the hard X-ray emission in the galaxy NGC 253 for the first time. As a follow up to our initial study of its nuclear region, we present the first results concerning the full galaxy from simultaneous NuSTAR, Chandra, and Very Long Baseline Array monitoring of the local starburst galaxy NGC 253. Above similar to 10 keV, nearly all the emission is concentrated within 100 '' of the galactic center, produced almost exclusively by three nuclear sources, an off-nuclear ultraluminous X-ray source (ULX), and a pulsar candidate that we identify for the first time in these observations. We detect 21 distinct sources in energy bands up to 25 keV, mostly consisting of intermediate state black hole X-ray binaries. The global X-ray emission of the galaxy-dominated by the off-nuclear ULX and nuclear sources, which are also likely ULXs-falls steeply (photon index greater than or similar to 3) above 10 keV, consistent with other NuSTAR-observed ULXs, and no significant excess above the background is detected at E > 40 keV. We report upper limits on diffuse inverse Compton emission for a range of spatial models. For the most extended morphologies considered, these hard X-ray constraints disfavor a dominant inverse Compton component to explain the. gamma-ray emission detected with Fermi and H.E.S.S. If NGC 253 is typical of starburst galaxies at higher redshift, their contribution to the E > 10 keV cosmic X-ray background is < 1%.",
"date": "2014-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "797",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 79",
"id_number": "CaltechAUTHORS:20150401-103251427",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150401-103251427",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Chandra",
"grant_number": "13620679"
}
]
},
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"id": "NuSTAR"
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"doi": "10.1088/0004-637X/797/2/79",
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"pub_year": "2014",
"author_list": "Wik, D. R.; Lehmer, B. D.; et el."
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{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "Deepto"
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
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"orcid": "0000-0001-5506-9855"
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{
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"family": "Grefenstette",
"given": "Brian W."
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"orcid": "0000-0002-1984-2932"
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{
"id": "Psaltis-Dmitrios",
"name": {
"family": "Psaltis",
"given": "Dimitrios"
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{
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"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
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{
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"name": {
"family": "Barret",
"given": "Didier"
},
"orcid": "0000-0002-0393-9190"
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{
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"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
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"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
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"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "Victoria M."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
{
"id": "Nowak-M-A",
"name": {
"family": "Nowak",
"given": "Michael A."
},
"orcid": "0000-0001-6923-1315"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram R."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "Daniel R."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
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]
},
"title": "A Hard X-Ray Power-law Spectral Cutoff in Centaurus X-4",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; binaries: close; stars: individual (Cen X-4); stars: neutron; X-rays: binaries",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 March 26; accepted 2014 October 8; published 2014 December 3. \n\nWe thank the referee, Craig Heinke, for several suggestions that greatly improved our paper. D.C. thanks Herman Marshall, Sera Markoff, Caroline D'Angelo, Stephen Reynolds, Federico Bernardini, Phil Charles, and Chris Done for useful discussions and Luca Zampieri and Roberto Soria for sharing their XSPEC additive table model zamp. We also thank Thorsten Brand for help with evaluating the level of photon pileup in the XMM-Newton data. This work was supported in part under NASA contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J.A.T. acknowledges partial support from the XMM-Newton Guest Observer program through NASA grant NNX13AB47G. \n\nFacilities: NuSTAR, XMM\n\nPublished - 0004-637X_797_2_92.pdf
Submitted - 1403.6751v2.pdf
",
"abstract": "The low-mass X-ray binary (LMXB) Cen X-4 is the brightest and closest (<1.2 kpc) quiescent neutron star transient. Previous 0.5-10 keV X-ray observations of Cen X-4 in quiescence identified two spectral components: soft thermal emission from the neutron star atmosphere and a hard power-law tail of unknown origin. We report here on a simultaneous observation of Cen X-4 with NuSTAR (3-79 keV) and XMM-Newton (0.3-10 keV) in 2013 January, providing the first sensitive hard X-ray spectrum of a quiescent neutron star transient. The 0.3-79 keV luminosity was 1.1 x 10^(33) D^2_(kpc erg s^(\u20131), with \u2243 60% in the thermal component. We clearly detect a cutoff of the hard spectral tail above 10 keV, the first time such a feature has been detected in this source class. We show that thermal Comptonization and synchrotron shock origins for the hard X-ray emission are ruled out on physical grounds. However, the hard X-ray spectrum is well fit by a thermal bremsstrahlung model with kT_e = 18 keV, which can be understood as arising either in a hot layer above the neutron star atmosphere or in a radiatively inefficient accretion flow. The power-law cutoff energy may be set by the degree of Compton cooling of the bremsstrahlung electrons by thermal seed photons from the neutron star surface. Lower thermal luminosities should lead to higher (possibly undetectable) cutoff energies. We compare Cen X-4's behavior with PSR J1023+0038, IGR J18245\u20132452, and XSS J12270\u20134859, which have shown transitions between LMXB and radio pulsar modes at a similar X-ray luminosity.",
"date": "2014-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "797",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 92",
"id_number": "CaltechAUTHORS:20141211-081434965",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141211-081434965",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX13AB47G"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2015-89",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/797/2/92",
"primary_object": {
"basename": "0004-637X_797_2_92.pdf",
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"basename": "1403.6751v2.pdf",
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],
"pub_year": "2014",
"author_list": "Chakrabarty, Deepto; Tomsick, John A.; et el."
},
{
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"eprint_id": 56285,
"eprint_status": "archive",
"datestamp": "2023-08-20 04:05:22",
"lastmod": "2023-10-23 15:16:35",
"type": "article",
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"creators": {
"items": [
{
"id": "Li-Kwan-Lok",
"name": {
"family": "Li",
"given": "K. L."
},
"orcid": "0000-0001-8229-2024"
},
{
"id": "Kong-Albert-K-H",
"name": {
"family": "Kong",
"given": "A. K. H."
},
"orcid": "0000-0002-5105-344X"
},
{
"id": "Takata-Jumpei",
"name": {
"family": "Takata",
"given": "J."
},
"orcid": "0000-0002-8731-0129"
},
{
"id": "Cheng-Kwongsang",
"name": {
"family": "Cheng",
"given": "K. S."
},
"orcid": "0000-0002-8043-9851"
},
{
"id": "Tam-Pak-Hin-Thomas",
"name": {
"family": "Tam",
"given": "P. H. T."
},
"orcid": "0000-0002-1262-7375"
},
{
"id": "Hui-David-C-Y",
"name": {
"family": "Hui",
"given": "C. Y."
},
"orcid": "0000-0003-1753-1660"
},
{
"id": "Jin-Ruolan",
"name": {
"family": "Jin",
"given": "Ruolan"
},
"orcid": "0000-0002-9652-0056"
}
]
},
"title": "NuSTAR Observations and broadband spectral energy distribution modeling of the millisecond pulsar binary PSR J1023+0038",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2014 May 19, accepted for publication 2014 October 16. Published 2014 December 5.\n\nK.L.L., A.K.H.K., and R.J. are supported by the Ministry of Science and Technology of the Republic of China (Taiwan) through grants 100-2628-M-007-002-MY3, 100-2923-M-007-001-MY3, and 101-2119-M-008-007-MY3. J.T. and K.S.C. are supported by a GRF grant of the HK Government under HKU 17300814P. P.H.T. is supported by the Ministry of Science and Technology of the Republic of China (Taiwan) through grant 101-2112-M-007-022-MY3. C.Y.H. is supported by the National Research Foundation of Korea through grant 2011-0023383. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA).\nFacilities: NuSTAR, Swift\n\nPublished - 0004-637X_797_2_111.pdf
",
"abstract": "We report the first hard X-ray (3-79 keV) observations of the millisecond pulsar (MSP) binary PSR J1023+0038 using NuSTAR. This system has been shown transiting between a low-mass X-ray binary (LMXB) state and a rotation-powered MSP state. The NuSTAR observations were taken in both LMXB state and rotation-powered state. The source is clearly seen in both states up to similar to 79 keV. During the LMXB state, the 3-79 keV flux is about a factor of 10 higher than in the rotation-powered state. The hard X-rays show clear orbital modulation during the X-ray faint rotation-powered state but the X-ray orbital period is not detected in the X-ray bright LMXB state. In addition, the X-ray spectrum changes from a flat power-law spectrum during the rotation-powered state to a steeper power-law spectrum in the LMXB state. We suggest that the hard X-rays are due to the intrabinary shock from the interaction between the pulsar wind and the injected material from the low-mass companion star. During the rotation-powered MSP state, the X-ray orbital modulation is due to Doppler boosting of the shocked pulsar wind. At the LMXB state, the evaporating matter of the accretion disk due to the gamma-ray irradiation from the pulsar stops almost all the pulsar wind, resulting in the disappearance of the X-ray orbital modulation.",
"date": "2014-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "797",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 111",
"id_number": "CaltechAUTHORS:20150401-112116690",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150401-112116690",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "100-2628-M-007-002-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "100-2923-M-007- 001-MY3"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "101-2119-M-008-007-MY3"
},
{
"agency": "General Research Fund (Hong Kong)",
"grant_number": "17300814P"
},
{
"agency": "Ministry of Science and Technology (Taipei)",
"grant_number": "101-2112-M-007-022-MY3"
},
{
"agency": "National Research Foundation of Korea",
"grant_number": "2011-0023383"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1088/0004-637X/797/2/111",
"primary_object": {
"basename": "0004-637X_797_2_111.pdf",
"url": "https://authors.library.caltech.edu/records/aj9gc-9m241/files/0004-637X_797_2_111.pdf"
},
"pub_year": "2014",
"author_list": "Li, K. L.; Kong, A. K. H.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/aq77y-mv063",
"eprint_id": 64050,
"eprint_status": "archive",
"datestamp": "2023-08-20 04:00:56",
"lastmod": "2023-10-17 18:36:20",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Agrawal-V-K",
"name": {
"family": "Agrawal",
"given": "V. K."
}
},
{
"id": "Nandi-A",
"name": {
"family": "Nandi",
"given": "A."
}
}
]
},
"title": "Discovery of a quasi-periodic oscillation in the ultraluminous X-ray source IC 342 X-1: XMM-Newton results",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 October 29. Received 2014 October 29; in original form 2013 December 27. \n\nThe authors thank the anonymous referee for a careful reading of the\narticle and constructive criticism, along with useful suggestions for\nimprovement of the manuscript. We also thank Drs Girish and Das\nfor careful reading and comments on the manuscript. This research\nhas made use of data and/or software provided by the High Energy\nAstrophysics Science Archive Research Center (HEASARC).\nWe thank Dr Anil Agarwal, GD, SAG, Mr Vasantha E DD, CDA\nand Dr S. K. Shivakumar, Director, ISAC, for encouragement and\ncontinuous support to carry out this research.\n\nPublished - MNRAS-2015-Agrawal-3926-31.pdf
",
"abstract": "We report the discovery of a quasi-periodic oscillation (QPO) at 642 mHz in an XMM\u2013Newton observation of the ultraluminous X-ray source (ULX) IC 342 X-1. The QPO has a centroid at \u03bdQPO = 642 \u00b1 20 mHz, a coherence factor Q = 11.6 and an amplitude (rms) of 4.1\u2009per\u2009cent with significance of 3.6\u03c3. The energy dependence study shows that the QPO is stronger in the energy range 0.3\u20135.0 keV. A subsequent observation (6 d later) does not show any signature of the QPO in the power-density spectrum. The broad-band energy spectra (0.3\u201340.0 keV) obtained by quasi-simultaneous observations of XMM\u2013Newton and NuSTAR can be described well by an absorbed diskbb plus cutoffpl model. The best-fitting spectral parameters are power-law index (\u0393) \u223c 1.1, cut-off energy (Ec) \u223c 7.9 keV and disc temperature (kT_in) \u223c 0.33 keV where the QPO is detected. The unabsorbed bolometric luminosity is \u223c5.34 \u00d7 1039 erg s\u22121. Comparing this with the well-known X-ray binary GRS 1915+105, our results are consistent with the mass of the compact object in IC 342 X-1 being in the range \u223c20\u201365\u2009M\u2299. We discuss the possible implications of our results.",
"date": "2014-12-10",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "446",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "3926-3931",
"id_number": "CaltechAUTHORS:20160128-132152642",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160128-132152642",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"local_group": {
"items": [
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stu2291",
"primary_object": {
"basename": "MNRAS-2015-Agrawal-3926-31.pdf",
"url": "https://authors.library.caltech.edu/records/aq77y-mv063/files/MNRAS-2015-Agrawal-3926-31.pdf"
},
"pub_year": "2014",
"author_list": "Agrawal, V. K. and Nandi, A."
},
{
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"eprint_id": 52254,
"eprint_status": "archive",
"datestamp": "2023-08-22 14:10:56",
"lastmod": "2023-10-18 19:42:37",
"type": "article",
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"items": [
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "Shriharsh P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Bhalerao-V-B",
"name": {
"family": "Bhalerao",
"given": "Varun B."
},
"orcid": "0000-0002-6112-7609"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William"
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Discovery of a Cyclotron Line in the Be/X-Ray Binary RX J0520.5\u20136932 during Outburst",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; pulsars: general; pulsars: individual (RX J0520.5-6932); stars: neutron; X-rays: binaries; X-rays: bursts; X-rays: stars",
"note": "\u00a9 2014 American Astronomical Society. Received 2014 August 3; accepted 2014 September 17; published 2014 October 23.\n\nWe thank the anonymous referee for detailed suggestions\nand comments. This work was supported under NASA contract\nNo. NNG08FD60C, and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_795_2_154.pdf
Submitted - 1409.5035v1.pdf
",
"abstract": "We present spectral and timing analysis of NuSTAR observations of RX J0520.5\u20136932 in the 3-79 keV band collected during its outburst in 2014 January. The target was observed on two epochs and we report the detection of a cyclotron resonant scattering feature with central energies of E_(CRSF) = 31.3_(-0.7)^(+0.8) keV and 31.5_(-0.6)^(+0.7) keV during the two observations, respectively, corresponding to a magnetic field of B \u2248 2 \u00d7 10^(12) G. The 3-79 keV luminosity of the system during the two epochs, assuming a nominal distance of 50 kpc, was 3.667 \u00b1 0.007 \u00d7 10^(38) erg s^(\u20131) and 3.983 \u00b1 0.007 \u00d7 10^(38) erg s^(\u20131). Both values are much higher than the critical luminosity of \u22481.5 \u00d7 10^(37) erg s^(\u20131), above which a radiation-dominated shock front may be expected. This adds a new object to the sparse set of three systems that have a cyclotron line observed at luminosities in excess of 10^(38) erg s^(\u20131). A broad (\u03c3 \u2248 0.45 keV) Fe emission line is observed in the spectrum at a central energy of 6.58_(-0.05)^(+0.05) keV in both epochs. The pulse profile of the pulsar was observed to be highly asymmetric with a sharply rising and slowly falling profile of the primary peak. We also observed minor variations in the cyclotron line energy and width as a function of the rotation phase.",
"date": "2014-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "795",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 154",
"id_number": "CaltechAUTHORS:20141202-071735385",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141202-071735385",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/Caltech/JPL"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
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},
"doi": "10.1088/0004-637X/795/2/154",
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"pub_year": "2014",
"author_list": "Tendulkar, Shriharsh P.; F\u00fcrst, Felix; et el."
},
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"eprint_id": 51809,
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"id": "Stern-D",
"name": {
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"given": "D."
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{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
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"name": {
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"given": "F. A."
},
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"title": "NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-selected Quasars at z ~ 2",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; quasars: individual (WISEA J181417.29+341224.8, WISEA J220743.82+193940.1, WISEA J235710.82+032802)",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 March 21; accepted 2014 July 23; published 2014 September 29.\n\nWe gratefully acknowledge the suggestions made by the anonymous referee, which have improved this manuscript. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.), and ST/J003697/1 (P.G.), and the Leverhulme Trust (D.M.A. and J.R.M.). R.J.A. was supported by Gemini-CONICYT grant number 32120009. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, and \"EMBIGGEN\" Anillo ACT1101) and Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" of Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo. A.C. acknowledges support from ASI-INAF grant I/37/012/0-011/13. R.C.H. acknowledges support from NASA through ADAP award NNX12AE38G and the National Science Foundation through grant number 1211096. M.K. acknowledges support from Swiss National Science Foundation (NSF) grant PP00P2 138979/1.\nFacilities: Keck (LRIS) - , NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Spitzer (IRAC) - Spitzer Space Telescope satellite, XMM - Newton X-Ray Multimirror Mission satellite, WISE - Wide-field Infrared Survey Explorer\n\nPublished - 0004-637X_794_2_102.pdf
Submitted - 1403.3078v1.pdf
",
"abstract": "We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected active galactic nuclei (AGNs) at z ~ 2 across a broad X-ray band (0.1 \u2212 79\u2009keV). The parent sample, selected to be faint or undetected in the WISE 3.4\u2009\u03bcm (W1) and 4.6\u2009\u03bcm (W2) bands but bright at 12\u2009\u03bcm (W3) and 22\u2009\u03bcm (W4), are extremely rare, with only ~1000 so-called \"W1W2-dropouts\" across the extragalactic sky. Optical spectroscopy reveals typical redshifts of z ~ 2 for this population, implying rest-frame mid-IR luminosities of \u03bdL_\u03bd(6\u2009\u03bcm) ~ 6 \u00d7 10^(46)\u2009erg\u2009s^(\u22121) and bolometric luminosities that can exceed L_bol ~ 10^(14)\u2009L_\u2609. The corresponding intrinsic, unobscured hard X-ray luminosities are L(2\u201310\u2009keV) ~ 4 \u00d7 10^(45)\u2009erg\u2009s^(\u22121) for typical quasar templates. These are among the most AGNs known, though the optical spectra rarely show evidence of a broad-line region and the selection criteria imply heavy obscuration even at rest-frame 1.5\u2009\u03bcm. We designed our X-ray observations to obtain robust detections for gas column densities NH \u2264 10^(24)\u2009cm^(\u22122). In fact, the sources prove to be fainter than these predictions. Two of the sources were observed by both NuSTAR and XMM-Newton, with neither being detected by NuSTAR (f_(3\u201324 keV) \u2272 10^(\u221213)\u2009erg\u2009cm^(\u22122)\u2009s^(\u22121)), and one being faintly detected by XMM-Newton (f_(0.5\u201310\u2009keV) ~ 5 \u00d7 10^(\u221215)\u2009erg\u2009cm^(\u22122)\u2009s^(\u22121)). A third source was observed only with XMM-Newton, yielding a faint detection (f_(0.5\u201310\u2009keV) ~ 7 \u00d7 10^(\u221215)\u2009erg\u2009cm^(\u22122)\u2009s^(\u22121)). The X-ray data imply these sources are either X-ray weak, or are heavily obscured by column densities NH \u2273 10^(24)\u2009cm^(\u22122). The combined X-ray and mid-IR analysis seems to favor this second possibility, implying the sources are extremely obscured, consistent with Compton-thick, luminous quasars. The discovery of a significant population of heavily obscured, extremely luminous AGNs would not conform to the standard paradigm of a receding torus, in which more luminous quasars are less likely to be obscured, and instead suggests that an additional source of obscuration is present in these extreme sources.",
"date": "2014-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "792",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 102",
"id_number": "CaltechAUTHORS:20141114-155415737",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141114-155415737",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/ K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "32120009"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "FONDECYT 1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo Project IC120009 \"Millennium Institute of Astrophysics (MAS)\""
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/37/012/0-011/13"
},
{
"agency": "NASA",
"grant_number": "NNX12AE38G"
},
{
"agency": "NSF",
"grant_number": "AST-1211096"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2 138979/1"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
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"doi": "10.1088/0004-637X/794/2/102",
"primary_object": {
"basename": "0004-637X_794_2_102.pdf",
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"basename": "1403.3078v1.pdf",
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],
"pub_year": "2014",
"author_list": "Stern, D.; Balokovi\u0107, M.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/cz3jk-9xn48",
"eprint_id": 51787,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:59:11",
"lastmod": "2023-10-18 17:10:11",
"type": "article",
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"creators": {
"items": [
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "E."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
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},
"title": "The NuSTAR View of Nearby Compton-thick Active Galactic Nuclei: The Cases of NGC 424, NGC 1320, and IC 2560",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: individual (NGC 424, NGC 1320, IC 2560); galaxies: nuclei; galaxies: Seyfert; techniques: spectroscopic; X-rays: galaxies",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2013 December 24; accepted 2014 August 14; published 2014 September 30.\n\nThe authors thank the anonymous referee for useful comments\nwhich have improved the manuscript. M.B. acknowledges\nsupport from the International Fulbright Science and\nTechnologyAward. A.C. acknowledges support fromASI-INAF\ngrant I/037/012/0-011/13. M.K. gratefully acknowledges\nsupport from Swiss National Science Foundation Grant\nPP00P2_138979/1. Thisworkwas supported under NASA contract\nNo. NNG08FD60C, and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by theASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research made use of the XRT Data Analysis Software (XRTDAS), archival data, software and on-line services provided by the ASDC. This research has made use of NASA's Astrophysics Data System.\nFacilities: NuSTAR, Swift, XMM-Newton\n\nPublished - 0004-637X_794_2_111.pdf
Submitted - 1408.5414v1.pdf
",
"abstract": "We present X-ray spectral analyses for three Seyfert 2 active galactic nuclei (AGNs), NGC 424, NGC 1320, and IC 2560, observed by NuSTAR in the 3\u201379 keV band. The high quality hard X-ray spectra allow detailed modeling of the Compton reflection component for the first time in these sources. Using quasi-simultaneous NuSTAR and Swift/XRT data, as well as archival XMM-Newton data, we find that all three nuclei are obscured by Compton-thick material with column densities in excess of ~5 \u00d7 10^(24) cm^(\u22122), and that their X-ray spectra above 3 keV are dominated by reflection of the intrinsic continuum on Compton-thick material. Due to the very high obscuration, absorbed intrinsic continuum components are not formally required by the data in any of the sources. We constrain the intrinsic photon indices and the column density of the reflecting medium through the shape of the reflection spectra. Using archival multi-wavelength data we recover the intrinsic X-ray luminosities consistent with the broadband spectral energy distributions. Our results are consistent with the reflecting medium being an edge-on clumpy torus with a relatively large global covering factor and overall reflection efficiency of the order of 1%. Given the unambiguous confirmation of the Compton-thick nature of the sources, we investigate whether similar sources are likely to be missed by commonly used selection criteria for Compton-thick AGNs, and explore the possibility of finding their high-redshift counterparts.",
"date": "2014-10-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "794",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 111",
"id_number": "CaltechAUTHORS:20141114-132213002",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141114-132213002",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/012/0-011/13"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2_138979/1"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
"items": [
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"id": "2014-27",
"name": "Space Radiation Laboratory"
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"doi": "10.1088/0004-637X/794/2/111",
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"pub_year": "2014",
"author_list": "Balokovi\u0107, M.; Harrison, F. A.; et el."
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"datestamp": "2023-08-22 13:55:36",
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{
"id": "Luo-Bin",
"name": {
"family": "Luo",
"given": "B."
},
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},
{
"id": "Brandt-W-N",
"name": {
"family": "Brandt",
"given": "W. N."
},
"orcid": "0000-0002-0167-2453"
},
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Teng-Stacy-H",
"name": {
"family": "Teng",
"given": "S. H."
}
},
{
"id": "Ar\u00e9valo-P",
"name": {
"family": "Ar\u00e9valo",
"given": "P."
}
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"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "F. E."
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"orcid": "0000-0002-8686-8737"
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"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
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"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
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"id": "Farrah-D",
"name": {
"family": "Farrah",
"given": "D."
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"orcid": "0000-0003-1748-2010"
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"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
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"orcid": "0000-0003-3105-2615"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
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{
"id": "Koss-M-J",
"name": {
"family": "Koss",
"given": "M."
},
"orcid": "0000-0002-7998-9581"
},
{
"id": "Ogle-P-M",
"name": {
"family": "Ogle",
"given": "P."
},
"orcid": "0000-0002-3471-981X"
},
{
"id": "Puccetti-S",
"name": {
"family": "Puccetti",
"given": "S."
},
"orcid": "0000-0002-2734-7835"
},
{
"id": "Saez-C",
"name": {
"family": "Saez",
"given": "C."
}
},
{
"id": "Scott-A-E",
"name": {
"family": "Scott",
"given": "A. E."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
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},
"title": "Weak Hard X-Ray Emission from Broad Absorption Line Quasars: Evidence for Intrinsic X-Ray Weakness",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars: absorption lines; quasars: emission lines; X-rays: galaxies",
"note": "\u00a9 2014. The American Astronomical Society. \n\nReceived 21 May 2014, accepted for publication 14 August 2014. Published 24 September 2014. \n\nWe acknowledge support from the California Institute of Technology (Caltech) NuSTAR subcontract 44A-1092750 (B.L., W.N.B.), NASA ADP grant NNX10AC99G (B.L., W.N.B.), NASA Postdoctoral Program (S.H.T.), CONICYT-Chile FONDECYT 1140304 (P.A.) and 1141218 (F.E.B.), \"EMBIGGEN\" Anillo ACT1101 (P.A., F.E.B.), Basal-CATA PFB-06/2007 (F.E.B.), Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" of Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo (F.E.B.), ASI/INAF grant I/037/12/0-011/13 (A.C.), STFC grant ST/J003697/1 (P.G.), and the Swiss National Science Foundation (NSF) grant PP00P2 138979/1 (M.K.). We thank K. Forster for help with the observation planning, and we thank T. Yaqoob for helpful discussions. We thank the referee for carefully reviewing the manuscript and providing helpful comments.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of NuSTARDAS jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA).\n\nPublished - 0004-637X_794_1_70.pdf
Submitted - 1408.3633v1.pdf
",
"abstract": "We report NuSTAR observations of a sample of six X-ray weak broad absorption line (BAL) quasars. These targets, at z = 0.148\u20131.223, are among the optically brightest and most luminous BAL quasars known at z < 1.3. However, their rest-frame \u22482 keV luminosities are 14 to >330 times weaker than expected for typical quasars. Our results from a pilot NuSTAR study of two low-redshift BAL quasars, a Chandra stacking analysis of a sample of high-redshift BAL quasars, and a NuSTAR spectral analysis of the local BAL quasar Mrk 231 have already suggested the existence of intrinsically X-ray weak BAL quasars, i.e., quasars not emitting X-rays at the level expected from their optical/UV emission. The aim of the current program is to extend the search for such extraordinary objects. Three of the six new targets are weakly detected by NuSTAR with \u227245 counts in the 3\u201324 keV band, and the other three are not detected. The hard X-ray (8\u201324 keV) weakness observed by NuSTAR requires Compton-thick absorption if these objects have nominal underlying X-ray emission. However, a soft stacked effective photon index (\u0393_eff \u2248 1.8) for this sample disfavors Compton-thick absorption in general. The uniform hard X-ray weakness observed by NuSTAR for this and the pilot samples selected with <10 keV weakness also suggests that the X-ray weakness is intrinsic in at least some of the targets. We conclude that the NuSTAR observations have likely discovered a significant population (\u227333%) of intrinsically X-ray weak objects among the BAL quasars with significantly weak <10 keV emission. We suggest that intrinsically X-ray weak quasars might be preferentially observed as BAL quasars.",
"date": "2014-10-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "794",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 70",
"id_number": "CaltechAUTHORS:20141106-132623873",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141106-132623873",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1140304"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2 138979"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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"items": [
{
"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
}
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},
"doi": "10.1088/0004-637X/794/1/70",
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"pub_year": "2014",
"author_list": "Luo, B.; Brandt, W. N.; et el."
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{
"id": "Ballantyne-D-R",
"name": {
"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
"id": "Bollenbacher-J-M",
"name": {
"family": "Bollenbacher",
"given": "J. M."
}
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{
"id": "Brenneman-L-W",
"name": {
"family": "Brenneman",
"given": "L. W."
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
},
"orcid": "0000-0003-0476-6647"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
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{
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"name": {
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"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
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"name": {
"family": "Lohfink",
"given": "A. M."
}
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"name": {
"family": "Marinucci",
"given": "A."
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"name": {
"family": "Markwardt",
"given": "C. B."
},
"orcid": "0000-0001-9803-3879"
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{
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"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Reveals the Comptonizing Corona of the Broad-line Radio Galaxy 3C 382",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; galaxies: active; galaxies: individual (3C 382); galaxies: nuclei; X-rays: galaxies",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 May 13; accepted 2014 August 14; published 2014 September 24. \n\nWe thank the referee for a helpful report that improved the\npaper. This work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by theASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of data, software and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. D.R.B.\nacknowledges support from NASA ADAP grant NNX13AI47G\nand NSF award AST 1008067. A.M. acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n.312789. M.B. acknowledges support from the International Fulbright Science and Technology Award.\n\nPublished - 0004-637X_794_1_62.pdf
Submitted - 1408.5281v1.pdf
",
"abstract": "Broad-line radio galaxies (BLRGs) are active galactic nuclei that produce powerful, large-scale radio jets, but appear as Seyfert 1 galaxies in their optical spectra. In the X-ray band, BLRGs also appear like Seyfert galaxies, but with flatter spectra and weaker reflection features. One explanation for these properties is that the X-ray continuum is diluted by emission from the jet. Here, we present two NuSTAR observations of the BLRG 3C 382 that show clear evidence that the continuum of this source is dominated by thermal Comptonization, as in Seyfert 1 galaxies. The two observations were separated by over a year and found 3C 382 in different states separated by a factor of 1.7 in flux. The lower flux spectrum has a photon-index of \u0393 = 1.68^)+0.03_(\u22120.02), while the photon-index of the higher flux spectrum is \u0393 = 1.78^(+0.02)_(\u22120.03). Thermal and anisotropic Comptonization models provide an excellent fit to both spectra and show that the coronal plasma cooled from kT_e = 330 \u00b1 30 keV in the low flux data to 231^(+50)_(\u221288) keV in the high flux observation. This cooling behavior is typical of Comptonizing corona in Seyfert galaxies and is distinct from the variations observed in jet-dominated sources. In the high flux observation, simultaneous Swift data are leveraged to obtain a broadband spectral energy distribution and indicates that the corona intercepts ~10% of the optical and ultraviolet emitting accretion disk. 3C 382 exhibits very weak reflection features, with no detectable relativistic Fe K\u03b1 line, that may be best explained by an outflowing corona combined with an ionized inner accretion disk.",
"date": "2014-10-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "794",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 62",
"id_number": "CaltechAUTHORS:20141106-132347774",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141106-132347774",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX13AI47G"
},
{
"agency": "NSF",
"grant_number": "AST-1008067"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/ 12/0-011/13"
},
{
"agency": "European Union",
"grant_number": "FP7/2007-2013"
},
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
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"items": [
{
"id": "2014-29",
"name": "Space Radiation Laboratory"
}
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},
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{
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"doi": "10.1088/0004-637X/794/1/62",
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"pub_year": "2014",
"author_list": "Ballantyne, D. R.; Bollenbacher, J. M.; et el."
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"items": [
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "D."
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
},
{
"id": "Beloborodov-A",
"name": {
"family": "Beloborodov",
"given": "A."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
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"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
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"name": {
"family": "Craig",
"given": "W. W."
}
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{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Hornschemeier-A-E",
"name": {
"family": "Hornschemeier",
"given": "A."
},
"orcid": "0000-0001-8667-2681"
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "V."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Kulkarni-S-R",
"name": {
"family": "Kulkarni",
"given": "S. R."
},
"orcid": "0000-0001-5390-8563"
},
{
"id": "Maccarone-T-J",
"name": {
"family": "Maccarone",
"given": "T."
},
"orcid": "0000-0003-0976-4755"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
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"name": {
"family": "Rana",
"given": "V."
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"orcid": "0000-0003-1703-8796"
},
{
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"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tendulkar-S-P",
"name": {
"family": "Tendulkar",
"given": "S. P."
},
"orcid": "0000-0003-2548-2926"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "J."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Webb-N-A",
"name": {
"family": "Webb",
"given": "N. A."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "An ultraluminous X-ray source powered by an accreting neutron star",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 Macmillan Publishers Limited.\n\nReceived 24 June; accepted 6 August 2014. Published online 08 October 2014.\n\nThis work was supported by NASA (grant no. NNG08FD60C), and\nmade use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a\nproject led by Caltech, managed by the Jet Propulsion Laboratory and funded by NASA.\nWe thank the NuSTAR operations, software and calibration teams for support with\nexecution and analysis of these observations. This work made use of data supplied by\nthe UK Swift Science Data Centre at the University of Leicester. M.B. thanks the Centre\nNational d'Etudes Spatiales (CNES) and the Centre National de la Recherche\nScientifique (CNRS) for support. Line plots were done using Veusz software by\nJ. Sanders.\n\nSubmitted - 1410.3590.pdf
Supplemental Material - nature13791-sf1.jpg
Supplemental Material - nature13791-sf2.jpg
Supplemental Material - nature13791-st1.jpg
Supplemental Material - nature13791-st2.jpg
Supplemental Material - nature13791-st3.jpg
Supplemental Material - nature13791-st4.jpg
",
"abstract": "The majority of ultraluminous X-ray sources are point sources that are spatially offset from the nuclei of nearby galaxies and whose X-ray luminosities exceed the theoretical maximum for spherical infall (the Eddington limit) onto stellar-mass black holes. Their X-ray luminosities in the 0.5\u201310 kiloelectronvolt energy band range from 10^(39) to 10^(41) ergs per second. Because higher masses imply less extreme ratios of the luminosity to the isotropic Eddington limit, theoretical models have focused on black hole rather than neutron star systems. The most challenging sources to explain are those at the luminous end of the range (more than 1040 ergs per second), which require black hole masses of 50\u2013100 times the solar value or significant departures from the standard thin disk accretion that powers bright Galactic X-ray binaries, or both. Here we report broadband X-ray observations of the nuclear region of the galaxy M82 that reveal pulsations with an average period of 1.37 seconds and a 2.5-day sinusoidal modulation. The pulsations result from the rotation of a magnetized neutron star, and the modulation arises from its binary orbit. The pulsed flux alone corresponds to an X-ray luminosity in the 3\u201330 kiloelectronvolt range of 4.9 \u00d7 10^(39) ergs per second. The pulsating source is spatially coincident with a variable source that can reach an X-ray luminosity in the 0.3\u201310 kiloelectronvolt range of 1.8 \u00d7 10^(40) ergs per second. This association implies a luminosity of about 100 times the Eddington limit for a 1.4-solar-mass object, or more than ten times brighter than any known accreting pulsar. This implies that neutron stars may not be rare in the ultraluminous X-ray population, and it challenges physical models for the accretion of matter onto magnetized compact objects.",
"date": "2014-10-09",
"date_type": "published",
"publication": "Nature",
"volume": "514",
"number": "7521",
"publisher": "Nature Publishing Group",
"pagerange": "202-204",
"id_number": "CaltechAUTHORS:20140804-165311189",
"issn": "0028-0836",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140804-165311189",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-25",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
},
{
"id": "Division-of-Geological-and-Planetary-Sciences"
}
]
},
"doi": "10.1038/nature13791",
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],
"pub_year": "2014",
"author_list": "Bachetti, M.; Harrison, F. A.; et el."
},
{
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"eprint_id": 50429,
"eprint_status": "archive",
"datestamp": "2023-08-20 03:14:54",
"lastmod": "2023-10-17 23:48:14",
"type": "article",
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"creators": {
"items": [
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "Eric V."
},
"orcid": "0000-0003-3847-3957"
},
{
"id": "Dufour-F",
"name": {
"family": "Dufour",
"given": "Francois"
}
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "Victoria M."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Halpern-J-P",
"name": {
"family": "Halpern",
"given": "Jules P."
}
},
{
"id": "Beloborodov-A-M",
"name": {
"family": "Beloborodov",
"given": "Andrei M."
}
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kouveliotou-C",
"name": {
"family": "Kouveliotou",
"given": "Chryssa"
},
"orcid": "0000-0003-1443-593X"
},
{
"id": "Pivovaroff-M-J",
"name": {
"family": "Pivovaroff",
"given": "Michael J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A broadband X-ray study of the Geminga pulsar with NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "X-rays: individual (Geminga)",
"note": "\u00a9 2014 American Astronomical Society. Received 2014 April 21; accepted 2014 July 24; published 2014 September 10. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). E.V.G. acknowledges support from NASA/Fermi grant NNX12AO89G and NASA/Chandra grant G03-14066X. V.M.K. acknowledges support from an NSERC\nDiscovery Grant, the FQRNT Centre de Recherche Astrophysique\ndu Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. acknowledges\nthe support by NASA grants NNX10AI72G and NNX13AI34G.\n\nPublished - 0004-637X_793_2_88.pdf
Submitted - 1408.1644v1.pdf
",
"abstract": "We report on the first hard X-ray detection of the Geminga pulsar above 10 keV using a 150 ks observation with the Nuclear Spectroscopic Telescope Array (NuSTAR) observatory. The double-peaked pulse profile of non-thermal emission seen in the soft X-ray band persists at higher energies. Broadband phase-integrated spectra over the 0.2-20 keV band with NuSTAR and archival XMM-Newton data do not fit to a conventional two-component model of a blackbody plus power law, but instead exhibit spectral hardening above ~5 keV. We find that two spectral models fit the data well: (1) a blackbody (kT_1 ~ 42 eV) with a broken power law (\u0393_1 ~ 2.0, \u0393_2 ~ 1.4 and E_(break) ~ 3.4 keV) and (2) two blackbody components (kT_1 ~ 44 eV and kT_2 ~ 195 eV) with a power-law component (\u0393 ~ 1.7). In both cases, the extrapolation of the Rayleigh-Jeans tail of the thermal component is consistent with the UV data, while the non-thermal component overpredicts the near-infrared data, requiring a spectral flattening at E ~ 0.05-0.5 keV. While strong phase variation of the power-law index is present below ~5 keV, our phase-resolved spectroscopy with NuSTAR indicates that another hard non-thermal component with \u0393 ~ 1.3 emerges above ~5 keV. The spectral hardening in non-thermal X-ray emission as well as spectral flattening between the optical and X-ray bands argue against the conjecture that a single power law may account for multi-wavelength non-thermal spectra of middle-aged pulsars.",
"date": "2014-10-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "793",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 88",
"id_number": "CaltechAUTHORS:20141016-074136515",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141016-074136515",
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"author_list": "Mori, Kaya; Gotthelf, Eric V.; et el."
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"title": "High-Energy X-ray Imaging of the Pulsar Wind Nebula MSH 15-52: Constraints on Particle Acceleration and Transport",
"ispublished": "pub",
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"keywords": "ISM: individual objects (G320.4-1.2); ISM: jets and outflows; ISM: supernova remnants; pulsars: individual (PSR B1509-58); stars: neutron; X-rays: ISM",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 June 16; accepted 2014 July 31; published 2014 September 10. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V.M.K. acknowledges support from an NSERC Discovery Grant and Accelerator Supplement, the FQRNT Centre de Recherche Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology.\n\nPublished - 0004-637X_793_2_90.pdf
Submitted - 1408.0174v1.pdf
",
"abstract": "We present the first images of the pulsar wind nebula (PWN) MSH 15\u201352 in the hard X-ray band (\u22738 keV), as measured with the Nuclear Spectroscopic Telescope Array (NuSTAR). Overall, the morphology of the PWN as measured by NuSTAR in the 3-7 keV band is similar to that seen in Chandra high-resolution imaging. However, the spatial extent decreases with energy, which we attribute to synchrotron energy losses as the particles move away from the shock. The hard-band maps show a relative deficit of counts in the northern region toward the RCW 89 thermal remnant, with significant asymmetry. We find that the integrated PWN spectra measured with NuSTAR and Chandra suggest that there is a spectral break at 6 keV, which may be explained by a break in the synchrotron-emitting electron distribution at ~200 TeV and/or imperfect cross calibration. We also measure spatially resolved spectra, showing that the spectrum of the PWN softens away from the central pulsar B1509\u201358, and that there exists a roughly sinusoidal variation of spectral hardness in the azimuthal direction. We discuss the results using particle flow models. We find non-monotonic structure in the variation with distance of spectral hardness within 50'' of the pulsar moving in the jet direction, which may imply particle and magnetic-field compression by magnetic hoop stress as previously suggested for this source. We also present two-dimensional maps of spectral parameters and find an interesting shell-like structure in the N_H map. We discuss possible origins of the shell-like structure and their implications.",
"date": "2014-10-01",
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"publication": "Astrophysical Journal",
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"title": "NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-selected Quasars at z ~ 2",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014. The American Astronomical Society. \n\nPublished 2014 September 29.\n\nWe gratefully acknowledge the suggestions made by the\nanonymous referee, which have improved this manuscript. This\nwork was supported under NASA Contract No. NNG08FD60C,\nand made use of data from the NuSTAR mission, a project\nled by the California Institute of Technology, managed by\nthe Jet Propulsion Laboratory, and funded by the National\nAeronautics and Space Administration. We thank the NuSTAR\nOperations, Software, and Calibration teams for support\nwith the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science\nData Center (ASDC, Italy) and the California Institute of\nTechnology (USA). This publication makes use of data products\nfrom the Wide-field Infrared Survey Explorer, which is\na joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.), and ST/J003697/1 (P.G.), and the Leverhulme Trust (D.M.A. and J.R.M.). R.J.A. was supported by Gemini-CONICYT\ngrant number 32120009. F.E.B. acknowledges support from\nCONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, and \"EMBIGGEN\" Anillo ACT1101) and Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" of\nIniciativa Cient\u00b4\u0131fica Milenio del Ministerio de Econom\u00b4\u0131a, Fomento y Turismo. A.C. acknowledges support from ASI-INAF\ngrant I/37/012/0-011/13. R.C.H. acknowledges support from\nNASA through ADAP award NNX12AE38G and the National\nScience Foundation through grant number 1211096. M.K.\nacknowledges support from Swiss National Science Foundation\n(NSF) grant PP00P2 138979/1.\n\nPublished - 2014-28.pdf
",
"abstract": "We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected active galactic nuclei (AGNs) at z ~ 2 across a broad X-ray band (0.1 - 79 keV). The parent sample, selected to be faint or undetected in the WISE 3.4 \u03bcm (W1) and 4.6 \u03bcm (W2) bands but bright at 12 \u03bcm (W3) and 22 \u03bcm (W4), are extremely rare, with only ~1000 so-called \"W1W2-dropouts\" across the extragalactic sky. Optical spectroscopy reveals typical redshifts of z ~ 2 for this population, implying rest-frame mid-IR luminosities of \u03bdL \u03bd(6 \u03bcm) ~ 6 \u00d7 1046 erg s^-1 and bolometric luminosities that can exceed L bol ~ 1014 L_\u2299. The corresponding intrinsic, unobscured hard X-ray luminosities are L(2-10 keV) ~ 4 \u00d7 1045 erg s-1 for typical quasar templates. These are among the most AGNs known, though the optical spectra rarely show evidence of a broad-line region and the selection criteria imply heavy obscuration even at rest-frame 1.5 \u03bcm. We designed our X-ray observations to obtain robust detections for gas column densities N H <= 1024 cm-2. In fact, the sources prove to be fainter than these predictions. Two of the sources were observed by both NuSTAR and XMM-Newton, with neither being detected by NuSTAR (f 3-24 keV <~ 10-13 erg cm^(-2)s^(-1), and one being faintly detected by XMM-Newton (f 0.5-10 keV ~ 5 \u00d7 10-15 erg cm-2 s-1). A third source was observed only with XMM-Newton, yielding a faint detection (f 0.5-10 keV ~ 7 \u00d7 10-15 erg cm-2 s-1). The X-ray data imply these sources are either X-ray weak, or are heavily obscured by column densities N H >~ 1024 cm-2. The combined X-ray and mid-IR analysis seems to favor this second possibility, implying the sources are extremely obscured, consistent with Compton-thick, luminous quasars. The discovery of a significant population of heavily obscured, extremely luminous AGNs would not conform to the standard paradigm of a receding torus, in which more luminous quasars are less likely to be obscured, and instead suggests that an additional source of obscuration is present in these extreme sources.",
"date": "2014-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "79",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art No.102",
"id_number": "CaltechAUTHORS:20160824-144504856",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160824-144504856",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
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},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "32120009"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
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{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
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{
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"grant_number": "EMBIGGEN Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio (ICM) del Ministerio de Econom\u00eda",
"grant_number": "IC120009"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/37/012/0-011/13"
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{
"agency": "NASA",
"grant_number": "NNX12AE38G"
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{
"agency": "NSF",
"grant_number": "1211096"
},
{
"agency": "Swiss Science Foundation (SNSF)",
"grant_number": "PP00P2138979/1"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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"author_list": "Stern, Daniel; Lansbury, G. B.; et el."
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"given": "A. C."
},
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},
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"name": {
"family": "Fuerst",
"given": "F."
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"name": {
"family": "Hailey",
"given": "C. J."
}
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"name": {
"family": "Madsen",
"given": "K. K."
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"family": "Parker",
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},
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"name": {
"family": "Ptak",
"given": "A."
},
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"name": {
"family": "Rana",
"given": "V."
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},
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"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Webb-N-A",
"name": {
"family": "Webb",
"given": "N."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Broadband X-Ray Spectra of the Ultraluminous X-Ray Source Holmberg IX X-1 Observed with NuSTAR, XMM-Newton, and Suzaku",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; X-rays: binaries; X-rays: individual (Holmberg IX X-1)",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 February 11; accepted 2014 July 7; published 2014 August 29. \n\nThe authors would like to thank the referee for providing\nuseful feedback, which helped to improve the manuscript. This research has made use of data obtained with the NuSTAR\nmission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and Suzaku, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research was supported under NASA grant No. NNG08FD60C, and has made use of the NuSTAR Data Analysis Software (NUSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). We also made use of the NASA/IPAC Extragalactic Database (NED), which is operated by JPL, Caltech, under contract with NASA. Many of the figures included in this work have been produced with the Veusz plotting package: http://home.gna.org/veusz, written and maintained by Jeremy Sanders. DB and MB are grateful to the Centre National d'Etudes Spatiales (CNES) for funding their activities. \n\nFacilites: NuSTAR, XMM, Suzaku\n\nPublished - 0004-637X_793_1_21.pdf
Submitted - 1402.2992v3.pdf
",
"abstract": "We present results from the coordinated broadband X-ray observations of the extreme ultraluminous X-ray source Holmberg IX X-1 performed by NuSTAR, XMM-Newton, and Suzaku in late 2012. These observations provide the first high-quality spectra of Holmberg IX X-1 above 10 keV to date, extending the X-ray coverage of this remarkable source up to ~30 keV. Broadband observations were undertaken at two epochs, between which Holmberg IX X-1 exhibited both flux and strong spectral variability, increasing in luminosity from L_X = (1.90 \u00b1 0.03) \u00d7 10^(40) erg s^(\u20131) to L_X = (3.35 \u00b1 0.03) \u00d7 10^(40) erg s^(\u20131). Neither epoch exhibits a spectrum consistent with emission from the standard low/hard accretion state seen in Galactic black hole binaries, which would have been expected if Holmberg IX X-1 harbors a truly massive black hole accreting at substantially sub-Eddington accretion rates. The NuSTAR data confirm that the curvature observed previously in the 3-10 keV bandpass does represent a true spectral cutoff. During each epoch, the spectrum appears to be dominated by two optically thick thermal components, likely associated with an accretion disk. The spectrum also shows some evidence for a nonthermal tail at the highest energies, which may further support this scenario. The available data allow for either of the two thermal components to dominate the spectral evolution, although both scenarios require highly nonstandard behavior for thermal accretion disk emission.",
"date": "2014-09-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "793",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 21",
"id_number": "CaltechAUTHORS:20141003-071241370",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141003-071241370",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
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"pub_year": "2014",
"author_list": "Walton, D. J.; Harrison, F. A.; et el."
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"id": "Puccetti-S",
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{
"id": "Comastri-A",
"name": {
"family": "Comastri",
"given": "Andrea"
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{
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"family": "Hailey",
"given": "Charles J."
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"family": "Koss",
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"given": "George B."
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"name": {
"family": "Walton",
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},
"title": "The Variable Hard X-Ray Emission of NGC 4945 as Observed by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 4945); X-rays: galaxies",
"note": "\u00a9 2014 American Astronomical Society. Received 2014 April 15; accepted 2014 July 14; published 2014 September 2.\n\nThis work was supported under NASA Contract NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support\nwith the execution and analysis of these observations.\nThis research has made use of the NuSTAR Data Analysis\nSoftware (NuSTARDAS) jointly developed by the ASI Science\nData Center (ASDC, Italy) and the California Institute\nof Technology (USA). S.P., A.C., F.F., and G.M. acknowledge\nsupport from the ASI/INAF grant I/037/12/0\u2013011/13. A.C.\nacknowledges the Caltech Kingsley visitor program. P.G. acknowledges support from STFC (grant reference ST/J003697/\n1). G.B.L. acknowledges support from STFC (grant reference\nST/K501979/1). D.M.A. acknowledges support from STFC\n(grant reference ST/I001573/1) and from the Leverhulme\nTrust. P.A. acknowledges financial support from Fondecyt grant 11100449 and Anillo ACT1101. G.R. acknowledges financial support from grant NASA GO3\u201314109X. M.K. gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. W.N.B. and B.L. acknowledge support from California Institute of Technology NuSTAR subcontract 44A\u20131092750 and NASA ADP Grant NNX10AC99G. F.E.B. acknowledges support from Basal\u2013CATA PFB\u201306/2007, CONICYT\u2013Chile (grants FONDECYT 1101024 and\n\"EMBIGGEN\" Anillo ACT1101), and Project IC120009\n\"Millennium Institute of Astrophysics (MAS)\" of Iniciativa\nCient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y\nTurismo. S.P. is grateful to Tahir Yaqoob for useful discussions on the mytorus model.\n\nPublished - 0004-637X_793_1_26.pdf
Submitted - 1407.3974v1.pdf
",
"abstract": "We present a broadband (~0.5-79 keV) spectral and temporal analysis of multiple NuSTAR observations combined with archival Suzaku and Chandra data of NGC 4945, the brightest extragalactic source at 100 keV. We observe hard X-ray (>10 keV) flux and spectral variability, with flux variations of a factor of two on timescales of 20 ks. A variable primary continuum dominates the high-energy spectrum (>10 keV) in all states, while the reflected/scattered flux that dominates at E <10 keV stays approximately constant. From modeling the complex reflection/transmission spectrum, we derive a Compton depth along the line of sight of \u03c4_(Thomson) ~ 2.9, and a global covering factor for the circumnuclear gas of ~0.15. This agrees with the constraints derived from the high-energy variability, which implies that most of the high-energy flux is transmitted rather than Compton-scattered. This demonstrates the effectiveness of spectral analysis at constraining the geometric properties of the circumnuclear gas, and validates similar methods used for analyzing the spectra of other bright, Compton-thick active galactic nuclei (AGNs). The lower limits on the e-folding energy are between 200 and 300 keV, consistent with previous BeppoSAX, Suzaku, and Swift Burst Alert Telescope observations. The accretion rate, estimated from the X-ray luminosity and assuming a bolometric correction typical of type 2 AGN, is in the range ~0.1-0.3 \u03bb_(Edd) depending on the flux state. The substantial observed X-ray luminosity variability of NGC 4945 implies that large errors can arise from using single-epoch X-ray data to derive L/L_(Edd) values for obscured AGNs.",
"date": "2014-09-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "793",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 26",
"id_number": "CaltechAUTHORS:20141003-074456235",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141003-074456235",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0\u2013011/13"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/ 1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "11100449"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "NASA",
"grant_number": "GO3\u201314109X"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2_138979/1"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1101024"
},
{
"agency": "Anillo project",
"grant_number": "ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo Millennium Institute of Astrophysics (MAS)",
"grant_number": "IC120009"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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},
"doi": "10.1088/0004-637X/793/1/26",
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"pub_year": "2014",
"author_list": "Puccetti, Simonetta; Comastri, Andrea; et el."
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"family": "Dauser",
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"given": "C. J."
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"family": "Kara",
"given": "E."
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"name": {
"family": "Komossa",
"given": "S."
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"id": "Marinucci-A",
"name": {
"family": "Marinucci",
"given": "A."
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"name": {
"family": "Miller",
"given": "J. M."
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"id": "Risaliti-G",
"name": {
"family": "Risaliti",
"given": "G."
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"name": {
"family": "Stern",
"given": "D."
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"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
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"name": {
"family": "Zhang",
"given": "W. W."
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},
"title": "The NuSTAR spectrum of Mrk 335: extreme relativistic effects within two gravitational radii of the event horizon?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active, galaxies: individual: Mrk 335, galaxies: Seyfert",
"note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 June 20. Received 2014 June 10; in original form 2013 October 17. First published online July 25, 2014. This work is based on observations made by the NuSTAR mission, a project led by the California Institute of Astronomy, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NUSTARDAS, jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). At Penn State Swift is supported by NASA contract NAS5-00136. MLP acknowledges financial support from the Science and Technology Facilities Council (STFC). ACF thanks the Royal Society for support. AM and GM acknowledge financial support\nfrom Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. DRW is supported by a CITA National Fellowship. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789.\n\nPublished - MNRAS-2014-Parker-1723-32.pdf
Submitted - 1407.8223v1.pdf
",
"abstract": "We present 3\u201350\u2009keV NuSTAR observations of the active galactic nuclei Mrk 335 in a very low flux state. The spectrum is dominated by very strong features at the energies of the iron line at 5\u20137\u2009keV and Compton hump from 10\u201330\u2009keV. The source is variable during the observation, with the variability concentrated at low energies, which suggesting either a relativistic reflection or a variable absorption scenario. In this work, we focus on the reflection interpretation, making use of new relativistic reflection models that self consistently calculate the reflection fraction, relativistic blurring and angle-dependent reflection spectrum for different coronal heights to model the spectra. We find that the spectra can be well fitted with relativistic reflection, and that the lowest flux state spectrum is described by reflection alone, suggesting the effects of extreme light-bending occurring within \u223c2 gravitational radii (R_G) of the event horizon. The reflection fraction decreases sharply with increasing flux, consistent with a point source moving up to above 10 R_G as the source brightens. We constrain the spin parameter to greater than 0.9 at the 3\u03c3 confidence level. By adding a spin-dependent upper limit on the reflection fraction to our models, we demonstrate that this can be a powerful way of constraining the spin parameter, particularly in reflection dominated states. We also calculate a detailed emissivity profile for the iron line, and find that it closely matches theoretical predictions for a compact source within a few R_G of the black hole.",
"date": "2014-09-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "443",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1723-1732",
"id_number": "CaltechAUTHORS:20140912-074949567",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140912-074949567",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NAS5-00136"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Royal Society"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/ 12/0-011/13"
},
{
"agency": "CITA National Fellowship"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"other_numbering_system": {
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"doi": "10.1093/mnras/stu1246",
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}
],
"pub_year": "2014",
"author_list": "Parker, M. L.; Wilkins, D. R.; et el."
},
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"items": [
{
"id": "Gandhi-Poshak",
"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
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},
"title": "NuSTAR Unveils a Compton-thick Type 2 Quasar in Mrk 34",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; X-rays: galaxies; X-rays: individual (Mrk 34)",
"note": "Grant and fellowship acknowledgments: STFC ST/J003697/1\n(P.G.), ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and\nA.D.M.), Leverhulme Trust (D.M.A.), NASA Postdoctoral Program (S.H.T), ASI-INAF grant (A.C.), Anillo ACT1101 and\nFONDECYT 1140304 (P.A.), International Fulbright Science\nand Technology Award (M.B.), and Swiss National Science\nFoundation (NSF) grant PP00P2 138979/1 (M.K.). In addition,\nF.A.H. acknowledges support from a Durham University\nCOFUND fellowship, and F. E. B. acknowledges support\nfrom Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT\n1141218 and \"EMBIGGEN\" Anillo ACT1101) Project IC120009 \"Millennium Institute of Astrophysics (MAS)\" funded by the Iniciativa Cient\u00b4\u0131fica Milenio del Ministerio de Econom\u00b4\u0131a, Fomento y Turismo. The authors thank Fred K.Y. Lo for megamaser discussions, and the referee for the report.\nP.G. thanks James R. Mullaney and Chris M. Harrison\nfor discussions. P.G. is also grateful to Matteo Guainazzi for his comments and insights on the origin of the soft X-ray spectrum. NuSTAR is a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). The NuSTAR Operations, Software, and Calibration teams are acknowledged for support with these observations. This research has made use of the NuSTAR Data Analysis Software (nustardas) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute\nof Technology (USA). This work has made use of data from\nXMM-Newton and the Sloan Digital Sky Survey. Figure 5 is\nbased upon data from with the NASA/ESA Hubble Space Telescope and obtained from the Hubble Legacy Archive. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by JPL, Caltech, under contract with NASA.\nFacilities: NuSTAR, XMM-Newton, Sloan, WISE, HST, Swift, CXO\n\nPublished - 0004-637X_792_2_117.pdf
Submitted - 1407.1844v1.pdf
Erratum - 0004-637X_794_2_176.pdf
",
"abstract": "We present Nuclear Spectroscopic Telescope Array (NuSTAR) 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and a strong Fe K\u03b1 fluorescence line with equivalent width >1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line of sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column and shows that N H lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L 2-10 ~ 1044 erg s\u20131, in contrast to previous low-energy X-ray measurements where L 2-10 lsim 1043 erg s\u20131 (i.e., X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk 34 is thus a \"gold standard\" CT QSO2 and is the nearest non-merging system in this class, in contrast to the other local CT quasar NGC 6240, which is currently undergoing a major merger coupled with strong star formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk 34 is high enough to potentially power the total infrared luminosity. X-ray spectral fitting also shows that thermal emission related to star formation is unlikely to drive the observed bright soft component below ~3 keV, favoring photoionization instead.",
"date": "2014-09-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "792",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 117",
"id_number": "CaltechAUTHORS:20140925-140514974",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140925-140514974",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1140304"
},
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2 138979/1"
},
{
"agency": "Durham University"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "EMBIGGEN Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
}
]
},
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"doi": "10.1088/0004-637X/792/2/117",
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"basename": "0004-637X_792_2_117.pdf",
"url": "https://authors.library.caltech.edu/records/m36av-6tb20/files/0004-637X_792_2_117.pdf"
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],
"pub_year": "2014",
"author_list": "Gandhi, P.; Balokovi\u0107, M.; et el."
},
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"datestamp": "2023-08-22 13:38:21",
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"items": [
{
"id": "Bellm-E-C",
"name": {
"family": "Bellm",
"given": "Eric C."
},
"orcid": "0000-0001-8018-5348"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "F\u00fcrst",
"given": "Felix"
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Pottschmidt-K",
"name": {
"family": "Pottschmidt",
"given": "Katja"
},
"orcid": "0000-0002-4656-6881"
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{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
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{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
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{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "Deepto"
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Confirmation of a High Magnetic Field in GRO J1008-57",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (GRO J1008\u201357); stars: neutron; X-rays: binaries",
"note": "\u00a9 2014 American Astronomical Society. Received 2014 March 20; accepted 2014 July 24; published 2014 August 21. \n\nThis work was supported under NASA contract No.\nNNG08FD60C and uses data from the NuSTAR mission, a\nproject led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the\nNuSTAR Operations team for executing the ToO observation\nand the Software and Calibration teams for analysis support.\nThis research has used the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J.W. acknowledges partial support from Deutsches Zentrum f\u00fcr Luftund Raumfahrt grant 50 OR 1113.\nFacilities: NuSTAR, Swift, Suzaku\n\nPublished - 0004-637X_792_2_108.pdf
Submitted - 1403.5249v1.pdf
",
"abstract": "GRO J1008\u201357 is a high-mass X-ray binary for which several claims of a cyclotron resonance scattering feature near 80 keV have been reported. We use NuSTAR, Suzaku, and Swift data from its giant outburst of 2012 November to confirm the existence of the 80 keV feature and perform the most sensitive search to date for cyclotron scattering features at lower energies. We find evidence for a 78^(+3)_(-2) keV line in the NuSTAR and Suzaku data at >4\u03c3 significance, confirming the detection using Suzaku alone by Yamamoto et al. A search of both the phase-averaged and phase-resolved data rules out a fundamental at lower energies with optical depth larger than 5% of the 78 keV line. These results indicate that GRO J1008\u201357 has a magnetic field of 6.7 \u00d7 10^(12)(1 + z) G, the highest among known accreting pulsars.",
"date": "2014-09-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "792",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 108",
"id_number": "CaltechAUTHORS:20140925-112538542",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140925-112538542",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luftund Raumfahrt (DLR)",
"grant_number": "50 OR 1113"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-36",
"name": "Space Radiation Laboratory"
}
]
},
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"doi": "10.1088/0004-637X/792/2/108",
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"pub_year": "2014",
"author_list": "Bellm, Eric C.; F\u00fcrst, Felix; et el."
},
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"eprint_id": 50024,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:35:44",
"lastmod": "2023-10-17 22:27:04",
"type": "article",
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"creators": {
"items": [
{
"id": "Wik-D-R",
"name": {
"family": "Wik",
"given": "Daniel R."
},
"orcid": "0000-0001-8952-676X"
},
{
"id": "Hornstrup-A",
"name": {
"family": "Hornstrup",
"given": "A."
}
},
{
"id": "Molendi-S",
"name": {
"family": "Molendi",
"given": "S."
}
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Zoglauer-A-C",
"name": {
"family": "Zoglauer",
"given": "A."
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Gastaldello-F",
"name": {
"family": "Gastaldello",
"given": "F."
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Westergaard-N-J",
"name": {
"family": "Westergaard",
"given": "N. J."
}
},
{
"id": "Ferreira-D-D-M",
"name": {
"family": "Ferreira",
"given": "D. D. M."
}
},
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "T."
}
},
{
"id": "Pedersen-K",
"name": {
"family": "Pedersen",
"given": "K."
}
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Observations of the Bullet Cluster: Constraints on Inverse Compton Emission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: clusters: general; galaxies: clusters: individual (Bullet cluster); intergalactic medium; magnetic fields; radiation mechanisms: non-thermal; X-rays: galaxies: clusters",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 March 11; accepted 2014 July 17; published 2014 August 13. \n\nThis research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with the National Aeronautics and Space Administration (NASA) and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors wish to thank Maxim Markevitch for providing a 0.5 Ms Chandra image of the Bullet cluster to confirm the cluster region lacks bright point sources and the referee for helpful comments that improved the paper.\n\nPublished - 0004-637X_792_1_48.pdf
Submitted - 1403.2722v1.pdf
",
"abstract": "The search for diffuse non-thermal inverse Compton (IC) emission from galaxy clusters at hard X-ray energies has been undertaken with many instruments, with most detections being either of low significance or controversial. Because all prior telescopes sensitive at E > 10 keV do not focus light and have degree-scale fields of view, their backgrounds are both high and difficult to characterize. The associated uncertainties result in lower sensitivity to IC emission and a greater chance of false detection. In this work, we present 266 ks NuSTAR observations of the Bullet cluster, which is detected in the energy range 3-30 keV. NuSTAR's unprecedented hard X-ray focusing capability largely eliminates confusion between diffuse IC and point sources; however, at the highest energies, the background still dominates and must be well understood. To this end, we have developed a complete background model constructed of physically inspired components constrained by extragalactic survey field observations, the specific parameters of which are derived locally from data in non-source regions of target observations. Applying the background model to the Bullet cluster data, we find that the spectrum is well\u2014but not perfectly\u2014described as an isothermal plasma with kT = 14.2 \u00b1 0.2 keV. To slightly improve the fit, a second temperature component is added, which appears to account for lower temperature emission from the cool core, pushing the primary component to kT ~ 15.3 keV. We see no convincing need to invoke an IC component to describe the spectrum of the Bullet cluster, and instead argue that it is dominated at all energies by emission from purely thermal gas. The conservatively derived 90% upper limit on the IC flux of 1.1 \u00d7 10^(\u201312) erg s^(\u20131) cm^(\u20132) (50-100 keV), implying a lower limit on B \u2273 0.2 \u03bcG, is barely consistent with detected fluxes previously reported. In addition to discussing the possible origin of this discrepancy, we remark on the potential implications of this analysis for the prospects for detecting IC in galaxy clusters in the future.",
"date": "2014-09-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "792",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 48",
"id_number": "CaltechAUTHORS:20140925-100352945",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140925-100352945",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Postdoctoral Program"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-37",
"name": "Space Radiation Laboratory"
}
]
},
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"id": "NuSTAR"
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{
"id": "Space-Radiation-Laboratory"
}
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},
"doi": "10.1088/0004-637X/792/1/48",
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}
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"pub_year": "2014",
"author_list": "Wik, Daniel R.; Hornstrup, A.; et el."
},
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"eprint_id": 49208,
"eprint_status": "archive",
"datestamp": "2023-08-22 13:26:02",
"lastmod": "2023-10-17 21:13:02",
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"items": [
{
"id": "Ar\u00e8valo-P",
"name": {
"family": "Ar\u00e8valo",
"given": "P."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
}
]
},
"title": "The 2-79 keV X-Ray Spectrum of the Circinus Galaxy with NuSTAR, XMM-Newton, and Chandra: A Fully Compton-thick Active Galactic Nucleus",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (Circinus); galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 December 23; accepted 2014 June 11; published 2014 July 30. \n\nWe thank the anonymous referee for a thorough review and\nmany useful suggestions that improved this paper. This work\nwas supported under NASA Contract No. NNG08FD60C, and\nmade use of data from the NuSTAR mission, a project led\nby the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge financial support from Basal-CATA PFB-06/2007 (FEB), CONICYT-Chile FONDECYT 1140304 (PA), 1141218 (FEB), 1120061 (ET), and Anillo ACT1101 (PA, FEB, ET). A.C., A.M., and G.M. acknowledge the ASI-INAF grant I/037/12/0.W.N.B. and B.L. acknowledge support from Caltech NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. M.K. gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. P.G. thanks STFC for support (grant reference ST/J003697/1).\n\nPublished - 0004-637X_791_2_81.pdf
",
"abstract": "The Circinus galaxy is one of the closest obscured active galactic nuclei (AGNs), making it an ideal target for detailed study. Combining archival Chandra and XMM-Newton data with new NuSTAR observations, we model the 2-79 keV spectrum to constrain the primary AGN continuum and to derive physical parameters for the obscuring material. Chandra's high angular resolution allows a separation of nuclear and off-nuclear galactic emission. In the off-nuclear diffuse emission, we find signatures of strong cold reflection, including high equivalent-width neutral Fe lines. This Compton-scattered off-nuclear emission amounts to 18% of the nuclear flux in the Fe line region, but becomes comparable to the nuclear emission above 30 keV. The new analysis no longer supports a prominent transmitted AGN component in the observed band. We find that the nuclear spectrum is consistent with Compton scattering by an optically thick torus, where the intrinsic spectrum is a power law of photon index \u0393 = 2.2-2.4, the torus has an equatorial column density of N_H = (6-10) \u00d7 10^(24) cm^(\u20132), and the intrinsic AGN 2-10 keV luminosity is (2.3-5.1) \u00d7 10^(42) erg s^(\u20131). These values place Circinus along the same relations as unobscured AGNs in accretion rate versus \u0393 and L_X versus L_(IR) phase space. NuSTAR's high sensitivity and low background allow us to study the short timescale variability of Circinus at X-ray energies above 10 keV for the first time. The lack of detected variability favors a Compton-thick absorber, in line with the spectral fitting results.",
"date": "2014-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "791",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 81",
"id_number": "CaltechAUTHORS:20140903-144941504",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140903-144941504",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1140304"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1141218"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2_138979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
}
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"pub_year": "2014",
"author_list": "Ar\u00e8valo, P.; Walton, D. J.; et el."
},
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{
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},
"title": "NuSTAR Observations of the State Transition of Millisecond Pulsar Binary PSR J1023+0038",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: general; pulsars: individual (PSR J1023+0038); stars: neutron; X-rays: stars",
"note": "\u00a9 2014 American Astronomical Society. Received 2014 February 18; accepted 2014 June 25; published 2014 July 29. We thank the anonymous referee for detailed suggestions\nand comments. This work was supported under NASA Contract\nNo. NNG08FD60C and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). VMK receives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en\nAstrophysique du Qu\u00e9bec, an R. Howard Webster Foundation\nFellowship from the Canadian Institute for Advanced Study,\nthe Canada Research Chairs Program, and the Lorne Trottier\nChair in Astrophysics and Cosmology. J.W.T.H. acknowledges\nfunding for this work from ERC starting grant DRAGNET. A.P.\nacknowledges support from the Netherlands Organization for\nScientic Research (NWO) Vidi fellowship.\n\nPublished - 0004-637X_791_2_77.pdf
Submitted - 1406.7009v1.pdf
",
"abstract": "We report NuSTAR observations of the millisecond pulsar-low-mass X-ray binary (LMXB) transition system PSR J1023+0038 from 2013 June and October, before and after the formation of an accretion disk around the neutron star. Between June 10 and 12, a few days to two weeks before the radio disappearance of the pulsar, the 3-79 keV X-ray spectrum was well fit by a simple power law with a photon index of \u0393 = 1.17^(+0.08)_(-0.07) (at 90% confidence) with a 3-79 keV luminosity of 7.4 \u00b1 0.4 \u00d7 10^(32) erg s^(\u20131). Significant orbital modulation was observed with a modulation fraction of 36% \u00b1 10%. During the October 19-21 observation, the spectrum is described by a softer power law (\u0393 = 1.66^(+0.06)_(-0.05)) with an average luminosity of 5.8 \u00b1 0.2 \u00d7 10^(33) erg s^(\u20131) and a peak luminosity of \u22481.2 \u00d7 10^(34) erg s^(\u20131) observed during a flare. No significant orbital modulation was detected. The spectral observations are consistent with previous and current multiwavelength observations and show the hard X-ray power law extending to 79 keV without a spectral break. Sharp-edged, flat-bottomed dips are observed with widths between 30 and 1000 s and ingress and egress timescales of 30-60 s. No change in hardness ratio was observed during the dips. Consecutive dip separations are log-normal in distribution with a typical separation of approximately 400 s. These dips are distinct from dipping activity observed in LMXBs. We compare and contrast these dips to observations of dips and state changes in the similar transition systems PSR J1824\u20132452I and XSS J1227.0\u20134859 and discuss possible interpretations based on the transitions in the inner disk.",
"date": "2014-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "791",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 77",
"id_number": "CaltechAUTHORS:20140903-141705608",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140903-141705608",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Centre de Recherche en Astrophysique du Qu\u00e9bec"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canada Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
},
{
"agency": "European Research Council (ERC)"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
}
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"doi": "10.1088/0004-637X/791/2/77",
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"pub_year": "2014",
"author_list": "Tendulkar, Shriharsh P.; Yang, Chengwei; et el."
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{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
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"family": "Krivonos",
"given": "Roman"
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"name": {
"family": "Bauer",
"given": "Franz E."
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"name": {
"family": "Fornasini",
"given": "Francesca M."
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"name": {
"family": "Hailey",
"given": "Charles J."
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"name": {
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"given": "Fiona A."
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"name": {
"family": "Hong",
"given": "Jaesub"
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"name": {
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"given": "Kaya"
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"orcid": "0000-0002-9709-5389"
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"name": {
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},
"title": "Initial Results from NuSTAR Observations of the Norma Arm",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "binaries: general; novae, cataclysmic variables; stars: neutron; X-rays: binaries",
"note": "\u00a9 2014 American Astronomical Society. Received 2014 February 12; accepted 2014 June 30; published 2014 July 28. This work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by theASI Science Data Center (ASDC, Italy) and the California Institute of Technology. This research has made use of: data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; NASA's Astrophysics\nData System Bibliographic Services; and the SIMBAD\ndatabase operated at CDS, Strasbourg, France. F.M.F. acknowledges support from the National Science Foundation Graduate Research Fellowship. F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218\nand \"EMBIGGEN\" Anillo ACT1101), and Project IC120009\n\"Millennium Institute of Astrophysics (MAS)\" of Iniciativa\nCient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y\nTurismo.\n\nPublished - Bodaghee_2014p68.pdf
Submitted - 1407.0023v1.pdf
",
"abstract": "Results are presented for an initial survey of the Norma Arm gathered with the focusing hard X-Ray Telescope NuSTAR. The survey covers 0.2 deg^2 of sky area in the 3-79 keV range with a minimum and maximum raw depth of 15 ks and 135 ks, respectively. Besides a bright black-hole X-ray binary in outburst (4U 1630\u201347) and a new X-ray transient (NuSTAR J163433\u2013473841), NuSTAR locates three sources from the Chandra survey of this region whose spectra are extended above 10 keV for the first time: CXOU J163329.5\u2013473332, CXOU J163350.9\u2013474638, and CXOU J163355.1\u2013473804. Imaging, timing, and spectral data from a broad X-ray range (0.3-79 keV) are analyzed and interpreted with the aim of classifying these objects. CXOU J163329.5\u2013473332 is either a cataclysmic variable or a faint low-mass X-ray binary. CXOU J163350.9\u2013474638 varies in intensity on year-long timescales, and with no multi-wavelength counterpart, it could be a distant X-ray binary or possibly a magnetar. CXOU J163355.1\u2013473804 features a helium-like iron line at 6.7 keV and is classified as a nearby cataclysmic variable. Additional surveys are planned for the Norma Arm and Galactic Center, and those NuSTAR observations will benefit from the lessons learned during this pilot study.",
"date": "2014-08-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "791",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 68",
"id_number": "CaltechAUTHORS:20140829-122711513",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140829-122711513",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NSF Graduate Research Fellowship"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "CONICYT-Chile",
"grant_number": "FONDECYT 1141218"
},
{
"agency": "CONICYT-Chile",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo",
"grant_number": "IC120009"
}
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"doi": "10.1088/0004-637X/791/1/68",
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"pub_year": "2014",
"author_list": "Bodaghee, Arash; Tomsick, John A.; et el."
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},
"title": "The 2013 outburst of a transient very faint X-ray binary, 23 arcsec from Sgr A*",
"ispublished": "pub",
"full_text_status": "restricted",
"note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 April 30. Received 2014 April 29. In original form 2014 March 24. First published online June 4, 2014\n\nWe are very grateful for the hard work by the staff and directors of the observatories, and in particular, to Scott Wolk, Patrick Slane, and Dillon Foight at the CXC, for enabling our monitoring campaigns of the Galactic Center. COH is supported by an NSERC Discovery Grant and an Alberta Ingenuity New Faculty Award. DH is supported by Chandra X-ray Observatory (CXO) Award numbers GO3-14121X, GO3-14099X, and G03-14060X, operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract and also by NASA Swift grant NNX14AC30G. NR is supported by a Ramon y Cajal Fellowship, NWO Vidi award, and grants AYA 2012-39303, SGR2009-811, and iLINK 2011-0303. ND is supported by NASA through Hubble Postdoctoral Fellowship grant number HST-HF-51287.01-A from STScI. This research made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center in the application packages CIAO, CHIPS, and SHERPA. The National Radio Astronomy Observatory is operated by Associated Universities Inc., under cooperative agreement with the National Science Foundation. The Swift/XRT Data Analysis Software (XRTDAS) is developed under the responsibility of the ASI Science Data Center (ASDC), Italy. We acknowledge extensive use of the ADS and arXiv.",
"abstract": "We report observations using the Swift/XRT, NuSTAR, and Chandra X-ray telescopes of the\ntransient X-ray source CXOGC J174540.0-290005 during its 2013 outburst. Due to its location\nin the field of multiple observing campaigns targeting Sgr A*, this is one of the best-studied\noutbursts of a very faint X-ray binary (VFXB; peak LX < 10^(36) erg s^(\u22121)) yet recorded, with\ndetections in 173 ks of X-ray observations over 50 d. VFXBs are of particular interest, due\nto their unusually low outburst luminosities and time-averaged mass transfer rates, which are\nhard to explain within standard accretion physics and binary evolution. The 2013 outburst of\nCXOGC J174540.0-290005 peaked at L_X(2\u201310 keV) = 5.0 \u00d7 10^(35) erg s^(\u22121), and all data above\n10^(34) erg s^(\u22121) were well fitted by an absorbed power law of photon index \u223c1.7, extending from\n2 keV out to \u2273 70 keV. We discuss the implications of these observations for the accretion\nstate of CXOGC J174540.0-290005.",
"date": "2014-07-21",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "442",
"number": "1",
"publisher": "Royal Astronomical Society",
"pagerange": "372-381",
"id_number": "CaltechAUTHORS:20150401-100203659",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150401-100203659",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Alberta Ingenuity New Faculty Award"
},
{
"agency": "NASA",
"grant_number": "GO3-14121X"
},
{
"agency": "NASA",
"grant_number": "GO3-14099X"
},
{
"agency": "NASA",
"grant_number": "G03-14060X"
},
{
"agency": "NASA",
"grant_number": "NNX14AC30G"
},
{
"agency": "Ramon y Cajal Fellowship"
},
{
"agency": "Ministerio de Educaci\u00f3n y Ciencia (MEC)",
"grant_number": "AYA 2012-39303"
},
{
"agency": "Agencia de Gesti\u00f3 D'Ajuts Universitaris I de Recerca Agaur",
"grant_number": "SGR2009-811"
},
{
"agency": "NASA",
"grant_number": "HST-HF-51287.01-A"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
}
]
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"doi": "10.1093/mnras/stu887",
"pub_year": "2014",
"author_list": "Koch, E. W.; Bahramian, A.; et el."
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"name": {
"family": "Zhang",
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},
"title": "NuSTAR Observations of X-Ray Bursts from the Magnetar 1E 1048.1\u20135937",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (1E 1048.1\u20135937); stars: magnetars; stars: neutron; X-rays: bursts",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 March 6; accepted 2014 June 12; published 2014 July 3.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V.M.K. acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. acknowledges the support by NASA grants NNX10AI72G and NNX13AI34G.\n\nPublished - 0004-637X_790_1_60.pdf
Supplemental Material - 1406.3377v1.pdf
",
"abstract": "We report the detection of eight bright X-ray bursts from the 6.5 s magnetar 1E 1048.1\u22125937, during a 2013 July observation campaign with the Nuclear Spectroscopic Telescope Array. We study the morphological and spectral properties of these bursts and their evolution with time. The bursts resulted in count rate increases by orders of magnitude, sometimes limited by the detector dead time, and showed blackbody spectra with kT ~ 6\u20138 keV in the T_(90) duration of 1\u20134 s, similar to earlier bursts detected from the source. We find that the spectra during the tail of the bursts can be modeled with an absorbed blackbody with temperature decreasing with flux. The burst flux decays followed a power law of index 0.8\u20130.9. In the burst tail spectra, we detect a ~13 keV emission feature, similar to those reported in previous bursts from this source as well as from other magnetars observed with the Rossi X-ray Timing Explorer. We explore possible origins of the spectral feature such as proton cyclotron emission, which implies a magnetic field strength of B ~ 2 \u00d7 10^(15)\u2009G in the emission region. However, the consistency of the energy of the feature in different objects requires further explanation.",
"date": "2014-07-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "790",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 60",
"id_number": "CaltechAUTHORS:20140815-092605389",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140815-092605389",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Fonds Qu\u00e9b\u00e9cois de la Recherche sur la Nature et les Technologies (FQRNT)"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canada Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
},
{
"agency": "NASA",
"grant_number": "NNX10AI72G"
},
{
"agency": "NASA",
"grant_number": "NNX13AI34G"
}
]
},
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"id": "2014-46",
"name": "Space Radiation Laboratory"
}
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"doi": "10.1088/0004-637X/790/1/60",
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],
"pub_year": "2014",
"author_list": "An, Hongjun; Kaspi, Victoria M.; et el."
},
{
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"eprint_id": 47515,
"eprint_status": "archive",
"datestamp": "2023-08-20 01:47:30",
"lastmod": "2023-10-26 20:40:01",
"type": "article",
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"items": [
{
"id": "Kaastra-J-S",
"name": {
"family": "Kaastra",
"given": "J. S."
},
"orcid": "0000-0001-5540-2822"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
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},
"title": "A fast and long-lived outflow from the supermassive black hole in NGC 5548",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 American Association for the Advancement of Science.\n\n24 March 2014; accepted 9 June 2014; Published online 19 June 2014.\n\nThe data used in this research are stored in the public archives of the international space observatories involved: XMM-Newton, HST, Swift, NuSTAR, INTEGRAL, and Chandra. We acknowledge support by the International Space Science Institute in Bern; the Netherlands Organization for Scientific Research; NASA HST program 13184 from the Space Telescope Science Institute, which is operated by Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555; the UK\nScience and Technology Facilities Council; the French Centre National d'Etudes Spatiales, CNRS/Project International de Coop\u00e9ration Scientific and CNRS/Programme National Hautes \u00c9nergies; Vicerrector\u00eda de Investigaci\u00f3n y Desarrollo Tecnol\u00f3gico (Chile); Israel's Ministry of Science, Technology, and Space, Israel Science\nFoundation (1163/10), and Israeli Centers of Research Excellence program (1937/12); the Swiss National Science Foundation; the Agenzia Spaziale Italiana grant INAF I/037/12/0-011/13 and INAF/Project for International Scientific Cooperation; NSF grant AST-1008882; and European Union Marie Curie contract FP-PEOPLE-2012-IEF-331095. We thank S. Paniagua for help with Fig. 4.\n\nSubmitted - 1406.5007.pdf
",
"abstract": "Supermassive black holes in the nuclei of active galaxies expel large amounts of matter through powerful winds of ionized gas. The archetypal active galaxy NGC 5548 has been studied for decades, and high-resolution x-ray and ultraviolet (UV) observations have previously shown a persistent ionized outflow. An observing campaign in 2013 with six space observatories shows the nucleus to be obscured by a long-lasting, clumpy stream of ionized gas not seen before. It blocks 90% of the soft x-ray emission and causes simultaneous deep, broad UV absorption troughs. The outflow velocities of this gas are up to five times faster than those in the persistent outflow, and, at a distance of only a few light days from the nucleus, it may likely originate from the accretion disk.",
"date": "2014-07-04",
"date_type": "published",
"publication": "Science",
"volume": "345",
"number": "6192",
"publisher": "American Association for the Advancement of Science",
"pagerange": "64-68",
"id_number": "CaltechAUTHORS:20140728-091348328",
"issn": "0036-8075",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140728-091348328",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "International Space Science Institute"
},
{
"agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)"
},
{
"agency": "NASA",
"grant_number": "HST 13184"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
},
{
"agency": "Vicerrector\u00eda de Investigaci\u00f3n y Desarrollo Tecnol\u00f3gico"
},
{
"agency": "Israel Science Foundation",
"grant_number": "1163/10"
},
{
"agency": "Israel Science Foundation",
"grant_number": "1937/12"
},
{
"agency": "Swiss National Science Foundation (SNSF)"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "NSF",
"grant_number": "AST-1008882"
},
{
"agency": "Marie Curie Fellowship",
"grant_number": "FP-PEOPLE-2012-IEF-331095"
}
]
},
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"doi": "10.1126/science.1253787",
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"author_list": "Kaastra, J. S. and Harrison, F. A."
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"name": {
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},
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"id": "An-Hongjun",
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}
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"title": "NuSTAR Observations of the Magnetar 1E 2259+586",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (1E 2259+586); stars: magnetars; stars: neutron; X-rays: bursts",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 February 24; Accepted 2014 May 19; Published 2014 June 17.\n\nPart of this work was performed under the auspices of the\nU.S. Department of Energy by Lawrence Livermore National\nLaboratory under Contract DE-AC52-07NA27344 with support\nfrom the LDRD program through grant 13-ERD-033. This work\nwas supported under NASA Contract No. NNG08FD60C, and\nmade use of data from the NuSTAR mission, a project led\nby the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V.M.K. receives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en Astrophysique du Qu\u00b4ebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. is supported by the NASA ATP grant NNX 13AI34G. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We also thank Dr. A. M. Archibald for helpful discussions.\n\nPublished - 0004-637X_789_1_75.pdf
",
"abstract": "We report on new broad band spectral and temporal observations of the magnetar 1E 2259+586, which is located in the supernova remnant CTB 109. Our data were obtained simultaneously with the Nuclear Spectroscopic Telescope Array (NuSTAR) and Swift, and cover the energy range from 0.5-79 keV. We present pulse profiles in various energy bands and compare them to previous RXTE results. The NuSTAR data show pulsations above 20 keV for the first time and we report evidence that one of the pulses in the double-peaked pulse profile shifts position with energy. The pulsed fraction of the magnetar is shown to increase strongly with energy. Our spectral analysis reveals that the soft X-ray spectrum is well characterized by an absorbed double blackbody or blackbody plus power-law model in agreement with previous reports. Our new hard X-ray data, however, suggest that an additional component, such as a power law, is needed to describe the NuSTAR and Swift spectrum. We also fit the data with the recently developed coronal outflow model by Beloborodov for hard X-ray emission from magnetars. The outflow from a ring on the magnetar surface is statistically preferred over outflow from a polar cap.",
"date": "2014-07-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "789",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 75",
"id_number": "CaltechAUTHORS:20140724-114420483",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140724-114420483",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"other_numbering_system": {
"items": [
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"id": "2014-47",
"name": "Space Radiation Laboratory"
}
]
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"local_group": {
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"doi": "10.1088/0004-637X/789/1/75",
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"family": "Cackett",
"given": "E. M."
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{
"id": "Reynolds-C",
"name": {
"family": "Reynolds",
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"given": "W. W."
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},
"title": "Observations of MCG-5-23-16 with Suzaku, XMM-Newton and NuSTAR: Disk Tomography and Compton Hump Reverberation",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; X-rays: galaxies; X-rays: individual (MCG-5-23-16)",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 March 24; Accepted 2014 May 14; Published 2014 June 13.\n\nThis work has been partly supported by NASA grant\nNNX14AF89G. The research in this article has made use of\ndata obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). We made use of data from the NuSTAR mission, a\nproject led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. Part of this work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.\n\nPublished - 0004-637X_789_1_56.pdf
Submitted - 1405.3674v1.pdf
",
"abstract": "MCG-5-23-16 is one of the first active galactic nuclei (AGNs) where relativistic reverberation in the iron K line originating in the vicinity of the supermassive black hole was found, based on a short XMM-Newton observation. In this work, we present the results from long X-ray observations using Suzaku, XMM-Newton, and NuSTAR designed to map the emission region using X-ray reverberation. A relativistic iron line is detected in the lag spectra on three different timescales, allowing the emission from different regions around the black hole to be separated. Using NuSTAR coverage of energies above 10 keV reveals a lag between these energies and the primary continuum, which is detected for the first time in an AGN. This lag is a result of the Compton reflection hump responding to changes in the primary source in a manner similar to the response of the relativistic iron K line.",
"date": "2014-07-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "789",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 56",
"id_number": "CaltechAUTHORS:20140728-114014890",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140728-114014890",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX14AF89G"
},
{
"agency": "ESA Member States"
}
]
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{
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"doi": "10.1088/0004-637X/789/1/56",
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"pub_year": "2014",
"author_list": "Zoghbi, A.; Cackett, E. M.; et el."
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{
"id": "Hailey-C-J",
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"given": "Hongjun"
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"family": "Grefenstette",
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"given": "Kerstin M."
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"given": "Daniel"
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"given": "Daniel R."
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
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"id": "Zoglauer-A-C",
"name": {
"family": "Zoglauer",
"given": "Andreas"
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},
"title": "NuSTAR Study of Hard X-Ray Morphology and Spectroscopy of PWN G21.5\u20130.9",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "ISM: individual objects (G21.5\u20130.9); ISM: supernova remnants; radiation mechanisms: general; stars: neutron; X-rays: ISM",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 November 11; accepted 2014 April 29; published 2014 June 17.\n\nThis work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by theASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_789_1_72.pdf
Submitted - 1405.3239v1.pdf
",
"abstract": "We present NuSTAR high-energy X-ray observations of the pulsar wind nebula (PWN)/supernova remnant G21.5\u22120.9. We detect integrated emission from the nebula up to ~40 keV, and resolve individual spatial features over a broad X-ray band for the first time. The morphology seen by NuSTAR agrees well with that seen by XMM-Newton and Chandra below 10 keV. At high energies, NuSTAR clearly detects non-thermal emission up to ~20 keV that extends along the eastern and northern rim of the supernova shell. The broadband images clearly demonstrate that X-ray emission from the North Spur and Eastern Limb results predominantly from non-thermal processes. We detect a break in the spatially integrated X-ray spectrum at ~9 keV that cannot be reproduced by current spectral energy distribution models, implying either a more complex electron injection spectrum or an additional process such as diffusion compared to what has been considered in previous work. We use spatially resolved maps to derive an energy-dependent cooling length scale, L(E)\u221dE^(m) with m = \u22120.21 \u00b1 0.01. We find this to be inconsistent with the model for the morphological evolution with energy described by Kennel & Coroniti. This value, along with the observed steepening in power-law index between radio and X-ray, can be quantitatively explained as an energy-loss spectral break in the simple scaling model of Reynolds, assuming particle advection dominates over diffusion. This interpretation requires a substantial departure from spherical magnetohydrodynamic, magnetic-flux-conserving outflow, most plausibly in the form of turbulent magnetic-field amplification.",
"date": "2014-07-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "789",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 72",
"id_number": "CaltechAUTHORS:20140724-081931132",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140724-081931132",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
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"id": "2014-48",
"name": "Space Radiation Laboratory"
}
]
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"doi": "10.1088/0004-637X/789/1/72",
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"pub_year": "2014",
"author_list": "Nynka, Melania; Hailey, Charles J.; et el."
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"datestamp": "2023-08-22 12:59:04",
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"items": [
{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "E. V."
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"orcid": "0000-0003-2992-8024"
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"id": "Christensen-F-E",
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"name": {
"family": "Craig",
"given": "W. W."
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"name": {
"family": "Hailey",
"given": "J. C."
}
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{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "V. M."
},
"orcid": "0000-0001-9345-0307"
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"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D. K."
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"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
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},
"title": "NuSTAR Discovery of a Young, Energetic Pulsar Associated with the Luminous Gamma-ray Source HESS J1640-465",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "ISM: individual objects (G338.3\u20130.0, HESS J1640\u2013465, 1FHL J1640.5\u20134634, AX J1640.7\u20134632, XMMU J164045.4\u2013463131); ISM: supernova remnants; pulsars: individual (PSR J1640-4631); stars: neutron",
"note": "\u00a9 2014 American Astronomical Society. Received 2013 December 19; accepted 2014 May 2; published 2014 June 3. This work made use of data from the NuSTAR mission, a\nproject led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This work has also made use of archival data from the Chandra X-ray Observatory. Partial support for E.V.G. and J.A.T were provided by NASA through Chandra Award Numbers SAOGO2-13097X and GO1-12068A, respectively, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. E.V.G acknowledges support by Fermi Guest Investigator Grant NNX12AO89G. Radio contours were obtained from Molonglo Observatory Synthesis Telescope (MOST) data provided by the University of Sydney with support from the Australian Research Council and the Science Foundation for Physics within The University of Sydney.\n\nPublished - 0004-637X_788_2_155.pdf
Submitted - 1405.0465v1.pdf
",
"abstract": "We report the discovery of a 206 ms pulsar associated with the TeV \u03b3-ray source HESS J1640\u2013465 using the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray observatory. PSR J1640\u20134631 lies within the shell-type supernova remnant (SNR) G338.3\u20130.0, and coincides with an X-ray point source and putative pulsar wind nebula (PWN) previously identified in XMM-Newton and Chandra images. It is spinning down rapidly with period derivative \u1e56 = 9.758(44) \u00d7 10^(\u201313), yielding a spin-down luminosity \u0116 = 4.4 \u00d7 10^(36) erg s^(\u20131), characteristic age \u03c4_c \u2261 P/2\u1e56 = 3350 yr, and surface dipole magnetic field strength B_s = 1.4 \u00d7 10^(13) G. For the measured distance of 12 kpc to G338.3\u20130.0, the 0.2-10 TeV luminosity of HESS J1640\u2013465 is 6% of the pulsar's present \u0116. The Fermi source 1FHL J1640.5\u20134634 is marginally coincident with PSR J1640\u20134631, but we find no \u03b3-ray pulsations in a search using five years of Fermi Large Area Telescope (LAT) data. The pulsar energetics support an evolutionary PWN model for the broadband spectrum of HESS J1640\u2013465, provided that the pulsar's braking index is n \u2248 2, and that its initial spin period was P_0 ~ 15 ms.",
"date": "2014-06-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "788",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 155",
"id_number": "CaltechAUTHORS:20140717-140551846",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140717-140551846",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "SAOGO2-13097X"
},
{
"agency": "NASA",
"grant_number": "GO1-12068A"
},
{
"agency": "NASA",
"grant_number": "NAS8-03060"
},
{
"agency": "NASA",
"grant_number": "NNX12AO89G"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
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"doi": "10.1088/0004-637X/788/2/155",
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],
"pub_year": "2014",
"author_list": "Gotthelf, E. V.; Tomsick, J. A.; et el."
},
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"datestamp": "2023-08-22 12:55:59",
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"items": [
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Rivers-E",
"name": {
"family": "Rivers",
"given": "E."
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},
"title": "NuSTAR and XMM-NEWTON Observations of NGC 1365: Extreme Absorption Variability and a Constant Inner Accretion Disk",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; galaxies : active; X-rays : individual (NGC 1365)",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 November 27; accepted 2014 April 18; published 2014 May 23.\n\nThe authors would like to thank the referee for providing\nuseful feedback, which helped improve the manuscript. This\nresearch has made use of data obtained with the NuSTAR mission,\na project led by the California Institute of Technology\n(Caltech), managed by the Jet Propulsion Laboratory (JPL)\nand funded by NASA, and XMM-Newton, an ESA science mission with instruments and contributions directly funded by\nESA Member States and NASA. We thank both the XMM Newton\nand the NuSTAR Operations, Software, and Calibration\nteams for support with the execution and analysis of these\ncoordinated observations. This research was supported under\nNASA grant No. NNG08FD60C and has made use of the\nNuSTAR Data Analysis Software (NUSTARDAS) jointly developed\nby the ASI Science Data Center (ASDC, Italy) and\nCaltech (USA). P.A. acknowledges financial support from Conicyt\nACT 1101, and P.G. acknowledges support from STFC\n(grant reference ST/J00369711).\nFacilites: NuSTAR, XMM\n\nPublished - 0004-637X_788_1_76.pdf
Submitted - 1404.5620v1.pdf
",
"abstract": "We present a spectral analysis of four coordinated NuSTAR+XMM-Newton observations of the Seyfert galaxy NGC 1365. These exhibit an extreme level of spectral variability, which is primarily due to variable line-of-sight absorption, revealing relatively unobscured states in this source for the first time. Despite the diverse range of absorption states, each of the observations displays the same characteristic signatures of relativistic reflection from the inner accretion disk. Through time-resolved spectroscopy, we find that the strength of the relativistic iron line and the Compton reflection hump relative to the intrinsic continuum are well correlated, which is expected if they are two aspects of the same broadband reflection spectrum. We apply self-consistent disk reflection models to these time-resolved spectra in order to constrain the inner disk parameters, allowing for variable, partially covering absorption to account for the vastly different absorption states that were observed. Each of the four observations is treated independently to test the consistency of the results obtained for the black hole spin and the disk inclination, which should not vary on observable timescales. We find both the spin and the inclination determined from the reflection spectrum to be consistent, confirming that NGC 1365 hosts a rapidly rotating black hole; in all cases the dimensionless spin parameter is constrained to be a* > 0.97 (at 90% statistical confidence or better.",
"date": "2014-06-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "788",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 76",
"id_number": "CaltechAUTHORS:20140707-144535458",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140707-144535458",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT 1101"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J00369711"
}
]
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"doi": "10.1088/0004-637X/788/1/76",
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},
"title": "The Broad-band X-Ray Spectrum of IC 4329A from a Joint NuSTAR/Suzaku Observation",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion; accretion disks; galaxies : active; galaxies : individual (IC 4329A); galaxies : nuclei; galaxies : Seyfert; X-rays : galaxies",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 February 28; accepted 2014 April 25; published 2014 May 21. \n\nThis work was supported under NASA Contract No.\nNNG08FD60C and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software, and Calibration teams for support\nwith the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by theASI Science Data Center\n(ASDC, Italy) and the California Institute of Technology\n(USA). L.B. thanks Koji Mukai and the Suzaku GOF at NASA/GSFC for all their assistance in obtaining and analyzing that\ndata, and also gratefully acknowledges funding from NASA\ngrant NNX13AE90G. G. Matt and A.M. acknowledge financial\nsupport from Italian Space Agency under contract ASI/INAF\nI/037/12/0-011/13.\n\nPublished - 0004-637X_788_1_61.pdf
Submitted - 1404.7486v1.pdf
",
"abstract": "We have obtained a deep, simultaneous observation of the bright, nearby Seyfert galaxy IC 4329A with Suzaku and NuSTAR. Through a detailed spectral analysis, we are able to robustly separate the continuum, absorption, and distant reflection components in the spectrum. The absorbing column is found to be modest (~6 X 10^(21) cm^(-2)), and does not introduce any significant curvature in the Fe K band. We are able to place a strong constraint on the presence of a broadened Fe K\u03b1 line (E_(rest) = 6.46^(+0.08)_(-0.07) keV with \u03c3 = 0.33^(0.08)_(-0.07) keV and EW = 34^(+8)_(-7) eV), though we are not able to constrain any of the parameters of a relativistic reflection model. These results highlight the range in broad Fe K line strengths observed in nearby, bright, active galactic nuclei (roughly an order of magnitude), and imply a corresponding range in the physical properties of the inner accretion disk in these sources. We have also updated our previously reported measurement of the high-energy cutoff of the hard X-ray emission using both observatories rather than just NuSTAR alone: E _(cut) = 186 \u00b1 14 keV. This high-energy cutoff acts as a proxy for the temperature of the coronal electron plasma, enabling us to further separate this parameter from the plasma's optical depth and to update our results for these parameters as well. We derive kT = 50^(+6)_(-3) keV with \u03c4 = 2.34^(0.16)_(-0.11) using a spherical geometry, kT = 61 \u00b1 1 keV with \u03c4 = 0.68 \u00b1 0.02 for a slab geometry, with both having an equivalent goodness-of-fit.",
"date": "2014-06-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "788",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 61",
"id_number": "CaltechAUTHORS:20140703-122140957",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-122140957",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX13AE90G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
}
]
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"author_list": "Brenneman, L. W.; Madejski, G.; et el."
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},
"title": "The Broadband Spectral Variability of MCG\u20136-30-15 Observed by NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; galaxies: active; galaxies: Seyfert; X-rays: individual (MCG\u20136-30-015)",
"note": "\u00a9 2014 American Astronomical Society. Received 2013 December 23; accepted 2014 April 11; published 2014 May 6. A.M. acknowledges financial support from Fondazione Angelo\nDella Riccia. A.M. and G.M. acknowledge financial support\nfrom Italian Space Agency under grant ASI/INAF I/037/\n12/0-011/13. A.M., G. Matt, G. Miniutti, A.C.F., and E.K. acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. P.A. acknowledges financial support from Anillo ACT1101. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_787_1_83.pdf
",
"abstract": "MCG\u20136-30-15, at a distance of 37 Mpc (z = 0.008), is the archetypical Seyfert 1 galaxy showing very broad Fe K\u03b1 emission. We present results from a joint NuSTAR and XMM-Newton observational campaign that, for the first time, allows a sensitive, time-resolved spectral analysis from 0.35 keV up to 80 keV. The strong variability of the source is best explained in terms of intrinsic X-ray flux variations and in the context of the light-bending model: the primary, variable emission is reprocessed by the accretion disk, which produces secondary, less variable, reflected emission. The broad Fe K\u03b1 profile is, as usual for this source, well explained by relativistic effects occurring in the innermost regions of the accretion disk around a rapidly rotating black hole. We also discuss the alternative model in which the broadening of the Fe K\u03b1 is due to the complex nature of the circumnuclear absorbing structure. Even if this model cannot be ruled out, it is disfavored on statistical grounds. We also detected an occultation event likely caused by broad-line region clouds crossing the line of sight.",
"date": "2014-05-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "787",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 83",
"id_number": "CaltechAUTHORS:20140617-103551890",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140617-103551890",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/ 12/0-011/13"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Anillo project",
"grant_number": "ACT1101"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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},
"title": "Timing and Flux Evolution of the Galactic Center Magnetar SGR J1745\u20132900",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2013 November 20; accepted 2014 March 17; published 2014 April 21. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by theASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge the use of public data from the Swift data archive. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. We thank the Swift SOT team for their work in scheduling. V.M.K. receives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. R.F.A. receives support from a Walter C. Sumner Memorial Fellowship. A.M.B. was supported by NASA grants\nNNX-10-AI72G and NNX-13-AI34G. J.A.K. was supported by\nsupported by NASA contract NAS5-00136. J.K.V.'s work was\nperformed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344.\n\nPublished - 0004-637X_786_2_84.pdf
",
"abstract": "We present the X-ray timing and spectral evolution of the Galactic Center magnetar SGR J1745\u22122900 for the first ~4 months post-discovery using data obtained with the Nuclear Spectroscopic Telescope Array and Swift observatories. Our timing analysis reveals a large increase in the magnetar spin-down rate by a factor of 2.60 \u00b1 0.07 over our data span. We further show that the change in spin evolution was likely coincident with a bright X-ray burst observed in 2013 June by Swift, and if so, there was no accompanying discontinuity in the frequency. We find that the source 3\u201310 keV flux has declined monotonically by a factor of ~2 over an 80 day period post-outburst accompanied by a ~20% decrease in the source's blackbody temperature, although there is evidence for both flux and kT having leveled off. We argue that the torque variations are likely to be magnetospheric in nature and will dominate over any dynamical signatures of orbital motion around Sgr A*.",
"date": "2014-05-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "786",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 84",
"id_number": "CaltechAUTHORS:20140618-104936732",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140618-104936732",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Centre de Recherche en Astrophysique du Qu\u00e9bec"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canada Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
},
{
"agency": "Walter C. Sumner Memorial Fellowship"
},
{
"agency": "NASA",
"grant_number": "NNX-10-AI72G"
},
{
"agency": "NASA",
"grant_number": "NNX-13-AI34G"
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{
"agency": "NASA",
"grant_number": "NAS5-00136"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-AC52-07NA27344"
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"given": "Shuo"
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},
"title": "NuSTAR Detection of High-energy X-Ray Emission and Rapid Variability from Sagittarius A* Flares",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; Galaxy: center; stars: black holes; stars: flare; stars: individual (Sgr A*); X-rays: general",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2013 August 16; accepted 2014 March 11; published 2014 April 15. \n\nThis work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors thank S. Nayakshin, S. Markoff, A. Eckart, G. Trap, M. Wardle, and F. Yusef-Zadeh for useful discussions. We also thank the Chandra Sgr A* XVP collaboration for information on absence of X-ray transients before and after the flares reported here. \n\nFacility: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission\n\nPublished - 0004-637X_786_1_46.pdf
Submitted - 1403.0900v2.pdf
",
"abstract": "Sagittarius A* harbors the supermassive black hole that lies at the dynamical center of our Galaxy. Sagittarius A* spends most of its time in a low luminosity emission state but flares frequently in the infrared and X-ray, increasing up to a few hundred fold in brightness for up to a few hours at a time. The physical processes giving rise to the X-ray flares are uncertain. Here we report the detection with the NuSTAR observatory in Summer and Fall 2012 of four low to medium amplitude X-ray flares to energies up to 79 keV. For the first time, we clearly see that the power-law spectrum of Sagittarius A* X-ray flares extends to high energy, with no evidence for a cutoff. Although the photon index of the absorbed power-law fits are in agreement with past observations, we find a difference between the photon index of two of the flares (significant at the 95% confidence level). The spectra of the two brightest flares (~55 times quiescence in the 2-10 keV band) are compared to simple physical models in an attempt to identify the main X-ray emission mechanism, but the data do not allow us to significantly discriminate between them. However, we confirm the previous finding that the parameters obtained with synchrotron models are, for the X-ray emission, physically more reasonable than those obtained with inverse Compton models. One flare exhibits large and rapid (<100 s) variability, which, considering the total energy radiated, constrains the location of the flaring region to be within ~10 Schwarzschild radii of the black hole.",
"date": "2014-05-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "786",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 46",
"id_number": "CaltechAUTHORS:20140618-092849218",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140618-092849218",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-57",
"name": "Space Radiation Laboratory"
}
]
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"items": [
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"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
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},
"doi": "10.1088/0004-637X/786/1/46",
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"pub_year": "2014",
"author_list": "Barri\u00e8re, Nicolas M.; Tomsick, John A.; et el."
},
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"datestamp": "2023-08-22 12:39:34",
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{
"id": "Del-Moro-A",
"name": {
"family": "Del Moro",
"given": "A."
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{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
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"name": {
"family": "Harrison",
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},
"title": "NuSTAR J033202-2746.8: Direct Constraints on the Compton Reflection in a Heavily Obscured Quasar at z \u2248 2",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; infrared: galaxies; quasars: general; quasars: individual (NuSTAR J033202-2746.8); X-rays: galaxies",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 December 23; accepted 2014 March 9; published 2014 April 10.\n\nWe thank the anonymous referee for careful reading and for\nthe helpful comments, which helped improving this manuscript.\nWe gratefully acknowledge financial support from the UK Science\nand Technology Facilities Council (STFC, ST/I001573/I,\nADM and DMA; ST/K501979/1, GBL; ST/J003697/1, PG)\nand the Leverhulme Trust (D.M.A. and J.R.M.). A.C., C.V.,\nR.G., and P.R. thank the ASI/INAF grant I/037/12/0-011/\n13. F.E.B. acknowledges support from Basal-CATA (PFB-06/\n2007) and CONICYT-Chile (FONDECYT 1101024 and Anillo\ngrant ACT1101) and E.T. acknowledges the FONDECYT grant\n1120061. W.N.B. and B.L. thank Caltech NuSTAR subcontract\n44A-1092750 and NASA ADP grant NNX10AC99G. M.B. acknowledges\nthe International Fulbright Science and Technology\nAward. This work was supported under NASA Contract\nNo. NNG08FD60C, and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by\nthe National Aeronautics and Space Administration. We thank\nthe NuSTAR Operations, Software and Calibration teams for\nsupport with the execution and analysis of these observations.\nThis research has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data\nCenter (ASDC, Italy) and the California Institute of Technology\n(USA). This work also used observations made with ESO Telescopes\nat the La Silla Paranal Observatory under the program\nID 092.A-0452.\n\nPublished - 0004-637X_786_1_16.pdf
Submitted - 1403.2491v1.pdf
",
"abstract": "We report Nuclear Spectroscopic Telescope Array (NuSTAR) observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (~400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E > 8 keV and has a very flat spectral slope in the NuSTAR energy band (\u0393 = 0.55^(+0.62)_(-0.64); 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N_H = 5.6^(+0.9)_(-0.8) x 10^(23) cm^(\u20132)) with luminosity L_(10-40 keV) \u22486.4 \u00d7 10^(44) erg s^(\u20131). Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z = 2.00 \u00b1 0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R = 0.55^(0.44)_(-0.37)), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R ~ 0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L_(1.4 GHz) \u224810^(27) W Hz^(\u20131). Constraining the spectral shape of active galactic nuclei (AGNs), including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift.",
"date": "2014-05-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "786",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 16",
"id_number": "CaltechAUTHORS:20140617-132453849",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140617-132453849",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/I001573/I"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "FONDECYT 1101024"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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"id": "COSMOS"
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"doi": "10.1088/0004-637X/786/1/16",
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"pub_year": "2014",
"author_list": "Del Moro, A.; Balokovi\u0107, M.; et el."
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},
"title": "Simultaneous NuSTAR/Chandra Observations of the Bursting Pulsar GRO J1744-28 during Its Third Reactivation",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: general; stars: individual (GRO J1744-28); X-rays: binaries; X-rays: bursts",
"note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2 December 2014; accepted for publication 18 February 2015; Published 29 April 2015.\n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_804_1_43.pdf
Submitted - 1502.05982v1.pdf
",
"abstract": "We report on a 10 ks simultaneous Chandra/High Energy Transmission Grating (HETG)\u2013Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the Bursting Pulsar, GRO J1744-28, during its third detected outburst since discovery and after nearly 18 yr of quiescence. The source is detected up to 60 keV with an Eddington persistent flux level. Seven bursts, followed by dips, are seen with Chandra, three of which are also detected with NuSTAR. Timing analysis reveals a slight increase in the persistent emission pulsed fraction with energy (from 10% to 15%) up to 10 keV, above which it remains constant. The 0.5\u201370 keV spectra of the persistent and dip emission are the same within errors and well described by a blackbody (BB), a power-law (PL) with an exponential rolloff, a 10 keV feature, and a 6.7 keV emission feature, all modified by neutral absorption. Assuming that the BB emission originates in an accretion disk, we estimate its inner (magnetospheric) radius to be about 4 \u00d7 10^7 cm, which translates to a surface dipole field B \u2248 9 \u00d7 10^(10) G. The Chandra/HETG spectrum resolves the 6.7 keV feature into (quasi-)neutral and highly ionized Fe xxv and Fe xxvi emission lines. XSTAR modeling shows these lines to also emanate from a truncated accretion disk. The burst spectra, with a peak flux more than an order of magnitude higher than Eddington, are well fit with a PL with an exponential rolloff and a 10 keV feature, with similar fit values compared to the persistent and dip spectra. The burst spectra lack a thermal component and any Fe features. Anisotropic (beamed) burst emission would explain both the lack of the BB and any Fe components.",
"date": "2014-05-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "804",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 43",
"id_number": "CaltechAUTHORS:20150605-135807207",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150605-135807207",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
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"id": "2015-64",
"name": "Space Radiation Laboratory"
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"title": "Simultaneous NuSTAR and XMM\u2013Newton 0.5\u201380 keV spectroscopy of the narrow-line Seyfert 1 galaxy SWIFT J2127.4+5654",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs; galaxies: active; galaxies: individual: SWIFT; J2127.4+5654; galaxies: Seyfert",
"note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: April 2, 2014. Accepted 2014 February 27. Received 2014 February 25; in original form 2013 November 27. \n\nWe thank the referee for her/his comments and suggestions that\ngreatly improved the paper. AM thanks Javier Garcia and Thomas Dauser for the efforts in producing XILLVER and RELXILL tables to use in this paper. AM and GM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. PA and FB acknowledge support from Basal-CATA PFB-06/2007 (FEB), CONICYT-Chile FONDECYT 1101024 (FEB) and Anillo ACT1101 (FEB, PA). MB acknowledges support from the International Fulbright Science and Technology Award. This work was supported under NASA Contract no. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory,\nand funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - MNRAS-2014-Marinucci-2347-56.pdf
Submitted - 1402.7245v1.pdf
",
"abstract": "We present a broad-band spectral analysis of the joint XMM\u2013Newton and Nuclear Spectroscopic Telescope Array observational campaign of the narrow-line Seyfert 1 SWIFT J2127.4+5654, consisting of 300 ks performed during three XMM\u2013Newton orbits. We detect a relativistic broadened iron K\u03b1 line originating from the innermost regions of the accretion disc surrounding the central black hole, from which we infer an intermediate spin of \u0251=0.58+0.11\u22120.17. The intrinsic spectrum is steep (\u0393 = 2.08 \u00b1 0.01) as commonly found in narrow-line Seyfert 1 galaxies, while the cutoff energy (E_c=108^(+11)_(\u221210)\u2009keV) falls within the range observed in broad-line Seyfert 1 galaxies. We measure a low-frequency lag that increases steadily with energy, while at high frequencies, there is a clear lag following the shape of the broad Fe K emission line. Interestingly, the observed Fe K lag in SWIFT J2127.4+5654 is not as broad as in other sources that have maximally spinning black holes. The lag amplitude suggests a continuum-to-reprocessor distance of about 10\u201320\u2009r_g. These timing results independently support an intermediate black hole spin and a compact corona.",
"date": "2014-05",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "440",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "2347-2356",
"id_number": "CaltechAUTHORS:20140530-100053201",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-100053201",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1101024"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "ACT1101"
},
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
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},
"title": "The soft-X-ray emission of Ark 120. XMM\u2013Newton, NuSTAR, and the importance of taking the broad view",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion discs\n galaxies: active\n galaxies: individual: Ark 120",
"note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: February 18, 2014. We thank the anonymous referee for useful comments which helped us to improve the clarity of the paper, and Chris Done for comments and advices on the OPTXAGNF model. This work has made use of data from the NuSTAR mission, a project led by the California Institute\nof Technology, managed by the Jet Propulsion Laboratory, and\nfunded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NUSTARDAS jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of\nTechnology (USA). The work is also based on observations obtained with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). GM and AM acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n.312789.\n\nPublished - MNRAS-2014-Matt-3016-21.pdf
Submitted - 1401.5235v1.pdf
",
"abstract": "We present simultaneous XMM\u2013Newton and NuSTAR observations of the 'bare' Seyfert 1 galaxy, Ark 120, a system in which ionized absorption is absent. The NuSTAR hard-X-ray spectral coverage allows us to constrain different models for the excess soft-X-ray emission. Among phenomenological models, a cutoff power law best explains the soft-X-ray emission. This model likely corresponds to Comptonization of the accretion disc seed UV photons by a population of warm electrons: using Comptonization models, a temperature of \u223c0.3 keV and an optical depth of \u223c13 are found. If the UV-to-X-ray OPTXAGNF model is applied, the UV fluxes from the XMM\u2013Newton Optical Monitor suggest an intermediate black hole spin. Contrary to several other sources observed by NuSTAR, no high-energy cutoff is detected with a lower limit of 190 keV.",
"date": "2014-04-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "439",
"number": "3",
"publisher": "Royal Astronomical Society",
"pagerange": "3016-3021",
"id_number": "CaltechAUTHORS:20140530-140105315",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-140105315",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/12/0-011/13"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "312789"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
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"doi": "10.1093/mnras/stu159",
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"pub_year": "2014",
"author_list": "Matt, G.; Marinucci, A.; et el."
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{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
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{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
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"name": {
"family": "Barret",
"given": "D."
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"name": {
"family": "Harrison",
"given": "F. A."
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{
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"name": {
"family": "Fabian",
"given": "A. C."
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"name": {
"family": "Webb",
"given": "N. A."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
},
"orcid": "0000-0003-1703-8796"
}
]
},
"title": "Patchy Accretion Disks in Ultraluminous X-ray Sources",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion disks, black hole physics, X-rays: binaries",
"note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 January 19; accepted 2014 March 6; published 2014 March 26. \n\nJMM acknowledges helpful conversations with Mitch Begelman, Jason Dexter, and Richard Mushotzky. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA.\n\nPublished - pdf.pdf
Submitted - 1403.1769.pdf
",
"abstract": "The X-ray spectra of the most extreme ultra-luminous X-ray sources - those with L \u2265 10^(40) erg s^(-1) remain something of a mystery. Spectral roll-over in the 5-10 keV band was originally detected in in the deepest XMM-Newton observations of the brightest sources; this is confirmed in subsequent NuSTAR spectra. This emission can be modeled via Comptonization, but with low electron temperatures (kT_e \u2243 2 keV) and high optical depths (T \u2243 10) that pose numerous difficulties. Moreover, evidence of cooler thermal emission that can be fit with thin disk models persists, even in fits to joint XMM-Newton and NuSTAR observations. Using NGC 1313 X-1 as a test case, we show that a patchy disk with a multiple temperature profile may provide an excellent description of such spectra. In principle, a number of patches within a cool disk might emit over a range of temperatures, but the data only require a two-temperature profile plus standard Comptonization, or three distinct blackbody components. A mechanism such as the photon bubble instability may naturally give rise to a patchy disk profile, and could give rise to super-Eddington luminosities. It is possible, then, that a patchy disk (rather than a disk with a standard single-temperature profile) might be a hallmark of accretion disks close to or above the Eddington limit. We discuss further tests of this picture, and potential implications for sources such as narrow-line Seyfert-1 galaxies (NLSy1s) and other low-mass active galactic nuclei (AGN).",
"date": "2014-04-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "785",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L7",
"id_number": "CaltechAUTHORS:20150105-080756612",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150105-080756612",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
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},
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"doi": "10.1088/2041-8205/785/1/L7",
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"family": "Teng",
"given": "Stacy H."
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"name": {
"family": "Harrison",
"given": "F. A."
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"family": "Grefenstette",
"given": "B. W."
},
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"family": "Madsen",
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"title": "NuSTAR Reveals an Intrinsically X-Ray Weak Broad Absorption Line Quasar in the Ultraluminous Infrared Galaxy Markarian 231",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; quasars: individual (Mrk 231); X-rays: galaxies",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 August 14; accepted 2014 February 18; published 2014 March 21. \n\nWe are grateful to the anonymous referee for providing useful comments which improved our manuscript. We thank Wayne Baumgartner, Bret Lehmer, Richard Mushotzky, Jeremy\nSchnittman, Tahir Yaqoob, and Andreas Zezas for useful discussions. We would also like to thank Lee Armus who provided useful comments in the early planning phase of the NuSTAR ULIRG program. We also thank Roberto Maiolino, David Rupke, and Eckhard Sturm who are co-investigators of the Chandra program. This work was supported under NASA Contract No.NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The scientific results reported in this article are based in part on observations made by the Chandra X-Ray Observatory and data obtained from the Chandra Data Archive published previously in cited articles. This work, in part, made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). We made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. S.H.T. is supported by a NASA Postdoctoral Program (NPP) Fellowship. W.N.B. and B.L. acknowledge support by California Institute of Technology (Caltech) NuSTAR subcontract 44A-1092750 and NASA ADP grant NNX10AC99G. F.E.B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (under grants FONDECYT 1101024 and Anillo ACT1101). A.C. acknowledges support from ASI/INAF grant I/037/12/0-011/13. P.G. acknowledges support from STFC grant reference ST/J003697/1. \n\nFacilities: NuSTAR, CXO\n\nPublished - 0004-637X_785_1_19.pdf
Submitted - 1402.4811v1.pdf
",
"abstract": "We present high-energy (3-30 keV) NuSTAR observations of the nearest quasar, the ultraluminous infrared galaxy (ULIRG) Markarian 231 (Mrk 231), supplemented with new and simultaneous low-energy (0.5-8 keV) data from Chandra. The source was detected, though at much fainter levels than previously reported, likely due to contamination in the large apertures of previous non-focusing hard X-ray telescopes. The full band (0.5-30 keV) X-ray spectrum suggests the active galactic nucleus (AGN) in Mrk 231 is absorbed by a patchy and Compton-thin (N_H ~ 1.2^(+0.3)_(-0.3) x 10^(23) cm^(\u20132)) column. The intrinsic X-ray luminosity (L_(0.5 \u2013 30 keV) ~ 1.0 \u00d7 10^(43) erg s^(\u20131)) is extremely weak relative to the bolometric luminosity where the 2-10 keV to bolometric luminosity ratio is ~0.03% compared to the typical values of 2%-15%. Additionally, Mrk 231 has a low X-ray-to-optical power law slope (\u03b1_(OX) ~ \u20131.7). It is a local example of a low-ionization broad absorption line quasar that is intrinsically X-ray weak. The weak ionizing continuum may explain the lack of mid-infrared [O IV], [Ne V], and [Ne VI] fine-structure emission lines which are present in sources with otherwise similar AGN properties. We argue that the intrinsic X-ray weakness may be a result of the super-Eddington accretion occurring in the nucleus of this ULIRG, and may also be naturally related to the powerful wind event seen in Mrk 231, a merger remnant escaping from its dusty cocoon.",
"date": "2014-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "785",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 19",
"id_number": "CaltechAUTHORS:20140609-070533275",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140609-070533275",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "NASA",
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},
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{
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},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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"agency": "NASA Postdoctoral Program"
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"grant_number": "44A-1092750"
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{
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},
{
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"grant_number": "Anillo ACT1101"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/J003697/1"
}
]
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"id": "2014-61",
"name": "Space Radiation Laboratory"
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"doi": "10.1088/0004-637X/785/1/19",
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"pub_year": "2014",
"author_list": "Teng, Stacy H.; Harrison, F. A.; et el."
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"id": "Lansbury-G-B",
"name": {
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"given": "G. B."
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{
"id": "Balokovi\u0107-M",
"name": {
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"given": "M."
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"title": "NuSTAR Observations of Heavily Obscured Quasars at z ~ 0.5",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; X-rays: galaxies",
"note": "\u00a9 2014 American Astronomical Society. Received 2013 November 12; accepted 2014 February 10; published 2014 March 21. We acknowledge financial support from the Science and Technology Facilities Council (STFC) grants ST/K501979/1\n(G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.) and ST/J003697/1 (P.G.), the Leverhulme Trust (D.M.A. and J.R.M.),\nGemini-CONICYT grant 32120009 (R.J.A.), NSF AST award 1008067 (D.R.B.), the International Fulbright Science\nand Technology Award (M.B.), Basal-CATA PFB-06/2007 (F.E.B.), CONICYT-Chile grant FONDECYT 1101024\n(F.E.B.), CONICYT-Chile grant Anillo ACT1101 (F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.),\nNASA ADP grant NNX10AC99G (W.N.B. and B.L.), NASA\nADAP award NNX12AE38G (R.C.H.), National Science Foundation\ngrant 1211096 (R.C.H.), and Swiss National Science\nFoundation grant PP00P2_138979/1 (M.K.). We thank the referee for the constructive comments, which helped improve our study. This work was supported under NASA contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_785_1_17.pdf
Submitted - 1402.2666v1.pdf
",
"abstract": "We present NuSTAR hard X-ray observations of three Type 2 quasars at z \u2248 0.4-0.5, optically selected from the Sloan Digital Sky Survey. Although the quasars show evidence for being heavily obscured, Compton-thick systems on the basis of the 2-10 keV to [O III] luminosity ratio and multiwavelength diagnostics, their X-ray absorbing column densities (N_H) are poorly known. In this analysis, (1) we study X-ray emission at >10 keV, where X-rays from the central black hole are relatively unabsorbed, in order to better constrain N_H. (2) We further characterize the physical properties of the sources through broad-band near-UV to mid-IR spectral energy distribution analyses. One of the quasars is detected with NuSTAR at >8 keV with a no-source probability of <0.1%, and its X-ray band ratio suggests near Compton-thick absorption with N_H\u22735 \u00d7 10^(23) cm^(\u20132). The other two quasars are undetected, and have low X-ray to mid-IR luminosity ratios in both the low-energy (2-10 keV) and high-energy (10-40 keV) X-ray regimes that are consistent with extreme, Compton-thick absorption (N_H\u227310^(24) cm^(\u20132)). We find that for quasars at z ~ 0.5, NuSTAR provides a significant improvement compared to lower energy (<10 keV) Chandra and XMM-Newton observations alone, as higher column densities can now be directly constrained.",
"date": "2014-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "785",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 17",
"id_number": "CaltechAUTHORS:20140606-142611348",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140606-142611348",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"agency": "Science and Technology Facilities Council (STFC)",
"grant_number": "ST/K501979/1"
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{
"agency": "Science and Technology Facilities Council (STFC)",
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},
{
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"grant_number": "ST/J003697/1"
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"agency": "Leverhulme Trust"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
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"agency": "NSF",
"grant_number": "AST-1008067"
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{
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"grant_number": "44A-1092750"
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{
"agency": "NASA",
"grant_number": "NNX10AC99G"
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{
"agency": "NASA",
"grant_number": "NNX12AE38G"
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{
"agency": "NSF",
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},
{
"agency": "Swiss National Science Foundation (SNSF)",
"grant_number": "PP00P2_138979/1"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
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"author_list": "Lansbury, G. B.; Balokovi\u0107, M.; et el."
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},
"title": "NuSTAR J163433-4738.7: A Fast X-Ray Transient in the Galactic Plane",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: stellar content; stars: variables: general; surveys; X-rays: individual (NuSTAR J1634334738.7); X-rays: stars",
"note": "\u00a9 2014 American Astronomical Society. Received 2013 November 6; accepted 2014 February 7; published 2014 March 19. This work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. The authors\nthank the NuSTAR Operations, Software, and Calibration teams\nfor support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI\nScience Data Center (Italy) and the California Institute of Technology (USA). R.J.A. was supported by Gemini-CONICYT\ngrant 32120009. F.E.B. was supported by Basal-CATA\nPFB-06/2007 and CONICYT-Chile (through FONDECYT\n1101024, Gemini-CONICYT 32120003, and Anillo ACT1101).\nL.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. The authors thank Harvey Tananbaum for providing Chandra Director's Discretionary Time for this project. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.\n\nPublished - 0004-637X_785_1_4.pdf
Submitted - 1402.2292v2.pdf
",
"abstract": "During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8\u03c3 in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower significance. The source is not significantly detected by NuSTAR, Swift, or Chandra in the days before or weeks after the discovery of the transient, indicating that the strong X-ray activity lasted between ~0.5 and 1.5 days. Near-infrared imaging observations were carried out before and after the X-ray activity, but we are not able to identify the counterpart. The combined NuSTAR and Swift energy spectrum is consistent with a power law with a photon index of \u0393 = 4.1^(+1.5)_(-1.0) (90% confidence errors), a blackbody with kT = 1.2 \u00b1 0.3 keV, or a Bremsstrahlung model with kT = 3.0^(+2.1)_(-1.2) keV. The reduced-\u03c7^2 values for the three models are not significantly different, ranging from 1.23 to 1.44 for 8 degrees of freedom. The spectrum is strongly absorbed with N_H = (2.8^(+2.3)_(-1.4)) x 10^(23) cm^(\u20132), (9^(+15)_(-7)) x 10^(22) cm^(\u20132), and (1.7^(+1.7)_(-0.9)) x 10^(23) cm^(\u20132), for the power-law, blackbody, and Bremsstrahlung models, respectively. Although the high column density could be due to material local to the source, it is consistent with absorption from interstellar material along the line of sight at a distance of 11 kpc, which would indicate an X-ray luminosity >10^(34) erg s^(\u20131). Although we do not reach a definitive determination of the nature of NuSTAR J163433-4738.7, we suggest that it may be an unusually bright active binary or a magnetar.",
"date": "2014-04-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "785",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 4",
"id_number": "CaltechAUTHORS:20140606-135843500",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140606-135843500",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "32120009"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "FONDECYT 1101024"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "32120003"
},
{
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"grant_number": "ACT1101"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
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"author_list": "Tomsick, John A.; Gotthelf, Eric V.; et el."
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"name": {
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"name": {
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"given": "Charles J."
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"given": "Daniel"
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"name": {
"family": "Tomsick",
"given": "John A."
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"id": "Walton-D-J",
"name": {
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},
"title": "NuStar Discovery of a cyclotron line in KS 1947+300",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; radiation: dynamics; stars: neutron; X-rays: binaries; X-rays: individual (KS 1947+300)",
"note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 February 12; accepted for publication 2014 March 5; Published 2014 March 19; Issue 2 (2014 April 1).\n\nWe would like to thank Matthias K\u00fchnel, Ralf Ballhausen,\nFritz Schwarm, and Peter Kretschmar for useful discussions.\nThis work was supported under NASA contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded\nby the National Aeronautics and Space Administration. We\nthank the NuSTAR Operations, Software, and Calibration teams\nfor support with the execution and analysis of these observations.\nThis research has made use of the NuSTAR Data Analysis\nSoftware (NuSTARDAS) jointly developed by the ASI\nScience Data Center (ASDC, Italy) and the California Institute\nof Technology (USA). This research has made use of\nISIS functions provided by ECAP/Remeis observatory and\nMIT (http://www.sternwarte.uni-erlangen.de/isis/). We thank\nthe Deutsches Zentrum f\u00fcr Luft- und Raumfahrt for partial support under DLR grant 50 OR 1113. We thank the anonymous\nreferee for useful comments.\nFacilities: NuSTAR, Swift\n\nPublished - 2041-8205_784_2_L40.pdf
Draft - 1403.1901v1.pdf
",
"abstract": "We present a spectral analysis of three simultaneous Nuclear Spectroscopy Telescope Array and Swift/XRT observations of the transient Be-neutron star binary KS 1947+300 taken during its outburst in 2013/2014. These broadband observations were supported by Swift/XRT monitoring snapshots every three days, which we use to study the evolution of the spectrum over the outburst. We find strong changes of the power-law photon index, which shows a weak trend of softening with increasing X-ray flux. The neutron star shows very strong pulsations with a period of P \u2248 18.8 s. The 0.8\u201379 keV broadband spectrum can be described by a power law with an exponential cutoff and a blackbody component at low energies. During the second observation we detect a cyclotron resonant scattering feature at 12.5 keV, which is absent in the phase-averaged spectra of observations 1 and 3. Pulse phase-resolved spectroscopy reveals that the strength of the feature changes strongly with pulse phase and is most prominent during the broad minimum of the pulse profile. At the same phases the line also becomes visible in the first and third observation at the same energy. This discovery implies that KS 1947+300 has a magnetic field strength of B \u2248 1.1 \u00d7 10^(12) (1 + z) G, which is at the lower end of known cyclotron line sources.",
"date": "2014-04-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "784",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L40",
"id_number": "CaltechAUTHORS:20140403-155508973",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140403-155508973",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Deutsches Zentrum f\u00fcr Luft-und Raumfahrt (DLR)",
"grant_number": "50 OR 1113"
},
{
"agency": "NASA/JPL/Caltech"
}
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"doi": "10.1088/2041-8205/784/2/L40",
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"author_list": "F\u00fcrst, Felix; Pottschmidt, Katja; et el."
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},
"title": "X-ray Spectral Components Observed in the Afterglow of GRB 130925A",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "gamma-ray burst: individual (GRB 130925A)",
"note": "\u00a9 American Astronomical Society. \n\nReceived 2014 January 17; accepted 2014 February 26; published 2014 March 11. \n\nThis work was supported under NASA contract No. NNG08FD60C and uses data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National\nAeronautics and Space Administration. We thank the NuSTAR\nOperations team for executing the target of opportunity observations. This research has used the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI\nScience Data Center (ASDC, Italy) and the California Institute of Technology (USA). These results are based in part on observations made by the Chandra X-ray Observatory. We thank the Chandra director for granting discretionary time and the Chandra team for prompt execution of the observations.\nFacilities: NuSTAR, Swift, Chandra.\n\nPublished - 2041-8205_784_2_L19.pdf
Submitted - 1402.6755v1.pdf
",
"abstract": "We have identified spectral features in the late-time X-ray afterglow of the unusually long, slow-decaying GRB 130925A using NuSTAR, Swift/X-Ray Telescope, and Chandra. A spectral component in addition to an absorbed power law is required at >4\u03c3 significance, and its spectral shape varies between two observation epochs at 2 \u00d7 10^5 and 10^6 s after the burst. Several models can fit this additional component, each with very different physical implications. A broad, resolved Gaussian absorption feature of several keV width improves the fit, but it is poorly constrained in the second epoch. An additive blackbody or second power-law component provide better fits. Both are challenging to interpret: the blackbody radius is near the scale of a compact remnant (10^8 cm), while the second power-law component requires an unobserved high-energy cutoff in order to be consistent with the non-detection by Fermi/Large Area Telescope.",
"date": "2014-04-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "784",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L19",
"id_number": "CaltechAUTHORS:20140520-095049434",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-095049434",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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"doi": "10.1088/2041-8205/784/2/L19",
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"title": "High-energy X-Ray Detection of G359.89\u20130.08 (Sgr A\u2013E): Magnetic Flux Tube Emission Powered by Cosmic Rays?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center; X-rays: individual (Sgr A\u2013E, G359.89\u20130.08, XMM J17450\u20132904); X-rays: ISM",
"note": "\u00a9 2014 American Astronomical Society. Received 2013 November 19; accepted 2014 January 25; published 2014 February 25. This work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software and Calibration teams for support\nwith the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data Center\n(ASDC, Italy) and the California Institute of Technology\n(USA). S.Z. is partially supported by NASA Headquarters under\nthe NASA Earth and Space Science Fellowship Program\u2014\nGrant \"NNX13AM31.\" The authors wish to thank Mark Morris\nfor allowing them to view the recently acquired JVLA 6 cm\ncontinuum radio map of Sgr A\u2212E.\n\nPublished - 0004-637X_784_1_6.pdf
Submitted - 1401.7706v1.pdf
",
"abstract": "We report the first detection of high-energy X-ray (E > 10 keV) emission from the Galactic center non-thermal filament G359.89\u20130.08 (Sgr A\u2013E) using data acquired with the Nuclear Spectroscopic Telescope Array (NuSTAR). The bright filament was detected up to ~50 keV during a NuSTAR Galactic center monitoring campaign. The featureless power-law spectrum with a photon index \u0393 \u2248 2.3 confirms a non-thermal emission mechanism. The observed flux in the 3-79 keV band is F_X = (2.0 \u00b1 0.1) \u00d7 10^(\u201312) erg cm^(\u20132) s^(\u20131), corresponding to an unabsorbed X-ray luminosity L_X = (2.6 \u00b1 0.8) \u00d7 10^(34) erg s^(\u20131) assuming a distance of 8.0 kpc. Based on theoretical predictions and observations, we conclude that Sgr A\u2013E is unlikely to be a pulsar wind nebula (PWN) or supernova remnant-molecular cloud (SNR-MC) interaction, as previously hypothesized. Instead, the emission could be due to a magnetic flux tube which traps TeV electrons. We propose two possible TeV electron sources: old PWNe (up to ~100 kyr) with low surface brightness and radii up to ~30 pc or MCs illuminated by cosmic rays (CRs) from CR accelerators such as SNRs or Sgr A^*.",
"date": "2014-03-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "784",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 6",
"id_number": "CaltechAUTHORS:20140605-111540676",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140605-111540676",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX13AM31"
}
]
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"doi": "10.1088/0004-637X/784/1/6",
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"author_list": "Zhang, Shou; Hailey, Charles J.; et el."
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"title": "The Disk Wind in the Rapidly Spinning Stellar-mass Black Hole 4U 1630\u2013472 Observed with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 black hole physics \u2013 stars: winds, outflows \u2013 X-rays: binaries",
"note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2013 September 26; accepted 2014 January 15; published 2014 March 4.\n\nWe would like to thank Julia Lee for her invaluable comments. This work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13.\n\nPublished - 2041-8205_784_1_L2.pdf
Submitted - 1401.3646v1.pdf
",
"abstract": "We present an analysis of a short NuSTAR observation of the stellar-mass black hole and low-mass X-ray binary\n4U 1630\u2212472. Reflection from the inner accretion disk is clearly detected for the first time in this source, owing\nto the sensitivity of NuSTAR. With fits to the reflection spectrum, we find evidence for a rapidly spinning black\nhole, a\u2217 = 0.985^(+0.005)_(\u22120.014) (1\u03c3 statistical errors). However, archival data show that the source has relatively low radio luminosity. Recently claimed relationships between jet power and black hole spin would predict either a lower spin or a higher peak radio luminosity. We also report the clear detection of an absorption feature at 7.03 \u00b1 0.03 keV, likely signaling a disk wind. If this line arises in dense, moderately ionized gas (log \u03be = 3.6+0.2 \u22120.3) and is dominated by He-like Fe xxv, the wind has a velocity of v/c = 0.043^(+0.002)_(\u22120.007) (12900^(+600)_(\u22122100) km s^(\u22121)). If the line is instead associated with a more highly ionized gas (log \u03be = 6.1+0.7 \u22120.6), and is dominated by Fe xxvi, evidence of a blueshift is only marginal, after taking systematic errors into account. Our analysis suggests the ionized wind may be launched within 200\u20131100 Rg, and may be magnetically driven.",
"date": "2014-03-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "784",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L2",
"id_number": "CaltechAUTHORS:20140429-083422136",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-083422136",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
}
]
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{
"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "M."
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{
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"name": {
"family": "Marinucci",
"given": "A."
}
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{
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"family": "Ballantyne",
"given": "D. R."
},
"orcid": "0000-0001-8128-6976"
},
{
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"name": {
"family": "Boggs",
"given": "S. E."
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},
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"family": "Christensen",
"given": "F. E."
},
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},
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"name": {
"family": "Comastri",
"given": "A."
},
"orcid": "0000-0003-3451-9970"
},
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"name": {
"family": "Craig",
"given": "W. W."
}
},
{
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"name": {
"family": "Gandhi",
"given": "P."
},
"orcid": "0000-0003-3105-2615"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
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"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
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"name": {
"family": "Madejski",
"given": "G."
}
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{
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"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The hard X-ray spectrum of NGC 5506 as seen by NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 December 12. Received 2014 November 25. In original form 2014 October 8. First published online January 14, 2015. \n\nThis work has made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). GM, AM and AC acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13. GM and AM also acknowledge financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. MB acknowledges support from the Fulbright International Science and Technology Award.\n\nPublished - MNRAS-2015-Matt-3029-33.pdf
",
"abstract": "NuSTAR observed the bright Compton-thin, narrow-line Seyfert 1 galaxy, NGC 5506, for about 56 ks. In agreement with past observations, the spectrum is well fitted by a power law with \u0393 \u223c 1.9, a distant reflection component and narrow ionized iron lines. A relativistically blurred reflection component is not required by the data. When an exponential high-energy cutoff is added to the power law, a value of 720+130/190 keV (90\u2009per\u2009cent confidence level) is found. Even allowing for systematic uncertainties, we find a 3\u03c3 lower limit to the high-energy cutoff of 350 keV, the highest lower limit to the cutoff energy found so far in an AGN by NuSTAR.",
"date": "2014-03-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "447",
"number": "4",
"publisher": "Royal Astronomical Society",
"pagerange": "3029-3033",
"id_number": "CaltechAUTHORS:20150404-122323766",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150404-122323766",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "ASI/INAF I/037/12/0- 011/13"
},
{
"agency": "European Community Seventh Framework Programme",
"grant_number": "FP7/2007-2013, 312789"
},
{
"agency": "Fulbright International Science and Technology Award"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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{
"id": "2015-69",
"name": "Space Radiation Laboratory"
}
]
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}
]
},
"doi": "10.1093/mnras/stu2653",
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"pub_year": "2014",
"author_list": "Matt, G.; Balokovi\u0107, M.; et el."
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"items": [
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "H."
}
},
{
"id": "Bhalerao-V-B",
"name": {
"family": "Bhalerao",
"given": "V."
},
"orcid": "0000-0002-6112-7609"
},
{
"id": "Bellm-E-C",
"name": {
"family": "Bellm",
"given": "E. C."
},
"orcid": "0000-0001-8018-5348"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V. R."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Tendulkar-S",
"name": {
"family": "Tendulkar",
"given": "S."
}
}
]
},
"title": "NuSTAR results and future plans for magnetar and rotation-powered pulsar observations",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "space vehicles; stars: neutron; telescopes; X-rays: stars",
"note": "\u00a9 2014 Wiley-VCH Verlag GmbH&Co. KGaA, Weinheim.\n\nReceived 2013 Dec 20; accepted 2014 Jan 14; Published online 2014 Mar 16.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support\nwith the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data Center\n(ASDC, Italy) and the California Institute of Technology (USA). V.M.K. acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program and the Lorne Trottier Chair in Astrophysics and Cosmology. A.M.B. acknowledges the support by NASA grants NNX10AI72G and NNX13AI34G. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DEAC52-07NA27344.\n\nSubmitted - 1402.1079v1.pdf
",
"abstract": "The Nuclear Spectroscopic Telescope Array (NuSTAR) is the first focusing hard X-ray mission in orbit and operates in the 3\u201379 keV range. NuSTAR's sensitivity is roughly two orders of magnitude better than previous missions in this energy band thanks to its superb angular resolution. Since its launch in 2012 June, NuSTAR has performed excellently and observed many interesting sources including four magnetars, two rotation-powered pulsars and the cataclysmic variable AE Aquarii. NuSTAR also discovered 3.76-s pulsations from the transient source SGR J1745\u201329 recently found by Swift very close to the Galactic center, clearly identifying the source as a transient magnetar. For magnetar 1E 1841\u2013045, we show that the spectrum is well fit by an absorbed blackbody plus broken power-law model with a hard power-law photon index of \u223c 1.3. This is consistent with previous results by INTEGRAL and RXTE. We also find an interesting double-peaked pulse profile in the 25\u201335 keV band. For AE Aquarii, we show that the spectrum can be described by a multi-temperature thermal model or a thermal plus non-thermal model; a multi-temperature thermal model without a non-thermal component cannot be ruled out. Furthermore, we do not see a spiky pulse profile in the hard X-ray band, as previously reported based on Suzaku observations. For other magnetars and rotation-powered pulsars observed with NuSTAR, data analysis results will be soon available.",
"date": "2014-03",
"date_type": "published",
"publication": "Astronomische Nachrichten",
"volume": "335",
"number": "3",
"publisher": "Wiley",
"pagerange": "280-284",
"id_number": "CaltechAUTHORS:20140410-114248478",
"issn": "0004-6337",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140410-114248478",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Fonds de recherche du Qu\u00e9be-Nature et technologies (FRQ-NT)"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canada Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
},
{
"agency": "NASA",
"grant_number": "NNX10AI72G"
},
{
"agency": "NASA",
"grant_number": "NNX13AI34G"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-AC52-07NA27344"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-68",
"name": "Space Radiation Laboratory"
}
]
},
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{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"corp_creators": {
"items": [
"NuSTAR Team"
]
},
"doi": "10.1002/asna.201312032",
"primary_object": {
"basename": "1402.1079v1.pdf",
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"pub_year": "2014",
"author_list": "An, H.; Bhalerao, V.; et el."
},
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"items": [
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Forster-K",
"name": {
"family": "Forster",
"given": "K."
},
"orcid": "0000-0001-5800-5531"
},
{
"id": "Mao-Peter-H",
"name": {
"family": "Mao",
"given": "P. H."
}
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "H."
},
"orcid": "0000-0002-8074-4186"
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{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "V."
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]
},
"title": "Asymmetries in core-collapse supernovae from maps of radioactive ^(44)Ti in Cassiopeia A",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "High-energy astrophysics; Particle astrophysics",
"note": "\u00a9 2014 Macmillan Publishers Limited. \n\nReceived 27 August 2013. Accepted 13 December 2013. Published online 19 February 2014.\n\nThis work was supported by NASA under grant no. NNG08FD60C, and made use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory and funded by NASA. We thank the NuSTAR operations, software and calibration teams for support with execution and analysis of these observations.\n\nSubmitted - 1403.4978v1.pdf
Supplemental Material - nature12997-sf1.jpg
Supplemental Material - nature12997-sf2.jpg
Supplemental Material - nature12997-sf3.jpg
Supplemental Material - nature12997-sf4.jpg
Supplemental Material - nature12997-sf5.jpg
Supplemental Material - nature12997-st1.jpg
Supplemental Material - nature12997-st2.jpg
Supplemental Material - nature12997-st3.jpg
",
"abstract": "Asymmetry is required by most numerical simulations of stellar core-collapse explosions, but the form it takes differs significantly among models. The spatial distribution of radioactive ^(44)Ti, synthesized in an exploding star near the boundary between material falling back onto the collapsing core and that ejected into the surrounding medium, directly probes the explosion asymmetries. Cassiopeia\u2009A is a young, nearby, core-collapse remnant from which ^(44)Ti emission has previously been detected but not imaged. Asymmetries in the explosion have been indirectly inferred from a high ratio of observed ^(44)Ti emission to estimated ^(56)Ni emission, from optical light echoes, and from jet-like features seen in the X-ray and optical ejecta. Here we report spatial maps and spectral properties of the ^(44)Ti in Cassiopeia A. This may explain the unexpected lack of correlation between the ^(44)Ti and iron X-ray emission, the latter being visible only in shock-heated material. The observed spatial distribution rules out symmetric explosions even with a high level of convective mixing, as well as highly asymmetric bipolar explosions resulting from a fast-rotating progenitor. Instead, these observations provide strong evidence for the development of low-mode convective instabilities in core-collapse supernovae.",
"date": "2014-02-20",
"date_type": "published",
"publication": "Nature",
"volume": "506",
"number": "7488",
"publisher": "Nature Publishing Group",
"pagerange": "339-342",
"id_number": "CaltechAUTHORS:20140326-135228627",
"issn": "0028-0836",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140326-135228627",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-02",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1038/nature12997",
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"pub_year": "2014",
"author_list": "Grefenstette, B. W.; Harrison, F. A.; et el."
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"items": [
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "Takao"
}
},
{
"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
}
},
{
"id": "Beloborodov-A-M",
"name": {
"family": "Beloborodov",
"given": "Andrei M."
}
},
{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "Eric V."
},
"orcid": "0000-0003-3847-3957"
},
{
"id": "Hayashi-Takayuki",
"name": {
"family": "Hayashi",
"given": "Takayuki"
}
},
{
"id": "Kaspi-V-M",
"name": {
"family": "Kaspi",
"given": "Victoria M."
},
"orcid": "0000-0001-9345-0307"
},
{
"id": "Rana-V-R",
"name": {
"family": "Rana",
"given": "Vikram R."
},
"orcid": "0000-0003-1703-8796"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "Will W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR and Swift observations of the fast rotating magnetized white dwarf AE Aquarii",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; novae, cataclysmic variables; stars: individual (AE Aquarii); white dwarfs; X-rays: stars",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 October 31; accepted 2013 December 17; published 2014 January 17. \n\nThis work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams and the Swift Operations team for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA) and the XRT Data Analysis Software (XRTDAS) developed under the responsibility of ASDC. T.K. was supported by Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Young Scientists (B) (No. 24740185). \n\nFacilities: NuSTAR, Swift\n\nPublished - 0004-637X_782_1_3.pdf
Submitted - 1312.5039v1.pdf
",
"abstract": "AE Aquarii is a cataclysmic variable with the fastest known rotating magnetized white dwarf (P_(spin) = 33.08 s). Compared to many intermediate polars, AE Aquarii shows a soft X-ray spectrum with a very low luminosity (L X ~ 10^(31) erg s^(\u20131)). We have analyzed overlapping observations of this system with the NuSTAR and the Swift X-ray observatories in 2012 September. We find the 0.5-30 keV spectra to be well fitted by either an optically thin thermal plasma model with three temperatures of 0.75^(+0.18)_(-0.45), 2.29^(+0.96)_(-0.82), and 9.33^(+6.07)_(-2.18) keV, or an optically thin thermal plasma model with two temperatures of 1.00^(+0.34)_(-0.23) and 4.64^(+1.58)_(-0.84) keV plus a power-law component with photon index of 2.50^(+0.17)_(-0.23). The pulse profile in the 3-20 keV band is broad and approximately sinusoidal, with a pulsed fraction of 16.6% \u00b1 2.3%. We do not find any evidence for a previously reported sharp feature in the pulse profile.",
"date": "2014-02-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "782",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 3",
"id_number": "CaltechAUTHORS:20140417-103033745",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-103033745",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "24740185"
}
]
},
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"items": [
{
"id": "2014-69",
"name": "Space Radiation Laboratory"
}
]
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"id": "NuSTAR"
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"id": "Space-Radiation-Laboratory"
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"doi": "10.1088/0004-637X/782/1/3",
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],
"pub_year": "2014",
"author_list": "Kitaguchi, Takao; An, Hongjun; et el."
},
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{
"id": "Brenneman-L-W",
"name": {
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"given": "L. W."
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{
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"name": {
"family": "Madejski",
"given": "G."
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{
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"name": {
"family": "Matt",
"given": "G."
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"family": "Elvis",
"given": "M."
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"name": {
"family": "Ballantyne",
"given": "D. R."
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"family": "Grefenstette",
"given": "B. W."
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{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
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"given": "K. K."
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"name": {
"family": "Marinucci",
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{
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"name": {
"family": "Walton",
"given": "D. J."
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{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "Measuring the Coronal Properties of IC 4329A with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; galaxies: active; galaxies: individual (IC 4329A); galaxies: nuclei; galaxies: Seyfert; X-rays: galaxies",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 October 18; accepted 2013 December 11; published 2014 January 13. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). L.B. gratefully acknowledges funding from NASA grant NNX13AE90G. G.M. and A.M. acknowledge financial support from the Italian Space Agency under contract ASI/INAF I/037/12/0-011/13.\n\nPublished - 0004-637X_781_2_83.pdf
",
"abstract": "We present an analysis of a ~160 ks NuSTAR observation of the nearby bright Seyfert galaxy IC 4329A. The high-quality broadband spectrum enables us to separate the effects of distant reflection from the direct coronal continuum, and to therefore accurately measure the high-energy cutoff to be E_(cut)=178^(+74)_(-40) keV. The coronal emission arises from accretion disk photons Compton up-scattered by a thermal plasma, with the spectral index and cutoff being due to a combination of the finite plasma temperature and optical depth. Applying standard Comptonization models, we measure both physical properties independently using the best signal to noise obtained to date in an active galactic nucleus over the 3-79 keV band. We derive kT_e=37^(+7)_(-6) keV with \u03c4 =1.25^(+0.20)_(-0.10) assuming a slab geometry for the plasma, and kT_e=33^(+6)_(-6)keV with \u03c4 = 3.41^(+0.58)_(-0.38) for a spherical geometry, with both having an equivalent goodness-of-fit.",
"date": "2014-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "781",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 83",
"id_number": "CaltechAUTHORS:20140320-153441616",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140320-153441616",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA",
"grant_number": "NNX13AE90G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-71",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/781/2/83",
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},
"pub_year": "2014",
"author_list": "Brenneman, L. W.; Madejski, G.; et el."
},
{
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"eprint_id": 44441,
"eprint_status": "archive",
"datestamp": "2023-08-22 11:41:05",
"lastmod": "2023-10-26 00:29:05",
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"items": [
{
"id": "Krivonos-R-A",
"name": {
"family": "Krivonos",
"given": "Roman A."
},
"orcid": "0000-0003-2737-5673"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "John A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "Franz E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Baganoff-F-K",
"name": {
"family": "Baganoff",
"given": "Frederick K."
}
},
{
"id": "Barriere-N-M",
"name": {
"family": "Barriere",
"given": "Nicolas M."
}
},
{
"id": "Bodaghee-A",
"name": {
"family": "Bodaghee",
"given": "Arash"
},
"orcid": "0000-0002-7315-3732"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
}
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "JaeSub"
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
},
{
"id": "Nynka-M",
"name": {
"family": "Nynka",
"given": "Melania"
},
"orcid": "0000-0002-3310-1946"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "First Hard X-Ray Detection of the Non-thermal Emission around the Arches Cluster: Morphology and Spectral Studies with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "cosmic rays; Galaxy: center; ISM: general; X-rays: individual (Arches cluster)",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 September 30; accepted 2013 December 7; published 2014 January 15. \n\nThis work was supported under NASA Contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software, and Calibration teams for support\nwith the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data Center\n(ASDC, Italy) and the California Institute of Technology\n(USA). F.E.B. acknowledges support from Basal-CATA\n(PFB-06/2007) and CONICYT-Chile (FONDECYT 1101024\nand Anillo ACT1101). R.K. thanks Eugene Churazov for fruitful\ndiscussions and valuable suggestions to the paper. \n\nFacility: NuSTAR\n\nPublished - 0004-637X_781_2_107.pdf
Submitted - 1312.2635v1.pdf
",
"abstract": "The Arches cluster is a young, densely packed massive star cluster in our Galaxy that shows a high level of star formation activity. The nature of the extended non-thermal X-ray emission around the cluster remains unclear. The observed bright Fe K\u03b1 line emission at 6.4 keV from material that is neutral or in a low ionization state can be produced either by X-ray photoionization or by cosmic-ray particle bombardment or both. In this paper, we report on the first detection of the extended emission around the Arches cluster above 10 keV with the NuSTAR mission, and present results on its morphology and spectrum. The spatial distribution of the hard X-ray emission is found to be consistent with the broad region around the cluster where the 6.4 keV line is observed. The interpretation of the hard X-ray emission within the context of the X-ray reflection model puts a strong constraint on the luminosity of the possible illuminating hard X-ray source. The properties of the observed emission are also in broad agreement with the low-energy cosmic-ray proton excitation scenario.",
"date": "2014-02-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "781",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 107",
"id_number": "CaltechAUTHORS:20140321-092114962",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140321-092114962",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1101024"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2014-70",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/781/2/107",
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],
"pub_year": "2014",
"author_list": "Krivonos, Roman A.; Tomsick, John A.; et el."
},
{
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"eprint_id": 43782,
"eprint_status": "archive",
"datestamp": "2023-08-22 11:30:56",
"lastmod": "2023-10-25 23:52:08",
"type": "article",
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"creators": {
"items": [
{
"id": "Ofek-E-O",
"name": {
"family": "Ofek",
"given": "Eran O."
},
"orcid": "0000-0002-6786-8774"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kulkarni-S-R",
"name": {
"family": "Kulkarni",
"given": "Shrinivas R."
},
"orcid": "0000-0001-5390-8563"
},
{
"id": "Bellm-E-C",
"name": {
"family": "Bellm",
"given": "Eric"
},
"orcid": "0000-0001-8018-5348"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "Brian"
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Laher-R-R",
"name": {
"family": "Laher",
"given": "Russ"
},
"orcid": "0000-0003-2451-5482"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin"
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Surace-J-A",
"name": {
"family": "Surace",
"given": "Jason"
},
"orcid": "0000-0001-7291-0087"
}
]
},
"title": "SN 2010jl: Optical to Hard X-Ray Observations Reveal an Explosion Embedded in a Ten Solar Mass Cocoon",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "stars: mass-loss; supernovae: general; supernovae: individual (SN 2010jl)",
"note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2013 July 2; accepted 2013 November 25; published 2014 January 6.\n\nWe thank an anonymous referee for a constructive report.\nE.O.O. thanks Roni Waldman, Nir Sapir, and Orly Gnat for\ndiscussions. This work was supported under NASA Contract\nNo. NNG08FD60C and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of\nTechnology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science, Israel Science Foundation, Minerva, and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant No 1829/12). A.V.F.'s SN group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916.\n\nPublished - 0004-637X_781_1_42.pdf
Submitted - 1307.2247v1.pdf
",
"abstract": "Some supernovae (SNe) may be powered by the interaction of the SN ejecta with a large amount of circumstellar matter (CSM). However, quantitative estimates of the CSM mass around such SNe are missing when the CSM material is optically thick. Specifically, current estimators are sensitive to uncertainties regarding the CSM density profile and the ejecta velocity. Here we outline a method to measure the mass of the optically thick CSM around such SNe. We present new visible-light and X-ray observations of SN 2010jl (PTF 10aaxf), including the first detection of an SN in the hard X-ray band using NuSTAR. The total radiated luminosity of SN 2010jl is extreme\u2014at least 9 \u00d7 10^50 erg. By modeling the visible-light data, we robustly show that the mass of the circumstellar material within ~10^16 cm of the progenitor of SN 2010jl was in excess of 10 M_\u2609. This mass was likely ejected tens of years prior to the SN explosion. Our modeling suggests that the shock velocity during shock breakout was ~6000 km s^\u20131, decelerating to ~2600 km s^\u20131 about 2 yr after maximum light. Furthermore, our late-time NuSTAR and XMM spectra of the SN presumably provide the first direct measurement of SN shock velocity 2 yr after the SN maximum light\u2014measured to be in the range of 2000-4500 km s^\u20131 if the ions and electrons are in equilibrium, and \u2273 2000 km s^\u20131 if they are not in equilibrium. This measurement is in agreement with the shock velocity predicted by our modeling of the visible-light data. Our observations also show that the average radial density distribution of the CSM roughly follows an r^\u20132 law. A possible explanation for the \u2273 10 M_\u2609 of CSM and the wind-like profile is that they are the result of multiple pulsational pair instability events prior to the SN explosion, separated from each other by years.",
"date": "2014-01-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "781",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 42",
"id_number": "CaltechAUTHORS:20140211-134538316",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140211-134538316",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "Ministry of Science (Israel)"
},
{
"agency": "Minerva"
},
{
"agency": "Planning and Budgeting Committee I-CORE Program"
},
{
"agency": "Israel Science Foundation",
"grant_number": "1829/12"
},
{
"agency": "Gary and Cynthia Bengier"
},
{
"agency": "Christopher R. Redlich Fund"
},
{
"agency": "Richard and Rhoda Goldman Fund"
},
{
"agency": "TABASGO Foundation"
},
{
"agency": "NSF",
"grant_number": "AST-1211916"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "Palomar-Transient-Factory"
},
{
"id": "Division-of-Geological-and-Planetary-Sciences"
}
]
},
"doi": "10.1088/0004-637X/781/1/42",
"primary_object": {
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],
"pub_year": "2014",
"author_list": "Ofek, Eran O.; Harrison, Fiona A.; et el."
},
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"name": {
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"given": "Katja"
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"orcid": "0000-0002-4656-6881"
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{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
},
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"name": {
"family": "Tomsick",
"given": "John A."
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"orcid": "0000-0001-5506-9855"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
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"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
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"family": "Christensen",
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"name": {
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"family": "Grefenstette",
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},
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"name": {
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"family": "Madsen",
"given": "Kristin K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "Jon M."
}
},
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"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
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"name": {
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},
"title": "NuSTAR Discovery of a Luminosity Dependent Cyclotron Line Energy in Vela X-1",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion; accretion disks; radiation: dynamics; stars: neutron; X-rays: binaries; X-rays: individual (Vela X-1)",
"note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2013 September 16; accepted 2013 November 19; published 2013 December 18.\n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data Center\n(ASDC, Italy) and the California Institute of Technology\n(USA). We would like to thank John E. Davis for the slxfig\nmodule, which was used to produce all figures in this work.\nWe would like to thank Fritz Schwarm for the helpful discussions about cyclotron line shapes. J.A.T. acknowledges partial support from NASA Astrophysics Data Analysis Program grant NNX13AE98G. M.B. was supported by the Centre National d'\u00c9tudes Spatiales (CNES). We would like to thank the anonymous referee for the useful comments.\nFacility: NuSTAR\n\nPublished - 0004-637X_780_2_133.pdf
Submitted - 1311.5514v1.pdf
",
"abstract": "We present NuSTAR observations of Vela X-1, a persistent, yet highly variable, neutron star high-mass X-ray binary (HMXB). Two observations were taken at similar orbital phases but separated by nearly a year. They show very different 3\u201379 keV flux levels as well as strong variability during each observation, covering almost one order of magnitude in flux. These observations allow, for the first time ever, investigations on kilo-second time-scales of how the centroid energies of cyclotron resonant scattering features (CRSFs) depend on flux for a persistent HMXB. We find that the line energy of the harmonic CRSF is correlated with flux, as expected in the sub-critical accretion regime. We argue that Vela X-1 has a very narrow accretion column with a radius of around 0.4 km that sustains a Coulomb interaction dominated shock at the observed luminosities of L_x ~ 3 \u00d7 10^36 erg s^\u22121. Besides the prominent harmonic line at 55 keV the fundamental line around 25 keV is clearly detected. We find that the strengths of the two CRSFs are anti-correlated, which we explain by photon spawning. This anti-correlation is a possible explanation for the debate about the existence of the fundamental line. The ratio of the line energies is variable with time and deviates significantly from 2.0, also a possible consequence of photon spawning, which changes the shape of the line. During the second observation, Vela X-1 showed a short off-state in which the power-law softened and a cut-off was no longer measurable. It is likely that the source switched to a different accretion regime at these low mass accretion rates, explaining the drastic change in spectral shape.",
"date": "2014-01-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "780",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 133",
"id_number": "CaltechAUTHORS:20140218-153815613",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140218-153815613",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX13AE98G"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
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"doi": "10.1088/0004-637X/780/2/133",
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"pub_year": "2014",
"author_list": "F\u00fcrst, Felix; Pottschmidt, Katja; et el."
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"given": "William W."
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"family": "Kretschmar",
"given": "P."
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"id": "Audard-M",
"name": {
"family": "Audard",
"given": "M."
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{
"id": "Falanga-M",
"name": {
"family": "Falanga",
"given": "M."
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"title": "NuSTAR detection of 4s Hard X-ray Lags from the Accreting Pulsar GS 0834-430",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 Owned by the authors, published by EDP Sciences, 2014. This is an Open Access article distributed under the terms of the Creative Commons Attribution License 2.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.\n\nPublished - epjconf_mag2013_06011.pdf
",
"abstract": "The NuSTAR hard X-ray telescope observed the transient Be/X-ray binary GS 0834-430 during its 2012 outburst. The source is detected between 3 - 79 keV with high statistical significance, and we were able to perform very accurate spectral and timing analysis. The phase-averaged spectrum is consistent with that observed in many other magnetized accreting pulsars. We fail to detect cyclotron resonance scattering features in either phase-averaged nor phase-resolved spectra that would allow us to constrain the pulsar's magnetic field. We detect a pulse period of ~ 12:29 s in all energy bands. The pulse profile can be modeled with a double Gaussian and shows a strong and smooth hard lag of up to 0.3 cycles in phase, or about 4s between the pulse at ~ 3 and \u2273 30 keV. This is the first report of such a strong lag in high-mass X-ray binary (HMXB) pulsars. Previously reported lags have been significantly smaller in phase and restricted to low-energies (E<10 keV). We investigate the possible mechanisms that might produce such lags. We find the most likely explanation for this effect to be a complex beam geometry.",
"date": "2014-01-08",
"date_type": "published",
"publication": "EPJ Web of Conferences",
"volume": "64",
"publisher": "EDP Sciences",
"pagerange": "Art. No. 06011",
"id_number": "CaltechAUTHORS:20161025-194735540",
"issn": "2100-014X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161025-194735540",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"other_numbering_system": {
"items": [
{
"id": "2014-72",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
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"doi": "10.1051/epjconf/20136406011",
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"pub_year": "2014",
"author_list": "Bozzo, E.; Bachetti, Matteo; et el."
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"family": "Ubertini",
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"given": "William W."
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},
"title": "NuSTAR and INTEGRAL Observations of a Low/Hard State of 1E1740.7-2942",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics; X-rays: binaries; X-rays: individual (1E 1740.7-2942)",
"note": "\u00a9 2014 American Astronomical Society. Received 2013 September 2; accepted 2013 October 29; published 2013 December 12. This work was supported under NASA contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by the\nNational Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software and Calibration teams for support\nwith the execution and analysis of these observations. This\nresearch has made use of the NuSTAR Data Analysis Software\n(NuSTARDAS) jointly developed by the ASI Science Data Center\n(ASDC, Italy) and the California Institute of Technology\n(USA). L.N. wishes to acknowledge the Italian Space Agency\n(ASI) for financial support by ASI/INAF grants I/037/12/\n0-011/13 and I/033/10/0 and the engineering support of M.\nFederici for setup and maintenance of the INTEGRAL archive\nand Data Analysis Software at IAPS. M.B. wishes to acknowledge\nthe support from the Centre National d'Etudes Spatiales\n(CNES).\n\nPublished - 0004-637X_780_1_63.pdf
Submitted - 1310.7870v1.pdf
",
"abstract": "The microquasar 1E1740.7-2942, also known as the \"Great Annihilator,\" was observed by NuSTAR in the summer of 2012. We have analyzed in detail two observations taken ~2 weeks apart, for which we measure hard and smooth spectra typical of the low/hard state. A few weeks later the source flux declined significantly. Nearly simultaneous coverage by INTEGRAL is available from its Galactic Center monitoring campaign lasting ~2.5 months. These data probe the hard state spectrum from 1E1740.7-2942 before the flux decline. We find good agreement between the spectra taken with IBIS/ISGRI and NuSTAR, with the measurements being compatible with a change in flux with no spectral variability. We present a detailed analysis of the NuSTAR spectral and timing data and upper limits for reflection of the high energy emission. We show that the high energy spectrum of this X-ray binary is well described by thermal Comptonization.",
"date": "2014-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "780",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 63",
"id_number": "CaltechAUTHORS:20140130-145205686",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140130-145205686",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/ 0-011/13"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/033/10/0"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
"local_group": {
"items": [
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"doi": "10.1088/0004-637X/780/1/63",
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"pub_year": "2014",
"author_list": "Natalucci, Lorenzo; Tomsick, John A.; et el."
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"given": "Charles J."
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"family": "Ross",
"given": "Randy R."
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},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "Dominic J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Wilms-J",
"name": {
"family": "Wilms",
"given": "J\u00f6rn"
},
"orcid": "0000-0003-2065-5410"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "The Reflection Component from Cygnus X-1 in the Soft State Measured by NuSTAR and Suzaku",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics; stars: individual (Cygnus X-1); X-rays: general; X-rays: stars",
"note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 September 3; accepted 2013 October 14; published 2013 December 13. \n\nThis work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). J.A.T. acknowledges partial support from NASA Astrophysics Data Analysis Program grant NNX13AE98G. L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13. J.A.T. thanks L. Brenneman, G. Matt, and D. Ballantyne for useful discussions about reflection modeling. This work made use of IDL software written by N. Barri\u00e8re for rebinning the NuSTAR spectra. This research has made use of the MAXI data provided by RIKEN, JAXA, and the MAXI team.\n\nPublished - 0004-637X_780_1_78.pdf
Submitted - 1310.3830v1.pdf
",
"abstract": "The black hole binary Cygnus X-1 was observed in late 2012 with the Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku, providing spectral coverage over the ~1-300 keV range. The source was in the soft state with a multi-temperature blackbody, power law, and reflection components along with absorption from highly ionized material in the system. The high throughput of NuSTAR allows for a very high quality measurement of the complex iron line region as well as the rest of the reflection component. The iron line is clearly broadened and is well described by a relativistic blurring model, providing an opportunity to constrain the black hole spin. Although the spin constraint depends somewhat on which continuum model is used, we obtain \u0251_* > 0.83 for all models that provide a good description of the spectrum. However, none of our spectral fits give a disk inclination that is consistent with the most recently reported binary values for Cyg X-1. This may indicate that there is a >13\u00b0 misalignment between the orbital plane and the inner accretion disk (i.e., a warped accretion disk) or that there is missing physics in the spectral models.",
"date": "2014-01-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "780",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 78",
"id_number": "CaltechAUTHORS:20140131-084009659",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140131-084009659",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA",
"grant_number": "NNX13AE98G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
}
]
},
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{
"id": "NuSTAR"
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"doi": "10.1088/0004-637X/780/1/78",
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"pub_year": "2014",
"author_list": "Tomsick, John A.; Nowak, Michael A.; et el."
},
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{
"id": "Walton-D-J",
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{
"id": "F\u00fcrst-F",
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"given": "M."
},
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"name": {
"family": "Barret",
"given": "D."
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"family": "Bauer",
"given": "F."
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"name": {
"family": "Boggs",
"given": "S. E."
},
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{
"id": "Christensen-F-E",
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"family": "Madsen",
"given": "K. K."
},
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"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
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"name": {
"family": "Ptak",
"given": "A."
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{
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"name": {
"family": "Rana",
"given": "V."
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"orcid": "0000-0003-1703-8796"
},
{
"id": "Webb-N-A",
"name": {
"family": "Webb",
"given": "N. A."
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "An Extremely Luminous and Variable Ultraluminous X-Ray Source in the Outskirts of Circinus Observed with NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "black hole physics; X-rays: binaries; X-rays: individual (Circinus ULX5)",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 August 18; accepted 2013 October 8; published 2013 December 3. \n\nThe authors thank Koji Mukai for useful discussion regarding Galactic CVs, and Rubens Reis for discussion regarding Galactic BHBs. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA,\nand the Suzaku observatory, a collaborative mission between\nthe space agencies of Japan (JAXA) and the USA (NASA). In\naddition, this research has also made use of data obtained from NASA's Swift, Chandra, and Spitzer satellites. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). We also made use of the NASA/IPAC Extragalactic Database (NED), which is operated by JPL, Caltech, under contract with NASA. Some of the figures included in this work have been produced with the Veusz plotting package: http://home.gna.org/veusz, written and maintained by Jeremy Sanders. F.E.B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (under grants FONDECYT 1101024 and Anillo ACT1101). M.B.\nwishes to acknowledge the support from the Centre National\nD\u00b4Etudes Spatiales (CNES).\n\nPublished - 0004-637X_779_2_148.pdf
Submitted - 1310.2633v1.pdf
",
"abstract": "Following a serendipitous detection with the Nuclear Spectroscopic Telescope Array (NuSTAR), we present a multi-epoch spectral and temporal analysis of an extreme ultraluminous X-ray source (ULX) located in the outskirts of the Circinus galaxy, hereafter Circinus ULX5, including coordinated XMM-Newton+NuSTAR follow-up observations. The NuSTAR data presented here represent one of the first instances of a ULX reliably detected at hard (E > 10 keV) X-rays. Circinus ULX5 is variable on long time scales by at least a factor of ~5 in flux, and was caught in a historically bright state during our 2013 observations (0.3-30.0 keV luminosity of 1.6 \u00d7 10^(40) erg s^(\u20131)). During this epoch, the source displayed a curved 3-10 keV spectrum, broadly similar to other bright ULXs. Although pure thermal models result in a high energy excess in the NuSTAR data, this excess is too weak to be modeled with the disk reflection interpretation previously proposed to explain the 3-10 keV curvature in other ULXs. In addition to flux variability, clear spectral variability is also observed. While in many cases the interpretation of spectral components in ULXs is uncertain, the spectral and temporal properties of all the high quality data sets currently available strongly support a simple disk-corona model reminiscent of that invoked for Galactic binaries, with the accretion disk becoming more prominent as the luminosity increases. However, although the disk temperature and luminosity are well correlated across all time scales currently probed, the observed luminosity follows L \u221d T^(1.70\u00b10.17), flatter than expected for simple blackbody radiation. The spectral variability displayed here is highly reminiscent of that observed from known Galactic black hole binaries (BHBs) at high luminosities. This comparison implies a black hole mass of ~90 M_\u2299 for Circinus ULX5. However, given the diverse behavior observed from Galactic BHB accretion disks, this mass estimate is still uncertain. Finally, the limits placed on any undetected iron absorption features with the 2013 data set imply that we are not viewing the central regions of Circinus ULX5 through any extreme super-Eddington outflow.",
"date": "2013-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "779",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 148",
"id_number": "CaltechAUTHORS:20140121-112443927",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140121-112443927",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1101024"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
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"doi": "10.1088/0004-637X/779/2/148",
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"pub_year": "2013",
"author_list": "Walton, D. J.; Fuerst, F.; et el."
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"id": "An-Hongjun",
"name": {
"family": "An",
"given": "Hongjun"
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"name": {
"family": "Hasco\u00ebt",
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"name": {
"family": "Kaspi",
"given": "Victoria M."
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"name": {
"family": "Beloborodov",
"given": "Andrei M."
}
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"name": {
"family": "Dufour",
"given": "Fran\u00e7ois"
}
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{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "Eric V."
},
"orcid": "0000-0003-3847-3957"
},
{
"id": "Archibald-R-F",
"name": {
"family": "Archibald",
"given": "Robert"
},
"orcid": "0000-0002-4017-8837"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
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},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
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"orcid": "0000-0001-5679-1946"
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"name": {
"family": "Craig",
"given": "William W."
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"name": {
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"given": "Brian W."
},
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},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
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{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Kitaguchi-Takao",
"name": {
"family": "Kitaguchi",
"given": "Takao"
}
},
{
"id": "Kouveliotou-C",
"name": {
"family": "Kouveliotou",
"given": "Chryssa"
},
"orcid": "0000-0003-1443-593X"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin K."
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"orcid": "0000-0003-1252-4891"
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{
"id": "Markwardt-C-B",
"name": {
"family": "Markwardt",
"given": "Craig B."
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"orcid": "0000-0001-9803-3879"
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{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
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{
"id": "Vogel-J-K",
"name": {
"family": "Vogel",
"given": "Julia K."
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},
"title": "NuSTAR Observations of Magnetar 1E 1841\u2013045",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "pulsars: individual (1E 1841\u2013045); stars: magnetars; stars: neutron",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 August 12; accepted 2013 October 22; published 2013 December 3. \n\nThis work was supported under NASA contract NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software, and Calibration Teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS), jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (US). V.M.K. acknowledges support from an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Qu\u00e9bec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics\nand Cosmology. A.M.B. acknowledges the support \nby NASA grants NNX10AI72G and NNX13AI34G. Part of this\nwork was performed under the auspices of the US Department\nof Energy by Lawrence Livermore National Laboratory under\ncontract DE-AC52-07NA27344.\n\nPublished - 0004-637X_779_2_163.pdf
Submitted - 1310.6221v2.pdf
",
"abstract": "We report new spectral and temporal observations of the magnetar 1E 1841\u2013045 in the Kes 73 supernova remnant obtained with the Nuclear Spectroscopic Telescope Array. Combined with new Swift and archival XMM-Newton and Chandra observations, the phase-averaged spectrum is well characterized by a blackbody plus double power law, in agreement with previous multimission X-ray results. However, we are unable to reproduce the spectral results reported based on Suzaku observations. The pulsed fraction of the source is found to increase with photon energy. The measured rms pulsed fractions are ~12% and ~17% at ~20 and ~50 keV, respectively. We detect a new feature in the 24-35 keV band pulse profile that is uniquely double peaked. This feature may be associated with a possible absorption or emission feature in the phase-resolved spectrum. We fit the X-ray data using the recently developed electron-positron outflow model by Beloborodov for the hard X-ray emission from magnetars. This produces a satisfactory fit, allowing a constraint on the angle between the rotation and magnetic axes of the neutron star of ~20\u00b0 and on the angle between the rotation axis and line of sight of ~50\u00b0. In this model, the soft X-ray component is inconsistent with a single blackbody; adding a second blackbody or a power-law component fits the data. The two-blackbody interpretation suggests a hot spot of temperature kT \u2248 0.9 keV occupying ~1% of the stellar surface.",
"date": "2013-12-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "779",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 163",
"id_number": "CaltechAUTHORS:20140121-141233775",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140121-141233775",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
},
{
"agency": "Fonds de recherche du Qu\u00e9bec \u2013 Nature et technologies (FRQNT)"
},
{
"agency": "R. Howard Webster Foundation"
},
{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Canada Research Chairs Program"
},
{
"agency": "Lorne Trottier Chair in Astrophysics and Cosmology"
},
{
"agency": "NASA",
"grant_number": "NNX10AI72G"
},
{
"agency": "NASA",
"grant_number": "NNX13AI34G"
},
{
"agency": "Department of Energy (DOE)",
"grant_number": "DE-AC52-07NA27344"
}
]
},
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"pub_year": "2013",
"author_list": "An, Hongjun; Hasco\u00ebt, Romain; et el."
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"given": "R\u00fcdiger"
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"id": "Bachetti-M",
"name": {
"family": "Bachetti",
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"orcid": "0000-0002-4576-9337"
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"name": {
"family": "Barret",
"given": "Didier"
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"orcid": "0000-0002-0393-9190"
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"name": {
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"name": {
"family": "Klochkov",
"given": "Dmitry"
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},
"title": "The Smooth Cyclotron Line in Her X-1 as Seen with Nuclear Spectroscopic Telescope Array",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; pulsars: individual (Her X-1); stars: neutron; X-rays: binaries",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 June 11; accepted 2013 September 20; published 2013 November 26. \n\nThis work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. F.F. would also like to thank the Remeis-Observatory Bamberg for their hospitality. J.A.T. acknowledges partial support from NASA Astrophysics\nData Analysis Program grant NNX13AE98G. M.B. was supported\nby the Centre National d'\u00c9tudes Spatiales (CNES).\n\nPublished - 0004-637X_779_1_69.pdf
Submitted - 1309.5361v1.pdf
",
"abstract": "Her X-1, one of the brightest and best studied X-ray binaries, shows a cyclotron resonant scattering feature (CRSF) near 37 keV. This makes it an ideal target for a detailed study with the Nuclear Spectroscopic Telescope Array (NuSTAR), taking advantage of its excellent hard X-ray spectral resolution. We observed Her X-1 three times, coordinated with Suzaku, during one of the high flux intervals of its 35 day superorbital period. This paper focuses on the shape and evolution of the hard X-ray spectrum. The broadband spectra can be fitted with a power law with a high-energy cutoff, an iron line, and a CRSF. We find that the CRSF has a very smooth and symmetric shape in all observations and at all pulse phases. We compare the residuals of a line with a Gaussian optical-depth profile to a Lorentzian optical-depth profile and find no significant differences, strongly constraining the very smooth shape of the line. Even though the line energy changes dramatically with pulse phase, we find that its smooth shape does not. Additionally, our data show that the continuum only changes marginally between the three observations. These changes can be explained with varying amounts of Thomson scattering in the hot corona of the accretion disk. The average, luminosity-corrected CRSF energy is lower than in past observations and follows a secular decline. The excellent data quality of NuSTAR provides the best constraint on the CRSF energy to date.",
"date": "2013-12-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "779",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 69",
"id_number": "CaltechAUTHORS:20140121-073921852",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140121-073921852",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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{
"agency": "NASA",
"grant_number": "NNX13AE98G"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
}
]
},
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"doi": "10.1088/0004-637X/779/1/69",
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"author_list": "F\u00fcrst, Felix; Grefenstette, Brian W.; et el."
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"family": "Tomsick",
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"title": "Constraints on the Neutron Star and Inner Accretion Flow in Serpens X-1 Using NuSTAR",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; equation of state; relativistic processes; X-rays: binaries",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 October 2; accepted 2013 October 18; published 2013 November 21. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA.\n\nPublished - 2041-8205_779_1_L2.pdf
Submitted - 1310.5776v1.pdf
",
"abstract": "We report on an observation of the neutron star low-mass X-ray binary Serpens X-1, made with NuSTAR. The extraordinary sensitivity afforded by NuSTAR facilitated the detection of a clear, robust, relativistic Fe K emission line from the inner disk. A relativistic profile is required over a single Gaussian line from any charge state of Fe at the 5\u03c3 level of confidence, and any two Gaussians of equal width at the same confidence. The Compton back-scattering \"hump\" peaking in the 10-20 keV band is detected for the first time in a neutron star X-ray binary. Fits with relativistically blurred disk reflection models suggest that the disk likely extends close to the innermost stable circular orbit (ISCO) or stellar surface. The best-fit blurred reflection models constrain the gravitational redshift from the stellar surface to be z_(NS) \u2265 0.16. The data are broadly compatible with the disk extending to the ISCO; in that case, z_(NS) \u2265 0.22 and R_(NS) \u2264 12.6 km (assuming M_(NS) = 1.4 M_\u2609 and a = 0, where a = cJ/GM^2). If the star is as large or larger than its ISCO, or if the effective reflecting disk leaks across the ISCO to the surface, the redshift constraints become measurements. We discuss our results in the context of efforts to measure fundamental properties of neutron stars, and models for accretion onto compact objects.",
"date": "2013-12-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "779",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L2",
"id_number": "CaltechAUTHORS:20140108-080908162",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140108-080908162",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
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"author_list": "Miller, J. M.; Parker, M. L.; et el."
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"name": {
"family": "Tagliaferri",
"given": "G."
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},
"title": "NuSTAR Observations of GRB 130427A Establish a Single Component Synchrotron Afterglow Origin for the Late Optical to Multi-GeV Emission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "acceleration of particles; gamma-ray burst: individual (GRB 130427A); magnetic fields; radiation mechanisms: non-thermal; shock waves",
"note": "\u00a9 2013 American Astronomical Society. Received 2013 October 15; accepted 2013 November 7; published 2013 November 21. This work was supported under NASA Contract\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by CalTech, managed by JPL, and funded by\nNASA. We thank the NuSTAR Operations, Software and Calibration\nteams for support with the execution and analysis of\nthese observations. This research has made use of the NuSTAR\nData Analysis Software (NuSTARDAS) jointly developed by\nthe ASI Science Data Center (ASDC, Italy) and CalTech. This\nwork made use of data supplied by the UK Swift Science Data\nCentre at the University of Leicester. The Fermi/LAT Collaboration\nacknowledges support from NASA and DOE (U.S.),\nCEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy),\nMEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg\nFoundation, the Swedish Research Council and the National\nSpace Board in Sweden. Additional support from INAF in Italy\nand CNES in France for science analysis during the operations\nphase is also gratefully acknowledged. The Liverpool Telescope\nis operated by Liverpool John Moores University at the Observatorio\ndel Roque de los Muchachos of the Instituto de Astrofisica\nde Canarias. C.G.M. acknowledges support from the\nRoyal Society.\n\nPublished - 2041-8205_779_1_L1.pdf
Submitted - 1311.5245v1.pdf
",
"abstract": "GRB 130427A occurred in a relatively nearby galaxy; its prompt emission had the largest GRB fluence ever recorded. The afterglow of GRB 130427A was bright enough for the Nuclear Spectroscopic Telescope ARray (NuSTAR) to observe it in the 3-79 keV energy range long after its prompt emission (~1.5 and 5 days). This range, where afterglow observations were previously not possible, bridges an important spectral gap. Combined with Swift, Fermi, and ground-based optical data, NuSTAR observations unambiguously establish a single afterglow spectral component from optical to multi-GeV energies a day after the event, which is almost certainly synchrotron radiation. Such an origin of the late-time Fermi/Large Area Telescope >10 GeV photons requires revisions in our understanding of collisionless relativistic shock physics.",
"date": "2013-12-10",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "779",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L1",
"id_number": "CaltechAUTHORS:20140108-072801401",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140108-072801401",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
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{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Department of Energy (DOE)"
},
{
"agency": "Institut de recherche sur les lois fondamentales de l'Univers (Irfu)"
},
{
"agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)"
},
{
"agency": "Agentschap voor Innovatie door Wetenschap en Technologie (IWT-Belgium)"
},
{
"agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)"
},
{
"agency": "KEK (Japan)"
},
{
"agency": "Japan Aerospace Exploration Agency (JAXA)"
},
{
"agency": "Knut and Alice Wallenberg Foundation"
},
{
"agency": "Swedish Research Council"
},
{
"agency": "Swedish National Space Board (SNSB)"
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{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Royal Society"
},
{
"agency": "Commissariat \u00e0 l'Energie Atomique (CEA)"
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{
"agency": "Centre National de la Recherche Scientifique (CNRS)"
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"title": "The Ultraluminous X-Ray Sources NGC 1313 X-1 and X-2: A Broadband Study with NuSTAR and XMM-Newton",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics; stars: black holes; X-rays: individual (NGC 1313 X-1, NGC 1313 X-2); X-rays: stars",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 July 25; accepted 2013 October 2; published 2013 November 13. \n\nM.B. wishes to acknowledge the support from the Centre National d'\u00c9tudes Spatiales (CNES). This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This work also makes use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and of observations made by the Chandra X-ray Observatory. For timing analysis and plotting, a set of Python codes making use of the NumPy and Scipy libraries was used. For some plots, we used the Veusz software. The authors wish to thank Olivier Godet and Chris Done for interesting discussions, and the referee Matt Middleton, whose comments and suggestions substantively improved the quality of the manuscript.\n\nPublished - 0004-637X_778_2_163.pdf
Submitted - 1310.0745v3.pdf
",
"abstract": "We present the results of NuSTAR and XMM-Newton observations of the two ultraluminous X-ray sources: NGC 1313 X-1 and X-2. The combined spectral bandpass of the two satellites enables us to produce the first spectrum of X-1 between 0.3 and 30 keV, while X-2 is not significantly detected by NuSTAR above 10 keV. The NuSTAR data demonstrate that X-1 has a clear cutoff above 10 keV, whose presence was only marginally detectable with previous X-ray observations. This cutoff rules out the interpretation of X-1 as a black hole in a standard low/hard state, and it is deeper than predicted for the downturn of a broadened iron line in a reflection-dominated regime. The cutoff differs from the prediction of a single-temperature Comptonization model. Further, a cold disk-like blackbody component at ~0.3 keV is required by the data, confirming previous measurements by XMM-Newton only. We observe a spectral transition in X-2, from a state with high luminosity and strong variability to a lower-luminosity state with no detectable variability, and we link this behavior to a transition from a super-Eddington to a sub-Eddington regime.",
"date": "2013-12-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "778",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 163",
"id_number": "CaltechAUTHORS:20140106-152234543",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-152234543",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "ESA Member States"
}
]
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"doi": "10.1088/0004-637X/778/2/163",
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"pub_year": "2013",
"author_list": "Bachetti, Matteo; Rana, Vikram; et el."
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"id": "Nynka-M",
"name": {
"family": "Nynka",
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{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "Charles J."
}
},
{
"id": "Mori-Kaya",
"name": {
"family": "Mori",
"given": "Kaya"
},
"orcid": "0000-0002-9709-5389"
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{
"id": "Baganoff-F-K",
"name": {
"family": "Baganoff",
"given": "Frederick K."
}
},
{
"id": "Bauer-F-E",
"name": {
"family": "Bauer",
"given": "Franz E."
},
"orcid": "0000-0002-8686-8737"
},
{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "Steven E."
},
"orcid": "0000-0001-9567-4224"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William W."
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},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "Finn E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Gotthelf-E-V",
"name": {
"family": "Gotthelf",
"given": "Eric V."
},
"orcid": "0000-0003-3847-3957"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "Fiona A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Hong-Jaesub",
"name": {
"family": "Hong",
"given": "Jaesub"
}
},
{
"id": "Perez-K-M",
"name": {
"family": "Perez",
"given": "Kerstin M."
},
"orcid": "0000-0002-6404-4737"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-Shou",
"name": {
"family": "Zhang",
"given": "Shou"
}
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "William W."
},
"orcid": "0000-0002-1426-9698"
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},
"title": "High-energy X-Rays from J174545.5-285829, the Cannonball: A Candidate Pulsar Wind Nebula Associated with Sgr A East",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center; ISM: individual objects (Sagittarius A, Sagittarius A East); ISM: supernova remnants; stars: neutron; X-rays: individual (Cannonball)",
"note": "\u00a9 2013 American Astronomical Society. Received 2013 September 25; accepted 2013 October 22; published 2013 November 13. This work was supported under NASA contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). The authors wish to thank Jules Halpern for useful discussions.\n\nPublished - 2041-8205_778_2_L31.pdf
Submitted - 1311.1832v2.pdf
",
"abstract": "We report the unambiguous detection of non-thermal X-ray emission up to 30 keV from the Cannonball, a few-arcsecond long diffuse X-ray feature near the Galactic Center, using the NuSTAR X-ray observatory. The Cannonball is a high-velocity (v_(proj) ~ 500 km s^(\u20131)) pulsar candidate with a cometary pulsar wind nebula (PWN) located ~2' north-east from Sgr A^*, just outside the radio shell of the supernova remnant Sagittarius A (Sgr A) East. Its non-thermal X-ray spectrum, measured up to 30 keV, is well characterized by a \u0393 ~ 1.6 power law, typical of a PWN, and has an X-ray luminosity of L(3-30 keV) = 1.3 \u00d7 10^(34) erg s^(\u20131). The spectral and spatial results derived from X-ray and radio data strongly suggest a runaway neutron star born in the Sgr A East supernova event. We do not find any pulsed signal from the Cannonball. The NuSTAR observations allow us to deduce the PWN magnetic field and show that it is consistent with the lower limit obtained from radio observations.",
"date": "2013-12-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "778",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L31",
"id_number": "CaltechAUTHORS:20140107-142025993",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140107-142025993",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
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"id": "NuSTAR"
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"id": "Space-Radiation-Laboratory"
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},
"doi": "10.1088/2041-8205/778/2/L31",
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],
"pub_year": "2013",
"author_list": "Nynka, Melania; Hailey, Charles J.; et el."
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"items": [
{
"id": "Sbarrato-T",
"name": {
"family": "Sbarrato",
"given": "T."
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{
"id": "Tagliaferri-G",
"name": {
"family": "Tagliaferri",
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{
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{
"id": "Puccetti-S",
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"family": "Puccetti",
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"orcid": "0000-0002-2734-7835"
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{
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"family": "Balokovi\u0107",
"given": "M."
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"family": "Nardini",
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"family": "Hailey",
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"family": "Harrison",
"given": "F. A."
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"orcid": "0000-0003-2992-8024"
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{
"id": "Hovatta-T",
"name": {
"family": "Hovatta",
"given": "T."
},
"orcid": "0000-0002-2024-8199"
},
{
"id": "Madejski-G-M",
"name": {
"family": "Madejski",
"given": "G. M."
}
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{
"id": "Rau-A",
"name": {
"family": "Rau",
"given": "A."
},
"orcid": "0000-0001-5990-6243"
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"id": "Schady-P",
"name": {
"family": "Schady",
"given": "P."
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{
"id": "Sudilovsky-V",
"name": {
"family": "Sudilovsky",
"given": "V."
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"id": "Urry-C-M",
"name": {
"family": "Urry",
"given": "C. M."
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"orcid": "0000-0002-0745-9792"
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"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
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},
"title": "NuSTAR Detection of the Blazar B2 1023+25 at Redshift 5.3",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; quasars: general; quasars: individual (B2 1023+25); X-rays: general",
"note": "\u00a9 2013 American Astronomical Society. Received 2013 August 12; accepted 2013 September 10; published 2013 October 23. We thank the anonymous referee for useful comments.\nWe acknowledge financial support from the ASI-INAF grant\nI/037/12/0. This work was supported under NASA Contract\nNo. NNG08FD60C and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology,\nmanaged by the Jet Propulsion Laboratory, and funded by\nthe National Aeronautics and Space Administration. We thank\nthe NuSTAR Operations, Software, and Calibration teams for\nsupport with the execution and analysis of these observations.\nThis research has made also use of the NuSTAR Data Analysis\nSoftware (NuSTARDAS) jointly developed by the ASI\nScience Data Center (ASDC, Italy) and the California Institute\nof Technology (Caltech, USA). The scientific results reported\nin this article are based in part on observations made\nby the Chandra X-ray Observatory and published previously\nin cited articles. This publication makes use of data products\nfrom the Wide-field Infrared Survey Explorer, which is a joint\nproject of the University of California, Los Angeles, and the\nJet Propulsion Laboratory/California Institute of Technology,\nfunded by the National Aeronautics and Space Administration.\nPart of this work is based on archival data, software, or on-line\nservices provided by the ASDC. This research has made use\nof the XRT Data Analysis Software (XRTDAS) developed under\nthe responsibility of the ASDC, Italy. Part of the funding\nfor GROND (both hardware as well as personnel) was generously\ngranted from the Leibniz Prize to Professor G. Hasinger\n(DFG grant HA 1850/28-1). Support for CARMA construction\nwas derived from the Gordon and Betty Moore Foundation,\nthe Kenneth T. and Eileen L. Norris Foundation, the James\nS. McDonnell Foundation, the Associates of the California Institute\nof Technology, the University of Chicago, the states of\nCalifornia, Illinois, and Maryland, and the National Science\nFoundation. Ongoing CARMA development and operations are\nsupported by the National Science Foundation under a cooperative\nagreement, and by the CARMA partner universities. The\noperation of the OVRO 40 m telescope is supported by NASA\nawards NNX08AW31G and NNX11AO43G and NSF awards\nAST-0808050 and AST-1109911. M.B. acknowledges support\nfrom an International Fulbright Science and Technology Award.\n\nPublished - 0004-637X_777_2_147.pdf
Submitted - 1309.3280v1.pdf
",
"abstract": "B2 1023+25 is an extremely radio-loud quasar at z = 5.3 that was first identified as a likely high-redshift blazar candidate in the SDSS+FIRST quasar catalog. Here, we use the Nuclear Spectroscopic Telescope Array (NuSTAR) to investigate its non-thermal jet emission, whose high-energy component we detected in the hard X-ray energy band. The X-ray flux is ~ 5.5 x 10^(-14)erg cm^(-2) s^(-1) (5-10 keV) and the photon spectral index is \u0393_X \u2243 1.3-1.6. Modeling the full spectral energy distribution, we find that the jet is oriented close to the line of sight, with a viewing angle of ~3\u00b0, and has significant Doppler boosting, with a large bulk Lorentz factor ~13, which confirms the identification of B2 1023+25 as a blazar. B2 1023+25 is the first object at redshift larger than 5 detected by NuSTAR, demonstrating the ability of NuSTAR to investigate the early X-ray universe and to study extremely active supermassive black holes located at very high redshift.",
"date": "2013-11-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "777",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 147",
"id_number": "CaltechAUTHORS:20131202-132341132",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131202-132341132",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "HA 1850/28-1"
},
{
"agency": "Gordon and Betty Moore Foundation"
},
{
"agency": "Kenneth T. and Eileen L. Norris Foundation"
},
{
"agency": "James S. McDonnell Foundation"
},
{
"agency": "Caltech Associates"
},
{
"agency": "University of Chicago"
},
{
"agency": "States of California"
},
{
"agency": "State of Illinois"
},
{
"agency": "State of Maryland"
},
{
"agency": "CARMA partner universities"
},
{
"agency": "NASA",
"grant_number": "NNX08AW31G"
},
{
"agency": "NASA",
"grant_number": "NNX11AO43G"
},
{
"agency": "NSF",
"grant_number": "AST-0808050"
},
{
"agency": "NSF",
"grant_number": "AST-1109911"
},
{
"agency": "International Fulbright Science and Technology Award"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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"pub_year": "2013",
"author_list": "Sbarrato, T.; Tagliaferri, G.; et el."
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"eprint_id": 41975,
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"datestamp": "2023-08-22 10:32:27",
"lastmod": "2023-10-25 14:59:03",
"type": "article",
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"creators": {
"items": [
{
"id": "Miller-J-M",
"name": {
"family": "Miller",
"given": "J. M."
}
},
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "M."
},
"orcid": "0000-0002-4576-9337"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Barret-D",
"name": {
"family": "Barret",
"given": "D."
},
"orcid": "0000-0002-0393-9190"
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{
"id": "Boggs-S-E",
"name": {
"family": "Boggs",
"given": "S. E."
},
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},
{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "D."
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},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
},
"orcid": "0000-0001-5679-1946"
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "W. W."
}
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Hailey-C-J",
"name": {
"family": "Hailey",
"given": "C. J."
}
},
{
"id": "King-A-L",
"name": {
"family": "King",
"given": "A. L."
}
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "D. K."
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Tomsick-J-A",
"name": {
"family": "Tomsick",
"given": "J. A."
},
"orcid": "0000-0001-5506-9855"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "NuSTAR Spectroscopy of GRS 1915+105: Disk Reflection, Spin, and Connections to Jets",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks; black hole physics; gravitation; relativistic processes; X-rays: binaries",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 July 26; accepted 2013 August 16; published 2013 September 18.\n\nThis work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. J.M.M. thanks Sergei Trushkin for communicating radio results.\n\nPublished - 2041-8205_775_2_L45.pdf
Submitted - 1308.4669v1.pdf
",
"abstract": "We report on the results of spectral fits made to a NuSTAR observation of the black hole GRS 1915+105 in a \"plateau\" state. This state is of special interest because it is similar to the \"low/hard\" state seen in other black holes, especially in that compact, steady jets are launched in this phase. The 3\u201379 keV bandpass of NuSTAR, and its ability to obtain moderate-resolution spectra free from distortions such as photon pile-up, are extremely well suited to studies of disk reflection in X-ray binaries. In only 15 ks of net exposure, an extraordinarily sensitive spectrum of GRS 1915+105 was measured across the full bandpass. Ionized reflection from a disk around a rapidly spinning black hole is clearly required to fit the spectra; even hybrid Comptonization models including ionized reflection from a disk around a Schwarzschild black hole proved inadequate. A spin parameter of a = 0.98 \u00b1 0.01 (1\u03c3 statistical error) is measured via the best-fit model; low spins are ruled out at a high level of confidence. This result suggests that jets can be launched from a disk extending to the innermost stable circular orbit. A very steep inner disk emissivity profile is also measured, consistent with models of compact coronae above Kerr black holes. These results support an emerging association between the hard X-ray corona and the base of the relativistic jet.",
"date": "2013-10-01",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "775",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L45",
"id_number": "CaltechAUTHORS:20131017-133805051",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131017-133805051",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/2041-8205/775/2/L45",
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"pub_year": "2013",
"author_list": "Miller, J. M.; Parker, M. L.; et el."
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{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "H."
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Bachetti-M",
"name": {
"family": "Bachetti",
"given": "Matteo"
},
"orcid": "0000-0002-4576-9337"
},
{
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"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
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"name": {
"family": "F\u00fcrst",
"given": "Felix"
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{
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"name": {
"family": "Barret",
"given": "D."
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"orcid": "0000-0002-0393-9190"
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{
"id": "Bellm-E-C",
"name": {
"family": "Bellm",
"given": "E. C."
},
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"family": "Boggs",
"given": "S. E."
},
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{
"id": "Chakrabarty-D",
"name": {
"family": "Chakrabarty",
"given": "D."
},
"orcid": "0000-0001-8804-8946"
},
{
"id": "Chenevez-J",
"name": {
"family": "Chenevez",
"given": "Jerome"
},
"orcid": "0000-0002-4397-8370"
},
{
"id": "Christensen-F-E",
"name": {
"family": "Christensen",
"given": "F. E."
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"orcid": "0000-0001-5679-1946"
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},
"title": "NuSTAR Detection of hard x-ray phase lags from the accreting pulsar GS 0834-430",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2013 June 3, accepted for publication 2013 July 25\nPublished 2013 September 5.\n\nThis work was supported under NASA contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Matteo Bachetti wishes to acknowledge the support from the Centre National d'Etudes Spatiales (CNES). Lorenzo Natalucci acknowledges financial support through contract ASI/INAF I/037/12/0.\n\nPublished - 0004-637X_775_1_65.pdf
",
"abstract": "The Nuclear Spectroscopic Telescope Array hard X-ray telescope observed the transient Be/X-ray binary GS 0834-430 during its 2012 outburst-the first active state of this system observed in the past 19 yr. We performed timing and spectral analysis and measured the X-ray spectrum between 3-79 keV with high statistical significance. We find the phase-averaged spectrum to be consistent with that observed in many other magnetized, accreting pulsars. We fail to detect cyclotron resonance scattering features that would allow us to constrain the pulsar's magnetic field in either phase-averaged or phase-resolved spectra. Timing analysis shows a clearly detected pulse period of similar to 12.29 s in all energy bands. The pulse profiles show a strong, energy-dependent hard phase lag of up to 0.3 cycles in phase, or about 4 s. Such dramatic energy-dependent lags in the pulse profile have never before been reported in high-mass X-ray binary pulsars. Previously reported lags have been significantly smaller in phase and restricted to low energies (E < 10 keV). We investigate the possible mechanisms that might produce this energy-dependent pulse phase shift. We find the most likely explanation for this effect is a complex beam geometry.",
"date": "2013-09-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "775",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 65",
"id_number": "CaltechAUTHORS:20150401-090934706",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150401-090934706",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NSF",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
},
{
"agency": "Agenxia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1088/0004-637X/775/1/65",
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"pub_year": "2013",
"author_list": "Miyasaka, H.; Bachetti, Matteo; et el."
},
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"items": [
{
"id": "Alexander-D-M",
"name": {
"family": "Alexander",
"given": "D. M."
},
"orcid": "0000-0002-5896-6313"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Bridge-C-R",
"name": {
"family": "Bridge",
"given": "C. R."
}
},
{
"id": "Miller-S-H",
"name": {
"family": "Miller",
"given": "S. H."
}
}
]
},
"title": "The NuSTAR Extragalactic Survey: A First Sensitive Look at the High-energy Cosmic X-Ray Background Population",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: high-redshift; infrared: galaxies; X-rays: diffuse background; X-rays: general",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 June 2; accepted 2013 June 28; published 2013 August 1. \n\nWe acknowledge financial support from the Leverhulme Trust (D.M.A. and J.R.M.), the Science and Technology Facilities\nCouncil (STFC; D.M.A., A.D.M., and G.B.L.), the SAO grant GO2-13164X (M.A.), NASA Postdoctoral Program at the Jet Propulsion Laboratory (R.J.A.), NSF award AST 1008067\n(D.R.B.), Center of Excellence in Astrophysics and Associated Technologies (PFB 06/2007; F.E.B. and E.T.), the Anillo project ACT1101 (F.E.B. and E.T.), FONDECYT Regular 1101024 (F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.),NASA ADP grant NNX10AC99G (W.N.B. and B.L.), ASI/INAF grant I/037/12/0 (A.C. and S.P.), CONICYT-Chile under grant FONDECYT 3120198 (C.S.), and FONDECYT regular grant 1120061 (E.T.). We thank the referee for a constructive and positive report. We also thank Michael Koss for the discussion of Swift-BAT results, and Mark Brodwin,Daniel Gettings, John Gizis, Richard Walters, Jingwen Wu, and Dominika Wylezalek for supporting the ground-based follow-up observations. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National\nAeronautics and Space Administration. We thank the NuSTAR\nOperations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA).\n\nPublished - 0004-637X_773_2_125.pdf
Submitted - 1307.1733v1.pdf
",
"abstract": "We report on the first 10 identifications of sources serendipitously detected by the Nuclear Spectroscopic Telescope Array (NuSTAR) to provide the first sensitive census of the cosmic X-ray background source population at \u227310 keV. We find that these NuSTAR-detected sources are \u2248100 times fainter than those previously detected at \u227310 keV and have a broad range in redshift and luminosity (z = 0.020-2.923 and L_(10-40 keV) \u2248 4 \u00d7 10^(41)-5 \u00d7 10^(45) erg s^(\u20131)); the median redshift and luminosity are z \u2248 0.7 and L_(10-40 keV) \u2248 3 \u00d7 10^(44) erg s^(\u20131), respectively. We characterize these sources on the basis of broad-band \u22480.5-32 keV spectroscopy, optical spectroscopy, and broad-band ultraviolet-to-mid-infrared spectral energy distribution analyses. We find that the dominant source population is quasars with L_(10-40 keV) > 10^(44) erg s^(\u20131), of which \u224850% are obscured with N_H \u2273 10^(22) cm^(\u20132). However, none of the 10 NuSTAR sources are Compton thick (N_H \u2273 10^(24) cm^(\u20132)) and we place a 90% confidence upper limit on the fraction of Compton-thick quasars (L_(10-40 keV) > 10^(44) erg s^(\u20131)) selected at \u227310 keV of \u227e33% over the redshift range z = 0.5-1.1. We jointly fitted the rest-frame \u224810-40 keV data for all of the non-beamed sources with L_(10-40 keV) > 10^(43) erg s^(\u20131) to constrain the average strength of reflection; we find R < 1.4 for \u0393 = 1.8, broadly consistent with that found for local active galactic nuclei (AGNs) observed at \u227310 keV. We also constrain the host-galaxy masses and find a median stellar mass of \u224810^(11) M_\u2609, a factor \u22485 times higher than the median stellar mass of nearby high-energy selected AGNs, which may be at least partially driven by the order of magnitude higher X-ray luminosities of the NuSTAR sources. Within the low source-statistic limitations of our study, our results suggest that the overall properties of the NuSTAR sources are broadly similar to those of nearby high-energy selected AGNs but scaled up in luminosity and mass.",
"date": "2013-08-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "773",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 125",
"id_number": "CaltechAUTHORS:20130923-094035250",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130923-094035250",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Leverhulme Trust"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Smithsonian Astrophysical Observatory",
"grant_number": "GO2-13164X"
},
{
"agency": "NASA Postdoctoral Program"
},
{
"agency": "NSF",
"grant_number": "AST-1008067"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1101024"
},
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)",
"grant_number": "I/037/12/0-011/13"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "3120198"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1120061"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Istituto Nazionale di Astrofisica (INAF)"
}
]
},
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"id": "COSMOS"
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},
"doi": "10.1088/0004-637X/773/2/125",
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"pub_year": "2013",
"author_list": "Alexander, D. M.; Grefenstette, B. W.; et el."
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"datestamp": "2023-08-19 21:00:27",
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"items": [
{
"id": "Luo-Bin",
"name": {
"family": "Luo",
"given": "B."
},
"orcid": "0000-0002-9036-0063"
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "F\u00fcrst-F",
"name": {
"family": "Fuerst",
"given": "F."
},
"orcid": "0000-0003-0388-0560"
},
{
"id": "Grefenstette-B-W",
"name": {
"family": "Grefenstette",
"given": "B. W."
},
"orcid": "0000-0002-1984-2932"
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "K. K."
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Ogle-P-M",
"name": {
"family": "Ogle",
"given": "P."
},
"orcid": "0000-0002-3471-981X"
}
]
},
"title": "Weak Hard X-Ray Emission from Two Broad Absorption Line Quasars Observed with NuSTAR: Compton-thick Absorption or Intrinsic X-Ray Weakness?",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "accretion, accretion disks \u2013 galaxies: active \u2013 galaxies: nuclei \u2013 quasars: absorption lines \u2013 quasars: emission lines \u2013 X-rays: general",
"note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2013 April 3; accepted 2013 June 14; published 2013 July 17.\n\nWe acknowledge support from the California Institute of\nTechnology (Caltech) NuSTAR subcontract 44A-1092750 (B.L.\nand W.N.B.), NASA ADP Grant NNX10AC99G (B.L. and\nW.N.B.), the Leverhulme trust and the Science Technology and\nFacilities Council (D.M.A.), Basal-CATA Grant PFB-06/2007\nand CONICYT-Chile Grants FONDECYT 1101024 and Anillo\nACT1101 (F.E.B.), and CONICYT-Chile Grant FONDECYT\n3120198 (C.S.). We thank M. Young for help with the planning\nof this project and K. Forster for help with the NuSTAR data\naccess, and we thank M. Balokovic, K. Boydstun, T. N. Lu, B.\nP. Miller, Jianfeng Wu, and T. Yaqoob for helpful discussions.\nWe thank the referee, S. C. Gallagher, for carefully reviewing\nthe manuscript and providing helpful comments.\nThis work was supported under NASA contract No.\nNNG08FD60C, and made use of data from the NuSTAR mission,\na project led by Caltech, managed by the Jet Propulsion\nLaboratory, and funded by the National Aeronautics and Space\nAdministration. We thank the NuSTAR Operations, Software and\nCalibration teams for support with the execution and analysis\nof these observations. This research has made use of NuSTAR-DAS\njointly developed by the ASI Science Data Center (ASDC,\nItaly) and Caltech (USA).\n\nPublished - 0004-637X_772_2_153.pdf
Submitted - 1306.3500v1.pdf
",
"abstract": "We present Nuclear Spectroscopic Telescope Array (NuSTAR) hard X-ray observations of two X-ray weak broad absorption line (BAL) quasars, PG 1004+130 (radio loud) and PG 1700+518 (radio quiet). Many BAL quasars appear X-ray weak, probably due to absorption by the shielding gas between the nucleus and the accretion-disk wind. The two targets are among the optically brightest BAL quasars, yet they are known to be significantly X-ray weak at rest-frame 2-10 keV (16-120 times fainter than typical quasars). We would expect to obtain \u2248400-600 hard X-ray (\u2273 10 keV) photons with NuSTAR, provided that these photons are not significantly absorbed (N_H \u227e10^(24) cm^(\u20132)). However, both BAL quasars are only detected in the softer NuSTAR bands (e.g., 4-20 keV) but not in its harder bands (e.g., 20-30 keV), suggesting that either the shielding gas is highly Compton-thick or the two targets are intrinsically X-ray weak. We constrain the column densities for both to be N_H \u2248 7 \u00d7 10^(24) cm^(\u20132) if the weak hard X-ray emission is caused by obscuration from the shielding gas. We discuss a few possibilities for how PG 1004+130 could have Compton-thick shielding gas without strong Fe K\u03b1 line emission; dilution from jet-linked X-ray emission is one likely explanation. We also discuss the intrinsic X-ray weakness scenario based on a coronal-quenching model relevant to the shielding gas and disk wind of BAL quasars. Motivated by our NuSTAR results, we perform a Chandra stacking analysis with the Large Bright Quasar Survey BAL quasar sample and place statistical constraints upon the fraction of intrinsically X-ray weak BAL quasars; this fraction is likely 17%-40%.",
"date": "2013-08-01",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "772",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 153",
"id_number": "CaltechAUTHORS:20130828-093434856",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130828-093434856",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Caltech NuSTAR subcontract",
"grant_number": "44A-1092750"
},
{
"agency": "NASA",
"grant_number": "NNX10AC99G"
},
{
"agency": "Leverhulme Trust"
},
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Basal-CATA",
"grant_number": "PFB-06/2007"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "1101024"
},
{
"agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)",
"grant_number": "Anillo ACT1101"
},
{
"agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)",
"grant_number": "3120198"
},
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
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"doi": "10.1088/0004-637X/772/2/153",
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"pub_year": "2013",
"author_list": "Luo, B.; Harrison, F. A.; et el."
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"family": "Hornschemeier",
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"name": {
"family": "Ptak",
"given": "A."
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"title": "NuSTAR and Chandra Insight into the Nature of the 3-40 keV Nuclear Emission in NGC 253",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "galaxies: active; galaxies: individual (NGC 253); galaxies: star formation; galaxies: starburst; X-rays: galaxies",
"note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2013 March 14; accepted 2013 May 17; published 2013 June 25.\n\nWe thank the anonymous referee for helpful comments,\nwhich have improved the quality of this paper. This work\nwas supported under NASA Contract No. NNG08FD60C, and\nmade use of data from the NuSTAR mission, a project led\nby the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software, and calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by theASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We thank the Chandra X-ray Center staff for providing faster than usual processing of the Chandra data.\n\nPublished - 0004-637X_771_2_134.pdf
Submitted - 1306.2639v1.pdf
",
"abstract": "We present results from three nearly simultaneous Nuclear Spectroscopic Telescope Array (NuSTAR) and Chandra monitoring observations between 2012 September 2 and 2012 November 16 of the local star-forming galaxy NGC 253. The 3-40 keV intensity of the inner ~20 arcsec (~400 pc) nuclear region, as measured by NuSTAR, varied by a factor of ~2 across the three monitoring observations. The Chandra data reveal that the nuclear region contains three bright X-ray sources, including a luminous (L_(2-10) keV ~ few \u00d7 10^39 erg s^\u20131) point source located ~1 arcsec from the dynamical center of the galaxy (within the 3\u03c3 positional uncertainty of the dynamical center); this source drives the overall variability of the nuclear region at energies \u22733 keV. We make use of the variability to measure the spectra of this single hard X-ray source when it was in bright states. The spectra are well described by an absorbed (N_H \u2248 1.6 \u00d7 10^23 cm^\u20132) broken power-law model with spectral slopes and break energies that are typical of ultraluminous X-ray sources (ULXs), but not active galactic nuclei (AGNs). A previous Chandra observation in 2003 showed a hard X-ray point source of similar luminosity to the 2012 source that was also near the dynamical center (\u03b8 \u2248 0.4 arcsec); however, this source was offset from the 2012 source position by \u22481 arcsec. We show that the probability of the 2003 and 2012 hard X-ray sources being unrelated is \u226b99.99% based on the Chandra spatial localizations. Interestingly, the Chandra spectrum of the 2003 source (3-8 keV) is shallower in slope than that of the 2012 hard X-ray source. Its proximity to the dynamical center and harder Chandra spectrum indicate that the 2003 source is a better AGN candidate than any of the sources detected in our 2012 campaign; however, we were unable to rule out a ULX nature for this source. Future NuSTAR and Chandra monitoring would be well equipped to break the degeneracy between the AGN and ULX nature of the 2003 source, if again caught in a high state.",
"date": "2013-07-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "771",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 134",
"id_number": "CaltechAUTHORS:20130813-114356742",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130813-114356742",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
}
]
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"author_list": "Lehmer, B. D.; Wik, D. R.; et el."
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"given": "Kristin K."
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"id": "Markwardt-C-B",
"name": {
"family": "Markwardt",
"given": "Craig B."
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"family": "Nynka",
"given": "Melania"
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"name": {
"family": "Tomsick",
"given": "John A."
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},
"title": "NuSTAR Discovery of a 3.76 s Transient Magnetar Near Sagittarius A*",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Galaxy: center; pulsars: general; pulsars: individual (SGR J1745-29); stars: neutron",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 May 7; accepted 2013 May 14; published 2013 May 30. \n\nThis work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. The authors thank Arash Bodaghee and Clio Sleator for their assistance with data analysis and Brian Metzger for helpful discussions.\n\nPublished - 2041-8205_770_2_L23.pdf
Submitted - 1305.1945v2.pdf
",
"abstract": "We report the discovery of 3.76 s pulsations from a new burst source near Sgr A^* observed by the NuSTAR observatory. The strong signal from SGR J1745\u201329 presents a complex pulse profile modulated with pulsed fraction 27% \u00b1 3% in the 3-10 keV band. Two observations spaced nine days apart yield a spin-down rate of \u1e56 =(6.5 \u00b1 1.4) \u00d7 10^(\u201312). This implies a magnetic field B = 1.6 \u00d7 10^(14) G, spin-down power \u0116 =5 \u00d7 10^(33) erg s^(\u20131), and characteristic age P/2\u1e56 =9 \u00d7 10^3 yr for the rotating dipole model. However, the current \u1e56 may be erratic, especially during outburst. The flux and modulation remained steady during the observations and the 3-79 keV spectrum is well fitted by a combined blackbody plus power-law model with temperature kT_(BB) = 0.96 \u00b1 0.02 keV and photon index \u0393 = 1.5 \u00b1 0.4. The neutral hydrogen column density (N_H ~ 1.4 \u00d7 10^(23) cm^(\u20132)) measured by NuSTAR and Swift suggests that SGR J1745\u201329 is located at or near the Galactic center. The lack of an X-ray counterpart in the published Chandra survey catalog sets a quiescent 2-8 keV luminosity limit of L_x \u227e 10^(32) erg s^(\u20131). The bursting, timing, and spectral properties indicate a transient magnetar undergoing an outburst with 2-79 keV luminosity up to 3.5 \u00d7 10^(35) erg s^(\u20131) for a distance of 8 kpc. SGR J1745\u201329 joins a growing subclass of transient magnetars, indicating that many magnetars in quiescence remain undetected in the X-ray band or have been detected as high-B radio pulsars. The peculiar location of SGR J1745\u201329 has important implications for the formation and dynamics of neutron stars in the Galactic center region.",
"date": "2013-06-20",
"date_type": "published",
"publication": "Astrophysical Journal Letters",
"volume": "770",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. L23",
"id_number": "CaltechAUTHORS:20130812-081440101",
"issn": "2041-8205",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130812-081440101",
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"items": [
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"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
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"name": {
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"id": "Balokovi\u0107-M",
"name": {
"family": "Balokovi\u0107",
"given": "Mislav"
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"title": "The Nuclear Spectroscopic Telescope Array (NuSTAR) High-energy X-Ray Mission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "space vehicles: instruments; X-rays: general",
"note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 January 22; accepted 2013 April 4; published 2013 May 30. \n\nThis work was supported under NASA No. NNG08FD60C and made use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a project led by Caltech, managed by\nthe Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. Additional support for development was provided by the National Space Institute, Technical University of Denmark. The Malindi ground station is provided by the Italian Space Agency (ASI) and support for science software development by the ASI Science Data Center (ASDC). Science team members acknowledge support from Centre National d'Etudes Spatiales (CNES) (D.B., M.B.), the NASA Postdoctoral Program D.R.W.), Leverhulme Research Fellowship and Science and Technology Facilities Council (D.M.A), NSF AST (D.R.B.), U.S. DOE/LLNL (W.W.C., M.P., J.V.), NSERC, CIFAR, FQRNT, and Killam Research Fellowship (V.K.). We thank David Burrows (PSU) for useful comments which improved the quality of the manuscript.\n\nPublished - 0004-637X_770_2_103.pdf
Submitted - 1301.7307v1.pdf
",
"abstract": "The Nuclear Spectroscopic Telescope Array (NuSTAR) mission, launched on 2012 June 13, is the first focusing high-energy X-ray telescope in orbit. NuSTAR operates in the band from 3 to 79 keV, extending the sensitivity of focusing far beyond the ~10 keV high-energy cutoff achieved by all previous X-ray satellites. The inherently low background associated with concentrating the X-ray light enables NuSTAR to probe the hard X-ray sky with a more than 100-fold improvement in sensitivity over the collimated or coded mask instruments that have operated in this bandpass. Using its unprecedented combination of sensitivity and spatial and spectral resolution, NuSTAR will pursue five primary scientific objectives: (1) probe obscured active galactic nucleus (AGN) activity out to the peak epoch of galaxy assembly in the universe (at z \u227e 2) by surveying selected regions of the sky; (2) study the population of hard X-ray-emitting compact objects in the Galaxy by mapping the central regions of the Milky Way; (3) study the non-thermal radiation in young supernova remnants, both the hard X-ray continuum and the emission from the radioactive element ^(44)Ti; (4) observe blazars contemporaneously with ground-based radio, optical, and TeV telescopes, as well as with Fermi and Swift, to constrain the structure of AGN jets; and (5) observe line and continuum emission from core-collapse supernovae in the Local Group, and from nearby Type Ia events, to constrain explosion models. During its baseline two-year mission, NuSTAR will also undertake a broad program of targeted observations. The observatory consists of two co-aligned grazing-incidence X-ray telescopes pointed at celestial targets by a three-axis stabilized spacecraft. Deployed into a 600 km, near-circular, 6\u00b0 inclination orbit, the observatory has now completed commissioning, and is performing consistent with pre-launch expectations. NuSTAR is now executing its primary science mission, and with an expected orbit lifetime of 10 yr, we anticipate proposing a guest investigator program, to begin in late 2014.",
"date": "2013-06-20",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "770",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 103",
"id_number": "CaltechAUTHORS:20130724-143120220",
"issn": "0004-637X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130724-143120220",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
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"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Technical University of Denmark National Space Institute"
},
{
"agency": "Centre National d'\u00c9tudes Spatiales (CNES)"
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"agency": "NASA Postdoctoral Program"
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"agency": "Leverhulme Trust"
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{
"agency": "Science and Technology Facilities Council (STFC)"
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{
"agency": "Department of Energy (DOE)"
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{
"agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)"
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{
"agency": "Canadian Institute for Advanced Research (CIFAR)"
},
{
"agency": "Fonds Qu\u00e9b\u00e9cois de la Recherche sur la Nature et les Technologies (FQRNT)"
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{
"agency": "Killam Research Fellowship"
},
{
"agency": "Agenzia Spaziale Italiana (ASI)"
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},
{
"id": "Nardini-E",
"name": {
"family": "Nardini",
"given": "E."
},
"orcid": "0000-0001-9226-8992"
},
{
"id": "Stern-D",
"name": {
"family": "Stern",
"given": "Daniel"
},
"orcid": "0000-0003-2686-9241"
},
{
"id": "Zhang-W-W",
"name": {
"family": "Zhang",
"given": "W. W."
},
"orcid": "0000-0002-1426-9698"
}
]
},
"title": "A rapidly spinning supermassive black hole at the centre of NGC\u20091365",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "High-energy astrophysics",
"note": "\u00a9 2013 Macmillan Publishers Limited.\nReceived 29 October 2012; Accepted 16 January 2013; Published online 27 February 2013.\n\n\nThis work was supported under NASA grant number\nNNG08FD60C, and made use of data from the Nuclear Spectroscopic Telescope Array\n(NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory,\nand funded by the National Aeronautics and Space Administration. We thank the\nNuSTAR Operations, Software and Calibration teams for support with execution and\nanalysis of these observations. This work also made use of observations obtained with\nXMM-Newton, an ESA science mission with instruments and contributions directly\nfunded by ESA Member States and NASA.\n\n\nAuthor Contributions: G.R. is the Principal Investigator of the XMM observations of\nNGC1365. He led the XMM data analysis and joint spectral analysis, modelling and\ninterpretation of the results. F.A.H. is the Principal Investigator of NuSTAR and led\nobservation planning, execution and participated in scientific interpretation and\nmanuscript preparation. D.J.W. analysed NuSTAR data and participated in modelling\nand interpretation. K.K.M. led NuSTAR calibration analysis for NGC1365. D.S. is the\nNuSTAR Project Scientist and participated in definition and interpretation of the\nobservations. B.W.G. assisted in adaptation of the NuSTAR data analysis to NGC1365.\nE.N. participated in XMM observations, reduction and interpretation. S.E.B., F.E.C.,\nW.W.C., C.J.H. and W.W.Z. led efforts in design, calibration and implementation of\nNuSTAR. All authors participated in review of the manuscript.\n\nSupplemental Material - nature11938-s1.pdf
",
"abstract": "Broad X-ray emission lines from neutral and partially ionized iron observed in active galaxies have been interpreted as fluorescence produced by the reflection of hard X-rays off the inner edge of an accretion disk. In this model, line broadening and distortion result from rapid rotation and relativistic effects near the black hole, the line shape being sensitive to its spin. Alternative models in which the distortions result from absorption by intervening structures provide an equally good description of the data, and there has been no general agreement on which is correct. Recent claims that the black hole (2\u2009\u00d7\u200910^6 solar masses) at the centre of the galaxy NGC\u20091365 is rotating at close to its maximum possible speed rest on the assumption of relativistic reflection. Here we report X-ray observations of NGC\u20091365 that reveal the relativistic disk features through broadened Fe-line emission and an associated Compton scattering excess of 10\u201330 kiloelectronvolts. Using temporal and spectral analyses, we disentangle continuum changes due to time-variable absorption from reflection, which we find arises from a region within 2.5 gravitational radii of the rapidly spinning black hole. Absorption-dominated models that do not include relativistic disk reflection can be ruled out both statistically and on physical grounds.",
"date": "2013-02-28",
"date_type": "published",
"publication": "Nature",
"volume": "494",
"number": "7438",
"publisher": "Nature Publishing Group",
"pagerange": "449-451",
"id_number": "CaltechAUTHORS:20130329-085204800",
"issn": "0028-0836",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130329-085204800",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNG08FD60C"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1038/nature11938",
"primary_object": {
"basename": "nature11938-s1.pdf",
"url": "https://authors.library.caltech.edu/records/p1zmw-hj976/files/nature11938-s1.pdf"
},
"pub_year": "2013",
"author_list": "Risaliti, G.; Harrison, F. A.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/3ax8p-gne43",
"eprint_id": 31717,
"eprint_status": "archive",
"datestamp": "2023-08-22 05:44:03",
"lastmod": "2023-10-17 20:19:56",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Liebe-C-C",
"name": {
"family": "Liebe",
"given": "Carl Christian"
}
},
{
"id": "Bauman-B-W",
"name": {
"family": "Bauman",
"given": "Bruce W."
}
},
{
"id": "Clark-G-R",
"name": {
"family": "Clark",
"given": "Gerald R."
}
},
{
"id": "Cook-R",
"name": {
"family": "Cook",
"given": "Rick"
}
},
{
"id": "Kecman-B",
"name": {
"family": "Kecman",
"given": "Branislav"
}
},
{
"id": "Madsen-K-K",
"name": {
"family": "Madsen",
"given": "Kristin Kruse"
},
"orcid": "0000-0003-1252-4891"
},
{
"id": "Mao-Peter-H",
"name": {
"family": "Mao",
"given": "Peter"
}
},
{
"id": "Meras-P-Jr",
"name": {
"family": "Meras",
"given": "Patrick, Jr."
}
},
{
"id": "Miyasaka-Hiromasa",
"name": {
"family": "Miyasaka",
"given": "Hiromasa"
},
"orcid": "0000-0002-8074-4186"
},
{
"id": "Cooper-M",
"name": {
"family": "Cooper",
"given": "Mark"
}
},
{
"id": "Scholz-C",
"name": {
"family": "Scholz",
"given": "Christopher"
}
},
{
"id": "Sedaka-J",
"name": {
"family": "Sedaka",
"given": "Jack"
}
}
]
},
"title": "Design, Qualification, Calibration and Alignment of Position Sensing Detector for the NuSTAR Space Mission",
"ispublished": "pub",
"full_text_status": "restricted",
"keywords": "Metrology system; NuSTAR; position sensing detector; space qualification",
"note": "\u00a9 2012 IEEE.\n\nManuscript received September 6, 2011; revised November 29, 2011; accepted December 8, 2011; Date of publication January 2, 2012; date of current version April 25, 2012.\n\nThis work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, Space Radiation Laboratory, California Institute of Technology, Space Sciences Laboratory, U.C. Berkeley, and Pacific Silicon Sensor, Inc., and was sponsored by the National Aeronautics and Space Administration. The associate editor\ncoordinating the review of this paper and approving it for publication was Prof. Julian C. C. Chan.",
"abstract": "A commercial position sensing detector (PSD) has been used to measure mast deflections on a space based X-ray telescope (NuSTAR). This paper describes the space qualification process for utilizing a commercial PSD sensor in space. This discussion includes packaging, environmental testing, selection of flight candidate devices, calibration and alignment.",
"date": "2012-06",
"date_type": "published",
"publication": "IEEE Sensors Journal",
"volume": "12",
"number": "6",
"publisher": "IEEE",
"pagerange": "2006-2013",
"id_number": "CaltechAUTHORS:20120530-131543504",
"issn": "1530-437X",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120530-131543504",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "Caltech Space Radiation Laboratory"
},
{
"agency": "U. C. Berkeley Space Sciences Laboratory"
},
{
"agency": "Pacific Silicon Sensor, Inc"
}
]
},
"collection": "CaltechAUTHORS",
"other_numbering_system": {
"items": [
{
"id": "12694671",
"name": "INSPEC Accession Number"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory",
"value": "Space Radiation Laboratory"
},
{
"id": "NuSTAR",
"value": "NuSTAR"
}
]
},
"doi": "10.1109/JSEN.2011.2181355",
"pub_year": "2012",
"author_list": "Liebe, Carl Christian; Bauman, Bruce W.; et el."
},
{
"id": "https://authors.library.caltech.edu/records/tspwr-n2r07",
"eprint_id": 31906,
"eprint_status": "archive",
"datestamp": "2023-08-22 05:21:59",
"lastmod": "2023-10-17 21:41:32",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Liebe-C-C",
"name": {
"family": "Liebe",
"given": "Carl Christian"
}
},
{
"id": "Craig-W-W",
"name": {
"family": "Craig",
"given": "William"
}
},
{
"id": "Kim-Yunjin",
"name": {
"family": "Kim",
"given": "Yunjin"
}
},
{
"id": "McLean-R",
"name": {
"family": "McLean",
"given": "Ryan"
}
},
{
"id": "Meras-P-Jr",
"name": {
"family": "Meras",
"given": "Patrick, Jr."
}
},
{
"id": "Raffanti-M",
"name": {
"family": "Raffanti",
"given": "Michael"
}
},
{
"id": "Scholz-C",
"name": {
"family": "Scholz",
"given": "Christopher"
}
}
]
},
"title": "Calibration and alignment of metrology system for the Nuclear Spectroscopic Telescope Array mission",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "NuSTAR; metrology system; alignment",
"note": "\u00a9 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nPaper 111097 received Sep 08, 2011; Accepted Feb 10, 2012; Revised Feb 08, 2012; Published online Apr 16, 2012. \n\nThe research described in this paper was carried out at the Jet\nPropulsion Laboratory, California Institute of Technology,\nSpace Radiation Laboratory, California Institute of Technology\nand Space Sciences Laboratory, U.C. Berkeley and was\nsponsored by the National Aeronautics and Space Administration.\nReferences herein to any specific commercial\nproduct, process or service by trademark, manufacturer, or\notherwise, does not constitute or imply its endorsement by\nthe United States Government or the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, Space Radiation\nLaboratory, California Institute of Technology or Space\nSciences Laboratory, U.C. Berkeley.\n\nPublished - Liebe2012p18436Opt_Eng.pdf
",
"abstract": "A metrology system to measure the on-orbit movement of a ten\nmeter mast has been built for the Nuclear Spectroscopic Telescope Array (NuSTAR) x-ray observatory. In this paper, the metrology system is described, and the performance is measured. The laser beam stability is discussed in detail. Pre-launch alignment and calibration are also described. The invisible infrared laser beams must be aligned to their corresponding detectors without deploying the telescope in Earth's gravity. Finally, a possible method for in-flight calibration of the metrology system is described.",
"date": "2012-04",
"date_type": "published",
"publication": "Optical Engineering",
"volume": "51",
"number": "4",
"publisher": "Society of Photo-optical Instrumentation Engineers",
"pagerange": "Art. No. 043605",
"id_number": "CaltechAUTHORS:20120614-122052306",
"issn": "0091-3286",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120614-122052306",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA"
}
]
},
"local_group": {
"items": [
{
"id": "NuSTAR"
},
{
"id": "Space-Radiation-Laboratory"
}
]
},
"doi": "10.1117/1.OE.51.4.043605",
"primary_object": {
"basename": "Liebe2012p18436Opt_Eng.pdf",
"url": "https://authors.library.caltech.edu/records/tspwr-n2r07/files/Liebe2012p18436Opt_Eng.pdf"
},
"pub_year": "2012",
"author_list": "Liebe, Carl Christian; Craig, William; et el."
},
{
"id": "https://authors.library.caltech.edu/records/myw02-wvz58",
"eprint_id": 69411,
"eprint_status": "archive",
"datestamp": "2023-08-19 18:36:00",
"lastmod": "2023-10-20 16:53:40",
"type": "article",
"metadata_visibility": "show",
"creators": {
"items": [
{
"id": "Parker-M-L",
"name": {
"family": "Parker",
"given": "M. L."
},
"orcid": "0000-0002-8466-7317"
},
{
"id": "Komossa-S",
"name": {
"family": "Komossa",
"given": "S."
}
},
{
"id": "Kollatschny-W",
"name": {
"family": "Kollatschny",
"given": "W."
}
},
{
"id": "Walton-D-J",
"name": {
"family": "Walton",
"given": "D. J."
},
"orcid": "0000-0001-5819-3552"
},
{
"id": "Schartel-N",
"name": {
"family": "Schartel",
"given": "N."
}
},
{
"id": "Santos-Lle\u00f3-M",
"name": {
"family": "Santos-Lle\u00f3",
"given": "M."
}
},
{
"id": "Harrison-F-A",
"name": {
"family": "Harrison",
"given": "F. A."
},
"orcid": "0000-0003-2992-8024"
},
{
"id": "Fabian-A-C",
"name": {
"family": "Fabian",
"given": "A. C."
},
"orcid": "0000-0002-9378-4072"
},
{
"id": "Zetzl-M",
"name": {
"family": "Zetzl",
"given": "M."
}
},
{
"id": "Grupe-D",
"name": {
"family": "Grupe",
"given": "D."
},
"orcid": "0000-0002-9961-3661"
},
{
"id": "Rodriguez-Pascual-P-M",
"name": {
"family": "Rodriguez-Pascual",
"given": "P. M."
}
}
]
},
"title": "The detection and X-ray view of the changing look AGN HE 1136-2304",
"ispublished": "pub",
"full_text_status": "public",
"note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 June 15. Received 2016 June 15. In original form 2016 March 5. First published online June 20, 2016. \n\nWe thank the anonymous referee for their detailed and constructive feedback. We thank Lutz Wisotzki for making available the optical spectrum of HE1136-2304 taken in 1993, and we thank Vassilis Karamanavis for a careful reading of the manuscript. MLP acknowledges financial support from the Science and Technology Facilities Council (STFC). This paper is based on observations taken with the SALT telescope. This work has been supported by DFG grant Ko 857/32-2. Based on observations with XMM\u2013Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would also like to thank Neil Gehrels for approving the Swift ToO requests, and the Swift science operation team for performing the observations.\n\nPublished - 2006-16.pdf
",
"abstract": "We report the detection of high-amplitude X-ray flaring of the AGN HE 1136-2304, which is accompanied by a strong increase in the flux of the broad Balmer lines, changing its Seyfert type from almost type 2 in 1993 down to 1.5 in 2014. HE 1136-2304 was detected by the XMM-Newton slew survey at >10 times the flux it had in the ROSAT all-sky survey, and confirmed with Swift follow-up after increasing in X-ray flux by a factor of 30. Optical spectroscopy with SALT shows that the AGN has changed from a Seyfert 1.95 to a Seyfert 1.5 galaxy, with greatly increased broad line emission and an increase in blue continuum AGN flux by a factor of > 4. The X-ray spectra from XMM-Newton and NuSTAR reveal moderate intrinsic absorption and a high energy cutoff at 100 keV. We consider several different physical scenarios for a flare, such as changes in obscuring material, tidal disruption events, and an increase in the accretion rate. We find that the most likely cause of the increased flux is an increase in the accretion rate, although it could also be due to a change in obscuration.",
"date": "2006-09-11",
"date_type": "published",
"publication": "Monthly Notices of the Royal Astronomical Society",
"volume": "461",
"number": "2",
"publisher": "Royal Astronomical Society",
"pagerange": "1927-1936",
"id_number": "CaltechAUTHORS:20160803-111444672",
"issn": "0035-8711",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160803-111444672",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "Science and Technology Facilities Council (STFC)"
},
{
"agency": "Deutsche Forschungsgemeinschaft (DFG)",
"grant_number": "857/32-2"
},
{
"agency": "ESA Member States"
},
{
"agency": "NASA/JPL/Caltech"
}
]
},
"other_numbering_system": {
"items": [
{
"id": "2006.16",
"name": "Space Radiation Laboratory"
}
]
},
"local_group": {
"items": [
{
"id": "Space-Radiation-Laboratory"
},
{
"id": "NuSTAR"
}
]
},
"doi": "10.1093/mnras/stw1449",
"primary_object": {
"basename": "2006-16.pdf",
"url": "https://authors.library.caltech.edu/records/myw02-wvz58/files/2006-16.pdf"
},
"pub_year": "2006",
"author_list": "Parker, M. L.; Komossa, S.; et el."
}
]