[ { "id": "https://authors.library.caltech.edu/records/wy3kc-jrr68", "eprint_id": 114811, "eprint_status": "archive", "datestamp": "2023-08-22 16:12:06", "lastmod": "2023-10-23 20:00:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bordoloi-Rongmon", "name": { "family": "Bordoloi", "given": "Rongmon" }, "orcid": "0000-0002-3120-7173" }, { "id": "O'Meara-John-M", "name": { "family": "O'Meara", "given": "John M." }, "orcid": "0000-0002-7893-1054" }, { "id": "Sharon-Keren", "name": { "family": "Sharon", "given": "Keren" }, "orcid": "0000-0002-7559-0864" }, { "id": "Rigby-Jane-R", "name": { "family": "Rigby", "given": "Jane R." }, "orcid": "0000-0002-7627-6551" }, { "id": "Cooke-Jeffrey", "name": { "family": "Cooke", "given": "Jeff" }, "orcid": "0000-0001-5703-2108" }, { "id": "Shaban-Ahmed", "name": { "family": "Shaban", "given": "Ahmed" }, "orcid": "0000-0002-8858-7875" }, { "id": "Matuszewski-Mateusz", "name": { "family": "Matuszewski", "given": "Mateusz" }, "orcid": "0000-0003-2821-1750" }, { "id": "Rizzi-Luca", "name": { "family": "Rizzi", "given": "Luca" }, "orcid": "0000-0003-0882-2327" }, { "id": "Doppmann-Greg-W", "name": { "family": "Doppmann", "given": "Greg" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Moore-Anna-M", "name": { "family": "Moore", "given": "Anna M." }, "orcid": "0000-0002-2894-6936" }, { "id": "Morrissey-Patrick", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neill-James-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Resolving the H i in damped Lyman \u03b1 systems that power star formation", "ispublished": "pub", "full_text_status": "public", "keywords": "Multidisciplinary", "note": "\u00a9 2022 Springer Nature Limited. \n\nReceived 18 August 2021. Accepted 04 March 2022. Published 18 May 2022. \n\nThis work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W.\u2009M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration (NASA) through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.\u2009M. Keck Foundation. This research was conducted, in part, by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. We wish to 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. This research made use of Montage. It is funded by the National Science Foundation under grant number ACI-1440620, and was previously funded by the NASA's Earth Science Technology Office, Computation Technologies Project, under cooperative agreement number NCC5-626 between NASA and the California Institute of Technology. \n\nData availability. Data that support the findings of this study are publicly available at the Keck Observatory Archive, https://www2.keck.hawaii.edu/koa/public/koa.php, under project codes N083 and K338 and the Barbara\u2009A. Mikulski Archive for Space Telescope under project code GO-13003. Fully reduced data are available from the corresponding author upon request. \n\nCode availability. All codes used in this work are publicly available. The H\u2009I column density measurements were performed using the linetools package (https://doi.org/10.5281/zenodo.168270). Reduction and analysis of the KCWI data cubes were done using the kcwitools package (https://doi.org/10.5281/zenodo.6079396). The lensing raytracing and absorption line measurements are done using the rbcodes package (https://doi.org/10.5281/zenodo.6079264). HST image analysis and lens modelling were performed with AstroDizzle software and Lenstool, respectively. \n\nContributions. R.B. and J.M.O. developed the idea for the project, wrote the NASA/Keck telescope proposal and designed and performed the observations. R.B. developed the analysis tools, performed the analysis, devised original ways to interpret the results and authored majority of the text. J.M.O. reduced the KCWI data. A.S. performed the metal absorption line measurements. K.S. performed the lens model and provided Extended Data Fig. 1. J.R.R. provided the ancillary data from MagE and metal absorber information from MagE spectra. J.C., J.M.O. and R.B. provided steps to correct astrometric offsets and J.C. confirmed the redshift of the second DLA, and contributed to the interpretations. M.M., L.R., G.D., D.C.M., A.M.M., P.M. and J.D.N. developed the KCWI data reduction pipeline and built and delivered the instrument when initial commissioning data provided the data needed to verify the target as an object of interest. All authors, including J.M.O., J.R.R. and J.C., contributed to the overall interpretation of the results and various aspects of the analysis and writing. \n\nThe authors declare no competing interests. \n\nPeer review information. Nature thanks Zachary Hafen and Marcel Neeleman for their contribution to the peer review of this work.\n\n
Accepted Version - 2205.08554.pdf
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Supplemental Material - 41586_2022_4616_Fig6_ESM.jpg
Supplemental Material - 41586_2022_4616_Fig7_ESM.jpg
Supplemental Material - 41586_2022_4616_Fig8_ESM.jpg
Supplemental Material - 41586_2022_4616_Tab1_ESM.jpg
Supplemental Material - 41586_2022_4616_Tab2_ESM.jpg
", "abstract": "Reservoirs of dense atomic gas (primarily hydrogen) contain approximately 90\u2009per\u2009cent of the neutral gas at a redshift of 3, and contribute to between 2 and 3\u2009per\u2009cent of the total baryons in the Universe. These 'damped Lyman\u2009\u03b1 systems'\u2014so called because they absorb Lyman\u2009\u03b1 photons within and from background sources\u2014have been studied for decades, but only through absorption lines present in the spectra of background quasars and \u03b3-ray bursts. Such pencil beams do not constrain the physical extent of the systems. Here we report integral-field spectroscopy of a bright, gravitationally lensed galaxy at a redshift of 2.7 with two foreground damped Lyman\u2009\u03b1 systems. These systems are greater than 238\u2009kiloparsecs\u2009squared in extent, with column densities of neutral hydrogen varying by more than an order of magnitude on scales of less than 3\u2009kiloparsecs. The mean column densities are between 10^(20.46) and 10^(20.84)\u2009centimetres squared and the total masses are greater than 5.5\u2009\u00d7\u200910\u2078\u20131.4\u2009\u00d7\u200910\u2079 times the mass of the Sun, showing that they contain the necessary fuel for the next generation of star formation, consistent with relatively massive, low-luminosity primeval galaxies at redshifts greater than\u20092.", "date": "2022-06-02", "date_type": "published", "publication": "Nature", "volume": "606", "number": "7912", "publisher": "Nature Publishing Group", "pagerange": "59-63", "id_number": "CaltechAUTHORS:20220519-375159000", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220519-375159000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Australian Research Council", "grant_number": "CE170100013" }, { "agency": "NSF", "grant_number": "ACI-1440620" }, { "agency": "NASA/Caltech", "grant_number": "NCC5-626" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/s41586-022-04616-1", "primary_object": { "basename": "41586_2022_4616_Tab1_ESM.jpg", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/41586_2022_4616_Tab1_ESM.jpg" }, "related_objects": [ { "basename": "41586_2022_4616_Tab2_ESM.jpg", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/41586_2022_4616_Tab2_ESM.jpg" }, { "basename": "2205.08554.pdf", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/2205.08554.pdf" }, { "basename": "41586_2022_4616_Fig5_ESM.jpg", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/41586_2022_4616_Fig5_ESM.jpg" }, { "basename": "41586_2022_4616_Fig6_ESM.jpg", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/41586_2022_4616_Fig6_ESM.jpg" }, { "basename": "41586_2022_4616_Fig7_ESM.jpg", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/41586_2022_4616_Fig7_ESM.jpg" }, { "basename": "41586_2022_4616_Fig8_ESM.jpg", "url": "https://authors.library.caltech.edu/records/wy3kc-jrr68/files/41586_2022_4616_Fig8_ESM.jpg" } ], "pub_year": "2022", "author_list": "Bordoloi, Rongmon; O'Meara, John M.; et el." }, { "id": "https://authors.library.caltech.edu/records/4s8gp-hg912", "eprint_id": 112928, "eprint_status": "archive", "datestamp": "2023-08-22 13:19:10", "lastmod": "2023-10-23 22:51:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Villaume-Alexa", "name": { "family": "Villaume", "given": "Alexa" }, "orcid": "0000-0003-1887-0621" }, { "id": "Romanowsky-Aaron-J", "name": { "family": "Romanowsky", "given": "Aaron J." }, "orcid": "0000-0003-2473-0369" }, { "id": "Brodie-Jean-P", "name": { "family": "Brodie", "given": "Jean" }, "orcid": "0000-0002-9658-8763" }, { "id": "van-Dokkum-Pieter", "name": { "family": "van Dokkum", "given": "Pieter" } }, { "id": "Conroy-Charlie", "name": { "family": "Conroy", "given": "Charlie" }, "orcid": "0000-0002-1590-8551" }, { "id": "Forbes-Duncan-A", "name": { "family": "Forbes", "given": "Duncan A." }, "orcid": "0000-0001-5590-5518" }, { "id": "Danieli-Shany", "name": { "family": "Danieli", "given": "Shany" }, "orcid": "0000-0002-1841-2252" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Matuszewski-Matt", "name": { "family": "Matuszewski", "given": "Matt" } } ] }, "title": "Spatially Resolved Stellar Spectroscopy of the Ultra-diffuse Galaxy Dragonfly 44. III. Evidence for an Unexpected Star Formation History under Conventional Galaxy Evolution Processes", "ispublished": "pub", "full_text_status": "public", "keywords": "Coma Cluster; Chemical abundances; Galaxy evolution; Galaxy quenching; Galaxy stellar content; 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 January 5; revised 2021 September 23; accepted 2021 October 26; published 2022 January 10. \n\nWe would like to thank the anonymous referee for their constructive comments, J. Gannon for some discussion about GC candidate selection, M. Gu for help with various technical odds and ends, S. Laine for discussions about SFHs, R. Schiavon for helping with EZ_Ages, and J. Taylor for very helpful discussion about the dynamics of satellites in clusters. This research was supported in part by the National Science Foundation under grant No. NSF PHY-1748958 through the Kavli Institute for Theoretical Physics workshop Globular Clusters at the Nexus of Star and Galaxy Formation for enabling useful discussions relevant to this paper. A.V. would like to acknowledge the NSF Graduate Fellowship, the UC Santa Cruz Chancellor's Dissertation Year Fellowship, and the Waterloo Centre Astrophysics Postdoctoral Fellowship for their support. A.J.R. was supported by National Science Foundation grant AST-1616710, and as a Research Corporation for Science Advancement Cottrell Scholar. S.D. is supported by NASA through Hubble Fellowship grant #HST-HF2-51454.001-A 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. \n\nSoftware: IPython (P\u00e9rez & Granger 2007), SciPy (Virtanen et al. 2020), NumPy (Van Der Walt et al. 2011), matplotlib (Hunter 2007), Astropy (Astropy Collaboration et al. 2018), PyMC3 (Salvatier & Wiecki 2016), SPI (Villaume et al. 2017) alf (Conroy et al. 2018), EZ_Ages (Schiavon 2007; Graves & Schiavon 2008).\n\nPublished - Villaume_2022_ApJ_924_32.pdf
Accepted Version - 2101.02220.pdf
", "abstract": "We use the Keck Cosmic Web Imager integral field unit spectrograph to (1) measure the global stellar population parameters for the ultra-diffuse galaxy (UDG) Dragonfly 44 (DF44) to much higher precision than previously possible for any UDG and (2) for the first time measure spatially resolved stellar population parameters of a UDG. We find that DF44 falls below the mass\u2013metallicity relation established by canonical dwarf galaxies both in and beyond the Local Group. We measure a flat radial age gradient (m_(logage) = +0.01_(-0.08)^(+0.08) log Gyr kpc\u207b\u00b9) and a flat to positive metallicity gradient (m_[Fe/H] = +0.09_(-0.12)^(+0.11) dex kpc\u207b\u00b9), which are inconsistent with the gradients measured in similarly pressure-supported dwarf galaxies. We also measure a negative [Mg/Fe] gradient (m_[Mg/Fe] = -0.20_(-0.18)^(+0.18)) dex kpc\u207b\u00b9 such that the central 1.5 kpc of DF44 has stellar population parameters comparable to metal-poor globular clusters. Overall, DF44 does not have internal properties similar to other dwarf galaxies and is inconsistent with it having been puffed up through a prolonged, bursty star formation history, as suggested by some simulations. Rather, the evidence indicates that DF44 experienced an intense epoch of \"inside-out\" star formation and then quenched early and catastrophically, such that star formation was cut off more quickly than in canonical dwarf galaxies.", "date": "2022-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "924", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 32", "id_number": "CaltechAUTHORS:20220114-265463000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220114-265463000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1748958" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "University of California, Santa Cruz" }, { "agency": "Waterloo Centre Astrophysics Postdoctoral Fellowship" }, { "agency": "NSF", "grant_number": "AST-1616710" }, { "agency": "Cottrell Scholar of Research Corporation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51454.001-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/ac341e", "primary_object": { "basename": "2101.02220.pdf", "url": "https://authors.library.caltech.edu/records/4s8gp-hg912/files/2101.02220.pdf" }, "related_objects": [ { "basename": "Villaume_2022_ApJ_924_32.pdf", "url": "https://authors.library.caltech.edu/records/4s8gp-hg912/files/Villaume_2022_ApJ_924_32.pdf" } ], "pub_year": "2022", "author_list": "Villaume, Alexa; Romanowsky, Aaron J.; et el." }, { "id": "https://authors.library.caltech.edu/records/hnfsd-1gs59", "eprint_id": 108134, "eprint_status": "archive", "datestamp": "2023-08-22 08:58:20", "lastmod": "2023-10-23 16:29:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Joshi-Ravi", "name": { "family": "Joshi", "given": "Ravi" }, "orcid": "0000-0002-5535-4186" }, { "id": "Fumagalli-Michele", "name": { "family": "Fumagalli", "given": "Michele" }, "orcid": "0000-0001-6676-3842" }, { "id": "Srianand-Raghunathan", "name": { "family": "Srianand", "given": "Raghunathan" }, "orcid": "0000-0002-9062-1921" }, { "id": "Noterdaeme-Pasquier", "name": { "family": "Noterdaeme", "given": "Pasquier" }, "orcid": "0000-0002-5777-1629" }, { "id": "Petitjean-Patrick", "name": { "family": "Petitjean", "given": "Patrick" } }, { "id": "Rafelski-M", "name": { "family": "Rafelski", "given": "Marc" }, "orcid": "0000-0002-9946-4731" }, { "id": "Mackenzie-Ruari", "name": { "family": "Mackenzie", "given": "Ruari" }, "orcid": "0000-0003-0417-385X" }, { "id": "Li-Qiong", "name": { "family": "Li", "given": "Qiong" }, "orcid": "0000-0002-3119-9003" }, { "id": "Cai-Zheng", "name": { "family": "Cai", "given": "Zheng" }, "orcid": "0000-0001-8467-6478" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Zou-Siwei", "name": { "family": "Zou", "given": "Siwei" }, "orcid": "0000-0002-3983-6484" }, { "id": "Wu-Xue-Bing", "name": { "family": "Wu", "given": "Xue-Bing" }, "orcid": "0000-0002-7350-6913" }, { "id": "Jiang-Linhua", "name": { "family": "Jiang", "given": "Linhua" }, "orcid": "0000-0003-4176-6486" }, { "id": "Ho-Luis-C", "name": { "family": "Ho", "given": "Luis C." }, "orcid": "0000-0001-6947-5846" } ] }, "title": "Discovery of a Damped Ly\u03b1 Galaxy at z \u223c 3 toward the Quasar SDSS J011852+040644", "ispublished": "pub", "full_text_status": "public", "keywords": "Quasar absorption line spectroscopy; Damped Ly\u03b1 systems; Star formation", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2019 September 4; revised 2020 November 10; accepted 2020 December 4; published 2021 February 18. \n\nWe thank the anonymous referee for useful comments. This research uses data obtained through the Telescope Access Program (TAP). This work was supported by the National Key R&D Program of China (2016YFA0400702, 2016YFA0400703), the National Science Foundation of China (11473002, 11721303, 11533001) and China Postdoctoral Science Foundation Grants (2018M630024, 2019T120011). M.F. acknowledges support by the Science and Technology Facilities Council [grant No. ST/P000541/1]. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 757535). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 757535). This work has been supported by Fondazione Cariplo, grant No. 2018-2329. P.N. acknowledges support from the French Agence Nationale de la Recherche under grant No. ANR-17-CE31-0011-01. Observations obtained with the Hale Telescope at Palomar Observatory were obtained as part of an agreement between the National Astronomical Observatories, Chinese Academy of Sciences, and the California Institute of Technology. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrof\u00edsica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut f\u00fcr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00fcr Astronomie (MPIA Heidelberg), Max-Planck-Institut f\u00fcr Astrophysik (MPA Garching), Max-Planck-Institut f\u00fcr Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observat\u00e1rio Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Aut\u00f3noma de M\u00e9xico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.\n\nPublished - Joshi_2021_ApJ_908_129.pdf
Accepted Version - 2012.07422.pdf
", "abstract": "We report the detection of the host galaxy of a damped Ly\u03b1 system (DLA) with log N(H i) [cm\u207b\u00b2] = 21.0 \u00b1 0.10 at z \u2248 3.0091 toward the background quasar SDSS J011852+040644 using the Palomar Cosmic Web Imager at the Hale (P200) telescope. We detect Ly\u03b1 emission in the dark core of the DLA trough at a 3.3\u03c3 confidence level, with Ly\u03b1 luminosity of L(Ly\u03b1) = (3.8 \u00b1 0.8) \u00d7 10\u2074\u00b2 erg s\u207b\u00b9, corresponding to a star formation rate of \u22732 M_\u2299 yr\u207b\u00b9 (considering a lower limit on Ly\u03b1 escape fraction f_(esc)^(Ly\u03b1) ~2%) as typical for Lyman break galaxies at these redshifts. The Ly\u03b1 emission is blueshifted with respect to the systemic redshift derived from metal absorption lines by 281 \u00b1 43 km s\u22121. The associated galaxy is at very small impact parameter of \u2a7d12 kpc from the background quasar, which is in line with the observed anticorrelation between column density and impact parameter in spectroscopic searches tracing the large-scale environments of DLA host galaxies.", "date": "2021-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "908", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 129", "id_number": "CaltechAUTHORS:20210222-100902868", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210222-100902868", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Key Research and Development Program of China", "grant_number": "2016YFA0400702" }, { "agency": "National Key Basic Research Program of China", "grant_number": "2016YFA0400703" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11473002" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11721303" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11533001" }, { "agency": "China Postdoctoral Science Foundation", "grant_number": "2018M630024" }, { "agency": "China Postdoctoral Science Foundation", "grant_number": "2019T120011" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000541/1" }, { "agency": "European Research Council (ERC)", "grant_number": "757535" }, { "agency": "Fondazione Cariplo", "grant_number": "2018-2329" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-17-CE31-0011-01" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/abd1d5", "primary_object": { "basename": "2012.07422.pdf", "url": "https://authors.library.caltech.edu/records/hnfsd-1gs59/files/2012.07422.pdf" }, "related_objects": [ { "basename": "Joshi_2021_ApJ_908_129.pdf", "url": "https://authors.library.caltech.edu/records/hnfsd-1gs59/files/Joshi_2021_ApJ_908_129.pdf" } ], "pub_year": "2021", "author_list": "Joshi, Ravi; Fumagalli, Michele; et el." }, { "id": "https://authors.library.caltech.edu/records/v96ve-stw79", "eprint_id": 104897, "eprint_status": "archive", "datestamp": "2023-08-22 07:38:43", "lastmod": "2023-10-23 19:31:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hoadley-Keri-L", "name": { "family": "Hoadley", "given": "Keri" }, "orcid": "0000-0002-8636-3309" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Metzger-B-D", "name": { "family": "Metzger", "given": "Brian D." }, "orcid": "0000-0002-4670-7509" }, { "id": "Seibert-Mark", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "McWilliam-Andrew", "name": { "family": "McWilliam", "given": "Andrew" } }, { "id": "Shen-Ken-J", "name": { "family": "Shen", "given": "Ken J." }, "orcid": "0000-0002-9632-6106" }, { "id": "Neill-James-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Stefansson-Gudmundur-K", "name": { "family": "Stefansson", "given": "Gudmundur" }, "orcid": "0000-0001-7409-5688" }, { "id": "Monson-Andrew-J", "name": { "family": "Monson", "given": "Andrew" }, "orcid": "0000-0002-0048-2586" }, { "id": "Schaefer-Bradley-E", "name": { "family": "Schaefer", "given": "Bradley E." }, "orcid": "0000-0002-2659-8763" } ] }, "title": "A blue ring nebula from a stellar merger several thousand years ago", "ispublished": "pub", "full_text_status": "public", "keywords": "Stars; Stellar evolution", "note": "\u00a9 2020 Springer Nature. \n\nReceived 04 May 2020. Accepted 01 September 2020. Published 18 November 2020. \n\nThis research is based on observations made with GALEX, obtained from the MAST data archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy under NASA contract NAS 5\u201326555. Some of the data presented were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership between the California Institute of Technology, the University of California and NASA. This research made use of the Keck Observatory Archive, which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute, under contract with NASA, and made possible by the financial support of the W. M. Keck Foundation. We recognize and acknowledge the very important cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are fortunate to have the opportunity to conduct observations from this mountain. Some of the data presented were obtained at the Palomar Observatory. This research made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We thank V. Scowcroft for obtaining Spitzer/IRAC photometry of TYC 2597-735-1. Funding for APASS was provided by the Robert Martin Ayers Sciences Fund. The DASCH data from the Harvard archival plates was partially supported from National Science Foundation (NSF) grants AST-0407380, AST-0909073 and AST-1313370. The American Association of Variable Star Observers has been helpful for finder charts, comparison star magnitudes and recruiting skilled observers, including S. Dufoer, K. Menzies, R. Sabo, G. Stone, R. Tomlin and G. Walker. These results are based on observations obtained with the HPF on the Hobby\u2013Eberly Telescope (HET), which is named in honour of its principal benefactors, William P. Hobby and Robert E. Eberly. These data were obtained during HPF's engineering and commissioning period. We thank the resident astronomers and telescope operators at the HET for the execution of our observations with HPF. We thank C. Ca\u00f1as for providing an independent verification of the HPF SERVAL pipeline using a CCF-based method to calculate the radial velocities, which resulted in fully consistent radial velocities to the SERVAL-based radial velocities presented here. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universit\u00e4t M\u00fcnchen and Georg-August Universit\u00e4t Gottingen. The HET collaboration acknowledges support and resources from the Texas Advanced Computing Center. This work was partially supported by funding from the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science and the Pennsylvania Space Grant Consortium. We thank A. Gil de Paz for obtaining the narrow-band-filter H\u03b1 imagery, J. Johnson for commissioning TYC 2597-735-1 radial velocity measurements as part of the California Planet Finder programme, and A. Howard for leading Keck\u2013HIRES spectra and performing the primary radial-velocity reduction on all HIRES data. K.H. acknowledges support from a David and Ellen Lee Postdoctoral Fellowship in Experimental Physics at Caltech, and thanks L. Hillenbrand and E. Hamden for discussions about aspects of this work. B.D.M. acknowledges support from the Hubble Space Telescope (number HST-AR-15041.001-A) and the NSF (number 80NSSC18K1708). K.J.S. received support from the NASA Astrophysics Theory Program (NNX17AG28G). G.S. and A.Mo. acknowledge support from NSF grants AST-1006676, AST-1126413, AST-1310885, AST-1517592, AST-1310875 and AST-1907622, the NASA Astrobiology Institute (NNA09DA76A) and PSARC in their pursuit of precision radial velocities in the near-infrared with HPF. We acknowledge support from the Heising-Simons Foundation via grant 2017-0494 and 2019-1177. Computations for this research were performed on the Pennsylvania State University's Institute for Computational and Data Sciences. G.S. acknowledges support by NASA HQ under the NASA Earth and Space Science Fellowship Program through grant NNX16AO28H, and is a Henry Norris Russell Fellow. \n\nData availability:\nAll GALEX imaging and grism data of TYC 2597-735-1 and its ultraviolet nebula are publicly available from the Mikulski Archive for Space Telescopes (MAST) in raw and reduced formats (http://galex.stsci.edu/GalexView/ or https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html). All Keck\u2013LRIS and Keck\u2013HIRES data for TYC 2597-735-1 are publicly available from the Keck Observatory Archive (https://koa.ipac.caltech.edu/cgi-bin/KOA/nph-KOAlogin). TYC 2597-735-1 raw photometric light-curve frames, plates and light curves from 1895 to 1985 are publicly available as a part of the DASCH programme (https://projects.iq.harvard.edu/dasch). Data for the more recent photmetry for the light-curve construction is available from the corresponding author on request. All other photometric data for TYC 2597-735-1 were obtained from publicly archived ground- and space-based imaging and surveys, stored on the SIMBAD Astronomical Database (http://simbad.u-strasbg.fr/simbad/) and the NASA/IPAC Infrared Science Archive (https://irsa.ipac.caltech.edu/frontpage/). The relevant data products from the Habitable-zone Planet Finder Spectrograph (HPF) campaign for TYC 2597-735-1 are publicly available at https://github.com/oglebee-chessqueen/BlueRingNebula.git. \n\nCode availability. We used MESA for a portion of our analysis. Although MESA is readily available for public use, we used a custom subroutine and MESA inline code to produce the TYC 2597-735-1 merger evolution model, publicly available at https://github.com/oglebee-chessqueen/BlueRingNebula.git. Use the ATLAS9 pre-set grid of synthetic stellar spectra to fit the TYC 2597-735-1 spectral energy distribution to representative stellar spectra. All synthetic stellar spectra are publicly available at https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogues/castelli-and-kurucz-atlas. Portions of our analysis used community-developed core Python packages for astronomy, photutils and astropy. \n\nThese authors contributed equally: Keri Hoadley, D. Christopher Martin, Brian D. Metzger, Mark Seibert. \n\nAuthor Contributions. K.H. and B.D.M. organized and wrote the main body of the paper. K.H. and M.S. performed the data reduction and analysis of the GALEX data, investigated the source of the ultraviolet emission, quantified the mass the far-ultraviolet nebula, and led the the analysis of the H\u03b1 emission and variability of TYC 2597-735-1. B.D.M. led all theoretical and analytic interpretation efforts of the ultraviolet nebula origins and TYC 2597-735-1 in the context of stellar mergers and present-day luminous red novae. D.C.M. and M.S. led the GALEX programme that led to the detection of the ultraviolet nebula in 2004 and all subsequent follow-up observations of the nebula with GALEX; both contributed to the overall interpretation of the observational data. D.C.M. contributed to the organization and writing of the paper. M.S. led the radial-velocity analysis and the interpretation and analysis of the infrared excess in the spectral energy distribution of TYC 2597-735-1, modelled this distribution (stellar and dust infrared excess components), and coordinated all ground-based observations of the blue ring nebula and TYC 2597-735-1 at Palomar Observatory and W. M. Keck Observatory. K.H. also helped in the interpretation and analysis of the infrared excess in the spectral energy distribution of TYC 2597-735-1. A.Mc. derived the physical parameters, performed the model atmosphere chemical abundance analysis of TYC 2597-735-1, and participated in discussions of observations, analysis and interpretation. K.J.S. performed the MESA calculations and participated in discussions of observations, analysis and interpretation. J.D.N. handled the data analysis, reported the result of the velocity structure of the H\u03b1 shock observed with Keck\u2013LRIS, and participated in discussions of observations, analysis and interpretation. G.S. performed the HET\u2013HPF radial-velocity and differential line-width indicator extractions and provided expertise on the interpretation of the combined radial-velocity datasets. A.Mo. coordinated HET\u2013HPF observations, and performed and reduced all TMMT B-band observations. B.E.S. extracted and analysed the long-term light-curve data from May 1897 to September 2019. \n\nThe authors declare no competing interests. \n\nPeer review information. Nature thanks the anonymous reviewer(s) for their contribution to the peer review of this work. Peer reviewer reports are available.\n\nAccepted Version - 2011.09589.pdf
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Supplemental Material - 41586_2020_2893_Fig9_ESM.jpg
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Supplemental Material - 41586_2020_2893_MOESM2_ESM.pdf
", "abstract": "Stellar mergers are a brief but common phase in the evolution of binary star systems. These events have many astrophysical implications; for example, they may lead to the creation of atypical stars (such as magnetic stars, blue stragglers and rapid rotators), they play an important part in our interpretation of stellar populations and they represent formation channels of compact-object mergers. Although a handful of stellar mergers have been observed directly, the central remnants of these events were shrouded by an opaque shell of dust and molecules, making it impossible to observe their final state (for example, as a single merged star or a tighter, surviving binary). Here we report observations of an unusual, ring-shaped ultraviolet ('blue') nebula and the star at its centre, TYC 2597-735-1. The nebula has two opposing fronts, suggesting a bipolar outflow of material from TYC 2597-735-1. The spectrum of TYC 2597-735-1 and its proximity to the Galactic plane suggest that it is an old star, yet it has abnormally low surface gravity and a detectable long-term luminosity decay, which is uncharacteristic for its evolutionary stage. TYC 2597-735-1 also exhibits H\u03b1 emission, radial-velocity variations, enhanced ultraviolet radiation and excess infrared emission\u2014signatures of dusty circumstellar disks, stellar activity and accretion. Combined with stellar evolution models, the observations suggest that TYC 2597-735-1 merged with a lower-mass companion several thousand years ago. TYC 2597-735-1 provides a look at an unobstructed stellar merger at an evolutionary stage between its dynamic onset and the theorized final equilibrium state, enabling the direct study of the merging process.", "date": "2020-11-19", "date_type": "published", "publication": "Nature", "volume": "587", "number": "7834", "publisher": "Nature Publishing Group", "pagerange": "387-391", "id_number": "CaltechAUTHORS:20200810-151015540", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200810-151015540", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-0407380" }, { "agency": "NSF", "grant_number": "AST-0909073" }, { "agency": "NSF", "grant_number": "AST-1313370" }, { "agency": "William P. Hobby" }, { "agency": "Robert E. Eberly" }, { "agency": "Texas Advanced Computing Center (TACC)" }, { "agency": "Center for Exoplanets and Habitable Worlds" }, { "agency": "Pennsylvania State University" }, { "agency": "Eberly College of Science" }, { "agency": "Pennsylvania Space Grant Consortium" }, { "agency": "David and Ellen Lee Postdoctoral Scholarship" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-AR-15041.001-A" }, { "agency": "NASA", "grant_number": "80NSSC18K1708" }, { "agency": "NASA", "grant_number": "NNX17AG28G" }, { "agency": "NSF", "grant_number": "AST-1006676" }, { "agency": "NSF", "grant_number": "AST-1126413" }, { "agency": "NSF", "grant_number": "AST-1310885" }, { "agency": "NSF", "grant_number": "AST-1517592" }, { "agency": "NSF", "grant_number": "AST-1310875" }, { "agency": "NSF", "grant_number": "AST-1907622" }, { "agency": "NASA Postdoctoral Program", "grant_number": "NNA09DA76A" }, { "agency": "Penn State Astrobiology Research Center (PSARC)" }, { "agency": "Heising-Simons Foundation", "grant_number": "2017-0494" }, { "agency": "Heising-Simons Foundation", "grant_number": "2019-1177" }, { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX16AO28H" }, { "agency": "Princeton University" }, { "agency": "Robert Martin Ayers Sciences Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/s41586-020-2893-5", "primary_object": { "basename": "41586_2020_2893_Fig7_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig7_ESM.jpg" }, "related_objects": [ { "basename": "41586_2020_2893_Fig8_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig8_ESM.jpg" }, { "basename": "41586_2020_2893_MOESM2_ESM.pdf", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_MOESM2_ESM.pdf" }, { "basename": "41586_2020_2893_Fig11_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig11_ESM.jpg" }, { "basename": "41586_2020_2893_Fig6_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig6_ESM.jpg" }, { "basename": "41586_2020_2893_Fig4_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig4_ESM.jpg" }, { "basename": "41586_2020_2893_Fig5_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig5_ESM.jpg" }, { "basename": "41586_2020_2893_Fig9_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig9_ESM.jpg" }, { "basename": "41586_2020_2893_MOESM1_ESM.pdf", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_MOESM1_ESM.pdf" }, { "basename": "2011.09589.pdf", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/2011.09589.pdf" }, { "basename": "41586_2020_2893_Fig10_ESM.jpg", "url": "https://authors.library.caltech.edu/records/v96ve-stw79/files/41586_2020_2893_Fig10_ESM.jpg" } ], "pub_year": "2020", "author_list": "Hoadley, Keri; Martin, D. Christopher; et el." }, { "id": "https://authors.library.caltech.edu/records/0f025-wgt69", "eprint_id": 102008, "eprint_status": "archive", "datestamp": "2023-08-22 04:24:28", "lastmod": "2023-10-19 23:44:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nick Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Sobral-D", "name": { "family": "Sobral", "given": "David" }, "orcid": "0000-0001-8823-4845" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "Bahram" } }, { "id": "Rettura-A", "name": { "family": "Rettura", "given": "Alessandro" }, "orcid": "0000-0002-5615-256X" }, { "id": "Matthee-J", "name": { "family": "Matthee", "given": "Jorryt" }, "orcid": "0000-0003-2871-127X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Chartab-Nima", "name": { "family": "Chartab", "given": "Nima" }, "orcid": "0000-0003-3691-937X" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Daniel" }, "orcid": "0000-0001-5382-6138" }, { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "Hooshang" }, "orcid": "0000-0001-8242-9983" }, { "id": "O'Sullivan-Donal", "name": { "family": "O'Sullivan", "given": "Donal" }, "orcid": "0000-0002-4959-9179" }, { "id": "Paulino-Afonso-A", "name": { "family": "Paulino-Afonso", "given": "Ana" }, "orcid": "0000-0002-0943-0694" }, { "id": "Sattari-Zahra", "name": { "family": "Sattari", "given": "Zahra" }, "orcid": "0000-0002-0364-1159" }, { "id": "Shahidi-Abtin", "name": { "family": "Shahidi", "given": "Abtin" }, "orcid": "0000-0001-6975-6293" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Lemaux-B-C", "name": { "family": "Lemaux", "given": "Brian C." }, "orcid": "0000-0002-1428-7036" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "Olivier" }, "orcid": "0000-0001-5891-2596" }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "Olga" }, "orcid": "0000-0002-9336-7551" } ] }, "title": "Spectroscopic Confirmation of a Coma Cluster Progenitor at z \u223c 2.2", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy clusters; High-redshift galaxy clusters; High-redshift galaxies; Large-scale structure of the universe; Galaxy evolution; Star formation; Galaxy environments", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 July 27; revised 2020 January 17; accepted 2020 February 10; published 2020 March 19. \n\nWe are thankful to the anonymous referee for useful comments and suggestions that improved the quality of this paper. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. B.D. is thankful to Andreas Faisst, Laura Danly, and Matthew Burlando for their companionship during the observing run. B.D. is grateful to the COSMOS team for their useful comments during the team meeting in New York City 2019 May 14\u201317. A.R. research was made possible by Friends of W. M. Keck Observatory who philanthropically support the Keck Science Collaborative (KSC) fund. The observations presented herein were obtained at the W. M. Keck Observatory (program C236, PI Scoville), 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 would like to recognize and acknowledge the very prominent cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are fortunate to have the opportunity to perform observations from this mountain.\n\nPublished - Darvish_2020_ApJ_892_8.pdf
Submitted - 2002.06207.pdf
", "abstract": "We report the spectroscopic confirmation of a new protocluster in the COSMOS field at z ~ 2.2, COSMOS Cluster 2.2 (CC2.2), originally identified as an overdensity of narrowband selected H\u03b1 emitting candidates. With only two masks of Keck/MOSFIRE near-IR spectroscopy in both H (~1.47\u20131.81 \u03bcm) and K (~1.92\u20132.40 \u03bcm) bands (~1.5 hr each), we confirm 35 unique protocluster members with at least two emission lines detected with S/N > 3. Combined with 12 extra members from the zCOSMOS-deep spectroscopic survey (47 in total), we estimate a mean redshift and a line-of-sight velocity dispersion of z_(mean) = 2.23224 \u00b1 0.00101 and \u03c3_(los) = 645 \u00b1 69 km s\u22121 for this protocluster, respectively. Assuming virialization and spherical symmetry for the system, we estimate a total mass of M_(vir) ~ (1\u20132) \u00d710\u00b9\u2074 M\u2299 for the structure. We evaluate a number density enhancement of \u03b4 g ~ 7 for this system and we argue that the structure is likely not fully virialized at z ~ 2.2. However, in a spherical collapse model, \u03b4 g is expected to grow to a linear matter enhancement of ~1.9 by z = 0, exceeding the collapse threshold of 1.69, and leading to a fully collapsed and virialized Coma-type structure with a total mass of M_(dyn)(z = 0) ~ 9.2 \u00d7 10\u00b9\u2074 M\u2299 by now. This observationally efficient confirmation suggests that large narrowband emission-line galaxy surveys, when combined with ancillary photometric data, can be used to effectively trace the large-scale structure and protoclusters at a time when they are mostly dominated by star-forming galaxies.", "date": "2020-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "892", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 8", "id_number": "CaltechAUTHORS:20200320-071214007", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200320-071214007", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AE20G" }, { "agency": "NSF", "grant_number": "AST-1716907" }, { "agency": "W. M. Keck Observatory" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/ab75c3", "primary_object": { "basename": "Darvish_2020_ApJ_892_8.pdf", "url": "https://authors.library.caltech.edu/records/0f025-wgt69/files/Darvish_2020_ApJ_892_8.pdf" }, "related_objects": [ { "basename": "2002.06207.pdf", "url": "https://authors.library.caltech.edu/records/0f025-wgt69/files/2002.06207.pdf" } ], "pub_year": "2020", "author_list": "Darvish, Behnam; Scoville, Nick Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/8eg7q-m4e14", "eprint_id": 101939, "eprint_status": "archive", "datestamp": "2023-08-22 03:30:42", "lastmod": "2023-10-19 23:40:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kyne-G", "name": { "family": "Kyne", "given": "Gillian" } }, { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } }, { "id": "Hoadley-K-L", "name": { "family": "Hoadley", "given": "Keri" }, "orcid": "0000-0002-8636-3309" }, { "id": "Jewell-A-D", "name": { "family": "Jewell", "given": "April" }, "orcid": "0000-0001-8834-3769" }, { "id": "Jones-Todd", "name": { "family": "Jones", "given": "Todd" }, "orcid": "0000-0001-5860-3419" }, { "id": "Hoenk-M-E", "name": { "family": "Hoenk", "given": "Michael" } }, { "id": "Cheng-Samuel-R", "name": { "family": "Cheng", "given": "Samuel" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Lingner-N", "name": { "family": "Lingner", "given": "Nicole" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Grange-R", "name": { "family": "Grange", "given": "Robert" } }, { "id": "Daigle-O", "name": { "family": "Daigle", "given": "Olivier" } } ] }, "title": "Delta-doped electron-multiplying CCDs for FIREBall-2", "ispublished": "pub", "full_text_status": "public", "keywords": "electron-multiplying CCD; photon counting; delta-doped; ultraviolet; detector; clocking; clock-induced-charge; dark current", "note": "\u00a9 2020 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nPaper 19089SS received Sep. 4, 2019; accepted for publication Feb. 20, 2020; published online Mar. 12, 2020. \n\nThe research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors would like to acknowledge generous and excellent collaborative support from e2v including A. Reinheimer, P. Jerram, P. Jorden, and their team on the 2-D doped EMCCDs.\n\nPublished - 011007_1.pdf
Accepted Version - 2004.05947.pdf
", "abstract": "We present the status of on-going detector development efforts for our joint NASA/Centre National d'\u00c9tudes Spatiales balloon-borne UV multiobject spectrograph, the Faint Intergalactic Redshifted Emission Balloon (FIREBall-2; FB-2). FB-2 demonstrates a UV detector technology, the delta-doped electron-multiplying CCD (EMCCD), in a low-risk suborbital environment, to prove the performance of EMCCDs for future space missions and technology readiness level advancement. EMCCDs can be used in photon-counting mode to achieve extremely low readout noise (<1 electron). Our testing has focused on reducing clock-induced-charge (CIC) through wave shaping and well-depth optimization with a N\u00fcv\u00fc V2 CCCP controller, measuring CIC at 0.001\u2009\u2009e\u207b/pixel/frame. This optimization also includes methods for reducing dark current, via cooling, and substrate voltage levels. We discuss the challenges of removing cosmic rays, which are also amplified by these detectors, as well as a data reduction pipeline designed for our noise measurement objectives. FB-2 flew in 2018, providing the first time an EMCCD, was used for UV observations in the stratosphere. FB-2 is currently being built up to fly again in 2020, and improvements are being made to the EMCCD to continue optimizing its performance for better noise control.", "date": "2020-01", "date_type": "published", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "volume": "6", "number": "1", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "pagerange": "Art. No. 011007", "id_number": "CaltechAUTHORS:20200316-151904591", "issn": "2329-4124", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200316-151904591", "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-Astrophysics-Laboratory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1117/1.jatis.6.1.011007", "primary_object": { "basename": "011007_1.pdf", "url": "https://authors.library.caltech.edu/records/8eg7q-m4e14/files/011007_1.pdf" }, "related_objects": [ { "basename": "2004.05947.pdf", "url": "https://authors.library.caltech.edu/records/8eg7q-m4e14/files/2004.05947.pdf" } ], "pub_year": "2020", "author_list": "Kyne, Gillian; Hamden, Erika T.; et el." }, { "id": "https://authors.library.caltech.edu/records/p9xn1-w2w15", "eprint_id": 93291, "eprint_status": "archive", "datestamp": "2023-08-19 14:42:15", "lastmod": "2023-10-20 17:00:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Relatores-N-C", "name": { "family": "Relatores", "given": "Nicole C." }, "orcid": "0000-0002-6041-6388" }, { "id": "Newman-A-B", "name": { "family": "Newman", "given": "Andrew B." }, "orcid": "0000-0001-7769-8660" }, { "id": "Simon-J-D", "name": { "family": "Simon", "given": "Joshua D." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard" }, "orcid": "0000-0001-7782-7071" }, { "id": "Truong-Phuongmai", "name": { "family": "Truong", "given": "Phuongmai" }, "orcid": "0000-0001-9248-6631" }, { "id": "Blitz-L", "name": { "family": "Blitz", "given": "Leo" }, "orcid": "0000-0002-4272-4432" }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "Alberto" }, "orcid": "0000-0002-5480-5686" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" } ] }, "title": "Dark Matter Distributions in Low-mass Disk Galaxies. I. H\u03b1 Observations Using the Palomar Cosmic Web Imager", "ispublished": "pub", "full_text_status": "public", "keywords": "dark matter \u2013 galaxies: dwarf \u2013 galaxies: kinematics and dynamics \u2013 galaxies: structure", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 December 21; revised 2019 January 22; accepted 2019 January 23; published 2019 February 27. \n\nWe would like to thank Joshua Adams, Rachel Kuzio de Naray, and Kristine Spekkens for providing the rotation curve data used for comparisons made in Figure 8. \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 the SIMBAD database, operated at CDS, Strasbourg, France.\n\nPublished - Relatores_2019_ApJ_873_5.pdf
", "abstract": "Dark-matter-only simulations predict that dark matter halos have cusp-like inner density profiles, while observations of low-mass galaxies have found a range of inner slopes that are typically much shallower. It is still not well established whether this discrepancy can be explained by baryonic feedback or if it may require modified dark matter models. To better understand the diversity of dark matter profiles in dwarf galaxies, we undertook a survey of 26 low-mass galaxies (log M*/M\u2299 = 8.4-9.8, v_(max) = 50\u2013140 km s^(\u22121)) within 30 Mpc using the Palomar Cosmic Web Imager, which is among the largest integral field spectroscopic surveys of its type. In this paper, we derive H\u03b1 velocity fields for the full sample with a typical spatial resolution of ~160 pc. We extract rotation curves and verify their robustness to several choices in the analysis. We present a method for improving the velocity precision obtained from image slicing spectrographs using narrowband H\u03b1 images. For 11 galaxies, we compare the H\u03b1 velocity fields to CO kinematics measured using CARMA, finding the maps to be in good agreement. The standard deviation of the difference is typically ~7 km s^(\u22121), comparable to the level of turbulence in the interstellar medium, showing that the two tracers have substantially the same bulk kinematics. In a companion paper, we will use the rotation curves produced here to construct mass models of the galaxies and determine their dark matter density profiles.", "date": "2019-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "873", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 5", "id_number": "CaltechAUTHORS:20190227-091113228", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190227-091113228", "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-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/ab0382", "primary_object": { "basename": "Relatores_2019_ApJ_873_5.pdf", "url": "https://authors.library.caltech.edu/records/p9xn1-w2w15/files/Relatores_2019_ApJ_873_5.pdf" }, "pub_year": "2019", "author_list": "Relatores, Nicole C.; Newman, Andrew B.; et el." }, { "id": "https://authors.library.caltech.edu/records/gqkx4-q1931", "eprint_id": 89357, "eprint_status": "archive", "datestamp": "2023-08-19 11:23:20", "lastmod": "2023-10-18 22:41:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Fucik-J-R", "name": { "family": "Fucik", "given": "Jason" } }, { "id": "Weber-R", "name": { "family": "Weber", "given": "Bob" } }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Belicki-J", "name": { "family": "Belicki", "given": "Justin" } }, { "id": "Crabill-M", "name": { "family": "Crabill", "given": "Marty" } }, { "id": "Delecroix-A", "name": { "family": "Delecroix", "given": "Alex" } }, { "id": "Kaye-S-A", "name": { "family": "Kaye", "given": "Steve" } }, { "id": "O'Sullivan-Donal", "name": { "family": "O'Sullivan", "given": "Donal" }, "orcid": "0000-0002-4959-9179" }, { "id": "Parihar-Prachi", "name": { "family": "Parihar", "given": "Prachi" } }, { "id": "Rodriguez-Hector", "name": { "family": "Rodriguez", "given": "Hector" } }, { "id": "Zarzaca-R", "name": { "family": "Zarzaca", "given": "Ray" } } ] }, "title": "The Keck Cosmic Web Imager Integral Field Spectrograph", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: kinematics and dynamics \u2013 instrumentation: spectrographs \u2013 intergalactic medium \u2013 quasars:\ngeneral \u2013 techniques: imaging spectroscopy \u2013 techniques: spectroscopic", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 February 20; revised 2018 July 4; accepted 2018 July 12; published 2018 September 4. \n\nThe Keck Cosmic Web Imager was developed through a collaboration of the California Institute of Technology, the University of California, and the W. M. Keck Observatory. The research described in this publication was carried out by the California Institute of Technology and by the Jet Propulsion Laboratory, which is managed by the California Institute of Technology. The work was sponsored by grants from the Telescope System Instrumentation Program (TSIP) and the Major Research Instrumentation Program (MRI) of the National Science Foundation, as well as grants from the Heising-Simons Foundation, the W. M. Keck Observatory, and the Caltech Division of Physics, Math and Astronomy. We acknowledge our major industrial partner Winlight Optics (Pertuis, France) for their cooperation and assistance in the fabrication of the IFU and powered reflective optics. We would also like to thank the referee for constructive and helpful comments. \n\nMuch 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. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThe 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. \n\nFacilities: GALEX - Galaxy Evolution Explorer satellite, Hale - , Keck:II (KCWI) - , Spitzer. -\n\nPublished - Morrissey_2018_ApJ_864_93.pdf
Accepted Version - 1807.10356.pdf
", "abstract": "We report on the design and performance of the Keck Cosmic Web Imager (KCWI), a general purpose optical integral field spectrograph that has been installed at the Nasmyth port of the 10 m Keck II telescope on Maunakea, Hawaii. The novel design provides blue-optimized seeing-limited imaging from 350\u2013560 nm with configurable spectral resolution from 1000\u201320,000 in a field of view up to 20'' \u00d7 33''. Selectable volume phase holographic (VPH) gratings and high-performance dielectric, multilayer silver, and enhanced-aluminum coatings provide end-to-end peak efficiency in excess of 45% while accommodating the future addition of a red channel that will extend wavelength coverage to 1 micron. KCWI takes full advantage of the excellent seeing and dark sky above Maunakea with an available nod-and-shuffle observing mode. The instrument is optimized for observations of faint, diffuse objects such as the intergalactic medium or cosmic web. In this paper, a detailed description of the instrument design is provided with measured performance results from the laboratory test program and 10 nights of on-sky commissioning during the spring of 2017. The KCWI team is lead by Caltech and JPL (project management, design, and implementation) in partnership with the University of California at Santa Cruz (camera optical and mechanical design) and the W. M. Keck Observatory (observatory interfaces).", "date": "2018-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "864", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 93", "id_number": "CaltechAUTHORS:20180904-103955908", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-103955908", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Heising-Simons Foundation" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/aad597", "primary_object": { "basename": "1807.10356.pdf", "url": "https://authors.library.caltech.edu/records/gqkx4-q1931/files/1807.10356.pdf" }, "related_objects": [ { "basename": "Morrissey_2018_ApJ_864_93.pdf", "url": "https://authors.library.caltech.edu/records/gqkx4-q1931/files/Morrissey_2018_ApJ_864_93.pdf" } ], "pub_year": "2018", "author_list": "Morrissey, Patrick; Matuszewski, Mateusz; et el." }, { "id": "https://authors.library.caltech.edu/records/jk9j1-afc58", "eprint_id": 77885, "eprint_status": "archive", "datestamp": "2023-08-21 21:42:26", "lastmod": "2023-10-25 23:32:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } }, { "id": "Jewell-A-D", "name": { "family": "Jewell", "given": "April D." }, "orcid": "0000-0001-8834-3769" }, { "id": "Hoenk-M-E", "name": { "family": "Hoenk", "given": "Michael E." } }, { "id": "Jones-T-J", "name": { "family": "Jones", "given": "Todd J." } }, { "id": "Hennessy-J-L", "name": { "family": "Hennessy", "given": "John" } }, { "id": "Goodsall-Tim-M", "name": { "family": "Goodsall", "given": "Tim" } }, { "id": "Carver-A-G", "name": { "family": "Carver", "given": "Alexander G." } }, { "id": "Shapiro-C", "name": { "family": "Shapiro", "given": "Charles" } }, { "id": "Cheng-Samuel-R", "name": { "family": "Cheng", "given": "Samuel R." } }, { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Kyne-G", "name": { "family": "Kyne", "given": "Gillian" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Scowen-P-A", "name": { "family": "Scowen", "given": "Paul" } }, { "id": "France-K", "name": { "family": "France", "given": "Kevin" }, "orcid": "0000-0002-1002-3674" }, { "id": "McCandliss-S", "name": { "family": "McCandliss", "given": "Stephan" } }, { "id": "Lupu-R-E", "name": { "family": "Lupu", "given": "Roxana E." } } ] }, "title": "High Efficiency UV/Optical/NIR Detectors for Large Aperture Telescopes and UV Explorer Missions: Development of and Field Observations with Delta-doped Arrays", "ispublished": "pub", "full_text_status": "public", "keywords": "detectors; delta doping; superlattice doping; UV; two-dimensional doping; atomic layer deposition; coatings; deployment; quantum efficiency; solar-blind silicon; silicon", "note": "\u00a9 2017 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nPaper 16061 received Jan. 9, 2017; accepted for publication Jul. 25, 2017; published online Sep. 1, 2017. \n\nThe research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors gratefully acknowledge the support from NASA-SAT, NASA-APRA, JPL' RTD program, the Keck Institute for Space Studies, and many years of other support from NASA and JPL and other agencies. E.T.K. acknowledges the support by Nancy Grace Roman Fellowship, the Millikan Prize in Experimental Physics, and the NSF Fellowship. The authors would like to acknowledge generous and excellent collaborative support from e2v including A. Reinheimer, P. Jerram, P. Pool, P. Jorden, and P. Fochi on the 2D-doped EMCCDs. The authors gratefully acknowledge the collaborative work with LBNL. S. Holland, C. Bebek, N. Roe, and their team that has led to the demonstration and development of 2D-doped, p-channel CCDs; as well as Bruno Milliard and Robert Grange of LAM for the FIREBall-2 spectrograph data. We acknowledge M. McClish of RMD for APD QE data and wafer processing. We also thank S. R. Kulkarni, R. Smith, and J. Milburn of Caltech Optical Observatories and Palomar Observatory for WaSP delta-doped array first-light images; as well as R. Goldstein and team for the MICA-LEES flight.\n\nPublished - 036002.pdf
Submitted - 1612.04734.pdf
", "abstract": "Exciting concepts are under development for flagship, probe class, explorer class, and suborbital class NASA missions in the ultraviolet/optical spectral range. These missions will depend on high-performance silicon detector arrays being delivered affordably and in high numbers. To that end, we have advanced delta-doping technology to high-throughput and high-yield wafer-scale processing, encompassing a multitude of state-of-the-art silicon-based detector formats and designs. We have embarked on a number of field observations, instrument integrations, and independent evaluations of delta-doped arrays. We present recent data and innovations from JPL's Advanced Detectors and Systems Program, including two-dimensional doping technology, JPL's end-to-end postfabrication processing of high-performance UV/optical/NIR arrays and advanced coatings for detectors. While this paper is primarily intended to provide an overview of past work, developments are identified and discussed throughout. Additionally, we present examples of past, in-progress, and planned observations and deployments of delta-doped arrays.", "date": "2017-09-01", "date_type": "published", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "volume": "3", "number": "3", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "pagerange": "Art. No. 036002", "id_number": "CaltechAUTHORS:20170601-085352803", "issn": "2329-4124", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170601-085352803", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "Nancy Grace Roman Fellowship" }, { "agency": "Millikan Prize in Experimental Physics" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Keck-Institute-for-Space-Studies" } ] }, "doi": "10.1117/1.JATIS.3.3.036002", "primary_object": { "basename": "036002.pdf", "url": "https://authors.library.caltech.edu/records/jk9j1-afc58/files/036002.pdf" }, "related_objects": [ { "basename": "1612.04734.pdf", "url": "https://authors.library.caltech.edu/records/jk9j1-afc58/files/1612.04734.pdf" } ], "pub_year": "2017", "author_list": "Nikzad, Shouleh; Jewell, April D.; et el." }, { "id": "https://authors.library.caltech.edu/records/c0dra-n0a61", "eprint_id": 78052, "eprint_status": "archive", "datestamp": "2023-08-21 21:14:06", "lastmod": "2023-10-25 23:42:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Darvish-B", "name": { "family": "Darvish", "given": "Behnam" }, "orcid": "0000-0003-4919-9017" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } } ] }, "title": "Quenching or Bursting: Star Formation Acceleration\u2014A New Methodology for Tracing Galaxy Evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: star formation; ultraviolet: galaxies", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 October 8. Accepted 2017 May 5. Published 2017 June 8. \n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in April 2003. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Behnam Darvish acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank the anonymous referee for valuable comments that strengthened the paper. \n\nFacilities: GALEX, SDSS.\n\nPublished - Martin_2017_ApJ_842_20.pdf
Submitted - 1705.03514.pdf
", "abstract": "We introduce a new methodology for the direct extraction of galaxy physical parameters from multiwavelength photometry and spectroscopy. We use semianalytic models that describe galaxy evolution in the context of large-scale cosmological simulation to provide a catalog of galaxies, star formation histories, and physical parameters. We then apply models of stellar population synthesis and a simple extinction model to calculate the observable broadband fluxes and spectral indices for these galaxies. We use a linear regression analysis to relate physical parameters to observed colors and spectral indices. The result is a set of coefficients that can be used to translate observed colors and indices into stellar mass, star formation rate, and many other parameters, including the instantaneous time derivative of the star formation rate, which we denote the Star Formation Acceleration (SFA), We apply the method to a test sample of galaxies with GALEX photometry and SDSS spectroscopy, deriving relationships between stellar mass, specific star formation rate, and SFA. We find evidence for a mass-dependent SFA in the green valley, with low-mass galaxies showing greater quenching and higher-mass galaxies greater bursting. We also find evidence for an increase in average quenching in galaxies hosting an active galactic nucleus. A simple scenario in which lower-mass galaxies accrete and become satellite galaxies, having their star-forming gas tidally and/or ram-pressure stripped, while higher-mass galaxies receive this gas and react with new star formation, can qualitatively explain our results.", "date": "2017-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "842", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 20", "id_number": "CaltechAUTHORS:20170609-093105834", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170609-093105834", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" }, { "agency": "NASA", "grant_number": "NNX12AE20G" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/aa71a9", "primary_object": { "basename": "1705.03514.pdf", "url": "https://authors.library.caltech.edu/records/c0dra-n0a61/files/1705.03514.pdf" }, "related_objects": [ { "basename": "Martin_2017_ApJ_842_20.pdf", "url": "https://authors.library.caltech.edu/records/c0dra-n0a61/files/Martin_2017_ApJ_842_20.pdf" } ], "pub_year": "2017", "author_list": "Martin, D. Christopher; Gon\u00e7alves, Thiago S.; et el." }, { "id": "https://authors.library.caltech.edu/records/zgr5v-rfs11", "eprint_id": 76828, "eprint_status": "archive", "datestamp": "2023-08-21 20:51:46", "lastmod": "2023-10-25 16:54:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael M." } }, { "id": "Doyle-T-F", "name": { "family": "Doyle", "given": "Trisha" }, "orcid": "0000-0001-7182-5307" }, { "id": "Lauer-T-R", "name": { "family": "Lauer", "given": "Tod R." } }, { "id": "Zurek-David", "name": { "family": "Zurek", "given": "David" } }, { "id": "Baltz-E-A", "name": { "family": "Baltz", "given": "Edward A." } }, { "id": "Kovetz-A", "name": { "family": "Kovetz", "given": "Attay" } }, { "id": "Madrid-J-P", "name": { "family": "Madrid", "given": "Juan P." } }, { "id": "Miko\u0142ajewska-J", "name": { "family": "Miko\u0142ajewska", "given": "Joanna" } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Prialnik-D", "name": { "family": "Prialnik", "given": "Dina" } }, { "id": "Welch-D-L", "name": { "family": "Welch", "given": "D. L." } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" } ] }, "title": "A Hubble Space Telescope Survey for Novae in M87. II. Snuffing out the Maximum Magnitude\u2013Rate of Decline Relation for Novae as a Non-standard Candle, and a Prediction of the Existence of Ultrafast Novae", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: numerical; neutrinos; radiative transfer; relativistic processes; (stars: supernovae: general)", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2015 December 24. Accepted 2016 May 1. Published 2017 April 21. \n\nWe are grateful to A. Juodagalvis for providing the data of electron capture rates on heavy nuclei. H.N. acknowledges to M. Shibata, Y. Sekiguchi and H. Okawa for valuable comments and discussions. H.N. also thanks Werner Marcus for proofreadings. The numerical computations were performed on the supercomputers at K, at AICS, FX10 at Information Technology Center of Tokyo University, SR16000 at YITP of Kyoto University, and SR16000 at KEK under the support of its Large Scale Simulation Program (14/15-17, 15/16-08), Research Center for Nuclear Physics (RCNP) at Osaka University. Large-scale storage of numerical data is supported by JLDG constructed over SINET4 of NII. H.N. was supported in part by JSPS Postdoctoral Fellowships for Research Abroad No. 27-348. This work was also supported by Grant-in-Aid for the Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan (15K05093, 24103006, 24740165, 24244036, 25870099) and HPCI Strategic Program of Japanese MEXT and K computer at the RIKEN (Project ID: hpci 130025, 140211, and 150225).\n\nPublished - Shara_2017_ApJ_839_109.pdf
Submitted - 1702.05788.pdf
", "abstract": "The extensive grid of numerical simulations of nova eruptions from the work of Yaron et al. first predicted that some classical novae might significantly deviate from the Maximum Magnitude\u2013Rate of Decline (MMRD) relation, which purports to characterize novae as standard candles. Kasliwal et al. have announced the observational detection of a new class of faint, fast classical novae in the Andromeda galaxy. These objects deviate strongly from the MMRD relationship, as predicted by Yaron et al. Recently, Shara et al. reported the first detections of faint, fast novae in M87. These previously overlooked objects are as common in the giant elliptical galaxy M87 as they are in the giant spiral M31; they comprise about 40% of all classical nova eruptions and greatly increase the observational scatter in the MMRD relation. We use the extensive grid of the nova simulations of Yaron et al. to identify the underlying causes of the existence of faint, fast novae. These are systems that have accreted, and can thus eject, only very low-mass envelopes, of the order of 10^(\u22127)\u201310^(\u22128) M_\u2299, on massive white dwarfs. Such binaries include, but are not limited to, the recurrent novae. These same models predict the existence of ultrafast novae that display decline times, t_2, to be as short as five hours. We outline a strategy for their future detection.", "date": "2017-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "839", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 109", "id_number": "CaltechAUTHORS:20170421-151346490", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170421-151346490", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "High Energy Accelerator Research Organization (KEK)", "grant_number": "14/15-17" }, { "agency": "High Energy Accelerator Research Organization (KEK)", "grant_number": "15/16-08" }, { "agency": "Osaka University Research Center for Nuclear Physics" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "27-348" }, { "agency": "Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) Japan", "grant_number": "15K05093" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24103006" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan", "grant_number": "24740165" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24244036" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "25870099" }, { "agency": "RIKEN", "grant_number": "130025" }, { "agency": "RIKEN", "grant_number": "140211" }, { "agency": "RIKEN", "grant_number": "150225" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/aa65cd", "primary_object": { "basename": "1702.05788.pdf", "url": "https://authors.library.caltech.edu/records/zgr5v-rfs11/files/1702.05788.pdf" }, "related_objects": [ { "basename": "Shara_2017_ApJ_839_109.pdf", "url": "https://authors.library.caltech.edu/records/zgr5v-rfs11/files/Shara_2017_ApJ_839_109.pdf" } ], "pub_year": "2017", "author_list": "Shara, Michael M.; Doyle, Trisha; et el." }, { "id": "https://authors.library.caltech.edu/records/ywdsf-jk416", "eprint_id": 75042, "eprint_status": "archive", "datestamp": "2023-08-19 01:55:57", "lastmod": "2023-10-25 14:41:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cai-Zheng", "name": { "family": "Cai", "given": "Zheng" }, "orcid": "0000-0001-8467-6478" }, { "id": "Fan-Xiaohui", "name": { "family": "Fan", "given": "Xiaohui" }, "orcid": "0000-0003-3310-0131" }, { "id": "Yang-Yujin", "name": { "family": "Yang", "given": "Yujin" }, "orcid": "0000-0003-3078-2763" }, { "id": "Bian-Fuyan", "name": { "family": "Bian", "given": "Fuyan" } }, { "id": "Prochaska-J-X", "name": { "family": "Prochaska", "given": "J. Xavier" }, "orcid": "0000-0002-7738-6875" }, { "id": "Zabludoff-A-I", "name": { "family": "Zabludoff", "given": "Ann" }, "orcid": "0000-0001-6047-8469" }, { "id": "McGreer-I-D", "name": { "family": "McGreer", "given": "Ian" }, "orcid": "0000-0002-3461-5228" }, { "id": "Zheng-Zhen-Ya", "name": { "family": "Zheng", "given": "Zhen-Ya" } }, { "id": "Greenberg-R", "name": { "family": "Greenberg", "given": "Richard" } }, { "id": "Cantalupo-S", "name": { "family": "Cantalupo", "given": "Sebastiano" }, "orcid": "0000-0001-5804-1428" }, { "id": "Frye-B-L", "name": { "family": "Frye", "given": "Brenda" } }, { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika" } }, { "id": "Jiang-Linhua", "name": { "family": "Jiang", "given": "Linhua" }, "orcid": "0000-0003-4176-6486" }, { "id": "Kashikawa-Nobunari", "name": { "family": "Kashikawa", "given": "Nobunari" } }, { "id": "Wang-Ran", "name": { "family": "Wang", "given": "Ran" }, "orcid": "0000-0003-4956-5742" } ] }, "title": "Discovery of an Enormous Ly\u03b1 Nebula in a Massive Galaxy Overdensity at z = 2.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift, intergalactic medium", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 13; revised 2017 January 20; accepted 2017 January 24; published 2017 March 3. \n\nZ.C. acknowledges the valuable comments from Fabrizio Arrigoni Battaia, Joe Hennawi, and Arjue Dey. Z.C., X.F., and I.M. thank the support from the US NSF grant AST 11-07682. Z.C. and J.X.P. acknowledge support from NSF AST-1412981. Y.Y.'s research was supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science, ICT & Future Planning (NRF 2016R1C1B2007782). A.Z. acknowledges support from NSF grant AST-0908280 and NASA grant ADP-NNX10AD47G. S.C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2_163824. N.K. acknowledges support from the JSPS grant 15H03645. This work is based on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 2013A-0434; PI: Z. Cai; NOAO Prop. ID: 2014A-0395; PI: Z. Cai), which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The LBT Corporation partners are The University of Arizona on behalf of the Arizona university system; Instituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia.\n\nPublished - Cai_2017_ApJ_837_71.pdf
Submitted - 1609.04021.pdf
", "abstract": "Enormous Ly\u03b1 nebulae (ELANe), unique tracers of galaxy density peaks, are predicted to lie at the nodes and intersections of cosmic filamentary structures. Previous successful searches for ELANe have focused on wide-field narrowband surveys or have targeted known sources such as ultraluminous quasi-stellar objects (QSOs) or radio galaxies. Utilizing groups of coherently strong Ly\u03b1 absorptions, we have developed a new method to identify high-redshift galaxy overdensities and have identified an extremely massive overdensity, BOSS1441, at z = 2-3. In its density peak, we discover an ELAN that is associated with a relatively faint continuum. To date, this object has the highest diffuse Ly\u03b1 nebular luminosity of L_(nebula) = 5.1 \u00b1 0.1 x 10^(44) erg s^(\u22121). Above the 2\u03c3 surface brightness limit of SB Ly\u03b1 = 4.8 x 10^(-18) erg s^(\u22121) cm^(\u22122) arcsec^(\u22122), this nebula has an end-to-end spatial extent of 442 kpc. This radio-quiet source also has extended C IV \u03bb1549 and He II \u03bb1640 emission on \u2273 30 kpc scales. Note that the Ly\u03b1, He II, and C IV emissions all have double-peaked line profiles. Each velocity component has an FWHM of \u2248700\u20131000 km s^(\u22121). We argue that this Ly\u03b1 nebula could be powered by shocks due to an active galactic nucleus\u2013driven outflow or photoionization by a strongly obscured source.", "date": "2017-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "837", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 71", "id_number": "CaltechAUTHORS:20170311-205211262", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170311-205211262", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 11-07682" }, { "agency": "NSF", "grant_number": "AST-1412981" }, { "agency": "National Research Foundation of Korea", "grant_number": "2016R1C1B2007782" }, { "agency": "NSF", "grant_number": "AST-0908280" }, { "agency": "NSF", "grant_number": "ADP-NNX10AD47G" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "PP00P2_163824" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H03645" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/aa5d14", "primary_object": { "basename": "1609.04021.pdf", "url": "https://authors.library.caltech.edu/records/ywdsf-jk416/files/1609.04021.pdf" }, "related_objects": [ { "basename": "Cai_2017_ApJ_837_71.pdf", "url": "https://authors.library.caltech.edu/records/ywdsf-jk416/files/Cai_2017_ApJ_837_71.pdf" } ], "pub_year": "2017", "author_list": "Cai, Zheng; Fan, Xiaohui; et el." }, { "id": "https://authors.library.caltech.edu/records/ax35c-rcy84", "eprint_id": 75792, "eprint_status": "archive", "datestamp": "2023-08-19 01:32:40", "lastmod": "2023-10-25 15:18:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mirek-R", "name": { "family": "Mirek", "given": "R" } }, { "id": "Kr\u00f3l-M", "name": { "family": "Kr\u00f3l", "given": "M." } }, { "id": "Lekenta-K", "name": { "family": "Lekenta", "given": "K." } }, { "id": "Rousset-J-G", "name": { "family": "Rousset", "given": "J.-G." } }, { "id": "Narocki-M", "name": { "family": "Nawrocki", "given": "M." } }, { "id": "Kulcyzkowski-M", "name": { "family": "Kulczykowski", "given": "M." } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "M." } }, { "id": "Szczytko-J", "name": { "family": "Szczytko", "given": "J." } }, { "id": "Pacuski-W", "name": { "family": "Pacuski", "given": "W." } }, { "id": "Pi\u0119tka-B", "name": { "family": "Pi\u0119tka", "given": "B." } } ] }, "title": "Angular dependence of giant Zeeman effect for semimagnetic cavity polariton", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Physical Society. \n\nReceived 29 August 2016; revised manuscript received 20 December 2016; published 21 February 2017. \n\nThis work was supported by the National Science Centre, Poland, under Projects No. 2014/13/N/ST3/03763, No. 2015/16/T/ST3/00506, No. 2015/18/E/ST3/00558, No. 2015/18/E/ST3/00559, No. 2013/09/B/ST3/02603, and No. 2015/17/B/ST3/02273, and by the Polish Ministry of Science and Higher Education as Iuventus Plus Research Grants No. IP2014 040473 and No. IP2014 034573 in years 2015\u20132017. This study was carried out with the use of CePT, CeZaMat, and NLTK infrastructures financed by the European Union, European Regional Development Fund. Scientific work was co-financed from the Polish Ministry of Science and Higher Education budget for education as a research project \"Diamentowy Grant\" No. 0010/DIA/2016/45 in years 2016\u20132020 and No. 0109/DIA/2015/44 in years 2015\u20132019.\n\nPublished - PhysRevB.95.085429.pdf
Submitted - 1609.00405.pdf
", "abstract": "The observation of spin-related phenomena of microcavity polaritons has been limited due to the weak Zeeman effect of nonmagnetic semiconductors. We demonstrate that the incorporation of magnetic ions into quantum wells placed in a nonmagnetic microcavity results in enhanced effects of magnetic field on exciton-polaritons. We show that in such a structure the Zeeman splitting of exciton-polaritons strongly depends on the photon-exciton detuning and polariton wave vector. Our experimental data are explained by a model where the impact of magnetic field on the lower polariton state is directly inherited from the excitonic component, and the coupling strength to the cavity photon is modified by an external magnetic field.", "date": "2017-02-15", "date_type": "published", "publication": "Physical Review B", "volume": "95", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 085429", "id_number": "CaltechAUTHORS:20170406-094552273", "issn": "2469-9950", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170406-094552273", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Centre (Poland)", "grant_number": "2014/13/N/ST3/03763" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/16/T/ST3/00506" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/18/E/ST3/00558" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/18/E/ST3/00559" }, { "agency": "National Science Centre (Poland)", "grant_number": "2013/09/B/ST3/02603" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/17/B/ST3/02273" }, { "agency": "Ministry of Science and Higher Education (Poland)", "grant_number": "IP2014 040473" }, { "agency": "Ministry of Science and Higher Education (Poland)", "grant_number": "IP2014 034573" }, { "agency": "European Union" }, { "agency": "European Regional Development Fund" }, { "agency": "Ministry of Science and Higher Education (Poland)", "grant_number": "0010/DIA/2016/45" }, { "agency": "Ministry of Science and Higher Education (Poland)", "grant_number": "0109/DIA/2015/44" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1103/PhysRevB.95.085429", "primary_object": { "basename": "1609.00405.pdf", "url": "https://authors.library.caltech.edu/records/ax35c-rcy84/files/1609.00405.pdf" }, "related_objects": [ { "basename": "PhysRevB.95.085429.pdf", "url": "https://authors.library.caltech.edu/records/ax35c-rcy84/files/PhysRevB.95.085429.pdf" } ], "pub_year": "2017", "author_list": "Mirek, R; Kr\u00f3l, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/n3b1a-23g34", "eprint_id": 75794, "eprint_status": "archive", "datestamp": "2023-08-19 01:32:46", "lastmod": "2023-10-25 15:18:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bobrovska-N", "name": { "family": "Bobrovska", "given": "N." } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "M." } }, { "id": "Liew-T-C-H", "name": { "family": "Liew", "given": "T. C. H." } }, { "id": "Kyriienko-O", "name": { "family": "Kyriienko", "given": "O." } } ] }, "title": "Interactive optomechanical coupling with nonlinear polaritonic systems", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Physical Society. \n\nReceived 3 November 2016; revised manuscript received 17 January 2017; published 21 February 2017. \n\nO.K. thanks I. A. Shelykh and A. S. S\u00f8rensen for useful discussions, and acknowledges support from the European Union Seventh Framework Programme through the ERC Grant QIOS (Grant No. 306576). N.B. and M.M. acknowledge support from the National Science Center, Poland Grants No. DEC-2011/01/D/ST3/00482 and No. 2015/17/B/ST3/02273. T.C.H.L. was supported by the MOE AcRF Tier 1 Grant No. 2016-T1-1-084 and MOE AcRF Tier 2 Grant No. 2015-T2-1-055.\n\nPublished - PhysRevB.95.085309.pdf
Submitted - 1611.03238.pdf
", "abstract": "We study a system of interacting matter quasiparticles strongly coupled to photons inside an optomechanical cavity. The resulting normal modes of the system are represented by hybrid polaritonic quasiparticles, which acquire effective nonlinearity. Its strength is influenced by the presence of a mechanical mode and depends on the resonance frequency of the cavity. This leads to an interactive type of optomechanical coupling, which is distinct from previously studied dispersive and dissipative couplings in optomechanical systems. The emergent interactive coupling is shown to generate effective optical nonlinearity terms of high order, which are quartic in the polariton number. We consider particular systems of exciton polaritons and dipolaritons, and show that the induced effective optical nonlinearity due to interactive coupling can exceed in magnitude the strength of Kerr nonlinear terms, such as those arising from polariton-polariton interactions. As applications, we show that the higher-order terms give rise to localized bright flattop solitons, which may form spontaneously in polariton condensates.", "date": "2017-02-15", "date_type": "published", "publication": "Physical Review B", "volume": "95", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 085309", "id_number": "CaltechAUTHORS:20170406-100412345", "issn": "2469-9950", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170406-100412345", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "306576" }, { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2011/01/D/ST3/00482" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/17/B/ST3/02273" }, { "agency": "Ministry of Science and Higher Education (Poland)", "grant_number": "2016-T1-1-084" }, { "agency": "Ministry of Science and Higher Education (Poland)", "grant_number": "2015-T2-1-055" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1103/PhysRevB.95.085309", "primary_object": { "basename": "1611.03238.pdf", "url": "https://authors.library.caltech.edu/records/n3b1a-23g34/files/1611.03238.pdf" }, "related_objects": [ { "basename": "PhysRevB.95.085309.pdf", "url": "https://authors.library.caltech.edu/records/n3b1a-23g34/files/PhysRevB.95.085309.pdf" } ], "pub_year": "2017", "author_list": "Bobrovska, N.; Matuszewski, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/hf1xt-a6873", "eprint_id": 75796, "eprint_status": "archive", "datestamp": "2023-08-19 01:32:53", "lastmod": "2023-10-25 15:19:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kulczykowski-M", "name": { "family": "Kulczykowski", "given": "Micha\u0142" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Micha\u0142" } } ] }, "title": "Phase ordering kinetics of a nonequilibrium exciton-polariton condensate", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Physical Society. \n\nReceived 23 September 2015; revised manuscript received 22 April 2016; published 13 February 2017. \n\nWe thank Alejandro Zamora, Marzena Szyma\u0144ska, and Nikolaos Proukakis for stimulating and valuable discussions. We acknowledge support from National Science Center, Poland Grants No. DEC-2011/01/D/ST3/00482 and No. 2015/17/B/ST3/02273.\n\nPublished - PhysRevB.95.075306.pdf
Submitted - 1702.00654.pdf
", "abstract": "We investigate the process of coarsening via annihilation of vortex-antivortex pairs, following the quench to the condensate phase in a nonresonantly pumped polariton system. We find that the late-time dynamics is an example of universal phase-ordering kinetics, characterized by scaling of correlation functions in time. Depending on the parameters of the system, the evolution of the characteristic length scale L(t) can be the same as for the two-dimensional XY model, described by a power law with the dynamical exponent z\u22482 and a logarithmic correction, or z\u22481 which agrees with previous studies of conservative superfluids.", "date": "2017-02-15", "date_type": "published", "publication": "Physical Review B", "volume": "95", "number": "7", "publisher": "American Physical Society", "pagerange": "Art. No. 075306", "id_number": "CaltechAUTHORS:20170406-101811209", "issn": "2469-9950", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170406-101811209", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2011/01/D/ST3/00482" }, { "agency": "National Science Centre (Poland)", "grant_number": "2015/17/B/ST3/02273" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1103/PhysRevB.95.075306", "primary_object": { "basename": "PhysRevB.95.075306.pdf", "url": "https://authors.library.caltech.edu/records/hf1xt-a6873/files/PhysRevB.95.075306.pdf" }, "related_objects": [ { "basename": "1702.00654.pdf", "url": "https://authors.library.caltech.edu/records/hf1xt-a6873/files/1702.00654.pdf" } ], "pub_year": "2017", "author_list": "Kulczykowski, Micha\u0142 and Matuszewski, Micha\u0142" }, { "id": "https://authors.library.caltech.edu/records/9k8b6-np546", "eprint_id": 73787, "eprint_status": "archive", "datestamp": "2023-08-19 01:21:15", "lastmod": "2023-10-24 16:27:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Hung-T-K", "name": { "family": "Hung", "given": "T." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K." }, "orcid": "0000-0002-2557-5180" }, { "id": "Kong-Albert-K-H", "name": { "family": "Kong", "given": "A. K. H." }, "orcid": "0000-0002-5105-344X" }, { "id": "Cantwell-T-M", "name": { "family": "Cantwell", "given": "T. M." } }, { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "P. C." }, "orcid": "0000-0001-8894-0854" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "C.-C." }, "orcid": "0000-0001-8771-7554" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "iPTF Discovery of the Rapid \"Turn-on\" of a Luminous Quasar", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: active \u2013 surveys", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 4; revised 2016 December 13; accepted 2016 December 13; published 2017 January 24. \n\nWe thank the anonymous referee for their helpful comments that improved the manuscript. S.G. is supported in part by NSF CAREER grant 1454816 and NASA Swift Cycle 12 grant NNX16AN85G. S.G. thanks Mike Koss for help with the X-ray data archives. These results made use of the Discovery Channel Telescope 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 W. M. Keck Observatory 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 research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. K.M.'s research is supported by the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. The AMI telescope gratefully acknowledges support from the European Research Council under grant ERC-2012- StG-307215 LODESTONE, the UK Science and Technology Facilities Council (STFC), and the University of Cambridge. We thank the AMI staff for scheduling the observations.\n\nPublished - Gezari_2017_ApJ_835_144.pdf
Submitted - 1612.04830v1.pdf
", "abstract": "We present a radio-quiet quasar at z = 0.237 discovered \"turning on\" by the intermediate Palomar Transient Factory (iPTF). The transient, iPTF 16bco, was detected by iPTF in the nucleus of a galaxy with an archival Sloan Digital Sky Survey spectrum with weak narrow-line emission characteristic of a low-ionization nuclear emission-line region (LINER). Our follow-up spectra show the dramatic appearance of broad Balmer lines and a power-law continuum characteristic of a luminous (L_(bol) \u2248 10^(45) erg s^(\u22121)) type 1 quasar 12 yr later. Our photometric monitoring with PTF from 2009\u20132012 and serendipitous X-ray observations from the XMM-Newton Slew Survey in 2011 and 2015 constrain the change of state to have occurred less than 500 days before the iPTF detection. An enhanced broad H\u03b1/[O III] \u03bb5007 line ratio in the type 1 state relative to other changing-look quasars also is suggestive of the most rapid change of state yet observed in a quasar. We argue that the >10 increase in Eddington ratio inferred from the brightening in UV and X-ray continuum flux is more likely due to an intrinsic change in the accretion rate of a preexisting accretion disk than an external mechanism such as variable obscuration, microlensing, or the tidal disruption of a star. However, further monitoring will be helpful in better constraining the mechanism driving this change of state. The rapid \"turn-on\" of the quasar is much shorter than the viscous infall timescale of an accretion disk and requires a disk instability that can develop around a ~ 10^8 M_\u2299 black hole on timescales less than 1 yr.", "date": "2017-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 144", "id_number": "CaltechAUTHORS:20170127-143119431", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-143119431", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "NASA", "grant_number": "NNX16AN85G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Oxford Centre for Astrophysical Surveys" }, { "agency": "Hintze Family Charitable Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "307215" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "University of Cambridge" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/835/2/144", "primary_object": { "basename": "1612.04830v1.pdf", "url": "https://authors.library.caltech.edu/records/9k8b6-np546/files/1612.04830v1.pdf" }, "related_objects": [ { "basename": "Gezari_2017_ApJ_835_144.pdf", "url": "https://authors.library.caltech.edu/records/9k8b6-np546/files/Gezari_2017_ApJ_835_144.pdf" } ], "pub_year": "2017", "author_list": "Gezari, S.; Hung, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/nhvkq-85x53", "eprint_id": 72968, "eprint_status": "archive", "datestamp": "2023-08-22 19:19:18", "lastmod": "2023-10-23 23:27:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hung-T-K", "name": { "family": "Hung", "given": "T." } }, { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Jones-D-O", "name": { "family": "Jones", "given": "D. O." }, "orcid": "0000-0002-6230-0151" }, { "id": "Kirshner-R-P", "name": { "family": "Kirshner", "given": "R. P." }, "orcid": "0000-0002-1966-3942" }, { "id": "Chornock-R", "name": { "family": "Chornock", "given": "R." }, "orcid": "0000-0002-7706-5668" }, { "id": "Berger-Edo", "name": { "family": "Berger", "given": "E." }, "orcid": "0000-0002-9392-9681" }, { "id": "Rest-A", "name": { "family": "Rest", "given": "A." } }, { "id": "Huber-M-E", "name": { "family": "Huber", "given": "M." } }, { "id": "Narayan-G", "name": { "family": "Narayan", "given": "G." }, "orcid": "0000-0001-6022-0484" }, { "id": "Scolnic-D", "name": { "family": "Scolnic", "given": "D." }, "orcid": "0000-0002-4934-5849" }, { "id": "Waters-C", "name": { "family": "Waters", "given": "C." }, "orcid": "0000-0003-1989-4879" }, { "id": "Wainscoat-R-J", "name": { "family": "Wainscoat", "given": "R." }, "orcid": "0000-0002-1341-0952" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "The GALEX Time Domain Survey. II. Wavelength-Dependent Variability of Active Galactic Nuclei in the Pan-STARRS1 Medium Deep Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: nuclei; surveys; ultraviolet: general", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 June 27. Accepted 2016 September 20. Published 2016 December 19. \n\nWe thank the anonymous referee for valuable comments and suggestions that helped to improve this paper. S.G. was supported in part by NSF CAREER grant 1454816. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We thank R. Foley for his contribution to the PS1 transients program. The Pan-STARRS1 Surveys (PS1) 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 institutes, 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, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, and the University of Maryland.\n\nPublished - Hung_2016_ApJ_833_226.pdf
Submitted - 1609.06307v1.pdf
", "abstract": "We analyze the wavelength-dependent variability of a sample of spectroscopically confirmed active galactic nuclei selected from near-UV (NUV) variable sources in the GALEX Time Domain Survey that have a large amplitude of optical variability (difference-flux S/N > 3) in the Pan-STARRS1 Medium Deep Survey (PS1 MDS). By matching GALEX and PS1 epochs in five bands (NUV, g_(P1), r_(P1), i_(P1), z_(P1)) in time, and taking their flux difference, we create co-temporal difference-flux spectral energy distributions (\u0394\u0192SEDs) using two chosen epochs for each of the 23 objects in our sample, on timescales of about a year. We confirm the \"bluer-when-brighter\" trend reported in previous studies, and measure a median spectral index of the \u0394\u0192SEDs of \u0251_\u22cb = 2.1 that is consistent with an accretion disk spectrum. We further fit the \u0394\u0192SEDs of each source with a standard accretion disk model in which the accretion rate changes from one epoch to the other. In our sample, 17 out of 23 (~74%) sources are described well by this variable accretion-rate disk model, with a median average characteristic disk temperature T^* of 1.2 x 10^5 K that is consistent with the temperatures expected, given the distribution of accretion rates and black hole masses inferred for the sample. Our analysis also shows that the variable accretion rate model is a better fit to the \u0394\u0192SEDs than a simple power law.", "date": "2016-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "833", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 226", "id_number": "CaltechAUTHORS:20161220-093154418", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161220-093154418", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "Institute for Astronomy" }, { "agency": "University of Hawaii" }, { "agency": "Pan-STARRS Project Office" }, { "agency": "Max-Planck Society" }, { "agency": "Max Planck Institute for Astronomy (MPIA)" }, { "agency": "Max Planck Institute for Extraterrestrial Physics" }, { "agency": "Johns Hopkins University" }, { "agency": "Durham University" }, { "agency": "University of Edinburgh" }, { "agency": "Queen's University Belfast" }, { "agency": "Harvard-Smithsonian Center for Astrophysics" }, { "agency": "Las Cumbres Observatory Global Telescope Network Incorporated" }, { "agency": "National Central University of Taiwan" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/1538-4357/833/2/226", "primary_object": { "basename": "1609.06307v1.pdf", "url": "https://authors.library.caltech.edu/records/nhvkq-85x53/files/1609.06307v1.pdf" }, "related_objects": [ { "basename": "Hung_2016_ApJ_833_226.pdf", "url": "https://authors.library.caltech.edu/records/nhvkq-85x53/files/Hung_2016_ApJ_833_226.pdf" } ], "pub_year": "2016", "author_list": "Hung, T.; Gezari, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/6zvqd-3a208", "eprint_id": 71808, "eprint_status": "archive", "datestamp": "2023-08-20 14:20:16", "lastmod": "2023-10-23 17:13:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael M." } }, { "id": "Doyle-T-F", "name": { "family": "Doyle", "given": "Trisha F." }, "orcid": "0000-0001-7182-5307" }, { "id": "Lauer-T-R", "name": { "family": "Lauer", "given": "Tod R." } }, { "id": "Zurek-David", "name": { "family": "Zurek", "given": "David" } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Madrid-J-P", "name": { "family": "Madrid", "given": "Juan P." } }, { "id": "Miko\u0142ajewska-J", "name": { "family": "Miko\u0142ajewska", "given": "Joanna" } }, { "id": "Welch-D-L", "name": { "family": "Welch", "given": "D. L." } }, { "id": "Baltz-E-A", "name": { "family": "Baltz", "given": "Edward A." } } ] }, "title": "A Hubble Space Telescope Survey for Novae in M87. I. Light and Color Curves, Spatial Distributions, and the Nova Rate", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 1; revised 2016 September 1; accepted 2016 September 10; published 2016 November 8. \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. \n\nWe gratefully acknowledge the support of the STScI team responsible for ensuring timely and accurate implementation of our M87 program. Support for program #10543 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This research has been partly supported by the Polish NCN grant DEC-2013/10/M/ST9/00086. M.M.S. gratefully acknowledges the support of Hilary and Ethel Lipsitz, longtime friends of the AMNH Astrophysics department. We thank a referee for a careful reading and useful suggestions that improved earlier versions of the paper.\n\nPublished - Shara_2016_ApJS_227_1.pdf
Submitted - 1602.00758v3.pdf
", "abstract": "The Hubble Space Telescope has imaged the central part of M87 over a 10 week span, leading to the discovery of 32 classical novae (CNe) and nine fainter, likely very slow, and/or symbiotic novae. In this first paper of a series, we present the M87 nova finder charts, and the light and color curves of the novae. We demonstrate that the rise and decline times, and the colors of M87 novae are uncorrelated with each other and with position in the galaxy. The spatial distribution of the M87 novae follows the light of the galaxy, suggesting that novae accreted by M87 during cannibalistic episodes are well-mixed. Conservatively using only the 32 brightest CNe we derive a nova rate for M87: 363^(+33)_(-45)novae yr^(\u22121). We also derive the luminosity-specific classical nova rate for this galaxy, which is 7.88^(+2.3)_(-2.6) yr^(-1)/10^(10) L\u2299K. Both rates are 3\u20134 times higher than those reported for M87 in the past, and similarly higher than those reported for all other galaxies. We suggest that most previous ground-based surveys for novae in external galaxies, including M87, miss most faint, fast novae, and almost all slow novae near the centers of galaxies.", "date": "2016-11", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "227", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 1", "id_number": "CaltechAUTHORS:20161108-110328433", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161108-110328433", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "National Science Center (Poland)", "grant_number": "DEC-2013/10/M/ST9/00086" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/0067-0049/227/1/1", "primary_object": { "basename": "Shara_2016_ApJS_227_1.pdf", "url": "https://authors.library.caltech.edu/records/6zvqd-3a208/files/Shara_2016_ApJS_227_1.pdf" }, "related_objects": [ { "basename": "1602.00758v3.pdf", "url": "https://authors.library.caltech.edu/records/6zvqd-3a208/files/1602.00758v3.pdf" } ], "pub_year": "2016", "author_list": "Shara, Michael M.; Doyle, Trisha F.; et el." }, { "id": "https://authors.library.caltech.edu/records/bz2w2-dyq04", "eprint_id": 75798, "eprint_status": "archive", "datestamp": "2023-08-20 14:06:04", "lastmod": "2023-10-25 15:19:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "\u015awis\u0142ocki-T", "name": { "family": "\u015awis\u0142ocki", "given": "Tomasz" } }, { "id": "Witkowska-E", "name": { "family": "Witkowska", "given": "Emilia" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Micha\u0142" } } ] }, "title": "Nonadiabatic quantum phase transition in a trapped spinor condensate", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\nReceived 12 September 2016; published 19 October 2016. \n\nThe authors would like to acknowledge J. Dziarmaga for his initial contribution to the project. E.W. acknowledges a discussion with B. Damski, and O. Hul for a careful reading of the manuscript. This work was supported by the National Science Center Grants No. DEC-2015/18/E/ST2/00760, No. DEC-2012/07/E/ST2/01389, No. DEC-2011/01/D/ST3/00482, and No. DEC-2015/17/D/ST2/03527.\n\nPublished - PhysRevA.94.043635.pdf
Submitted - 1609.03736.pdf
", "abstract": "We study the effect of an external harmonic trapping potential on an outcome of the nonadiabatic quantum phase transition from an antiferromagnetic to a phase-separated state in a spin-1 atomic condensate. Previously, we demonstrated that the dynamics of an untrapped system exhibits double universality with two different scaling laws appearing due to the conservation of magnetization. We show that in the presence of a trap, double universality persists. However, the corresponding scaling exponents are strongly modified by the transfer of local magnetization across the system. The values of these exponents cannot be explained by the effect of causality alone, as in the spinless case. We derive the appropriate scaling laws based on a slow diffusive-drift relaxation process in the local density approximation.", "date": "2016-10", "date_type": "published", "publication": "Physical Review A", "volume": "94", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 043635", "id_number": "CaltechAUTHORS:20170406-102510411", "issn": "2469-9926", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170406-102510411", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2015/18/E/ST2/00760" }, { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2012/07/E/ST2/01389" }, { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2011/01/D/ST3/00482" }, { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2015/17/D/ST2/03527" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1103/PhysRevA.94.043635", "primary_object": { "basename": "1609.03736.pdf", "url": "https://authors.library.caltech.edu/records/bz2w2-dyq04/files/1609.03736.pdf" }, "related_objects": [ { "basename": "PhysRevA.94.043635.pdf", "url": "https://authors.library.caltech.edu/records/bz2w2-dyq04/files/PhysRevA.94.043635.pdf" } ], "pub_year": "2016", "author_list": "\u015awis\u0142ocki, Tomasz; Witkowska, Emilia; et el." }, { "id": "https://authors.library.caltech.edu/records/pb8yh-5pw65", "eprint_id": 72048, "eprint_status": "archive", "datestamp": "2023-08-20 13:18:46", "lastmod": "2024-01-13 20:20:22", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kyne-G", "name": { "family": "Kyne", "given": "Gillian" } }, { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Lingner-N", "name": { "family": "Lingner", "given": "Nicole" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "The faint intergalactic-medium red-shifted emission balloon: future UV observations with EMCCDs", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomical instrumentation, EMCCD, UV, dark current, CIC, photon counting", "note": "\u00a9 2016 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was partially supported by KISS, the W. M. Keck Institute for Space Studies, and by NASA Headquarters under NASA Grant NNX12AF29G.\n\nPublished - 991507.pdf
", "abstract": "We present the latest developments in our joint NASA/CNES suborbital project. This project is a balloon-borne UV multi-object spectrograph, which has been designed to detect faint emission from the circumgalactic medium (CGM) around low redshift galaxies. One major change from FIREBall-1 has been the use of a delta-doped Electron Multiplying CCD (EMCCD). EMCCDs can be used in photon-counting (PC) mode to achieve extremely low readout noise (\u00a1 1e-). Our testing initially focused on reducing clock-induced-charge (CIC) through wave shaping and well depth optimisation with the CCD Controller for Counting Photons (CCCP) from N\u00fcv\u00fc. This optimisation also includes methods for reducing dark current, via cooling and substrate voltage adjustment. We present result of laboratory noise measurements including dark current. Furthermore, we will briefly present some initial results from our first set of on-sky observations using a delta-doped EMCCD on the 200 inch telescope at Palomar using the Palomar Cosmic Web Imager (PCWI).", "date": "2016-08-05", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 991507", "id_number": "CaltechAUTHORS:20161116-094042789", "isbn": "978-1-5106-0209-0", "book_title": "High Energy, Optical, and Infrared Detectors for Astronomy VII", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161116-094042789", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NASA", "grant_number": "NNX12AF29G" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Holland-A-D", "name": { "family": "Holland", "given": "Andrew D." } }, { "id": "Beletic-J", "name": { "family": "Beletic", "given": "James" } } ] }, "doi": "10.1117/12.2232879", "primary_object": { "basename": "991507.pdf", "url": "https://authors.library.caltech.edu/records/pb8yh-5pw65/files/991507.pdf" }, "pub_year": "2016", "author_list": "Kyne, Gillian; Hamden, Erika T.; et el." }, { "id": "https://authors.library.caltech.edu/records/9gyr2-rqf92", "eprint_id": 70754, "eprint_status": "archive", "datestamp": "2023-08-20 13:16:00", "lastmod": "2023-10-20 23:28:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hagen-L-M-Z", "name": { "family": "Hagen", "given": "Lea M. Z." }, "orcid": "0000-0001-8918-1597" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Hagen-A", "name": { "family": "Hagen", "given": "Alex" } }, { "id": "Nyland-K", "name": { "family": "Nyland", "given": "Kristina" }, "orcid": "0000-0003-1991-370X" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Young-L-M", "name": { "family": "Young", "given": "Lisa M." } }, { "id": "Rich-J-A", "name": { "family": "Rich", "given": "Jeffrey A." }, "orcid": "0000-0002-5807-5078" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" } ] }, "title": "On the Classification of UGC 1382 as a Giant Low Surface Brightness Galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (UGC 1382)", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 October 15; revised 2016 May 11; accepted 2016 May 23; published 2016 August 1. \n\nWe thank the referee for helpful comments that improved this paper. M.H.S. acknowledges support from NASA grant NNX12AE19G. L.M.Y. acknowledges support from NSF AST-1109803 and thanks ASIAA for their hospitality during a sabbatical visit. 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. This research has made use of NASA's Astrophysics Data System. 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. We thank the Research Computer and Cyberinfrastructure Unit of Information Technology Services at The Pennsylvania State University for providing computational support and resources. In particular, we appreciate the very helpful William Brouwer. The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University. Observations are based in part on data obtained at the duPont 2.5 m telescope at the Las Campanas Observatories of the Carnegie Institution for Science.\n\nPublished - apj_826_2_210.pdf
Submitted - 1607.02147v1.pdf
", "abstract": "We provide evidence that UGC 1382, long believed to be a passive elliptical galaxy, is actually a giant low surface brightness (GLSB) galaxy that rivals the archetypical GLSB Malin 1 in size. Like other GLSB galaxies, it has two components: a high surface brightness disk galaxy surrounded by an extended low surface brightness (LSB) disk. For UGC 1382, the central component is a lenticular system with an effective radius of 6 kpc. Beyond this, the LSB disk has an effective radius of ~38 kpc and an extrapolated central surface brightness of ~26 mag arcsec^(\u22122). Both components have a combined stellar mass of ~8 \u00d7 10^(10) M_\u2299, and are embedded in a massive (10^(10) M_\u2299) low-density (<3 M_\u2299 pc^(\u22122)) HI disk with a radius of 110 kpc, making this one of the largest isolated disk galaxies known. The system resides in a massive dark matter halo of at least 2 \u00d7 10^(12) M_\u2299. Although possibly part of a small group, its low-density environment likely plays a role in the formation and retention of the giant LSB and HI disks. We model the spectral energy distributions and find that the LSB disk is likely older than the lenticular component. UGC 1382 has UV\u2013optical colors typical of galaxies transitioning through the green valley. Within the LSB disk are spiral arms forming stars at extremely low efficiencies. The gas depletion timescale of ~10^(11) years suggests that UGC 1382 may be a very-long-term resident of the green valley. We find that the formation and evolution of the LSB disk in UGC 1382 is best explained by the accretion of gas-rich LSB dwarf galaxies.", "date": "2016-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "826", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 210", "id_number": "CaltechAUTHORS:20161003-095121320", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161003-095121320", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AE19G" }, { "agency": "NSF", "grant_number": "AST-1109803" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/0004-637X/826/2/210", "primary_object": { "basename": "1607.02147v1.pdf", "url": "https://authors.library.caltech.edu/records/9gyr2-rqf92/files/1607.02147v1.pdf" }, "related_objects": [ { "basename": "apj_826_2_210.pdf", "url": "https://authors.library.caltech.edu/records/9gyr2-rqf92/files/apj_826_2_210.pdf" } ], "pub_year": "2016", "author_list": "Hagen, Lea M. Z.; Seibert, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/s9beg-7ee33", "eprint_id": 73545, "eprint_status": "archive", "datestamp": "2023-08-20 12:53:06", "lastmod": "2024-01-13 20:23:34", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grange-R", "name": { "family": "Grange", "given": "R." } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Lemaitre-G", "name": { "family": "Lemaitre", "given": "G." } }, { "id": "Quiret-S", "name": { "family": "Quiret", "given": "S." } }, { "id": "Hamden-E", "name": { "family": "Hamden", "given": "E." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } } ] }, "title": "Fireball Multi Object Spectrograph: As-built optic performances", "ispublished": "unpub", "full_text_status": "public", "keywords": "Spectrograph, Ultraviolet, Multi-object spectroscopy", "note": "\u00a9 2016 Society of Photo-Optical Instrumentation Engineers (SPIE).\n\nPublished - 990531.pdf
", "abstract": "Fireball (Faint Intergalactic Redshifted Emission Balloon) is a NASA/CNES balloon-borne experiment to study the faint diffuse circumgalactic medium from the line emissions in the ultraviolet (200 nm) above 37 km flight altitude. Fireball relies on a Multi Object Spectrograph (MOS) that takes full advantage of the new high QE, low noise 13 \u03bcm pixels UV EMCCD. The MOS is fed by a 1 meter diameter parabola with an extended field (1000 arcmin2) using a highly aspherized two mirror corrector. All the optical train is working at F/2.5 to maintain a high signal to noise ratio. The spectrograph (R~ 2200 and 1.5 arcsec FWHM) is based on two identical Schmidt systems acting as collimator and camera sharing a 2400 g/mm aspherized reflective Schmidt grating. This grating is manufactured from active optics methods by double replication technique of a metal deformable matrix whose active clear aperture is built-in to a rigid elliptical contour. The payload and gondola are presently under integration at LAM. We will present the alignment procedure and the as-built optic performances of the Fireball instrument.", "date": "2016-07-18", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 990531", "id_number": "CaltechAUTHORS:20170119-101500681", "isbn": "978-1-5106-0189-5", "book_title": "Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170119-101500681", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "den-Herder-J-W-A", "name": { "family": "den Herder", "given": "Jan-Willem A." } }, { "id": "Takahashi-Tadayuki", "name": { "family": "Takahashi", "given": "Tadayuki" } }, { "id": "Bautz-M", "name": { "family": "Bautz", "given": "Marshall" } } ] }, "doi": "10.1117/12.2233267", "primary_object": { "basename": "990531.pdf", "url": "https://authors.library.caltech.edu/records/s9beg-7ee33/files/990531.pdf" }, "pub_year": "2016", "author_list": "Grange, R.; Milliard, B.; et el." }, { "id": "https://authors.library.caltech.edu/records/bkyt5-y3d68", "eprint_id": 70959, "eprint_status": "archive", "datestamp": "2023-08-22 18:13:47", "lastmod": "2023-10-23 15:13:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Jewell-A-D", "name": { "family": "Jewell", "given": "April D." }, "orcid": "0000-0001-8834-3769" }, { "id": "Shapiro-C-A", "name": { "family": "Shapiro", "given": "Charles A." } }, { "id": "Cheng-Samuel-R", "name": { "family": "Cheng", "given": "Samuel R." } }, { "id": "Goodsall-Tim-M", "name": { "family": "Goodsall", "given": "Tim M." } }, { "id": "Hennessy-J-L", "name": { "family": "Hennessy", "given": "John" } }, { "id": "Hoenk-M-E", "name": { "family": "Hoenk", "given": "Michael" } }, { "id": "Jones-T-J", "name": { "family": "Jones", "given": "Todd" } }, { "id": "Gordon -S", "name": { "family": "Gordon", "given": "Sam" } }, { "id": "Ong-Hwei-Ru", "name": { "family": "Ong", "given": "Hwei Ru" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } } ] }, "title": "Charge-coupled devices detectors with high quantum efficiency at UV wavelengths", "ispublished": "pub", "full_text_status": "public", "keywords": "UV; antireflection coatings; thin-films; charge-coupled devices", "note": "\u00a9 2016 The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. \n\nReceived January 19, 2016; Accepted August 22, 2016. \n\nThe authors wish to thank the reviewers for their detailed, helpful comments and suggestions. In addition, we wish to thank Frank Greer, Michael Lee, and Layton Baker, all of JPL, for their assistance with ALD processes, and Leslie Wulff for helpful discussions. The research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was partially supported by KISS, the W. M. Keck Institute for Space Studies, and by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, NASA Grant NNX11AO07H, and NASA Grant NNX12AF29G. E. T. H. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1402206.\n\nPublished - JATIS_2_3_036003.pdf
", "abstract": "We report on multilayer high efficiency antireflection coating (ARC) design and development for use at UV wavelengths on CCDs and other Si-based detectors. We have previously demonstrated a set of single-layer coatings, which achieve >50% quantum efficiency (QE) in four bands from 130 to 300 nm. We now present multilayer coating designs that significantly outperform our previous work between 195 and 215 nm. Using up to 11 layers, we present several model designs to reach QE above 80%. We also demonstrate the successful performance of 5 and 11 layer ARCs on silicon and fused silica substrates. Finally, we present a five-layer coating deposited onto a thinned, delta-doped CCD and demonstrate external QE greater than 60% between 202 and 208 nm, with a peak of 67.6% at 206 nm.", "date": "2016-07", "date_type": "published", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "volume": "2", "number": "3", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "pagerange": "Art. No. 036003", "id_number": "CaltechAUTHORS:20161007-152230649", "issn": "2329-4124", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161007-152230649", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NASA", "grant_number": "NNX11AO07H" }, { "agency": "NASA", "grant_number": "NNX12AF29G" }, { "agency": "NSF Astronomy and Astrophysics Postdoctoral Fellowship", "grant_number": "AST-1402206" }, { "agency": "NASA Earth and Space Science Fellowship" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1117/1.JATIS.2.3.036003", "primary_object": { "basename": "JATIS_2_3_036003.pdf", "url": "https://authors.library.caltech.edu/records/bkyt5-y3d68/files/JATIS_2_3_036003.pdf" }, "pub_year": "2016", "author_list": "Hamden, Erika T.; Jewell, April D.; et el." }, { "id": "https://authors.library.caltech.edu/records/raavv-3gb41", "eprint_id": 68880, "eprint_status": "archive", "datestamp": "2023-09-15 05:29:20", "lastmod": "2023-10-23 21:18:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan" }, "orcid": "0000-0002-6967-7322" } ] }, "title": "A Newly Forming Cold Flow Protogalactic Disk, a Signature of Cold Accretion from the Cosmic Web", "ispublished": "pub", "full_text_status": "public", "keywords": "dark matter; galaxies: evolution; galaxies: formation; galaxies: high-redshift; intergalactic medium; quasars: general", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 23; revised 2016 April 11; accepted 2016 April 13; published 2016 June 3. \n\nThis work was supported by the National Science Foundation and the California Institute of Technology. R.F.T. receives financial support from the UC Berkeley Miller Institute for Basic Research in Science.\n\nPublished - apjl_824_1_L5.pdf
", "abstract": "How galaxies form from, and are fueled by, gas from the intergalactic medium (IGM) remains one of the major unsolved problems in galaxy formation. While the classical Cold Dark Matter paradigm posits galaxies forming from cooling virialized gas, recent theory and numerical simulations have highlighted the importance of cold accretion flows\u2014relatively cool (T ~ few \u00d7 104 K) unshocked gas streaming along filaments into dark matter halos, including hot, massive, high-redshift halos. These flows are thought to deposit gas and angular momentum into the circumgalactic medium resulting in disk- or ring-like structures, eventually coalescing into galaxies forming at filamentary intersections. We earlier reported a bright, Ly\u03b1 emitting filament near the QSO HS1549+19 at redshift z = 2.843 discovered with the Palomar Cosmic Web Imager. We now report that the bright part of this filament is an enormous (R > 100 kpc) rotating structure of hydrogen gas with a disk-like velocity profile consistent with a 4 \u00d7 10^(12) M_\u2299 halo. The orbital time of the outer part of the what we term a \"protodisk\" is comparable to the virialization time and the age of the universe at this redshift. We propose that this protodisk can only have recently formed from cold gas flowing directly from the cosmic web.", "date": "2016-06-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "824", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L5", "id_number": "CaltechAUTHORS:20160707-085528559", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160707-085528559", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" }, { "agency": "Miller Institute for Basic Research in Science" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.3847/2041-8205/824/1/L5", "primary_object": { "basename": "apjl_824_1_L5.pdf", "url": "https://authors.library.caltech.edu/records/raavv-3gb41/files/apjl_824_1_L5.pdf" }, "pub_year": "2016", "author_list": "Martin, D. Christopher; Matuszewski, Mateusz; et el." }, { "id": "https://authors.library.caltech.edu/records/jfm20-yf848", "eprint_id": 62660, "eprint_status": "archive", "datestamp": "2023-08-20 10:57:11", "lastmod": "2023-10-25 17:18:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ganot-N", "name": { "family": "Ganot", "given": "Noam" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sagiv-I", "name": { "family": "Sagiv", "given": "Ilan" } }, { "id": "Waxman-E", "name": { "family": "Waxman", "given": "Eli" }, "orcid": "0000-0002-9038-5877" }, { "id": "Lapid-O", "name": { "family": "Lapid", "given": "Ofer" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Chelouche-D", "name": { "family": "Chelouche", "given": "Doron" } }, { "id": "Rafter-S", "name": { "family": "Rafter", "given": "Stephen" } }, { "id": "Behar-E", "name": { "family": "Behar", "given": "Ehud" } }, { "id": "Laor-A", "name": { "family": "Laor", "given": "Ari" } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Nakar-U", "name": { "family": "Nakar", "given": "Udi" } }, { "id": "Maoz-D", "name": { "family": "Maoz", "given": "Dan" } }, { "id": "Trakhtenbrot-B", "name": { "family": "Trakhtenbrot", "given": "Benny" }, "orcid": "0000-0002-3683-7297" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Thomas A." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Gezari-S", "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" } ] }, "title": "The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 December 19. Accepted 2016 February 4. Published 2016 March 17. \n\nThis research was supported by grants from the Israeli Space Agency (ISA) and the Ministry of Science, Technology and Space (MOS). Additional funding was provided by the EU via ERC grant 307260, the ISF, and a Kimmel award.\n\nPublished - apj_820_1_57.pdf
Submitted - 1412.4063v2.pdf
", "abstract": "The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early UV observations of core collapse supernovae (SNe). We present the first results from a simultaneous GALEX/PTF search for early UV emission from SNe. Six Type II SNe and one Type II superluminous SN (SLSN-II) are clearly detected in the GALEX NUV data. We compare our detection rate with theoretical estimates based on early, shock-cooling UV light curves calculated from models that fit existing Swift and GALEX observations well, combined with volumetric SN rates. We find that our observations are in good agreement with calculated rates assuming that red supergiants (RSGs) explode with fiducial radii of 500R_\u2299, explosion energies of 10^(51) erg, and ejecta masses of 10 M_\u2299. Exploding blue supergiants and Wolf-Rayet stars are poorly constrained. We describe how such observations can be used to derive the progenitor radius, surface composition and explosion energy per unit\nmass of such SN events, and we demonstrate why UV observations are critical for such measurements. We use the fiducial RSG parameters to estimate the detection rate of SNe during the shock-cooling phase (< 1 d after explosion)\nfor several ground-based surveys (PTF, ZTF, and LSST). We show that the proposed wide-field UV explorer ULTRASAT mission, is expected to find > 100 SNe per year (~ 0.5 SN per deg^2), independent of host galaxy extinction, down\nto an NUV detection limit of 21.5mag AB. Our pilot GALEX/PTF project thus convincingly demonstrates that a dedicated, systematic SN survey at the NUV band is a compelling method to study how massive stars end their life.", "date": "2016-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "820", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 57", "id_number": "CaltechAUTHORS:20151207-145315969", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151207-145315969", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israeli Space Agency" }, { "agency": "Ministry of Science, Technology and Space (Israel)" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israel Science Foundation" }, { "agency": "Kimmel Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "ULTRASAT Science Team", "WTTH Consortium", "GALEX Science Team", "Palomar Transient Factory Collaboration" ] }, "doi": "10.3847/0004-637X/820/1/57", "primary_object": { "basename": "1412.4063v2.pdf", "url": "https://authors.library.caltech.edu/records/jfm20-yf848/files/1412.4063v2.pdf" }, "related_objects": [ { "basename": "apj_820_1_57.pdf", "url": "https://authors.library.caltech.edu/records/jfm20-yf848/files/apj_820_1_57.pdf" } ], "pub_year": "2016", "author_list": "Ganot, Noam; Gal-Yam, Avishay; et el." }, { "id": "https://authors.library.caltech.edu/records/r6dtw-ya157", "eprint_id": 63133, "eprint_status": "archive", "datestamp": "2023-08-20 09:03:54", "lastmod": "2023-10-25 23:34:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Olmedo-M", "name": { "family": "Olmedo", "given": "Manuel" } }, { "id": "Lloyd-J-P", "name": { "family": "Lloyd", "given": "James" } }, { "id": "Mamajek-E-E", "name": { "family": "Mamajek", "given": "Eric E." }, "orcid": "0000-0003-2008-1488" }, { "id": "Ch\u00e1vez-M", "name": { "family": "Ch\u00e1vez", "given": "Miguel" } }, { "id": "Bertone-E", "name": { "family": "Bertone", "given": "Emanuele" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Deep GALEX UV Survey of the Kepler Field. I. Point Source Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2013 stars: activity \u2013 stars: chromospheres \u2013 techniques: photometric \u2013 ultraviolet: stars", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 May 18; accepted 2015 October 1; published 2015 November 3. \n\nThe Kepler field observation was funded by Cornell University. M.O. wishes to express his gratitude to the Astronomy Group of the University of Rochester for their hospitality and to CONACyT for the financial support received through the \"Beca Mixta\" program. M.C., E.B., and M.O. also thank CONACyT for financial support through grants SEP-2009-134985 and SEP-2011-169554. E.E.M. acknowledges support from NSF award AST-1313029. We thank Chase Million for useful discussions. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'\u00c9tudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - Olmedo_2015.pdf
Submitted - 1510.00748v1.pdf
", "abstract": "We report observations of a deep near-ultraviolet (NUV) survey of the Kepler field made in 2012 with the Galaxy Evolution Explorer (GALEX) Complete All-Sky UV Survey Extension (CAUSE). The GALEX-CAUSE Kepler survey (GCK) covers 104 square degrees of the Kepler field and reaches a limiting magnitude of NUV ~ 22.6 at 3\u03c3. Analysis of the GCK survey has yielded a catalog of 669,928 NUV sources, of which 475,164 are cross-matched with stars in the Kepler Input Catalog. Approximately 327 of 451 confirmed exoplanet host stars and 2614 of 4696 candidate exoplanet host stars identified by Kepler have NUV photometry in the GCK survey. The GCK catalog should enable the identification and characterization of UV-excess stars in the Kepler field (young solar-type and low-mass stars, chromospherically active binaries, white dwarfs, horizontal branch stars, etc.), and elucidation of various astrophysics problems related to the stars and planetary systems in the Kepler field.", "date": "2015-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "813", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 100", "id_number": "CaltechAUTHORS:20151222-100903580", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151222-100903580", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Cornell University" }, { "agency": "University of Rochester" }, { "agency": "Consejo Nacional de Ciencia y Tecnologia (CONACyT)", "grant_number": "SEP-2009-134985" }, { "agency": "Consejo Nacional de Ciencia y Tecnologia (CONACyT)", "grant_number": "SEP-2011-169554" }, { "agency": "NSF", "grant_number": "AST-1313029" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/813/2/100", "primary_object": { "basename": "1510.00748v1.pdf", "url": "https://authors.library.caltech.edu/records/r6dtw-ya157/files/1510.00748v1.pdf" }, "related_objects": [ { "basename": "Olmedo_2015.pdf", "url": "https://authors.library.caltech.edu/records/r6dtw-ya157/files/Olmedo_2015.pdf" } ], "pub_year": "2015", "author_list": "Olmedo, Manuel; Lloyd, James; et el." }, { "id": "https://authors.library.caltech.edu/records/v0pzc-k8n18", "eprint_id": 62556, "eprint_status": "archive", "datestamp": "2023-08-22 16:22:30", "lastmod": "2023-10-25 17:14:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Curtin-C", "name": { "family": "Curtin", "given": "C." } }, { "id": "Shafter-A-W", "name": { "family": "Shafter", "given": "A. W." } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "C. J." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Kundu-A", "name": { "family": "Kundu", "given": "A." } }, { "id": "Maccarone-T-J", "name": { "family": "Maccarone", "given": "T. J." }, "orcid": "0000-0003-0976-4755" } ] }, "title": "Exploring the Role of Globular Cluster Specific Frequency on the Nova Rates in Three Virgo Elliptical Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (M49, M84, M87); galaxies: star clusters: general; novae, cataclysmic variables", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 May 15; accepted 2015 August 13; published 2015 September 17. \n\nWe thank an anonymous referee for constructive comments on our original manuscript. This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. A.W.S. and C.C. acknowledge financial support through NSF grant AST1009566. C.J.P. acknowledges financial support from the Natural Sciences and Engineering Research Council of Canada.\n\nPublished - Curtin_2015p34.pdf
Submitted - 1508.03319v1.pdf
", "abstract": "It has been proposed that a galaxy's nova rate might be enhanced by the production of nova progenitor binaries in the dense cores of its globular clusters (GCs). To explore this idea, relative nova rates in three Virgo elliptical galaxies, M87, M49, and M84, which have significantly different GC specific frequencies (SN) of 14, 3.6, and 1.6, respectively, were measured over the course of 4 epochs spanning a period of 14 months. To simplify the analysis, observations of the nearly equidistant galaxies were made on the same nights, with the same integration times, and through the same filter (H\u03b1), so that the relative numbers of novae discovered would reflect the relative nova rates. At the conclusion of our survey we found a total of 27 novae associated with M87, 37 with M49, and 19 with M84. After correcting for survey completeness, we found annual nova rates of 154_(-19)^(+23), 189_(-22)^(+26), and 95_(-14)^(+15), for M87, M49, and M84, respectively, corresponding to K-band luminosity-specific nova rates of 3.8 \u00b1 1.0, 3.4 \u00b1 0.6, and 3.0 \u00b1 0.6 novae per year per 10^(10) L_K_\u2299. The overall results of our study suggest that a galaxy's nova rate simply scales with its luminosity, and is insensitive to its GC specific frequency. Two novae, one in M87 and one in M84, were found to be spatially coincident with known GCs. After correcting for the mass fraction in GCs, we estimate that novae are likely enhanced relative to the field by at least an order of magnitude in the GC systems of luminous Virgo ellipticals.", "date": "2015-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "811", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 34", "id_number": "CaltechAUTHORS:20151202-144445643", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151202-144445643", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1009566" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/811/1/34", "primary_object": { "basename": "1508.03319v1.pdf", "url": "https://authors.library.caltech.edu/records/v0pzc-k8n18/files/1508.03319v1.pdf" }, "related_objects": [ { "basename": "Curtin_2015p34.pdf", "url": "https://authors.library.caltech.edu/records/v0pzc-k8n18/files/Curtin_2015p34.pdf" } ], "pub_year": "2015", "author_list": "Curtin, C.; Shafter, A. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/cz9b3-ad007", "eprint_id": 63327, "eprint_status": "archive", "datestamp": "2023-08-20 08:14:32", "lastmod": "2024-01-13 16:30:42", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Lingner-N", "name": { "family": "Lingner", "given": "Nicole" } }, { "id": "Kyne-G", "name": { "family": "Kyne", "given": "Gillian" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "Noise and dark performance for FIREBall-2 EMCCD delta-doped CCD detector", "ispublished": "unpub", "full_text_status": "public", "keywords": "EMCCD, Photon-counting, Ultraviolet detectors, Dark current, NUVU, CGM, FIREBall", "note": "\u00a9 2015 SPIE. September 18, 2015. \n\nThe research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was partially supported by KISS, the W. M. Keck Institute for Space Studies, and by NASA Headquarters under NASA Grant NNX12AF29G. Dr. Hamden is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1402206.\n\nPublished - 96010O.pdf
", "abstract": "The Faint Intergalactic-medium Redshifted Emission Balloon (FIREBall-2) is an experiment designed to observe low density emission from HI, CIV, and OVI in the circum-galactic medium around low-redshift galaxies. To detect this diffuse emission, we use a high-efficiency photon-counting EMCCD as part of FIREBall-2's detector. The flight camera system includes a custom printed circuit board, a mechanical cryo-cooler, zeolite and charcoal getters, and a N\u00fcv\u00fc controller, for fast read-out speeds and waveform shaping. Here we report on overall detector system performance, including pressure and temperature stability. We describe dark current and CIC measurements at several temperatures and substrate voltages, with the flight set-up.", "date": "2015-09-18", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_pub": "Belingham, WA", "pagerange": "Art. No. 96010O", "id_number": "CaltechAUTHORS:20160104-112557628", "isbn": "978-1-62841-767-8", "book_title": "UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XIX", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160104-112557628", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Institute for Space Studies" }, { "agency": "NASA", "grant_number": "NNX12AF29G" }, { "agency": "NSF Astronomy and Astrophysics Postdoctoral Fellowship", "grant_number": "AST-1402206" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Siegmund-O-H-W", "name": { "family": "Siegmund", "given": "Oswald H. W." } } ] }, "doi": "10.1117/12.2190679", "primary_object": { "basename": "96010O.pdf", "url": "https://authors.library.caltech.edu/records/cz9b3-ad007/files/96010O.pdf" }, "pub_year": "2015", "author_list": "Hamden, Erika T.; Lingner, Nicole; et el." }, { "id": "https://authors.library.caltech.edu/records/1h009-e6q95", "eprint_id": 61563, "eprint_status": "archive", "datestamp": "2023-08-20 08:10:53", "lastmod": "2023-10-25 15:00:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wu-Po-Feng", "name": { "family": "Wu", "given": "Po-Feng" } }, { "id": "Kudritzki-R-P", "name": { "family": "Kudritzki", "given": "Rolf-Peter" } }, { "id": "Tully-R-B", "name": { "family": "Tully", "given": "R. Brent" }, "orcid": "0000-0002-9291-1981" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "The Influence of Galaxy Surface Brightness on the Mass\u2013Metallicity Relation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances \u2013 galaxies: formation \u2013 galaxies: spiral", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 June 15; accepted 2015 July 31; published 2015 September 9. \n\nR.P.K. acknowledges support by the National Science Foundation under grants AST-1108906 and AST-1008798. R.B.T. acknowledges support from the US National Science Foundation award AST09-08846 and NAA award NNX12AE70G. This publication makes use of data products from the Wide-field Infrared Survey Explorer (WISE), 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 the usage of the HyperLeda database (http://leda.univ-lyon1.fr). This work makes use of data products from the SDSS. 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/. P.F W. acknowledges the writing retreat of IfA students and postdocs, SWOOP, where part of the manuscript is written.\n\nPublished - Wu_2015.pdf
Submitted - 1508.00015v1.pdf
", "abstract": "We study the effect of surface brightness on the mass\u2013metallicity relation using nearby galaxies whose gas content and metallicity profiles are available. Previous studies using fiber spectra indicated that lower surface brightness galaxies have systematically lower metallicities for their stellar mass, but the results were uncertain because of aperture effects. With stellar masses and surface brightnesses measured at Wide-field Infrared Explorer W1 and W2 bands, we re-investigate the surface brightness dependence with spatially resolved metallicity profiles and find similar results. We further demonstrate that the systematical difference cannot be explained by the gas content of galaxies. For two galaxies with similar stellar and gas masses, the one with lower surface brightness tends to have a lower metallicity. Using chemical evolution models, we investigate the inflow and outflow properties of galaxies of different masses and surface brightnesses. We find that, on average, high mass galaxies have lower inflow and outflow rates relative to the star formation rate. On the other hand, galaxies with a lower surface brightness experience stronger inflow than galaxies with a higher surface brightness of a similar mass. The surface brightness effect is more significant for low-mass galaxies. We discuss implications on the different inflow properties between low and high surface brightness galaxies, including star formation efficiency, environment, and mass assembly history.", "date": "2015-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "810", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 151", "id_number": "CaltechAUTHORS:20151027-121308658", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151027-121308658", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1108906" }, { "agency": "NSF", "grant_number": "AST-1008798" }, { "agency": "NSF", "grant_number": "AST09-08846" }, { "agency": "NASA", "grant_number": "NNX12AE70G" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/810/2/151", "primary_object": { "basename": "1508.00015v1.pdf", "url": "https://authors.library.caltech.edu/records/1h009-e6q95/files/1508.00015v1.pdf" }, "related_objects": [ { "basename": "Wu_2015.pdf", "url": "https://authors.library.caltech.edu/records/1h009-e6q95/files/Wu_2015.pdf" } ], "pub_year": "2015", "author_list": "Wu, Po-Feng; Kudritzki, Rolf-Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/am531-fjv59", "eprint_id": 57707, "eprint_status": "archive", "datestamp": "2023-08-20 07:44:57", "lastmod": "2023-10-23 17:39:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Cantalupo-S", "name": { "family": "Cantalupo", "given": "Sebastiano" }, "orcid": "0000-0001-5804-1428" }, { "id": "Prochaska-J-X", "name": { "family": "Prochaska", "given": "J. Xavier" }, "orcid": "0000-0002-7738-6875" }, { "id": "Chang-Daphne", "name": { "family": "Chang", "given": "Daphne" } } ] }, "title": "A Giant Protogalactic Disk Linked to the Cosmic Web", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 Macmillan Publishers Limited. \n\nReceived 18 February; accepted 21 May 2015. Published online 5 August 2015. \n\nWe thank T. Tombrello and S. Kulkarni for their support of PCWI. This work was supported by the National Science Foundation and the California Institute of Technology. \n\nContributions: D.C.M. is the principal investigator of PCWI, led the observations and analysis of UM287, and was principal author on the paper. M.M., D.C., and P.M. designed, constructed, and operated PCWI. A.M. was the project and technical manager (2006\u20132010). J.D.N., M.M., and D.C.M. developed the PCWI/KCWI data pipeline and produced the final data cubes. M.M., P.M., S.C., and J.X.P. contributed Keck data and helped edit the paper. \n\nCompeting financial interests: The authors declare no competing financial interests.\n\nSupplemental Material - nature14616-sf1.jpg
Supplemental Material - nature14616-sf2.jpg
Supplemental Material - nature14616-sf3.jpg
Supplemental Material - nature14616-sf4.jpg
Supplemental Material - nature14616-sf5.jpg
Supplemental Material - nature14616-sf6.jpg
", "abstract": "The specifics of how galaxies form from, and are fuelled by, gas from the intergalactic medium remain uncertain. Hydrodynamic simulations suggest that 'cold accretion flows'\u2014relatively cool (temperatures of the order of 10^4 kelvin), unshocked gas streaming along filaments of the cosmic web into dark-matter halos\u2014are important. These flows are thought to deposit gas and angular momentum into the circumgalactic medium, creating disk- or ring-like structures that eventually coalesce into galaxies that form at filamentary intersections. Recently, a large and luminous filament, consistent with such a cold accretion flow, was discovered near the quasi-stellar object QSO UM287 at redshift 2.279 using narrow-band imaging. Unfortunately, imaging is not sufficient to constrain the physical characteristics of the filament, to determine its kinematics, to explain how it is linked to nearby sources, or to account for its unusual brightness, more than a factor of ten above what is expected for a filament. Here we report a two-dimensional spectroscopic investigation of the emitting structure. We find that the brightest emission region is an extended rotating hydrogen disk with a velocity profile that is characteristic of gas in a dark-matter halo with a mass of 10^(13) solar masses. This giant protogalactic disk appears to be connected to a quiescent filament that may extend beyond the virial radius of the halo. The geometry is strongly suggestive of a cold accretion flow.", "date": "2015-08-13", "date_type": "published", "publication": "Nature", "volume": "524", "number": "7564", "publisher": "Nature Publishing Group", "pagerange": "192-195", "id_number": "CaltechAUTHORS:20150520-105840835", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150520-105840835", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/nature14616", "primary_object": { "basename": "nature14616-sf6.jpg", "url": "https://authors.library.caltech.edu/records/am531-fjv59/files/nature14616-sf6.jpg" }, "related_objects": [ { "basename": "nature14616-sf1.jpg", "url": "https://authors.library.caltech.edu/records/am531-fjv59/files/nature14616-sf1.jpg" }, { "basename": "nature14616-sf2.jpg", "url": "https://authors.library.caltech.edu/records/am531-fjv59/files/nature14616-sf2.jpg" }, { "basename": "nature14616-sf3.jpg", "url": "https://authors.library.caltech.edu/records/am531-fjv59/files/nature14616-sf3.jpg" }, { "basename": "nature14616-sf4.jpg", "url": "https://authors.library.caltech.edu/records/am531-fjv59/files/nature14616-sf4.jpg" }, { "basename": "nature14616-sf5.jpg", "url": "https://authors.library.caltech.edu/records/am531-fjv59/files/nature14616-sf5.jpg" } ], "pub_year": "2015", "author_list": "Martin, D. Christopher; Matuszewski, Mateusz; et el." }, { "id": "https://authors.library.caltech.edu/records/c0gaq-27s96", "eprint_id": 58068, "eprint_status": "archive", "datestamp": "2023-08-22 15:31:32", "lastmod": "2023-10-23 18:03:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" } ] }, "title": "GALEX Detection of Shock Breakout in Type IIP Supernova PS1-13arp: Implications for the Progenitor Star Wind", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual (PS1-13arp); surveys; ultraviolet: general", "note": "\u00a9 2015 American Astronomical Society. Received 2015 January 26; accepted 2015 February 23; published 2015 April 27.\n\nS.G. thanks the Gemini Deputy Director for approving a change of program for the TOO program GN-2013A-Q-32 to observe PS1-13arp. The Pan-STARRS1 Surveys (PS1) 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 institutes, 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, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE).\n\nPublished - 0004-637X_804_1_28.pdf
Submitted - 1502.06964v1.pdf
", "abstract": "We present the GALEX detection of a UV burst at the time of explosion of an optically normal supernova (SN) IIP (PS1-13arp) from the Pan-STARRS1 survey at z = 0.1665. The temperature and luminosity of the UV burst match the theoretical predictions for shock breakout in a red supergiant (RSG), but with a duration a factor of ~50 longer than expected. We compare the NUV light curve of PS1-13arp to previous GALEX detections of SNe IIP and find clear distinctions that indicate that the UV emission is powered by shock breakout, and not by the subsequent cooling envelope emission previously detected in these systems. We interpret the ~1 day duration of the UV signal with a shock breakout in the wind of an RSG with a pre-explosion mass-loss rate of ~ 10^(-3) M_\u2609 yr^(\u22121). This mass-loss rate is enough to prolong the duration of the shock breakout signal, but not enough to produce an excess in the optical plateau light curve or narrow emission lines powered by circumstellar interaction. This detection of non-standard, potentially episodic high mass loss in an RSG SN progenitor has favorable consequences for the prospects of future wide-field UV surveys to detect shock breakout directly in these systems, and provide a sensitive probe of the pre-explosion conditions of SN progenitors.", "date": "2015-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "804", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 28", "id_number": "CaltechAUTHORS:20150608-080924860", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150608-080924860", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/804/1/28", "primary_object": { "basename": "0004-637X_804_1_28.pdf", "url": "https://authors.library.caltech.edu/records/c0gaq-27s96/files/0004-637X_804_1_28.pdf" }, "related_objects": [ { "basename": "1502.06964v1.pdf", "url": "https://authors.library.caltech.edu/records/c0gaq-27s96/files/1502.06964v1.pdf" } ], "pub_year": "2015", "author_list": "Gezari, S. and Martin, D. C." }, { "id": "https://authors.library.caltech.edu/records/baqgn-7bw24", "eprint_id": 44099, "eprint_status": "archive", "datestamp": "2023-08-22 14:27:02", "lastmod": "2023-10-26 00:11:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Zheng-Zheng", "name": { "family": "Zheng", "given": "Z." } }, { "id": "Juric-M", "name": { "family": "Juric", "given": "M." }, "orcid": "0000-0003-1996-9252" } ] }, "title": "Giant Sparks at Cosmological Distances?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (SMC); ISM: general; pulsars: general; radio continuum: general", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 February 28; accepted 2014 September 23; published 2014 November 25. \n\nS.R.K. thanks the hospitality of the Institute for Advanced\nStudy (IAS). The sylvan surroundings and verdant intellectual ambiance of IAS resulted in a fecund mini-sabbatical stay (Fall 2007). We are grateful to M. Bailes, S. Burke-Spolaor, and D. Lorimer for sharing with us the details of the Parkes multibeam Survey. We thank M. Putman and S. Stanimirovic for help with the Hi data on the SMC and S. B. Cenko, D.B. Fox, and J. Kanner for discussions about X-ray transients. We gratefully acknowledge C. Hirata for careful reading, feedback, and\ninstructions of basic physics and P. Kumar and J.-P. Macquart for discussions about relativistic flows. We thank J. Cordes for sharing his ideas about detection strategies. We acknowledge useful discussions with D. Bhattacharya, G. Bower, Y.-H. Chu, J. Condon, D. A. Frail, P. M. Goldreich, A. Gruzinov, G. Hallinan, C. Heiles, E. S. Phinney, S. Thorsett, D. Q. Wang, and E. Witten. We especially thank Y. Cao, S. Tendulkar, and M. H. van Kerkwijk for a careful reading of the paper. We acknowledge robust discussions with authors of several recent papers attempting to explain the origin of FRBs: H. Falcke, J. I. Katz, A. Loeb, P. M\u00b4esz\u00b4aros, T. Totani, and B. Zhang. Finally, we thank the anonymous referee, whose thorough reading and thoughtful comments helped to improve the paper. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), Israeli\nMinistry of Science, Israel Science Foundation, Minerva\nand the I-CORE Program of the Planning and Budgeting Committee, and The Israel Science Foundation. This work is supported in part by grants from NSF and NASA. We gratefully acknowledge the use of the following archives:\nSouthern H\u03b1 Sky Survey, UK Schmidt Surveys, the Digital\nSky Survey, GALEX, and the ATNF Pulsar catalog. As usual,\nthe authors are indebted to the librarians who maintain ADS\nand Simbad. Z.Z. was partially supported by NSF grant AST-\n1208891 and NASA grant NNX14AC89G. M.J. acknowledges the support of the Washington Research Foundation through its\nData Science Chair and the University of Washington Provost's Initiative in Data-Intensive Discovery.\n\nPublished - 0004-637X_797_1_70.pdf
Submitted - 1402.4766v2.pdf
", "abstract": "Millisecond-duration bright radio pulses at 1.4 GHz with high dispersion measures (DMs) were reported by Lorimer et al., Keane et al., and Thornton et al. Their all-sky rate is \u224810^4 day^(\u20131) above ~1 Jy. Related events are \"Perytons\"\u2014similar pulsed, dispersed sources, but most certainly local. Suggested models of fast radio bursts (FRBs) can originate in Earth's atmosphere, in stellar coronae, in other galaxies, and even at cosmological distances. Using physically motivated assumptions combined with observed properties, we explore these models. In our analysis, we focus on the Lorimer event: a 30 Jy, 5 ms duration burst with DM = 375 cm^(\u20133) pc, exhibiting a steep frequency-dependent pulse width (the Sparker). To be complete, we drop the assumption that high DMs are produced by plasma propagation and assume that the source produces pulses with frequency-dependent arrival time (\"chirped signals\"). Within this framework, we explore a scenario in which Perytons, the Sparker, and the FRBs are all atmospheric phenomena occurring at different heights. This model is ad hoc in that we cannot explain why Perytons at higher altitudes show greater DMs or exhibit narrower pulses. Nonetheless, we argue that the Sparker may be a Peryton. We end with two remarks. First, the detection of a single FRB by an interferometer with a kilometer (or longer) baseline will prove that FRBs are of extraterrestrial origin. Second, we urge astronomers to pursue observations and understanding of Perytons since they form (at least) a formidable foreground for the FRBs.", "date": "2014-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "797", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 70", "id_number": "CaltechAUTHORS:20140303-141859375", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140303-141859375", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "NSF", "grant_number": "AST-1208891" }, { "agency": "NASA", "grant_number": "NNX14AC89G" }, { "agency": "Washington Research Foundation" }, { "agency": "University of Washington" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/797/1/70", "primary_object": { "basename": "0004-637X_797_1_70.pdf", "url": "https://authors.library.caltech.edu/records/baqgn-7bw24/files/0004-637X_797_1_70.pdf" }, "related_objects": [ { "basename": "1402.4766v2.pdf", "url": "https://authors.library.caltech.edu/records/baqgn-7bw24/files/1402.4766v2.pdf" } ], "pub_year": "2014", "author_list": "Kulkarni, S. R.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/6qvhw-5ys84", "eprint_id": 53174, "eprint_status": "archive", "datestamp": "2023-08-22 14:27:37", "lastmod": "2023-10-23 19:10:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zheng-Zheng", "name": { "family": "Zheng", "given": "Z." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Juric-M", "name": { "family": "Juric", "given": "M." }, "orcid": "0000-0003-1996-9252" } ] }, "title": "Probing the Intergalactic Medium with Fast Radio Bursts", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: miscellaneous; intergalactic medium; pulsars: general; radio continuum: general", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 September 9; accepted 2014 October 13; published 2014 November 25. \n\nWe thank Shude Mao for useful comments. Z.Z. was partially supported by NSF grant AST-1208891 and NASA grant NNX14AC89G. M.J. acknowledges the support of the Washington Research Foundation through its Data Science Chair and the University of Washington Provost's Initiative in Data-Intensive Discovery. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee, and The Israel Science Foundation. S.R.K. thanks the hospitality of the Institute for Advanced Study (IAS). The sylvan surroundings and verdant intellectual ambiance of IAS resulted in a fecund mini-sabbatical stay (Fall 2007).\n\nPublished - 0004-637X_797_1_71.pdf
Submitted - 1409.3244v2.pdf
Erratum - Zheng_2016p83.pdf
", "abstract": "The recently discovered fast radio bursts (FRBs), presumably of extragalactic origin, have the potential to become a powerful probe of the intergalactic medium (IGM). We point out a few such potential applications. We provide expressions for the dispersion measure and rotation measure as a function of redshift, and we discuss the sensitivity of these measures to the He II reionization and the IGM magnetic field. Finally, we calculate the microlensing effect from an isolated, extragalactic stellar-mass compact object on the FRB spectrum. The time delays between the two lensing images will induce constructive and destructive interference, leaving a specific imprint on the spectra of FRBs. With a high all-sky rate, a large statistical sample of FRBs is expected to make these applications feasible.", "date": "2014-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "797", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 71", "id_number": "CaltechAUTHORS:20150105-110011210", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150105-110011210", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1208891" }, { "agency": "NASA", "grant_number": "NNX14AC89G" }, { "agency": "Washington Research Foundation" }, { "agency": "University of Washington" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/797/1/71", "primary_object": { "basename": "0004-637X_797_1_71.pdf", "url": "https://authors.library.caltech.edu/records/6qvhw-5ys84/files/0004-637X_797_1_71.pdf" }, "related_objects": [ { "basename": "1409.3244v2.pdf", "url": "https://authors.library.caltech.edu/records/6qvhw-5ys84/files/1409.3244v2.pdf" }, { "basename": "Zheng_2016p83.pdf", "url": "https://authors.library.caltech.edu/records/6qvhw-5ys84/files/Zheng_2016p83.pdf" } ], "pub_year": "2014", "author_list": "Zheng, Z.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/j8a7z-6j360", "eprint_id": 51804, "eprint_status": "archive", "datestamp": "2023-08-20 03:19:16", "lastmod": "2023-10-18 17:10:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sorce-J-G", "name": { "family": "Sorce", "given": "J. G." } }, { "id": "Tully-R-B", "name": { "family": "Tully", "given": "R. B." }, "orcid": "0000-0002-9291-1981" }, { "id": "Courtois-H-M", "name": { "family": "Courtois", "given": "H. M." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Shaya-E-J", "name": { "family": "Shaya", "given": "E. J." } } ] }, "title": "From Spitzer Galaxy photometry to Tully\u2013Fisher distances", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: photometry\n distance scale\n infrared: galaxies", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 July 17. Received 2014 July 17; in original form 2014 June 19. First published online August 18, 2014. \n\nThe data used in this paper are available at the EDD. We especially thanks our CFS collaborators Wendy Freedman, Barry Madore, Eric Persson and Mark Seibert. We are indebted to James Schombert for the development of the ARCHANGEL software and we thank him for his useful comments as a referee. We thank Kartik Sheth for discussions regarding Spitzer photometry. NASA through the Spitzer Science Center provides support for CFS, Cosmicflows with Spitzer, cycle 8 programme 80072. 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. We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). HC and JS acknowledge support from the Lyon Institute of Origins under grant ANR-10-LABX-66\nand from CNRS under PICS-06233. RBT acknowledges support\nfrom the US National Science Foundation award AST09-08846.\nTJ acknowledges the Astronomy Department of the University of Cape Town.\n\nPublished - MNRAS-2014-Sorce-527-41.pdf
Supplemental Material - tableCalib_spitzerpaper.txt
Supplemental Material - tableDist_spitzerpaper.txt
", "abstract": "This paper involves a data release of the observational campaign: Cosmicflows with Spitzer (CFS). Surface photometry of the 1270 galaxies constituting the survey is presented. An additional \u223c400 galaxies from various other Spitzer surveys are also analysed. CFS complements the Spitzer Survey of Stellar Structure in Galaxies, that provides photometry for an additional 2352 galaxies, by extending observations to low galactic latitudes (|b| < 30\u00b0). Among these galaxies are calibrators, selected in the K band, of the Tully\u2013Fisher relation. The addition of new calibrators demonstrates the robustness of the previously released calibration. Our estimate of the Hubble constant using supernova host galaxies is unchanged, H_0 = 75.2 \u00b1 3.3 km s^(\u22121) Mpc^(\u22121). Distance-derived radial peculiar velocities, for the 1935 galaxies with all the available parameters, will be incorporated into a new data release of the Cosmicflows project. The size of the previous catalogue will be increased by 20 per\u2009cent, including spatial regions close to the Zone of Avoidance.", "date": "2014-10-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "444", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "527-541", "id_number": "CaltechAUTHORS:20141114-151330820", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141114-151330820", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Spitzer Science Center" }, { "agency": "Spitzer-Cosmicflows cycle 8 programme", "grant_number": "80072" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-10-LABX-66" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)", "grant_number": "PICS-06233" }, { "agency": "NSF", "grant_number": "AST09-08846" }, { "agency": "Lyon Institute of Origins (LIO)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stu1450", "primary_object": { "basename": "MNRAS-2014-Sorce-527-41.pdf", "url": "https://authors.library.caltech.edu/records/j8a7z-6j360/files/MNRAS-2014-Sorce-527-41.pdf" }, "related_objects": [ { "basename": "tableCalib_spitzerpaper.txt", "url": "https://authors.library.caltech.edu/records/j8a7z-6j360/files/tableCalib_spitzerpaper.txt" }, { "basename": "tableDist_spitzerpaper.txt", "url": "https://authors.library.caltech.edu/records/j8a7z-6j360/files/tableDist_spitzerpaper.txt" } ], "pub_year": "2014", "author_list": "Sorce, J. G.; Tully, R. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/6yc82-mba20", "eprint_id": 50101, "eprint_status": "archive", "datestamp": "2023-08-22 13:38:54", "lastmod": "2023-10-17 22:30:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Tully-R-B", "name": { "family": "Tully", "given": "R. Brent" }, "orcid": "0000-0002-9291-1981" }, { "id": "Courtois-H", "name": { "family": "Courtois", "given": "H\u00e9l\u00e8ne" } }, { "id": "Sorce-J-G", "name": { "family": "Sorce", "given": "Jenny G." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Scowcroft-V", "name": { "family": "Scowcroft", "given": "Victoria" }, "orcid": "0000-0001-8829-4653" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" } ] }, "title": "The Calibration of the WISE W1 and W2 Tully-Fisher Relation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters; distance scale; galaxies: clusters: general; galaxies: distances and redshifts; galaxies: photometry; radio lines: galaxies", "note": "\u00a9 2014 American Astronomical Society. Received 2014 June 2; accepted 2014 July 21; published 2014 August 25.\n\nWe acknowledge useful conversations with the following\npeople: Wendy Freedman, Barry Madore, Eric Persson, and\nAndrew Monson. J.D.N. and M.S. acknowledge support from the NASA Astrophysical Data Analysis Program under grant NNX12AE19G for the WISE Nearby Galaxies Atlas. H.C. and J.S. acknowledge support from the Lyon Institute of Origins under grant ANR-10-LABX-66 and from CNRS under PICS-06233. R.B.T. acknowledges support from the US National Science Foundation award AST09-08846. We acknowledge the use of the HyperLeda database (http://leda.univ-lyon1.fr). This publication makes use of data products from the Widefield\nInfrared Survey Explorer (WISE), which is a joint project of\ntheUniversity of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.\nThis research has made use of the NASA/IPAC Extragalactic\nDatabase (NED), which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - 0004-637X_792_2_129.pdf
Submitted - 1407.7528v1.pdf
", "abstract": "In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities\u2014capable of providing such distance measures\u2014to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (3.4 \u03bcm) and W2 (4.6 \u03bcm) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M^(b,i,k,\u0251)_(W1) = -20.35 - 9.56(log W^i_(mx) - 2.5) (0.54 mag rms) and M^(b,i,k,\u0251)_(W2) = -19.76 - 9.74 (log W^i_(mx)-2.5)(0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully & Courtois. We derive M^(b,i,k)_I = -21.34 - 8.95 (log W^i_(mx) - 2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M^(b,i,k,\u0251)_(W1) = -20.48 - 8.36 (log W^i_(mx) - 2.5) + 3.60(log W^i_(mx) - 2.5)^2(0.52 mag rms) and M^(b,i,k,\u0251)_(W2) = -19.91 - 8.40(log W^i_(mx) - 2.5) + 4.32 (log W^i_(mx) - 2.5)^2 (0.55 mag rms). We apply an I-band \u2013WISE color correction to lower the scatter and derive M_C_(W1)} = -20.22 - 9.12(log W^i_(mx) - 2.5) and M_C_(W2) = -19.63 - 9.11(log W^i_(mx) - 2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate the UNION2 Type Ia supernova sample distance scale and derive H_0 = 74.4 \u00b1 1.4(stat) \u00b1 2.4(sys) km s^(\u20131) Mpc^(\u20131) with 4% total error.", "date": "2014-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "792", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 129", "id_number": "CaltechAUTHORS:20140929-133613804", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140929-133613804", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AE19G" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-10-LABX-66" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)", "grant_number": "PICS-06233" }, { "agency": "NSF", "grant_number": "AST09-08846" }, { "agency": "Lyon Institute of Origins (LIO)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/792/2/129", "primary_object": { "basename": "0004-637X_792_2_129.pdf", "url": "https://authors.library.caltech.edu/records/6yc82-mba20/files/0004-637X_792_2_129.pdf" }, "related_objects": [ { "basename": "1407.7528v1.pdf", "url": "https://authors.library.caltech.edu/records/6yc82-mba20/files/1407.7528v1.pdf" } ], "pub_year": "2014", "author_list": "Neill, J. D.; Seibert, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/txa7p-d1n46", "eprint_id": 49056, "eprint_status": "archive", "datestamp": "2023-08-20 02:22:58", "lastmod": "2023-10-17 20:38:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara" } }, { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik A." } }, { "id": "P\u00e9rez-L-M", "name": { "family": "P\u00e9rez", "given": "Laura" }, "orcid": "0000-0002-1199-9564" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "Molecular gas properties of UV-bright star-forming galaxies at low redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation \u2013 galaxies: ISM\u2013 galaxies: starburst", "note": "\u00a9 2014 The Authors.\nPublished by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 April 28. \nReceived 2014 April 4. \nIn original form 2013 December 10. \nFirst published online June 16, 2014. \n\nWe thank the anonymous referee for suggestions that helped improve\nthis paper. We would also like to thank Andrew Baker and\nTim Heckman for useful comments. TSG gratefully acknowledges\nCAPES (Coordena\u00e7\u00e3o de Aperfei\u00e7oamento de Pessoal de N\u00edvel\nSuperior) for financial support. Support for CARMA construction\nwas derived from the states of California, Illinois, and Maryland,\nthe James S. McDonnell Foundation, the Gordon and Betty Moore\nFoundation, the Kenneth T. and Eileen L. Norris Foundation, the\nUniversity of Chicago, the Associates of the California Institute\nof Technology, and the National Science Foundation. Ongoing\nCARMA development and operations are supported by the National\nScience Foundation under a cooperative agreement, and by\nthe CARMA partner universities.\n\nPublished - MNRAS-2014-Gon\u00e7alves-1429-39.pdf
", "abstract": "Lyman break analogues (LBAs) are a population of star-forming galaxies at low redshift (z \u223c 0.2) selected in the ultraviolet (UV). These objects present higher star formation rates and lower dust extinction than other galaxies with similar masses and luminosities in the local universe. In this work, we present results from a survey with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) array to detect CO(1\u20130) emission in LBAs, in order to analyse the properties of the molecular gas in these galaxies. Our results show that LBAs follow the same Schmidt\u2013Kennicutt law as local galaxies. On the other hand, they have higher gas fractions (up to 66 per cent) and faster gas depletion time-scales (below 1 Gyr). These characteristics render these objects more akin to high-redshift star-forming galaxies. We conclude that LBAs are a great nearby laboratory for studying the cold interstellar medium in low-metallicity, UV-bright compact star-forming galaxies.", "date": "2014-08-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "442", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1429-1439", "id_number": "CaltechAUTHORS:20140829-092052049", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140829-092052049", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Coordena\u00e7\u00e3o de Aperfei\u00e7oamento de Pessoal de N\u00edvel Superior (CAPES)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/stu852", "primary_object": { "basename": "MNRAS-2014-Gon\u00e7alves-1429-39.pdf", "url": "https://authors.library.caltech.edu/records/txa7p-d1n46/files/MNRAS-2014-Gon\u00e7alves-1429-39.pdf" }, "pub_year": "2014", "author_list": "Gon\u00e7alves, Thiago S.; Basu-Zych, Antara; et el." }, { "id": "https://authors.library.caltech.edu/records/d7z0k-adk61", "eprint_id": 58266, "eprint_status": "archive", "datestamp": "2023-08-20 01:59:34", "lastmod": "2024-01-13 16:22:14", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Jewell-A-D", "name": { "family": "Jewell", "given": "April D." }, "orcid": "0000-0001-8834-3769" }, { "id": "Gordon -S", "name": { "family": "Gordon", "given": "Samuel" } }, { "id": "Hennessy-J-L", "name": { "family": "Hennessy", "given": "John" } }, { "id": "Hoenk-M-E", "name": { "family": "Hoenk", "given": "Michael E." } }, { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "High efficiency CCD detectors at UV wavelengths", "ispublished": "unpub", "full_text_status": "public", "keywords": "Thin Films, Red Blocking, Anti-Reflection Coatings, Ultraviolet, delta doping", "note": "\u00a9 2014 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was partially supported by KISS, the W. M. Keck Institute for Space Studies, and by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, NASA Grant NNX11AO07H, and NASA Grant NNX12AF29G. This research was supported in part through an appointment to the NASA Postdoctoral Program at the Jet Propulsion Lab, administered by Oak Ridge Associated Universities through a contract with NASA.\n\nPublished - Hamden_2014p91442X.pdf
", "abstract": "The Faint Intergalactic Redshifted Emission Balloon (FIREBall) is a NASA/CNES balloon-borne ultraviolet\nmulti-object spectrograph designed to observe the diffuse gas around galaxies (the circumgalactic medium) via\nline emission redshifted to ~ 205 nm. FIREBall uses a ultraviolet-optimized delta doped e2v CCD201 with a\ncustom designed high efficiency five layer anti-re\nection coating. This combination achieves very high quantum\nefficiency (QE) and photon-counting capability, a first for a CCD detector in this wavelength range. We also present new work on red blocking mirror coatings to reduce red leak.", "date": "2014-07-24", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 91442X", "id_number": "CaltechAUTHORS:20150616-075402384", "isbn": "978-0-8194-9612-6", "book_title": "Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150616-075402384", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NASA", "grant_number": "NNX11AO07H" }, { "agency": "NASA", "grant_number": "NNX12AF29G" }, { "agency": "NASA Oak Ridge Associated Universities" }, { "agency": "NASA Postdoctoral Program" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Takahashi-Tadayuki", "name": { "family": "Takahashi", "given": "Tadayuki" } }, { "id": "den-Herder-J-W-A", "name": { "family": "den Herder", "given": "Jan-Willem A." } }, { "id": "Bautz-M", "name": { "family": "Bautz", "given": "Mark" } } ] }, "doi": "10.1117/12.2056204", "primary_object": { "basename": "Hamden_2014p91442X.pdf", "url": "https://authors.library.caltech.edu/records/d7z0k-adk61/files/Hamden_2014p91442X.pdf" }, "pub_year": "2014", "author_list": "Hamden, Erika T.; Jewell, April D.; et el." }, { "id": "https://authors.library.caltech.edu/records/2y8zz-4pj06", "eprint_id": 48288, "eprint_status": "archive", "datestamp": "2023-08-20 01:19:49", "lastmod": "2023-10-17 18:40:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kazin-E-A", "name": { "family": "Kazin", "given": "Eyal A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: improved distance measurements to z = 1 with reconstruction of the baryonic acoustic feature", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters\n distance scale\n large-scale structure of the universe", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 April 17. Received 2014 March 14. In original form 2013 December 31. First published online June 1, 2014. We thank Florian Beutler, Daniel Eisenstein, Shahab Joudaki,\nAntony Lewis, Felipe Marin and Ariel Sanchez for useful discussions. EK and JK are supported by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. CB acknowledges the support of the Australian Research Council through the award of a Future Fellowship. TMD acknowledges the support of the Australian Research Council through a Future Fellowship award, FT100100595. The numerical simulation was supported by the\nSwinSTAR supercomputer at Swinburne University of Technology\nand the Raijin supercomputer through the Flagship Allocation\nScheme of the NCI National Facility at the ANU.\n\nPublished - MNRAS-2014-Kazin-3524-42.pdf
", "abstract": "We present significant improvements in cosmic distance measurements from the WiggleZ Dark Energy Survey, achieved by applying the reconstruction of the baryonic acoustic feature technique. We show using both data and simulations that the reconstruction technique can often be effective despite patchiness of the survey, significant edge effects and shot-noise. We investigate three redshift bins in the redshift range 0.2 < z < 1, and in all three find improvement after reconstruction in the detection of the baryonic acoustic feature and its usage as a standard ruler. We measure model-independent distance measures D_V(r_s^(fid)/r_s) of 1716 \u00b1 83, 2221 \u00b1 101, 2516 \u00b1 86 Mpc (68 per\u2009cent CL) at effective redshifts z = 0.44, 0.6, 0.73, respectively, where D_V is the volume-averaged distance, and r_s is the sound horizon at the end of the baryon drag epoch. These significantly improved 4.8, 4.5 and 3.4 per cent accuracy measurements are equivalent to those expected from surveys with up to 2.5 times the volume of WiggleZ without reconstruction applied. These measurements are fully consistent with cosmologies allowed by the analyses of the Planck Collaboration and the Sloan Digital Sky Survey. We provide the D_V(r_s^(fid)/r_s) posterior probability distributions and their covariances. When combining these measurements with temperature fluctuations measurements of Planck, the polarization of Wilkinson Microwave Anisotropy Probe 9, and the 6dF Galaxy Survey baryonic acoustic feature, we do not detect deviations from a flat \u039b cold dark matter (\u039bCDM) model. Assuming this model, we constrain the current expansion rate to H_0 = 67.15 \u00b1 0.98 km s^(\u22121)Mpc^(\u22121). Allowing the equation of state of dark energy to vary, we obtain w_(DE) = \u22121.080 \u00b1 0.135. When assuming a curved \u039bCDM model we obtain a curvature value of \u03a9_K = \u22120.0043 \u00b1 0.0047.", "date": "2014-06-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "441", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3524-3542", "id_number": "CaltechAUTHORS:20140811-091252086", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140811-091252086", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)", "grant_number": "CE110001020" }, { "agency": "Australian Research Council", "grant_number": "FT100100595" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/stu778", "primary_object": { "basename": "MNRAS-2014-Kazin-3524-42.pdf", "url": "https://authors.library.caltech.edu/records/2y8zz-4pj06/files/MNRAS-2014-Kazin-3524-42.pdf" }, "pub_year": "2014", "author_list": "Kazin, Eyal A.; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/bdwkr-1zy75", "eprint_id": 44109, "eprint_status": "archive", "datestamp": "2023-08-20 00:54:36", "lastmod": "2023-10-26 00:11:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Chang-Daphne", "name": { "family": "Chang", "given": "Daphne" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Matt" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahin" } }, { "id": "Moore-A", "name": { "family": "Moore", "given": "Anna" } }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "title": "Intergalactic Medium Emission Observations with the Cosmic Web Imager. I. The Circum-QSO Medium of QSO 1549+19, and Evidence for a Filamentary Gas Inflow", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014. The American Astronomical Society. \n\nReceived 9 February 2013, accepted for publication 10 February 2014. Published 24 April 2014. \n\nWe thank Tom Tombrello and Shri Kulkarni for their support of PCWI. We thank Marty Crabill, Steve Kaye and the staff of the Palomar Observatory for their constant support. Nicole Lingner participated in the observations. We are deeply grateful to Dean Joe Shepard, to the Caltech Counselling Office, and to the family of Daphne Chang for their strength and support. We acknowledge the detailed and helpful comments from the anonymous referee. This work was supported by the National Science Foundation and the California Institute of Technology.\n\nPublished - 0004-637X_786_2_106.pdf
Submitted - 1402.4816.pdf
", "abstract": "The Palomar Cosmic Web Imager (PCWI), an integral field spectrograph designed to detect and map low surface brightness emission, has obtained imaging spectroscopic maps of Ly\u03b1 from the circum-QSO medium (CQM) of QSO HS1549+19 at redshift z=2.843. Extensive extended emission is detected from the CQM, consistent with fluorescent and pumped Ly\u03b1 produced by the ionizing and Ly\u03b1 continuum of the QSO. Many features present in PCWI spectral images match those detected in narrow-band images. Filamentary structures with narrow line profiles are detected in several cases as long as 250-400 kpc. One of these is centered at a velocity redshifted with respect to the systemic velocity, and displays a spatially collimated and\nkinematically cold line profile increasing in velocity width approaching the QSO. This suggests that the filament gas is infalling onto the QSO, perhaps in a cold accretion flow. Because of the strong ionizing flux, the neutral column density is low, typically N(HI) ~ 10^(12)\u221210^(15) cm^(\u22122), and the line center optical depth is also low (typically \u03c4_0 <10), insufficient to display well-separated\ndouble peak emission characteristic of higher line optical depths. With a simple ionization and cloud model we can very roughly estimate the total gas mass (log M_(gas) = 12.5 \u00b1 0.5) and the total (log M_(tot) = 13.3\u00b1 0.5). We can also calculate a kinematic mass from the total line profile (2\u00d710^(13)M_\u2609), which agrees with the mass estimated from the gas emission. The intensity-binned\nspectrum of the CQM shows a progression in kinematic properties consistent with heirarchical structure formation.", "date": "2014-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "768", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 106", "id_number": "CaltechAUTHORS:20140303-152428640", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140303-152428640", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/786/2/106", "primary_object": { "basename": "0004-637X_786_2_106.pdf", "url": "https://authors.library.caltech.edu/records/bdwkr-1zy75/files/0004-637X_786_2_106.pdf" }, "related_objects": [ { "basename": "1402.4816.pdf", "url": "https://authors.library.caltech.edu/records/bdwkr-1zy75/files/1402.4816.pdf" } ], "pub_year": "2014", "author_list": "Martin, D. Christopher; Chang, Daphne; et el." }, { "id": "https://authors.library.caltech.edu/records/mtwgn-gkm57", "eprint_id": 44105, "eprint_status": "archive", "datestamp": "2023-08-20 00:54:29", "lastmod": "2023-10-26 00:11:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Chang-Daphne", "name": { "family": "Chang", "given": "Daphne" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Matt" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahin" } }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Matsuda-Yuichi", "name": { "family": "Matsuda", "given": "Yuichi" } } ] }, "title": "Intergalactic Medium Emission Observations with the Cosmic Web Imager. II. Discovery of Extended, Kinematically-Linked Emission around SSA22 Ly\u03b1 Blob 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: formation \u2013 galaxies: high-redshift \u2013 intergalactic medium \u2013\ntechniques: imaging spectroscopy", "note": "\u00a9 2014. The American Astronomical Society. \n\nReceived 2013 May 24; accepted 2013 October 31; published 2014 April 24. \n\nWe thank Tom Tombrello and Shri Kulkarni for their support of CWI. We thank Marty Crabill, Steve Kaye and the staff of the Palomar Observatory for their constant support. Nicole Ligner participated in the observations. We are deeply grateful to Dean Joe Shepard, to the Caltech Counselling Office, and to the family of Daphne Chang for their strength and support. The anonymous referee provided excellent suggestions that significantly improved the paper. This\nwork was supported by the National Science Foundation and the California Institute of Technology.\n\nPublished - 0004-637X_786_2_107.pdf
Submitted - 1402.4809.pdf
", "abstract": "The intergalactic medium (IGM) is the dominant reservoir of baryons, delineates the large scale structure of the universe at low to moderate overdensities, and provides gas from which galaxies form and evolve. Simulations of a Cold Dark Matter (CDM) dominated universe predict that the\nIGM is distributed in a cosmic web of filaments, and that galaxies should form along and at the intersections of these filaments (Bond, Kofman, & Pogosyan 1994; Miralda-Escude et al. 1996). While observations of QSO absorption lines and the large-scale distribution of galaxies have\nconfirmed the CDM paradigm, the cosmic web of IGM has never been confirmed by direct imaging. Here we report our observation of the Ly\u03b1 blob-2 (LAB2) in SSA22, with the Cosmic Web Imager. This is an integral field spectrograph optimized for low surface brightness, extended emission. With 22 hours of total on- and off-source exposure, CWI has revealed that LAB2 has extended Ly\u03b1 emission which is organized into azimuthal zones consistent with filaments. We perform numerous tests with simulations and the data to secure the robustness of this result, which relies on data with modest signal-to-noise ratio. We have developed a\nsmoothing algorithm that permits visualization of data cube slices along image or spectral-image planes. With both raw and smoothed data cubes we demonstrate that the filaments are kinematically associated with LAB2 and display double-peaked profiles characteristic of optically thick Ly\u03b1 emission. The flux is 10-20 times brighter than expected for the average emission from the IGM but is consistent with boosted fluorescence from a buried QSO or gravitation cooling radiation. Using simple emission models we infer a baryon mass in the filaments of at least 1\u22124 \u00d7 10^(11)M_\u2609, and the dark halo mass is at least 2 \u00d7 10^(12)M_\u2609. The spatial-kinematic morphology is more consistent with inflow from the cosmic web than outflow from LAB2, although an outflow feature maybe present at one azimuth. LAB2 and the surrounding gas have significant and coaligned angular momentum, strengthening the case for their association.", "date": "2014-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "786", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20140303-145821259", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140303-145821259", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/786/2/107", "primary_object": { "basename": "0004-637X_786_2_107.pdf", "url": "https://authors.library.caltech.edu/records/mtwgn-gkm57/files/0004-637X_786_2_107.pdf" }, "related_objects": [ { "basename": "1402.4809.pdf", "url": "https://authors.library.caltech.edu/records/mtwgn-gkm57/files/1402.4809.pdf" } ], "pub_year": "2014", "author_list": "Martin, D. Christopher; Chang, Daphne; et el." }, { "id": "https://authors.library.caltech.edu/records/24ext-p0c44", "eprint_id": 46284, "eprint_status": "archive", "datestamp": "2023-08-22 12:30:33", "lastmod": "2023-10-26 19:38:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Margon-B", "name": { "family": "Margon", "given": "Bruce" }, "orcid": "0000-0002-7837-3363" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "Gregg" }, "orcid": "0000-0002-7083-4049" }, { "id": "Harding-L-K", "name": { "family": "Harding", "given": "Leon K." } }, { "id": "Kyne-G", "name": { "family": "Kyne", "given": "Gillian" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Rutten-R-G-M", "name": { "family": "Rutten", "given": "Ren\u00e9 G. M." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "PTF1 J191905.19+481506.2--A Partially Eclipsing AM CVn System Discovered in the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; binaries: close; novae, cataclysmic variables; stars: individual (PTF1J191905.19+481506.2); white dwarfs", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 September 28; accepted 2014 February 27; published 2014 April 2.\n\nT.K. acknowledges support by the Netherlands Research\nSchool of Astronomy (NOVA).We thank Dong Xu for reducing\nthe initial classification spectra.\nObservations obtained with the Samuel Oschin Telescope at\nthe Palomar Observatory as part of the Palomar Transient Factory\nproject, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory,\nthe Lawrence Berkeley National Laboratory, the National\nEnergy Research Scientific Computing Center, the University\nof Oxford, and the Weizmann Institute of Science. Some\nof the data presented herein were obtained at the W. M. Keck\nObservatory, which is operated as a scientific partnership among\nthe California Institute of Technology, the University of California\nand the National Aeronautics and Space Administration.\nThe Observatory was made possible by the generous financial\nsupport of the W. M. Keck Foundation. The authors wish to\nrecognize and acknowledge the very significant cultural role\nand reverence that the summit of Mauna Kea has always had\nwithin the indigenous Hawaiian community. We are most fortunate\nto have the opportunity to conduct observations from this\nmountain. Based in part on observations obtained at the Gemini\nObservatory, which is operated by the Association of Universities\nfor Research in Astronomy, Inc., under a cooperative\nagreement with the NSF on behalf of the Gemini partnership:\nthe National Science Foundation (United States), the National\nResearch Council (Canada), CONICYT (Chile), the Australian\nResearch Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia\ne Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e\nInnovaci\u00f3n Productiva (Argentina). The Gemini data were obtained\nunder Program ID GN-2012B-Q-110. Based in part on\nobservations made with the Gran Telescopio Canarias (GTC)\ninstalled in the Spanish Observatorio del Roque de los Muchachos\nof the Instituto de Astrof\u00edsica de Canarias, on the island of\nLa Palma.\n\nFacilities: PO:1.2m, PO:1.5m, Gemini:Gillett (GMOS-N),\nGTC (OSIRIS), Hale (CHIMERA, DBSP), Keck:I (LRIS),\nShane (Kast Double spectrograph)\n\nPublished - 0004-637X_785_2_114.pdf
Submitted - 1402.7129v1.pdf
", "abstract": "We report on PTF1 J191905.19+481506.2, a newly discovered, partially eclipsing, outbursting AM CVn system found in the Palomar Transient Factory synoptic survey. This is only the second known eclipsing AM CVn system. We use high-speed photometric observations and phase-resolved spectroscopy to establish an orbital period of 22.4559(3) minutes. We also present a long-term light curve and report on the normal and super-outbursts regularly seen in this system, including a super-outburst recurrence time of 36.8(4) days. We use the presence of the eclipse to place upper and lower limits on the inclination of the system and discuss the number of known eclipsing AM CVn systems versus what would be expected.", "date": "2014-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "785", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 114", "id_number": "CaltechAUTHORS:20140616-132349713", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-132349713", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/785/2/114", "primary_object": { "basename": "0004-637X_785_2_114.pdf", "url": "https://authors.library.caltech.edu/records/24ext-p0c44/files/0004-637X_785_2_114.pdf" }, "related_objects": [ { "basename": "1402.7129v1.pdf", "url": "https://authors.library.caltech.edu/records/24ext-p0c44/files/1402.7129v1.pdf" } ], "pub_year": "2014", "author_list": "Levitan, David; Kupfer, Thomas; et el." }, { "id": "https://authors.library.caltech.edu/records/2x49c-2sc87", "eprint_id": 44533, "eprint_status": "archive", "datestamp": "2023-08-22 11:26:40", "lastmod": "2023-10-26 14:45:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hillman-Y", "name": { "family": "Hillman", "given": "Y." } }, { "id": "Prialnik-D", "name": { "family": "Prialnik", "given": "D." } }, { "id": "Kovetz-A", "name": { "family": "Kovetz", "given": "A." } }, { "id": "Shara-M-M", "name": { "family": "Shara", "given": "M. M." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Nova multiwavelength light curves: predicting UV precursor flashes and pre-maximum halts", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis; methods: numerical; binaries: close; novae, cataclysmic variables; white dwarfs.", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 October 18. Received 2013 October 17. In original form 2013 August 6. This work was supported by Grant No.2010220 of the United States \u2013 Israel Binational Science Foundation. MS gratefully acknowledges ongoing support from Hilary and Ethel Lipsitz, and very helpful conversations with J. Mikolajewska concerning symbiotic novae. A very helpful referee report by Mike Bode is also gratefully acknowledged.\n\nPublished - MNRAS-2014-Hillman-1962-75.pdf
", "abstract": "The dramatic brightenings of classical novae have yielded rich data sets of detailed light curves. Modelling these light curves is a challenge for any theory of classical novae. We have used our extended grid of nova outburst calculations to predict the luminosities of erupting novae expected in three electromagnetic bands \u2013 the visual, the near UV and the X-ray. Our models predict and explain many features of novae before eruption, as well as detailed characterizations of nova outbursts and post-nova declines. The evolutionary time-scales of eruption features vary by orders of magnitude, and depend on the basic nova parameters: white dwarf mass, luminosity and accretion rate. However, all light curves are found to share common features. Some of these features are unique to only one electromagnetic passband, while others show up in two, or in all three of the analysed bands. One extraordinary feature, common to all of our low-mass white dwarfs (0.65\u2009M_\u2299) novae, is that all exhibit a sharp rise followed by a more gradual decline in the near-UV luminosity, prior to the eruption in the visual luminosity. This is because the expansion of the outer layers lags behind the rise in bolometric luminosity. These predicted precursor-UV-flashes last between a few hours and a few days, and the predicted luminosity increase is between \u223c0.5 and \u223c3 mag. These flashes should be easily observable if a nova event is detected early and its time coverage is dense. Many observed novae exhibit a pre-maximum halt, and this feature is found in all three electromagnetic bands of many, but not all, of our nova models. We explain the presence or absence of pre-maximum halts as due to changes in the convective energy transfer regime. Finally we note cases where the maximum visual magnitude reaches as high as \u22128.5 mag for low-mass white dwarfs. This re-emphasizes the fact that white dwarf mass is not always the determining factor in setting a nova's peak luminosity.", "date": "2014-01-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "437", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1962-1975", "id_number": "CaltechAUTHORS:20140326-132742017", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140326-132742017", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Binational Science Foundation (USA-Israel)", "grant_number": "2010220" }, { "agency": "Hilary and Ethel Lipsitz" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/stt2027", "primary_object": { "basename": "MNRAS-2014-Hillman-1962-75.pdf", "url": "https://authors.library.caltech.edu/records/2x49c-2sc87/files/MNRAS-2014-Hillman-1962-75.pdf" }, "pub_year": "2014", "author_list": "Hillman, Y.; Prialnik, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/r32nx-0ef16", "eprint_id": 43589, "eprint_status": "archive", "datestamp": "2023-08-22 11:21:55", "lastmod": "2023-10-25 23:41:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chornock-R", "name": { "family": "Chornock", "given": "R." }, "orcid": "0000-0002-7706-5668" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "The Ultraviolet-bright, Slowly Declining Transient PS1-11af as a Partial Tidal Disruption Event", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: nuclei", "note": "\u00a9 2014 American Astronomical Society. Received 2013 September 11; accepted 2013 November 9; published 2013 December 11. We thank the staffs at PS1, Magellan, Gemini, the MMT, and the VLA for their assistance with scheduling and performing these observations. We acknowledge useful discussions with E. Ramirez-Ruiz, the assistance of T. Laskar with some of the MMT observations, and the help of A. Monson with FourStar data reduction. B.A.Z. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302954. This paper includes data gathered with the 6.5m Magellan Telescopes located at Las Campanas Observatory, Chile. Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The Pan-STARRS1 Surveys (PS1) have been made possible through the contributions of the Institute\nfor Astronomy, the University of Hawaii, the Pan-STARRS\nProject Office, the Max-Planck Society and its participating\ninstitutes, the Max Planck Institute for Astronomy, Heidelberg and theMax 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, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, and the University of Maryland. Some observations were obtained under Program ID GS-2011A-Q-29 (PI: Berger) at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative\nagreement with the NSF on behalf of the Gemini partnership:\nthe National Science Foundation (United States), the\nNational Research Council (Canada), CONICYT (Chile), the\nAustralian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva (Argentina). S.J.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 291222. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. R.P.K.'s work on SNe is supported in part by NSF grant AST-1211196. Partial support for this work was also provided by NSF grant AST-1009749 to J.T.. STSDAS is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. Development of the BOXFIT code was supported in part by NASA through grant NNX10AF62G issued through the Astrophysics Theory Program and by the NSF through grant AST-1009863. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University.\nFacilities: PS1 (GPC1),Magellan:Baade (IMACS, FourStar),\nMagellan:Clay (LDSS3), MMT (Blue Channel spectrograph),\nGemini:South (GMOS-S), EVLA\n\nPublished - 0004-637X_780_1_44.pdf
Submitted - 1309.3009v1.pdf
", "abstract": "We present the Pan-STARRS1 discovery of the long-lived and blue transient PS1-11af, which was also detected by Galaxy Evolution Explorer with coordinated observations in the near-ultraviolet (NUV) band. PS1-11af is associated with the nucleus of an early type galaxy at redshift z = 0.4046 that exhibits no evidence for star formation or active galactic nucleus activity. Four epochs of spectroscopy reveal a pair of transient broad absorption features in the UV on otherwise featureless spectra. Despite the superficial similarity of these features to P-Cygni absorptions of supernovae (SNe), we conclude that PS1-11af is not consistent with the properties of known types of SNe. Blackbody fits to the spectral energy distribution are inconsistent with the cooling, expanding ejecta of a SN, and the velocities of the absorption features are too high to represent material in homologous expansion near a SN photosphere. However, the constant blue colors and slow evolution of the luminosity are similar to previous optically selected tidal disruption events (TDEs). The shape of the optical light curve is consistent with models for TDEs, but the minimum accreted mass necessary to power the observed luminosity is only ~0.002 M \u2609, which points to a partial disruption model. A full disruption model predicts higher bolometric luminosities, which would require most of the radiation to be emitted in a separate component at high energies where we lack observations. In addition, the observed temperature is lower than that predicted by pure accretion disk models for TDEs and requires reprocessing to a constant, lower temperature. Three deep non-detections in the radio with the Very Large Array over the first two years after the event set strict limits on the production of any relativistic outflow comparable to Swift J1644+57, even if off-axis.", "date": "2014-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "780", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 44", "id_number": "CaltechAUTHORS:20140130-140916310", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140130-140916310", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Astronomy and Astrophysics Postdoctoral Fellowship", "grant_number": "AST-1302954" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "European Research Council (ERC)", "grant_number": "291222" }, { "agency": "NSF", "grant_number": "AST-1211196" }, { "agency": "NSF", "grant_number": "AST-1009749" }, { "agency": "NASA", "grant_number": "NNX10AF62G" }, { "agency": "NSF", "grant_number": "AST-1009863" }, { "agency": "Harvard University" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/780/1/44", "primary_object": { "basename": "0004-637X_780_1_44.pdf", "url": "https://authors.library.caltech.edu/records/r32nx-0ef16/files/0004-637X_780_1_44.pdf" }, "related_objects": [ { "basename": "1309.3009v1.pdf", "url": "https://authors.library.caltech.edu/records/r32nx-0ef16/files/1309.3009v1.pdf" } ], "pub_year": "2014", "author_list": "Chornock, R.; Martin, D. C.; et el." }, { "id": "https://authors.library.caltech.edu/records/p8hmn-b3584", "eprint_id": 41891, "eprint_status": "archive", "datestamp": "2023-08-22 10:27:30", "lastmod": "2023-10-25 14:53:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Petty-Sara-M", "name": { "family": "Petty", "given": "S. M." }, "orcid": "0000-0003-0624-3276" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D. G." }, "orcid": "0000-0003-1748-2010" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Tsai-Chao-Wei", "name": { "family": "Tsai", "given": "C.-W." }, "orcid": "0000-0002-9390-9672" }, { "id": "Benford-D-J", "name": { "family": "Benford", "given": "D. J." }, "orcid": "0000-0002-9884-4206" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Lake-S-E", "name": { "family": "Lake", "given": "S. E." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "E. L." }, "orcid": "0000-0001-5058-1593" } ] }, "title": "UV-bright Nearby Early-type Galaxies Observed in the Mid-infrared: Evidence for a Multi-stage Formation History by Way of WISE and GALEX Imaging", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2012 April 22; accepted 2013 July 22; published 2013 August 21.\n\nWe thank the anonymous referee for thorough comments\nthat greatly improved this paper. We thank Marcio Catelan for discussions on evolved stellar populations, and D. Stern for numerous\ninsights into the discussion of galaxy evolution.We also\nthank R. Assef for his feedback on the analysis and early development\nof this project. This publication makes use of data\nproducts from the Wide-field Infrared Survey Explorer, which\nis a joint project of the University of California, Los Angeles,\nand the Jet Propulsion Laboratory/California Institute of Technology,\nfunded by the National Aeronautics and Space Administration.\nThe publication is based on observations made with\nthe NASA Galaxy Evolution Explorer. GALEX is operated for\nNASA by the California Institute of Technology under NASA\ncontract NAS5-98034. This publication makes use of data products\nfrom the Sloan Digital Sky Survey. Funding for the SDSS\nand SDSS-II has been provided by the Alfred P. Sloan Foundation,\nthe Participating Institutions, the National Science Foundation,\nthe U.S. Department of Energy, the National Aeronautics\nand Space Administration, the Japanese Monbukagakusho, the\nMax Planck Society, and the Higher Education Funding Council\nfor England. The SDSS Web site is http://www.sdss.org/.\nThis publication makes use of data products from the Two Micron\nAll Sky Survey, which is a joint project of the University\nof Massachusetts and the Infrared Processing and Analysis\nCenter/California Institute of Technology, funded by the National\nAeronautics and Space Administration and the National\nScience Foundation. This research has made use of the NASA/\nIPAC Extragalactic Database (NED) which is operated by the\nJet Propulsion Laboratory, California Institute of Technology,\nunder contract with the National Aeronautics and Space Administration.\n\nPublished - 1538-3881_146_4_77.pdf
Submitted - 1307.6282v1.pdf
", "abstract": "In the local universe, 10% of massive elliptical galaxies are observed to exhibit a peculiar property: a substantial excess of ultraviolet emission than what is expected from their old, red stellar populations. Several origins for this ultraviolet excess (UVX) have been proposed including a population of hot young stars and a population of old, blue horizontal branch or extended horizontal branch (BHB or EHB) stars that have undergone substantial mass loss from their outer atmospheres. We explore the radial distribution of UVX in a selection of 49 nearby E/S0-type galaxies by measuring their extended photometry in the UV through mid-infrared (mid-IR) with the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the Wide-field Infrared Survey Explorer (WISE). We compare UV/optical and UV/mid-IR colors with the Flexible Stellar Population Synthesis models, which allow for the inclusion of EHB stars. We find that combined WISE mid-IR and GALEX UV colors are more effective in distinguishing models than optical colors, and that the UV/mid-IR combination is sensitive to the EHB fraction. There are strong color gradients, with the outer radii bluer than the inner half-light radii by ~1 mag. This color difference is easily accounted for with an increase in the BHB fraction of 0.25 with radius. We estimated that the average ages for the inner and outer radii are 7.0 \u00b1 0.3 Gyr, and 6.2 \u00b1 0.2 Gyr, respectively, with the implication that the outer regions are likely to have formed ~1 Gyr after the inner regions. Additionally, we find that metallicity gradients are likely not a significant factor in the color difference. The separation of color between the inner and outer regions, which agrees with a specific stellar population difference (e.g., higher EHB populations), and the ~0.5\u20132 Gyr age difference suggests multi-stage formation. Our results are best explained by inside-out formation: rapid star formation within the core at early epochs (>4 Gyr ago) and at least one later stage starburst event coinciding with z ~ 1.", "date": "2013-10", "date_type": "published", "publication": "Astronomical Journal", "volume": "146", "number": "4", "publisher": "American Astronomical Society", "pagerange": "Art. No. 77", "id_number": "CaltechAUTHORS:20131011-105108149", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131011-105108149", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-98034" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-6256/146/4/77", "primary_object": { "basename": "1307.6282v1.pdf", "url": "https://authors.library.caltech.edu/records/p8hmn-b3584/files/1307.6282v1.pdf" }, "related_objects": [ { "basename": "1538-3881_146_4_77.pdf", "url": "https://authors.library.caltech.edu/records/p8hmn-b3584/files/1538-3881_146_4_77.pdf" } ], "pub_year": "2013", "author_list": "Petty, S. M.; Neill, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/9jrba-a4g54", "eprint_id": 42503, "eprint_status": "archive", "datestamp": "2023-08-22 10:18:03", "lastmod": "2023-10-25 16:43:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jurek-R-J", "name": { "family": "Jurek", "given": "Russell J." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: star formation in UV-luminous galaxies from their luminosity functions", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: luminosity function, mass function; galaxies: starburst; ultraviolet: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 June 6. Received 2013 May 2; in original form 2012 November 17.\n\nFirst published online: July 8, 2013.\n\nThis project would not have been possible without the superb\nAAOmega/2dF facility provided by the Australian Astronomical\nObservatory. We wish to thank all the AAO staff for their support, especially the night assistants, support astronomers and Russell Cannon (who greatly assisted with the quality control of the 2dF system). We wish to acknowledge financial support from the Australian Research Council (grants DP0772084, DP1093738 and LX0881951 directly for the WiggleZ project, and grant LE0668442 for programming\nsupport), Swinburne University of Technology, the University\nof Queensland, the Anglo-Australian Observatory and the Gregg Thompson Dark Energy Travel Fund. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National\nScience Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, theMax Planck Society and theHigher Education Funding Council for England. The SDSS website is http://www.sdss.org/. Funding for the DEEP2 survey has been provided by NSF grants AST95-09298, AST-0071048, AST-0071198, AST-0507428 and AST-0507483 as well as NASA LTSA grant NNG04GC89G. 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. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.\n\nPublished - MNRAS-2013-Jurek-257-81.pdf
Submitted - 1306.4031v1.pdf
", "abstract": "We present the ultraviolet (UV) luminosity function of galaxies from the GALEX Medium Imaging Survey with measured spectroscopic redshifts from the first data release of the WiggleZ Dark Energy Survey. Our sample consists of 39 996 NUV < 22.8 emission line galaxies in the redshift range 0.1 < z < 0.9. This sample selects galaxies with high star formation rates: at 0.6 < z < 0.9 the median star formation rate is at the upper 95th percentile of optically selected (r < 22.5) galaxies and the sample contains about 50\u2009per\u2009cent of all NUV < 22.8, 0.6 < z < 0.9 starburst galaxies within the volume sampled. The most luminous galaxies in our sample (\u221221.0 > M_NUV > \u221222.5) evolve very rapidly with a number density declining as (1 + z)5\u00b11 from redshift z = 0.9 to 0.6. These starburst galaxies (MNUV < \u221221 is approximately a star formation rate of 30\u2009M_\u2299\u2009yr^\u22121) contribute about 1\u2009per\u2009cent of cosmic star formation over the redshift range z = 0.6\u20130.9. The star formation rate density of these very luminous galaxies evolves rapidly, as (1 + z)^4\u00b11. Such a rapid evolution implies that the majority of star formation in these large galaxies must have occurred before z = 0.9. We measure the UV luminosity function in \u0394z = 0.05 redshift intervals spanning 0.1 < z < 0.9, and provide analytic fits to the results. Our measurements of the luminosity function over this redshift range probe further into the bright end (1\u20132 mag further) than previous measurements, e.g. Arnouts et al., Budav\u00e1ri et al. and Treyer et al., due to our much larger sample size and sampled volume. At all redshifts z > 0.55 we find that the bright end of the luminosity function is not well described by a pure Schechter function due to an excess of very luminous (MNUV < \u221222) galaxies. These luminosity functions can be used to create a radial selection function for the WiggleZ survey or test models of galaxy formation and evolution. Here we test the AGN feedback model in Scannapieco, Silk & Bouwens, and find that this AGN feedback model requires AGN feedback efficiency to vary with one or more of the following: stellar mass, star formation rate and redshift.", "date": "2013-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "434", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "257-281", "id_number": "CaltechAUTHORS:20131115-120041384", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131115-120041384", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "DP1093738" }, { "agency": "Australian Research Council", "grant_number": "LX0881951" }, { "agency": "Swinburne University of Technology" }, { "agency": "University of Queensland" }, { "agency": "Anglo-Australian Observatory" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" }, { "agency": "NASA" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "NSF", "grant_number": "AST95-09298" }, { "agency": "NSF", "grant_number": "AST-0071048" }, { "agency": "NSF", "grant_number": "AST-0071198" }, { "agency": "NSF", "grant_number": "AST-0507428" }, { "agency": "NSF", "grant_number": "AST-0507483" }, { "agency": "NASA LTSA", "grant_number": "NNG04GC89G" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/stt1015", "primary_object": { "basename": "1306.4031v1.pdf", "url": "https://authors.library.caltech.edu/records/9jrba-a4g54/files/1306.4031v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Jurek-257-81.pdf", "url": "https://authors.library.caltech.edu/records/9jrba-a4g54/files/MNRAS-2013-Jurek-257-81.pdf" } ], "pub_year": "2013", "author_list": "Jurek, Russell J.; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/tbzbs-avr25", "eprint_id": 39803, "eprint_status": "archive", "datestamp": "2023-08-19 20:44:57", "lastmod": "2023-10-24 17:12:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mar\u00edn-F-A", "name": { "family": "Mar\u00edn", "given": "Felipe A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: constraining galaxy bias and cosmic growth with three-point correlation functions", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical \u2013 cosmological parameters \u2013 cosmology: observations \u2013\nlarge-scale structure of \u2013 Universe", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 March 22. Received 2013 March 22; in original form 2012 November 1.\nFirst published online: May 23, 2013.\n\nWe thank Eyal Kazin for fruitful discussions and suggestions, and the anonymous referee for valuable comments and suggestions. We acknowledge financial support from the Australian Research Council through Discovery Project grants which have funded the positions of MP, GP, TD and FM. SMC acknowledges the support of the Australian Research Council through a QEII Fellowship. CB acknowledges the financial support of the ARC through a Future Fellowship award. We are also grateful for support from the Centre for All-sky Astrophysics, an Australian Research Council Centre of Excellence funded by grant CE11000102. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Finally, the WiggleZ survey would not be possible without the dedicated work of the staff of the Australian Astronomical Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT.\n\nPublished - stt520.pdf
Submitted - 1303.6644v1.pdf
", "abstract": "Higher order statistics are a useful and complementary tool for measuring the clustering of galaxies, containing information on the non-Gaussian evolution and morphology of large-scale structure in the Universe. In this work we present measurements of the three-point correlation function (3PCF) for 187\u2009000 galaxies in the WiggleZ spectroscopic galaxy survey. We explore the WiggleZ 3PCF scale and shape dependence at three different epochs z = 0.35, 0.55 and 0.68, the highest redshifts where these measurements have been made to date. Using N-body simulations to predict the clustering of dark matter, we constrain the linear and non-linear bias parameters of WiggleZ galaxies with respect to dark matter, and marginalize over them to obtain constraints on \u03c38(z), the variance of perturbations on a scale of 8 h^\u22121 Mpc and its evolution with redshift. These measurements of \u03c3_8(z), which have 10\u201320 per cent accuracies, are consistent with the predictions of the \u039b cold dark matter concordance cosmology and test this model in a new way.", "date": "2013-07-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "432", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2654-2668", "id_number": "CaltechAUTHORS:20130807-115748472", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130807-115748472", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "CE110001020" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/stt520", "primary_object": { "basename": "1303.6644v1.pdf", "url": "https://authors.library.caltech.edu/records/tbzbs-avr25/files/1303.6644v1.pdf" }, "related_objects": [ { "basename": "stt520.pdf", "url": "https://authors.library.caltech.edu/records/tbzbs-avr25/files/stt520.pdf" } ], "pub_year": "2013", "author_list": "Mar\u00edn, Felipe A.; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/9s9qh-cyk96", "eprint_id": 38930, "eprint_status": "archive", "datestamp": "2023-08-19 19:58:31", "lastmod": "2023-10-20 22:17:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Banerji-M", "name": { "family": "Banerji", "given": "Manda" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The stellar masses of \u223c40 000 UV selected Galaxies from the WiggleZ survey at 0.3 < z < 1.0: analogues of Lyman break galaxies?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution\n galaxies: formation\n galaxies: stellar content", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 February 18. In original form 2013 February 12. Received 2012 December 4. First published online: March 20, 2013. We thank the anonymous referee for a constructive report that has helped improve this paper. MB acknowledges Paul Hewett and Richard McMahon for many constructive discussions and Claudia Maraston and Joel Brownstein for access to the BOSS LRG stellar masses. MB wishes to acknowledge financial support from the STFC through grants held both at the Institute of Astronomy, Cambridge, and University College London. We acknowledge financial support from the Australian Research Council (grants DP1093738, DP0772084, LX0881951, LE0668442), Swinburne University of\nTechnology, the University of Queensland and the Anglo-Australian Observatory for the WiggleZ survey. The WiggleZ survey would not be possible without the dedicated work of the staff of the Australian Astronomical Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT. KG also acknowledges support from Australian Research Council grant DP1094370 for galaxy evolution studies. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASAs support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National\ndEtudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - MNRAS-2013-Banerji-2209-29.pdf
Erratum - MNRAS-2015-Banerji-325.pdf
", "abstract": "We characterize the stellar masses and star formation rates in a sample of \u223c40 000 spectroscopically confirmed UV-luminous galaxies at 0.3 < z < 1.0 selected from within the WiggleZ Dark Energy Survey. In particular, we match this UV bright population to wide-field infrared surveys such as the near-infrared (NIR) UKIDSS Large Area Survey (LAS) and the mid-infrared Wide-Field Infrared Survey Explorer (WISE) All-Sky Survey. We find that \u223c30 per cent of the UV-luminous WiggleZ galaxies, corresponding to the brightest and reddest subset, are detected at >5\u03c3 in the UKIDSS-LAS at all redshifts. An even more luminous subset of 15 per cent are also detected in the WISE 3.4 and 4.6\u2009\u03bcm bands. In addition, 22 of the WiggleZ galaxies are extremely luminous at 12 and 22\u2009\u03bcm and have colours consistent with being star formation dominated. We compute stellar masses for this very large sample of extremely blue galaxies and quantify the sensitivity of the stellar mass estimates to various assumptions made during the spectral energy distribution (SED) fitting. The median stellar masses are log10(M_*/M_\u2299) = 9.6 \u00b1 0.7, 10.2 \u00b1 0.5 and 10.4 \u00b1 0.4 for the IR undetected, UKIDSS detected and UKIDSS+WISE detected galaxies, respectively. We demonstrate that the inclusion of NIR photometry can lead to tighter constraints on the stellar masses by bringing down the upper bound on the stellar mass estimate. The mass estimates are found to be most sensitive to the inclusion of secondary bursts of star formation as well as changes in the stellar population synthesis models, both of which can lead to median discrepancies of the order of 0.3\u2009dex in the stellar masses. We conclude that even for these extremely blue galaxies, different SED fitting codes therefore produce extremely robust stellar mass estimates. We find, however, that the best-fitting M/L_K is significantly lower than that predicted by simple optical colour-based estimators for many of the WiggleZ galaxies. The simple colour-based estimator overpredicts M/L_K by \u223c0.4\u2009dex on average. The effect is more pronounced for bluer galaxies with younger best-fitting ages. The WiggleZ galaxies have star formation rates of 3\u201310 M_\u2299 yr^(\u22121) and mostly lie at the upper end of the main sequence of star-forming galaxies at these redshifts. Their rest-frame UV luminosities and stellar masses are comparable to both local compact UV-luminous galaxies as well as Lyman break galaxies at z \u223c 2\u20133. The stellar masses from this paper will be made publicly available with the next WiggleZ data release.", "date": "2013-05-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "431", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2209-2229", "id_number": "CaltechAUTHORS:20130612-145312186", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-145312186", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Australian Research Council", "grant_number": "DP1093738" }, { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "LX0881951" }, { "agency": "Australian Research Council", "grant_number": "LE0668442" }, { "agency": "Swinburne University of Technology" }, { "agency": "University of Queensland" }, { "agency": "Anglo-Australian Observatory" }, { "agency": "Australian Research Council", "grant_number": "DP1094370" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/stt320", "primary_object": { "basename": "MNRAS-2013-Banerji-2209-29.pdf", "url": "https://authors.library.caltech.edu/records/9s9qh-cyk96/files/MNRAS-2013-Banerji-2209-29.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Banerji-325.pdf", "url": "https://authors.library.caltech.edu/records/9s9qh-cyk96/files/MNRAS-2015-Banerji-325.pdf" } ], "pub_year": "2013", "author_list": "Banerji, Manda; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/37n90-87b86", "eprint_id": 38936, "eprint_status": "archive", "datestamp": "2023-08-19 19:15:45", "lastmod": "2023-10-24 14:52:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Contreras-C", "name": { "family": "Contreras", "given": "Carlos" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: measuring the cosmic growth rate with the two-point galaxy correlation function", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys\n cosmological parameters\n large-scale structure of Universe", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: February 7, 2013. We acknowledge financial support from the Australian Research Council through Discovery Project grants which have funded the positions of MP, GP, TD and FM. SMC acknowledges the support of the Australian Research Council through a QEII Fellowship. MJD and TD thank the Gregg Thompson Dark Energy Travel Fund for financial support. CC thanks David Parkinson for sharing his expertise on MCMC techniques, and Ana Mar\u00eda Mart\u00ednez for her invaluable feedback and support in the building of this paper. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation and science analysis for the GALEX mission, developed in co-operation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Finally, the WiggleZ survey would not have been possible without the dedicated work of the staff of the Australian Astronomical Observatory in the development and support of the AAOmega spectrograph,\nand the running of the AAT. This research was supported by CAASTRO: http://caastro.org.\n\nPublished - MNRAS-2013-Contreras-924-33.pdf
", "abstract": "The growth history of large-scale structure in the Universe is a powerful probe of the cosmological model, including the nature of dark energy. We study the growth rate of cosmic structure to redshift z = 0.9 using more than 162\u2009000 galaxy redshifts from the WiggleZ Dark Energy Survey. We divide the data into four redshift slices with effective redshifts z = [0.2, 0.4, 0.6, 0.76] and in each of the samples measure and model the two-point galaxy correlation function in parallel and transverse directions to the line of sight. After simultaneously fitting for the galaxy bias factor we recover values for the cosmic growth rate which are consistent with our assumed \u039bcold dark matter (\u039bCDM) input cosmological model, with an accuracy of around 20 per cent in each redshift slice. We investigate the sensitivity of our results to the details of the assumed model and the range of physical scales fitted, making close comparison with a set of N-body simulations for calibration. Our measurements are consistent with an independent power-spectrum analysis of a similar data set, demonstrating that the results are not driven by systematic errors. We determine the pairwise velocity dispersion of the sample in a non-parametric manner, showing that it systematically increases with decreasing redshift, and investigate the Alcock\u2013Paczynski effects of changing the assumed fiducial model on the results. Our techniques should prove useful for current and future galaxy surveys mapping the growth rate of structure using the two-dimensional correlation function.", "date": "2013-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "430", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "924-933", "id_number": "CaltechAUTHORS:20130613-091253896", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130613-091253896", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council Discovery Project grants" }, { "agency": "Australian Research Council QEII Fellowship" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" }, { "agency": "NASA" }, { "agency": "CAASTRO" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/sts608", "primary_object": { "basename": "MNRAS-2013-Contreras-924-33.pdf", "url": "https://authors.library.caltech.edu/records/37n90-87b86/files/MNRAS-2013-Contreras-924-33.pdf" }, "pub_year": "2013", "author_list": "Contreras, Carlos; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/cy6pk-13941", "eprint_id": 37905, "eprint_status": "archive", "datestamp": "2023-08-22 08:56:41", "lastmod": "2023-10-23 19:31:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Huber-M-E", "name": { "family": "Huber", "given": "M." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "L." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S. G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } }, { "id": "Burgett-W-S", "name": { "family": "Burgett", "given": "W. S." } }, { "id": "Chambers-K-C", "name": { "family": "Chambers", "given": "K. C." }, "orcid": "0000-0001-6965-7789" }, { "id": "Kaiser-N", "name": { "family": "Kaiser", "given": "N." }, "orcid": "0000-0001-6511-4306" }, { "id": "Magnier-E-A", "name": { "family": "Magnier", "given": "E. A." }, "orcid": "0000-0002-7965-2815" }, { "id": "Price-P-A", "name": { "family": "Price", "given": "P. A." } }, { "id": "Tonry-J-L", "name": { "family": "Tonry", "given": "J. L." }, "orcid": "0000-0003-2858-9657" } ] }, "title": "The GALEX Time Domain Survey. I. Selection and Classification of Over a Thousand Ultraviolet Variable Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; ultraviolet: general", "note": "\u00a9 2013 American Astronomical Society. Received 2012 November 19; accepted 2013 February 1; published 2013 March 7. We thank the anonymous referee for their constructive comments which improved the paper. GALEX (Galaxy Evolution\nExplorer) is a NASA Small Explorer, launched in 2003\nApril. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The Pan-STARRS1 survey has 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 institutes, 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 National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate.\n\nPublished - 0004-637X_766_1_60.pdf
", "abstract": "We present the selection and classification of over a thousand ultraviolet (UV) variable sources discovered in\n\u223c40 deg^2 of GALEX Time Domain Survey (TDS) NUV images observed with a cadence of 2 days and a baseline\nof observations of \u223c3 years. The GALEX TDS fields were designed to be in spatial and temporal coordination with\nthe Pan-STARRS1 Medium Deep Survey, which provides deep optical imaging and simultaneous optical transient\ndetections via image differencing.We characterize the GALEX photometric errors empirically as a function of mean\nmagnitude, and select sources that vary at the 5\u03c3 level in at least one epoch. We measure the statistical properties\nof the UV variability, including the structure function on timescales of days and years. We report classifications for\nthe GALEX TDS sample using a combination of optical host colors and morphology, UV light curve characteristics,\nand matches to archival X-ray, and spectroscopy catalogs. We classify 62% of the sources as active galaxies (358\nquasars and 305 active galactic nuclei), and 10% as variable stars (including 37 RR Lyrae, 53 M dwarf flare stars, and 2 cataclysmic variables). We detect a large-amplitude tail in the UV variability distribution for M-dwarf flare stars and RR Lyrae, reaching up to |\u0394m| = 4.6 mag and 2.9 mag, respectively. The mean amplitude of the structure function for quasars on year timescales is five times larger than observed at optical wavelengths. The remaining unclassified sources include UV-bright extragalactic transients, two of which have been spectroscopically confirmed to be a young core-collapse supernova and a flare from the tidal disruption of a star by dormant supermassive black hole. We calculate a surface density for variable sources in the UV with NUV < 23 mag and |\u0394m| > 0.2 mag of \u223c8.0, 7.7, and 1.8 deg^(\u22122) for quasars, active galactic nuclei, and RR Lyrae stars, respectively. We also calculate a surface density rate in the UV for transient sources, using the effective survey time at the cadence appropriate to each class, of \u223c15 and 52 deg^(\u22122) yr^(\u22121) for M dwarfs and extragalactic transients, respectively.", "date": "2013-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "766", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 60", "id_number": "CaltechAUTHORS:20130412-100925592", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130412-100925592", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AR22G" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/766/1/60", "primary_object": { "basename": "0004-637X_766_1_60.pdf", "url": "https://authors.library.caltech.edu/records/cy6pk-13941/files/0004-637X_766_1_60.pdf" }, "pub_year": "2013", "author_list": "Gezari, S.; Martin, D. C.; et el." }, { "id": "https://authors.library.caltech.edu/records/26mnw-hb118", "eprint_id": 39074, "eprint_status": "archive", "datestamp": "2023-08-19 18:57:00", "lastmod": "2023-10-24 16:22:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Poole-G-B", "name": { "family": "Poole", "given": "Gregory B." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: probing the epoch of radiation\n domination using large-scale structure", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys\n cosmological parameters\n large-scale structure of Universe", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: January 4, 2013. Accepted 2012 November 16. Received 2012 November 16; in original form 2012 August 31. We thank Francesco Montesano for his constructive and insightful examination of our manuscript. We acknowledge financial support from the Australian Research Council through Discovery Project grants DP0772084 and DP1093738 and Linkage International travel grant LX0881951. GBP thanks Simon Mutch for his help with developing the MCMC code used for the analysis in this study. CB acknowledges\nthe support of the Australian Research Council through\nthe award of a Future Fellowship. SC and DJC acknowledge the support of Australian Research Council QEII Fellowships. MJD and TD thank the Gregg Thompson Dark Energy Travel Fund for financial support. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge\nNASA\u00d5's support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology.We thank the Anglo-Australian Telescope\nAllocation Committee for supporting theWiggleZ survey over nine\nsemesters, and we are very grateful for the dedicated work of the\nstaff of the Australian Astronomical Observatory in the development\nand support of the AAOmega spectrograph, and the running\nof the Anglo-Australian Telescope.We are also grateful for support from the Centre for All-sky Astrophysics, an Australian Research\nCouncil Centre of Excellence funded by grant CE11000102.\n\nPublished - MNRAS-2013-Poole-1902-12.pdf
", "abstract": "We place the most robust constraint to date on the scale of the turnover in the cosmological matter power spectrum using data from the WiggleZ Dark Energy Survey. We find this feature to lie at a scale of k_0 = 0.0160^(+ 0.0035)_(\u2212 0.0041) (h Mpc^\u22121) (68 per cent confidence) for an effective redshift of z_(eff) = 0.62 and obtain from this the first ever turnover-derived distance and cosmology constraints: a measure of the cosmic distance\u2013redshift relation in units of the horizon scale at the redshift of radiation\u2013matter equality (r_H) of D_V(z_(eff) = 0.62)/r_H = 18.3^(+6.3)_(\u22123.3) and, assuming a prior on the number of extra relativistic degrees of freedom N_(eff) = 3, constraints on the cosmological matter density parameter \u03a9_M\u2009h^2 = 0.136^(+0.026)_(\u22120.052) and on the redshift of matter\u2013radiation equality z_(eq) = 3274^(+631)_(\u22121260). We stress that these results are obtained within the theoretical framework of Gaussian primordial fluctuations and linear large-scale bias. With this caveat, all results are in excellent agreement with the predictions of standard \u039bCDM models. Our constraints on the logarithmic slope of the power spectrum on scales larger than the turnover are bounded in the lower limit with values only as low as \u22121 allowed, with the prediction of P(k) \u221d k from standard \u039bCDM models easily accommodated by our results. Finally, we generate forecasts to estimate the achievable precision of future surveys at constraining k_0, \u03a9_M\u2009h^2, z_(eq) and N_(eff). We find that the Baryon Oscillation Spectroscopic Survey should substantially improve upon the WiggleZ turnover constraint, reaching a precision on k_0 of \u00b19 per cent (68 per cent confidence), translating to precisions on \u03a9_M\u2009h^2 and z_(eq) of \u00b110 per cent (assuming a prior N_(eff) = 3) and on Neff of + 78\u2212 56 per cent (assuming a prior \u03a9_M\u2009h^2 = 0.135). This represents sufficient precision to sharpen the constraints on N_(eff) from WMAP, particularly in its upper limit. For Euclid, we find corresponding attainable precisions on (k_0, \u03a9_M\u2009h^2,\u2009N_(eff)) of (3, 4,^(+ 17)_(\u2212 21)) per cent. This represents a precision approaching our forecasts for the Planck Surveyor.", "date": "2013-03-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "429", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1902-1912", "id_number": "CaltechAUTHORS:20130625-101556024", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130625-101556024", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council Discovery Project", "grant_number": "DP0772084" }, { "agency": "Australian Research Council Discovery Project", "grant_number": "DP1093738" }, { "agency": "Linkage International Travel Grant", "grant_number": "LX0881951" }, { "agency": "Australian Research Council Future Fellowship" }, { "agency": "Australian Research Council QEII Fellowships" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" }, { "agency": "Australian Research Council Centre of Excellence", "grant_number": "CE110001020" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/sts431", "primary_object": { "basename": "MNRAS-2013-Poole-1902-12.pdf", "url": "https://authors.library.caltech.edu/records/26mnw-hb118/files/MNRAS-2013-Poole-1902-12.pdf" }, "pub_year": "2013", "author_list": "Poole, Gregory B.; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/2np38-st973", "eprint_id": 76851, "eprint_status": "archive", "datestamp": "2023-08-19 14:24:42", "lastmod": "2023-10-25 16:55:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Krause-E", "name": { "family": "Krause", "given": "Elisabeth" } }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "Halo occupation distribution modelling of green valley galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 large-scale structure of Universe", "note": "\u00a9 2012 The Authors.\nPublished by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2012 October 15. Received 2012 October 16; in original form 2012 August 30\n\nWe thank David Weinberg and Zheng Zheng for helpful discussions about HOD modelling of binned samples.\n\nDuring the preparation of this work, EK and CMH were supported by the US National Science Foundation (AST-0807337) and the David & Lucile Packard Foundation. CH was additionally supported by the US Department of Energy (DE-SC0006624). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/.\n\nThe SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.\n\nPublished - sts221.pdf
", "abstract": "We present a clustering analysis of near-ultraviolet (NUV)\u2013optical colour selected luminosity bin samples of green valley galaxies. These galaxy samples are constructed by matching the Sloan Digital Sky Survey Data Release 7 with the latest Galaxy Evolution Explorer source catalogue which provides NUV photometry. We present cross-correlation function measurements and determine the halo occupation distribution of green valley galaxies using a new multiple tracer analysis technique.\nWe extend the halo occupation formalism, which describes the relation between galaxies and halo mass in terms of the probability P(N, Mh) that a halo of given mass Mh contains N galaxies, to model the cross-correlation function between a galaxy sample of interest and multiple tracer populations simultaneously. This method can be applied to commonly used luminosity threshold samples as well as to colour and luminosity bin selected galaxy samples, and improves the accuracy of clustering analyses for sparse galaxy populations.\nWe confirm the previously observed trend that red galaxies reside in more massive haloes and are more likely to be satellite galaxies than average galaxies of similar luminosity. While the change in central galaxy host mass as a function of colour is only weakly constrained, the satellite fraction and characteristic halo masses of green satellite galaxies are found to be intermediate between those of blue and red satellite galaxies.", "date": "2013-01-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "428", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2548-2564", "id_number": "CaltechAUTHORS:20170424-111909219", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170424-111909219", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0807337" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0006624" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NASA" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1093/mnras/sts221", "primary_object": { "basename": "sts221.pdf", "url": "https://authors.library.caltech.edu/records/2np38-st973/files/sts221.pdf" }, "pub_year": "2013", "author_list": "Krause, Elisabeth; Hirata, Christopher M.; et el." }, { "id": "https://authors.library.caltech.edu/records/vkj8x-hp913", "eprint_id": 36371, "eprint_status": "archive", "datestamp": "2023-08-22 08:03:35", "lastmod": "2023-10-20 23:05:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Tsai-Chao-Wei", "name": { "family": "Tsai", "given": "C. W." }, "orcid": "0000-0002-9390-9672" }, { "id": "Petty-Sara-M", "name": { "family": "Petty", "given": "S." }, "orcid": "0000-0003-0624-3276" }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "M. E." }, "orcid": "0000-0002-9871-6490" }, { "id": "Assef-R-J", "name": { "family": "Assef", "given": "Roberto J." }, "orcid": "0000-0002-9508-3667" }, { "id": "Benford-D-J", "name": { "family": "Benford", "given": "D. J." }, "orcid": "0000-0002-9884-4206" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C." } }, { "id": "Donoso-E", "name": { "family": "Donoso", "given": "E." } }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "P." } }, { "id": "Koribalski-B-S", "name": { "family": "Koribalski", "given": "B." } }, { "id": "Lake-S", "name": { "family": "Lake", "given": "S." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Stanford-S-A", "name": { "family": "Stanford", "given": "S. Adam" } }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "E." }, "orcid": "0000-0001-5058-1593" } ] }, "title": "Extending the Nearby Galaxy Heritage with WISE: First Results from the WISE Enhanced Resolution Galaxy Atlas", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters; galaxies: statistics; infrared: galaxies; surveys; techniques: image processing", "note": "\u00a9 2013 American Astronomical Society. Received 2012 March 26; accepted 2012 September 30; published 2012 November 30.\nWe thank G. Meurer, S. Lord, J. Mazzarella, and B. Madore\nfor tapping their vast knowledge base of nearby galaxies. Discussions with S. Meidt and N. Taylor were very helpful in understanding the (ongoing) difficulties with M/L modeling. This work is based (in part) on observations made with the Spitzer and research using the NASA/IPAC Extragalactic Database (NED) and IPAC Infrared Science Archive, all of which are operated by JPL, Caltech under a contract with the National Aeronautics and Space Administration. Support for this work was provided by\nNASA through an award issued by JPL/Caltech. R.J.A.was supported by an appointment to the NASA Postdoctoral Program\nat the Jet Propulsion Laboratory, administered by Oak Ridge\nAssociated Universities through a contract with NASA. M.E.C.\nacknowledges support from the Australian Research Council\n(FS110200023). This publication makes use of data products\nfrom 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\nPublished - 1538-3881_145_1_6.pdf
", "abstract": "The Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at mid-infrared wavelengths 3.4 \u03bcm, 4.6 \u03bcm, 12 \u03bcm, and 22 \u03bcm. The mission was primarily designed to extract point sources, leaving resolved and extended sources, for the most part, unexplored. Accordingly, we have begun a dedicated WISE Enhanced Resolution Galaxy Atlas (WERGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we demonstrate the first results of the WERGA project for a sample of 17 galaxies, chosen to be of large angular size, diverse morphology, and covering a range in color, stellar mass, and star formation. It includes many well-studied galaxies, such as M 51, M 81, M 87, M 83, M 101, and IC 342. Photometry and surface brightness decomposition is carried out after special super-resolution processing, achieving spatial resolutions similar to that of Spitzer Infrared Array Camera. The enhanced resolution method is summarized in the first paper of this two-part series. In this second work, we present WISE, Spitzer, and Galaxy Evolution Explorer (GALEX) photometric and characterization measurements for the sample galaxies, combining the measurements to study the global properties. We derive star formation rates using the polycyclic aromatic hydrocarbon sensitive 12 \u03bcm (W3) fluxes, warm-dust sensitive 22 \u03bcm (W4) fluxes, and young massive-star sensitive ultraviolet (UV) fluxes. Stellar masses are estimated using the 3.4 \u03bcm (W1) and 4.6 \u03bcm (W2) measurements that trace the dominant stellar mass content. We highlight and showcase the detailed results of M 83, comparing the WISE/Spitzer results with the Australia Telescope Compact Array H I gas distribution and GALEX UV emission, tracing the evolution from gas to stars. In addition to the enhanced images, WISE's all-sky coverage provides a tremendous advantage over Spitzer for building a complete nearby galaxy catalog, tracing both stellar mass and star formation histories. We discuss the construction of a complete mid-infrared catalog of galaxies and its complementary role of studying the assembly and evolution of galaxies in the local universe.", "date": "2013-01", "date_type": "published", "publication": "Astronomical Journal", "volume": "145", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 6", "id_number": "CaltechAUTHORS:20130115-090532935", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-090532935", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "Australian Research Council", "grant_number": "FS110200023" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-6256/145/1/6", "primary_object": { "basename": "1538-3881_145_1_6.pdf", "url": "https://authors.library.caltech.edu/records/vkj8x-hp913/files/1538-3881_145_1_6.pdf" }, "pub_year": "2013", "author_list": "Jarrett, T. H.; Masci, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/s6fk1-zff26", "eprint_id": 36337, "eprint_status": "archive", "datestamp": "2023-08-19 13:31:18", "lastmod": "2023-10-20 23:01:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Parkinson-D", "name": { "family": "Parkinson", "given": "David" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: Final data release and cosmological results", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Physical Society.\n\nReceived 31 August 2012; published 16 November 2012.\n\nD. P. thanks Antony Lewis, Andrew Liddle and Beth Reid\nfor helpful discussions. We acknowledge financial support\nfrom the Australian Research Council through Discovery\nProject Grants No. DP0772084 and No. DP1093738, funding\nthe positions of S. B., D. P., M. P., G. P. and T.M. D., and\nLinkage International travel Grant No. LX0881951. D.C.\nand S.C. acknowledge the support of an Australian\nResearch Council through QEII Fellowships. M. J.D. and\nT. M.D. thank the Gregg Thompson Dark Energy Travel\nFund for financial support. GALEX (the Galaxy Evolution\nExplorer) is a NASA Small Explorer, launched in 2003\nApril. We gratefully acknowledge NASAs support for\nconstruction, operation and science analysis for the\nGALEX mission, developed in cooperation with the\nCentre National dEtudes Spatiales of France and the\nKorean Ministry of Science and Technology. Finally,\nwe thank the Anglo-Australian Telescope Allocation\nCommittee for supporting the WiggleZ survey over nine\nsemesters, and we are very grateful for the dedicated work\nof the staff of the Australian Astronomical Observatory in\nthe development and support of the AAOmega spectrograph,\nand the running of the AAT.\n\nPublished - PhysRevD.86.103518.pdf
", "abstract": "This paper presents cosmological results from the final data release of the WiggleZ Dark Energy Survey. We perform full analyses of different cosmological models using the WiggleZ power spectra measured at z=0.22, 0.41, 0.60, and 0.78, combined with other cosmological data sets. The limiting factor in this analysis is the theoretical modeling of the galaxy power spectrum, including nonlinearities, galaxy bias, and redshift-space distortions. In this paper we assess several different methods for modeling the theoretical power spectrum, testing them against the Gigaparsec WiggleZ simulations (GiggleZ). We fit for a base set of six cosmological parameters, {\u03a9_(b)h^2,\u03a9_(CDM)h^2,H_0,\u03c4,A_s,n_s}, and five supplementary parameters {n_(run),r,w,\u03a9_k,\u2211m_\u03bd}. In combination with the cosmic microwave background, our results are consistent with the \u039bCDM concordance cosmology, with a measurement of the matter density of \u03a9m=0.29\u00b10.016 and amplitude of fluctuations \u03c3_8=0.825\u00b10.017. Using WiggleZ data with cosmic microwave background and other distance and matter power spectra data, we find no evidence for any of the extension parameters being inconsistent with their \u039bCDM model values. The power spectra data and theoretical modeling tools are available for use as a module for CosmoMC, which we here make publicly available at http://smp.uq.edu.au/wigglez-data. We also release the data and random catalogs used to construct the baryon acoustic oscillation correlation function.", "date": "2012-11-16", "date_type": "published", "publication": "Physical Review D", "volume": "86", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 103518", "id_number": "CaltechAUTHORS:20130111-161415492", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130111-161415492", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "DP1093738" }, { "agency": "Linkage International travel Grant", "grant_number": "LX0881951" }, { "agency": "Australian Research Council QEII Fellowship" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1103/PhysRevD.86.103518", "primary_object": { "basename": "PhysRevD.86.103518.pdf", "url": "https://authors.library.caltech.edu/records/s6fk1-zff26/files/PhysRevD.86.103518.pdf" }, "pub_year": "2012", "author_list": "Parkinson, David; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/xqg3r-fk809", "eprint_id": 36020, "eprint_status": "archive", "datestamp": "2023-08-22 07:42:44", "lastmod": "2023-10-20 22:08:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Men\u00e9ndez-Delmestre-K", "name": { "family": "Men\u00e9ndez-Delmestre", "given": "Kar\u00edn" }, "orcid": "0000-0003-3153-5123" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" } ] }, "title": "Quenching Star Formation at Intermediate Redshifts: Downsizing of the Mass Flux Density in the Green Valley", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: luminosity function, mass function", "note": "\u00a9 2012 American Astronomical Society. Received 2011 December 9; accepted 2012 September 14; published 2012 October 17. We thank the anonymous referee for comments that have significantly improved this paper, with special attention to the luminosity functions and co-added spectra. T.S.G. thanks Samir Salim for useful comments and suggestions. Some of the data presented here 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 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. This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT,MMT, Subaru, Palomar, Spitzer, VLA, and other telescopes and supported in part by the NSF, NASA, and the STFC. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of\nFrance, and the University of Hawaii. This work is based in\npart on data products produced at TERAPIX and the Canadian\nAstronomy Data Centre as part of the Canada\u2013France\u2013Hawaii\nTelescope Legacy Survey, a collaborative project of NRC and\nCNRS.\n\nPublished - 0004-637X_759_1_67.pdf
", "abstract": "The bimodality in galaxy properties has been observed at low and high redshifts, with a clear distinction between star-forming galaxies in the blue cloud and passively evolving objects in the red sequence; the absence of galaxies with intermediate properties indicates that the quenching of star formation and subsequent transition between populations must happen rapidly. In this paper, we present a study of over 100 transiting galaxies in the so-called green valley at intermediate redshifts (z ~ 0.8). By using very deep spectroscopy with the DEIMOS instrument at the Keck telescope we are able to infer the star formation histories of these objects and measure the stellar mass flux density transiting from the blue cloud to the red sequence when the universe was half its current age. Our results indicate that the process happened more rapidly and for more massive galaxies in the past, suggesting a top-down scenario in which the massive end of the red sequence is forming first. This represents another aspect of downsizing, with the mass flux density moving toward smaller galaxies in recent times.", "date": "2012-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "759", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 67", "id_number": "CaltechAUTHORS:20121218-080817415", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121218-080817415", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF" }, { "agency": "NASA" }, { "agency": "STFC" }, { "agency": "NSF", "grant_number": "AST-0071048" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/759/1/67", "primary_object": { "basename": "0004-637X_759_1_67.pdf", "url": "https://authors.library.caltech.edu/records/xqg3r-fk809/files/0004-637X_759_1_67.pdf" }, "pub_year": "2012", "author_list": "Gon\u00e7alves, Thiago S.; Martin, D. Christopher; et el." }, { "id": "https://authors.library.caltech.edu/records/nwb92-mpw64", "eprint_id": 35892, "eprint_status": "archive", "datestamp": "2023-08-22 07:11:39", "lastmod": "2023-10-20 21:53:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael M." } }, { "id": "Doyle-T-F", "name": { "family": "Mizusawa", "given": "Trisha" }, "orcid": "0000-0001-7182-5307" }, { "id": "Wehinger-P", "name": { "family": "Wehinger", "given": "Peter" } }, { "id": "Zurek-David", "name": { "family": "Zurek", "given": "David" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher D." }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" } ] }, "title": "AT Cnc: A Second Dwarf Nova with a Classical Nova Shell", "ispublished": "pub", "full_text_status": "public", "keywords": "novae, cataclysmic variables; stars: individual (AT Cancri)", "note": "\u00a9 2012 American Astronomical Society. Received 2012 July 31; accepted 2012 August 23; published 2012 October 8. Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis\nfor the GALEX mission. M.M.S. gratefully acknowledges helpful conversations about AT Cnc and dwarf nova shells with Howard Bond and Christian Knigge.\n\nPublished - 0004-637X_758_2_121.pdf
", "abstract": "We are systematically surveying all known and suspected Z Cam-type dwarf novae for classical nova shells. This survey is motivated by the discovery of the largest known classical nova shell, which surrounds the archetypal dwarf nova Z Camelopardalis. The Z Cam shell demonstrates that at least some dwarf novae must have undergone classical nova eruptions in the past, and that at least some classical novae become dwarf novae long after their nova thermonuclear outbursts, in accord with the hibernation scenario of cataclysmic binaries. Here we report the detection of a fragmented \"shell,\" 3 arcmin in diameter, surrounding the dwarf nova AT Cancri. This second discovery demonstrates that nova shells surrounding Z Cam-type dwarf novae cannot be very rare. The shell geometry is suggestive of bipolar, conical ejection seen nearly pole-on. A spectrum of the brightest AT Cnc shell knot is similar to that of the ejecta of the classical nova GK Per, and of Z Cam, dominated by [N II] emission. Galaxy Evolution Explorer FUV imagery reveals a similar-sized, FUV-emitting shell. We determine a distance of 460 pc to AT Cnc, and an upper limit to its ejecta mass of ~5 \u00d7 10^(\u20135) M_\u2609, typical of classical novae.", "date": "2012-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "758", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 121", "id_number": "CaltechAUTHORS:20121210-100445844", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121210-100445844", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/758/2/121", "primary_object": { "basename": "0004-637X_758_2_121.pdf", "url": "https://authors.library.caltech.edu/records/nwb92-mpw64/files/0004-637X_758_2_121.pdf" }, "pub_year": "2012", "author_list": "Shara, Michael M.; Mizusawa, Trisha; et el." }, { "id": "https://authors.library.caltech.edu/records/eeycs-46m77", "eprint_id": 64610, "eprint_status": "archive", "datestamp": "2023-08-19 12:54:12", "lastmod": "2024-01-13 16:40:56", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Greer-F", "name": { "family": "Greer", "given": "Frank" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "UV photon-counting CCD detectors that enable the next generation of UV spectroscopy missions: AR coatings that can achieve 80-90% QE", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe authors wish to thank Mike Lee of JPL for his assistance with ALD processes. The research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work was partially supported by KISS, the W. M. Keck Institute for Space Studies, and by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, NASA Grant NX11AO07H, and NASA Grant NNX12AF29G.\n\nPublished - UV_photon.pdf
", "abstract": "We describe recent progress in the development of anti-reflection coatings for use at UV wavelengths on CCDs and other Si-based detectors. We have previously demonstrated a set of coatings which are able to achieve greater than 50% QE in 4 bands from 130nm to greater than 300nm. We now present new refinements of these AR-coatings which will improve performance in a narrower bandpass by 50% over previous work. Successful test films have been made to optimize transmission at 190nm, reaching 80% potential transmission.", "date": "2012-09-25", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 845309", "id_number": "CaltechAUTHORS:20160219-142226920", "isbn": "9780819491541", "book_title": "High Energy, Optical, and Infrared Detectors for Astronomy V", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160219-142226920", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NASA", "grant_number": "NNX11AO07H" }, { "agency": "NASA", "grant_number": "NNX12AF29G" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Holland-A-D", "name": { "family": "Holland", "given": "Andrew D." } }, { "id": "Beletic-J-W", "name": { "family": "Beletic", "given": "James W." } } ] }, "doi": "10.1117/12.927208", "primary_object": { "basename": "UV_photon.pdf", "url": "https://authors.library.caltech.edu/records/eeycs-46m77/files/UV_photon.pdf" }, "pub_year": "2012", "author_list": "Hamden, Erika T.; Greer, Frank; et el." }, { "id": "https://authors.library.caltech.edu/records/sajjk-3r572", "eprint_id": 37748, "eprint_status": "archive", "datestamp": "2023-08-19 12:51:45", "lastmod": "2024-01-13 06:00:16", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Chris" }, "orcid": "0000-0002-8650-1644" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Adkins-S-M", "name": { "family": "Adkins", "given": "Sean" } }, { "id": "Epps-H-W", "name": { "family": "Epps", "given": "Harland" } }, { "id": "Bartos-R", "name": { "family": "Bartos", "given": "Randy" } }, { "id": "Cabak-J", "name": { "family": "Cabak", "given": "Jerry" } }, { "id": "Cowley-D", "name": { "family": "Cowley", "given": "Dave" } }, { "id": "Davis-J", "name": { "family": "Davis", "given": "Jack" } }, { "id": "Delacroix-A", "name": { "family": "Delacroix", "given": "Alex" } }, { "id": "Fucik-J", "name": { "family": "Fucik", "given": "Jason" } }, { "id": "Hilliard-D", "name": { "family": "Hilliard", "given": "David" } }, { "id": "James-E", "name": { "family": "James", "given": "Ean" } }, { "id": "Kaye-S", "name": { "family": "Kaye", "given": "Steve" } }, { "id": "Lingner-N", "name": { "family": "Lingner", "given": "Nicole" } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Pistor-C", "name": { "family": "Pistor", "given": "Christoph" } }, { "id": "Phillips-D", "name": { "family": "Phillips", "given": "Drew" } }, { "id": "Rockosi-C", "name": { "family": "Rockosi", "given": "Connie" } }, { "id": "Weber-B", "name": { "family": "Weber", "given": "Bob" } } ] }, "title": "The Keck Cosmic Web Imager: a capable new integral field spectrograph for the W. M. Keck Observatory", "ispublished": "unpub", "full_text_status": "public", "keywords": "Integral Field Spectrograph Keck Observatory KCWI", "note": "\u00a9 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThis material is based upon work supported by AURA through the National Science Foundation under Scientific Program Order No. 5 as issued for support of the Telescope Systems Instrumentation Program (TSIP), in accordance with Proposal No. AST-0335461 submitted by AURA. We also acknowledge and thank the Caltech Optical Observatories for continued support of both CWI and KCWI.\n\nPublished - 844613.pdf
", "abstract": "The Keck Cosmic Web Imager (KCWI) is a new facility instrument being developed for the W. M. Keck Observatory and funded for construction by the Telescope System Instrumentation Program (TSIP) of the National Science Foundation (NSF). KCWI is a bench-mounted spectrograph for the Keck II right Nasmyth focal station, providing integral field spectroscopy over a seeing-limited field up to 20\"x33\" in extent. Selectable Volume Phase Holographic (VPH) gratings provide high efficiency and spectral resolution in the range of 1000 to 20000. The dual-beam design of KCWI passed a Preliminary Design Review in summer 2011. The detailed design of the KCWI blue channel (350 to 700 nm) is now nearly complete, with the red channel (530 to 1050 nm) planned for a phased implementation contingent upon additional funding. KCWI builds on the experience of the Caltech team in implementing the Cosmic Web Imager (CWI), in operation since 2009 at Palomar Observatory. KCWI adds considerable flexibility to the CWI design, and will take full advantage of the excellent seeing and dark sky above Mauna Kea with a selectable nod-and-shuffle observing mode. In this paper, models of the expected KCWI sensitivity and background subtraction capability are presented, along with a detailed description of the instrument design. The KCWI team is lead by Caltech (project management, design and implementation) in partnership with the University of California at Santa Cruz (camera optical and mechanical design) and the W. M. Keck Observatory (program oversight and observatory interfaces).", "date": "2012-09-24", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 844613", "id_number": "CaltechAUTHORS:20130403-143938745", "isbn": "978-0-8194-9147-3", "book_title": "Ground-based and Airborne Instrumentation for Astronomy IV", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130403-143938745", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "NSF", "grant_number": "AST-0335461" }, { "agency": "Caltech Optical Observatories" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } }, { "id": "Ramsay-S-K", "name": { "family": "Ramsay", "given": "Suzanne K." } }, { "id": "Takami-Hideki", "name": { "family": "Takami", "given": "Hideki" } } ] }, "doi": "10.1117/12.924729", "primary_object": { "basename": "844613.pdf", "url": "https://authors.library.caltech.edu/records/sajjk-3r572/files/844613.pdf" }, "pub_year": "2012", "author_list": "Morrissey, Patrick; Matuszewski, Mateusz; et el." }, { "id": "https://authors.library.caltech.edu/records/tbb7z-92v41", "eprint_id": 36590, "eprint_status": "archive", "datestamp": "2023-08-19 12:47:35", "lastmod": "2024-01-13 05:58:46", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna M." }, "orcid": "0000-0002-2894-6936" }, { "id": "Ahmed-S", "name": { "family": "Ahmed", "given": "Sara" } }, { "id": "Ashley-M-C-B", "name": { "family": "Ashley", "given": "Michael C. B." } }, { "id": "Croner-E", "name": { "family": "Croner", "given": "Ernest" } }, { "id": "Delacroix-A", "name": { "family": "Delacroix", "given": "Alex" } }, { "id": "Ebihara-Y", "name": { "family": "Ebihara", "given": "Yusuke" } }, { "id": "Fucik-J", "name": { "family": "Fucik", "given": "Jason" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Velur-V", "name": { "family": "Velur", "given": "Viswa" } }, { "id": "Weatherwax-A", "name": { "family": "Weatherwax", "given": "Allan" } } ] }, "title": "The Gattini South Pole UV Experiment", "ispublished": "unpub", "full_text_status": "public", "keywords": "Gattini, South Pole, Antarctic wide field surveys, cosmic web, site testing, cloud cover, aurora, night sky\nbrightness, UV astronomy", "note": "\u00a9 2012 SPIE. This research is financially supported by the US National Science Foundation, the United States Antarctic Program and Caltech Optical Observatories.\n\nPublished - 84441Q.pdf
", "abstract": "The Gattini South Pole UV experiment (Gattini SPUV) was deployed to the South Pole dark sector in February 2010 and has recently completed a highly successful first season of winter time observations. The experiment has, for the first time ever, measured and categorized the optical night sky brightness at the very blue wavelengths. The experiment consists of a remotely operated 6\" aperture custom designed telescope. The telescope feeds a blue sensitive imager with 4 degree field of view that contains a bank of 3 filters: SDSS g', Bessel U and a custom \"super U\" filter specifically designed to probe the sky emission at wavelengths approaching the atmospheric cut-off. The filters are continually cycled with exposure times ranging from 30 to 300 seconds throughout the winter period. The telescope, in addition, feeds a 2 degree long slit VPH grating spectrograph with R~1000. The bandwidth is 350-450nm. The spectra are recorded simultaneously with the imager exposures. The experiment is designed for low temperature Antarctic operation and resides on the roof of the MAPO building in the South Pole Antarctic sector. The primary science goals are to categorize the Antarctic winter-time sky background at the very bluest of wavelengths as a pathfinder for the Antarctic Cosmic Web Imager. We present a technical overview of the experiment and results from the first winter season.", "date": "2012-09-17", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 84441Q", "id_number": "CaltechAUTHORS:20130125-103057334", "isbn": "978-0-8194-9145-9", "book_title": "Ground-based and Airborne Telescopes IV", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130125-103057334", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "United States Antarctic Program" }, { "agency": "Caltech Optical Observatories" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Stepp-L-M", "name": { "family": "Stepp", "given": "Larry M." } }, { "id": "Gilmozzi-R", "name": { "family": "Gilmozzi", "given": "Roberto" } }, { "id": "Hall-H-J", "name": { "family": "Hall", "given": "Helen J." } } ] }, "doi": "10.1117/12.927313", "primary_object": { "basename": "84441Q.pdf", "url": "https://authors.library.caltech.edu/records/tbb7z-92v41/files/84441Q.pdf" }, "pub_year": "2012", "author_list": "Moore, Anna M.; Ahmed, Sara; et el." }, { "id": "https://authors.library.caltech.edu/records/ttzbf-3jg22", "eprint_id": 35305, "eprint_status": "archive", "datestamp": "2023-08-22 06:52:11", "lastmod": "2023-10-20 15:57:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael M." } }, { "id": "Doyle-T-F", "name": { "family": "Mizusawa", "given": "Trisha" }, "orcid": "0000-0001-7182-5307" }, { "id": "Zurek-David", "name": { "family": "Zurek", "given": "David" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher D." }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" } ] }, "title": "The Inter-eruption Timescale of Classical Novae from Expansion of the Z Camelopardalis Shell", "ispublished": "pub", "full_text_status": "public", "keywords": "novae, cataclysmic variables; stars: individual (Z Cam)", "note": "\u00a9 2012 American Astronomical Society. Received 2012 May 14; accepted 2012 July 9; published 2012 August 21. M.M.S. gratefully acknowledges helpful conversations with\nand suggestions from Lars Bildsten, David Kaplan, and Michael Bode.\n\nPublished - 0004-637X_756_2_107.pdf
", "abstract": "The dwarf nova Z Camelopardalis is surrounded by the largest known classical nova shell. This shell demonstrates that at least some dwarf novae must have undergone classical nova eruptions in the past, and that at least some classical novae become dwarf novae long after their nova thermonuclear outbursts. The current size of the shell, its known distance, and the largest observed nova ejection velocity set a lower limit to the time since Z Cam's last outburst of 220 years. The radius of the brightest part of Z Cam's shell is currently ~880 arcsec. No expansion of the radius of the brightest part of the ejecta was detected, with an upper limit of \u22640.17 arcsec yr^(\u20131). This suggests that the last Z Cam eruption occurred \u22655000 years ago. However, including the important effect of deceleration as the ejecta sweeps up interstellar matter in its snowplow phase reduces the lower limit to 1300 years. This is the first strong test of the prediction of nova thermonuclear runaway theory that the interoutburst times of classical novae are longer than 1000 years. The intriguing suggestion that Z Cam was a bright nova, recorded by Chinese imperial astrologers in October-November 77 B.C.E., is consistent with our measurements. If Z Cam was indeed the nova of 77 B.C.E. we predict that its ejecta are currently expanding at 85 km s^(\u20131), or 0.11 arcsec yr^(\u20131). Detection and measurement of this rate of expansion should be possible in just a few years.", "date": "2012-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "756", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20121106-120738783", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121106-120738783", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/756/2/107", "primary_object": { "basename": "0004-637X_756_2_107.pdf", "url": "https://authors.library.caltech.edu/records/ttzbf-3jg22/files/0004-637X_756_2_107.pdf" }, "pub_year": "2012", "author_list": "Shara, Michael M.; Mizusawa, Trisha; et el." }, { "id": "https://authors.library.caltech.edu/records/h84m8-na451", "eprint_id": 34519, "eprint_status": "archive", "datestamp": "2023-08-22 06:48:35", "lastmod": "2023-10-19 20:42:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blake-C", "name": { "family": "Blake", "given": "Chris" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: joint measurements of the expansion and growth history at z < 1", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; distance scale; large-scale structure of Universe", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS.\n\nAccepted 2012 June 7. Received 2012 May 25; in original form 2012 April 16.\nArticle first published online: 19 Jul. 2012.\nWe thank the anonymous referee for very useful feedback which greatly improved the presentation of this paper. CB acknowledges useful discussions with Eric Linder, Berian James, Eiichiro Komatsu, David Rapetti, Steve Allen, Eyal Kazin, Licia Verde and Raul Jimenez, and thanks the astronomy groups at Berkeley and Stanford for hospitality during the completion of this work. We acknowledge financial support from the Australian Research Council\nthrough Discovery Project grants DP0772084 and DP1093738\nand Linkage International travel grant LX0881951. SC and DC\nacknowledge the support of an Australian Research Council QEII Fellowship. We are also grateful for support from the Centre for All-sky Astrophysics, an Australian Research Council Centre of Excellence funded by grant CE11E0090.\n\nPublished - mnr21473.pdf
", "abstract": "We perform a joint determination of the distance\u2013redshift relation and cosmic expansion rate at redshifts z = 0.44, 0.6 and 0.73 by combining measurements of the baryon acoustic peak and Alcock\u2013Paczynski distortion from galaxy clustering in the WiggleZ Dark Energy Survey, using a large ensemble of mock catalogues to calculate the covariance between the measurements. We find that D_A(z) = (1205 \u00b1 114, 1380 \u00b1 95, 1534 \u00b1 107)\u2009Mpc and H(z) = (82.6 \u00b1 7.8, 87.9 \u00b1 6.1, 97.3 \u00b1 7.0)\u2009km\u2009s^(\u22121)\u2009Mpc^(\u22121) at these three redshifts. Further combining our results with other baryon acoustic oscillation and distant supernovae data sets, we use a Monte Carlo Markov Chain technique to determine the evolution of the Hubble parameter H(z) as a stepwise function in nine redshift bins of width \u0394z = 0.1, also marginalizing over the spatial curvature. Our measurements of H(z), which have precision better than 7 per cent in most redshift bins, are consistent with the expansion history predicted by a cosmological constant dark energy model, in which the expansion rate accelerates at redshift z < 0.7.", "date": "2012-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "425", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "405-414", "id_number": "CaltechAUTHORS:20120927-133201364", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120927-133201364", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "DP1093738" }, { "agency": "Linkage International Travel Grant", "grant_number": "LX0881951" }, { "agency": "Australian Research Council QEII Fellowship" }, { "agency": "Centre for All-sky Astrophysics" }, { "agency": "Australian Research Council Centre of Excellence", "grant_number": "CE11E0090" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2012.21473.x", "primary_object": { "basename": "mnr21473.pdf", "url": "https://authors.library.caltech.edu/records/h84m8-na451/files/mnr21473.pdf" }, "pub_year": "2012", "author_list": "Blake, Chris; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/5ewez-mjj04", "eprint_id": 34516, "eprint_status": "archive", "datestamp": "2023-09-14 19:34:37", "lastmod": "2023-10-23 20:53:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scrimgeour-S-I", "name": { "family": "Scrimgeour", "given": "Morag I." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: the transition to large-scale cosmic homogeneity", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: statistics; cosmology: observations; large-scale structure of Universe", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS.\n\nMIS would like to thank Florian Beutler for many helpful comments on the paper. We also thank Eyal Kazin, David Parkinson, Luigi Guzzo and Andy Taylor for helpful discussions. MIS acknowledges support from a Jean Rogerson Scholarship and a UWATop-up Scholarship from the University of Western Australia. GBP acknowledges support from two Australian Research Council (ARC) Discovery Projects (DP0772084 and DP1093738). The Centre for All-sky Astrophysics (CAASTRO) is an Australian Research Council\nCentre of Excellence, funded by grant CE11E0090.\nGALEX is a NASA Small Explorer, launched in 2003 April. We\ngratefully acknowledgeNASA's support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The WiggleZ survey would not have been possible without the dedicated work of the staff of the Australian Astronomical Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT.\n\nPublished - mnr21402.pdf
", "abstract": "We have made the largest volume measurement to date of the transition to large-scale homogeneity in the distribution of galaxies. We use the WiggleZ survey, a spectroscopic survey of over 200\u2009000 blue galaxies in a cosmic volume of \u223c1\u2009h^(\u22123)\u2009Gpc^3. A new method of defining the 'homogeneity scale' is presented, which is more robust than methods previously used in the literature, and which can be easily compared between different surveys. Due to the large cosmic depth of WiggleZ (up to z = 1), we are able to make the first measurement of the transition to homogeneity over a range of cosmic epochs. The mean number of galaxies N(< r) in spheres of comoving radius r is proportional to r^3 within 1\u2009per cent, or equivalently the fractal dimension of the sample is within 1\u2009per cent of D_2 = 3, at radii larger than 71 \u00b1 8\u2009h^(\u22121) Mpc at z \u223c 0.2, 70 \u00b1 5\u2009h^(\u22121)\u2009Mpc at z \u223c 0.4, 81 \u00b1 5\u2009h^(\u22121) \u2009Mpc at z \u223c 0.6 and 75 \u00b1 4\u2009h^(\u22121)\u2009Mpc at z \u223c 0.8. We demonstrate the robustness of our results against selection function effects, using a \u039b cold dark matter (\u039bCDM) N-body simulation and a suite of inhomogeneous fractal distributions. The results are in excellent agreement with both the \u039bCDM N-body simulation and an analytical \u039bCDM prediction. We can exclude a fractal distribution with fractal dimension below D_2 = 2.97 on scales from \u223c80\u2009h^(\u22121)\u2009Mpc up to the largest scales probed by our measurement, \u223c300 h^(\u22121)\u2009Mpc, at 99.99\u2009per cent confidence.", "date": "2012-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "425", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "116-134", "id_number": "CaltechAUTHORS:20120927-132913439", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120927-132913439", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Jean Rogerson Scholarship" }, { "agency": "University of Western Australia UWATop-up Scholarship" }, { "agency": "Australian Research Council Discovery Project", "grant_number": "DP0772084" }, { "agency": "Australian Research Council Discovery Project", "grant_number": "DP1093738" }, { "agency": "Australian Research Council Centre of Excellence", "grant_number": "CE11E0090" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2012.21402.x", "primary_object": { "basename": "mnr21402.pdf", "url": "https://authors.library.caltech.edu/records/5ewez-mjj04/files/mnr21402.pdf" }, "pub_year": "2012", "author_list": "Scrimgeour, Morag I.; Martin, D. Christopher; et el." }, { "id": "https://authors.library.caltech.edu/records/8gckr-m6b29", "eprint_id": 33555, "eprint_status": "archive", "datestamp": "2023-08-22 06:16:59", "lastmod": "2023-10-18 20:25:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Tsai-Chao-Wei", "name": { "family": "Tsai", "given": "C. W." }, "orcid": "0000-0002-9390-9672" }, { "id": "Petty-Sara-M", "name": { "family": "Petty", "given": "S." }, "orcid": "0000-0003-0624-3276" }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "M." }, "orcid": "0000-0002-9871-6490" }, { "id": "Assef-R-J", "name": { "family": "Assef", "given": "Roberto J." }, "orcid": "0000-0002-9508-3667" }, { "id": "Benford-D-J", "name": { "family": "Benford", "given": "D. J." }, "orcid": "0000-0002-9884-4206" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C." } }, { "id": "Donoso-E", "name": { "family": "Donoso", "given": "E." } }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "P." } }, { "id": "Fowler-J", "name": { "family": "Fowler", "given": "J." } }, { "id": "Koribalski-B-S", "name": { "family": "Koribalski", "given": "B." } }, { "id": "Lake-S", "name": { "family": "Lake", "given": "S." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Stanford-S", "name": { "family": "Stanford", "given": "S." } }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "E." }, "orcid": "0000-0001-5058-1593" } ] }, "title": "Constructing a WISE High Resolution Galaxy Atlas", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters; galaxies: statistics; infrared: galaxies; surveys; techniques: image processing", "note": "\u00a9 2012 The American Astronomical Society.\nReceived 2011 November 12; accepted 2012 June 19; published 2012 July 16.\nThis work is based (in part) on observations made with\nthe Spitzer and research using the NASA/IPAC Extragalactic\nDatabase (NED) and IPAC Infrared Science Archive, all are operated\nby JPL, Caltech, under a contract with the National Aeronautics\nand Space Administration. Support for this work was\nprovided by NASA through an award issued by JPL/Caltech.\nR.J.A. was supported by an appointment to the NASA Postdoctoral\nProgram at the Jet Propulsion Laboratory, administered\nby Oak Ridge Associated Universities through a contract with\nNASA. This publication makes use of data products from the\nWide-field Infrared Survey Explorer, which is a joint project of\nthe University of California, Los Angeles, and the Jet Propulsion\nLaboratory/California Institute of Technology, funded by\nthe National Aeronautics and Space Administration.\n\nPublished - Jarrett2012p19286Astron_J.pdf
Submitted - 1208.0362v1.pdf
", "abstract": "After eight months of continuous observations, the Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at 3.4 \u03bcm, 4.6 \u03bcm, 12 \u03bcm, and 22 \u03bcm. We have begun a dedicated WISE High Resolution Galaxy Atlas project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we summarize the deconvolution techniques used to significantly improve the spatial resolution of WISE imaging, specifically designed to study the internal anatomy of nearby galaxies. As a case study, we present results for the galaxy NGC 1566, comparing the WISE enhanced-resolution image processing to that of Spitzer, Galaxy Evolution Explorer, and ground-based imaging. This is the first paper in a two-part series; results for a larger sample of nearby galaxies are presented in the second paper.", "date": "2012-08", "date_type": "published", "publication": "Astronomical Journal", "volume": "144", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 68", "id_number": "CaltechAUTHORS:20120827-101936774", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120827-101936774", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Postdoctoral Program" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-6256/144/2/68", "primary_object": { "basename": "1208.0362v1.pdf", "url": "https://authors.library.caltech.edu/records/8gckr-m6b29/files/1208.0362v1.pdf" }, "related_objects": [ { "basename": "Jarrett2012p19286Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/8gckr-m6b29/files/Jarrett2012p19286Astron_J.pdf" } ], "pub_year": "2012", "author_list": "Jarrett, T. H.; Masci, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/8d9zc-b0g08", "eprint_id": 33525, "eprint_status": "archive", "datestamp": "2023-08-22 06:16:52", "lastmod": "2023-10-18 20:23:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Perrett-K", "name": { "family": "Perrett", "given": "K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Evolution in the Volumetric Type Ia Supernova Rate from the Supernova Legacy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; surveys", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 September 15; accepted 2012 June 3; published 2012 July 12.\n\nWe are sincerely grateful to the entire Queued-Service Observations team and staff at CFHT for their patience and assistance throughout the SNLS real-time observing period. We are particularly indebted to Pierre Martin, Jean-Charles Cuillandre, Kanoa Withington, and Herb Woodruff. Canadian collaboration members acknowledge support from NSERC and CIAR; French collaboration members from CNRS/IN2P3, CNRS/INSU, and CEA. M.S. acknowledges support from the Royal Society. This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/\nDAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC)\nof Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of\nUniversities 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 Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). Gemini program IDs: GS-2003BQ- 8, GN-2003B-Q-9, GS-2004A-Q-11, GN-2004A-Q-19, GS-2004B-Q-31, GN-2004B-Q-16, GS-2005A-Q-11, GN-2005AQ-11, GS-2005B-Q-6, GN-2005B-Q-7, GN-2006A-Q-7, GN-\n2006B-Q-10, and GN-2007A-Q-8. Observations made with\nESO Telescopes at the Paranal Observatory under program IDs\n171.A-0486 and 176.A-0589. Some of the data presented herein\nwere 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.\n\nPublished - Perrett2012p19283Astron_J.pdf
", "abstract": "We present a measurement of the volumetric Type Ia supernova (SN Ia) rate (SNR_Ia) as a function of redshift for the first four years of data from the Canada-France-Hawaii Telescope Supernova Legacy Survey (SNLS). This analysis includes 286 spectroscopically confirmed and more than 400 additional photometrically identified SNe Ia within the redshift range 0.1 \u2264 z \u2264 1.1. The volumetric SNR_Ia evolution is consistent with a rise to z ~ 1.0 that follows a power law of the form (1+z)^\u03b1, with \u03b1 = 2.11 \u00b1 0.28. This evolutionary trend in the SNLS rates is slightly shallower than that of the cosmic star formation history (SFH) over the same redshift range. We combine the SNLS rate measurements with those from other surveys that complement the SNLS redshift range, and fit various simple SN Ia delay-time distribution (DTD) models to the combined data. A simple power-law model for the DTD (i.e., \u221d t^(\u2013\u03b2)) yields values from \u03b2 = 0.98 \u00b1 0.05 to \u03b2 = 1.15 \u00b1 0.08 depending on the parameterization of the cosmic SFH. A two-component model, where SNR_Ia is dependent on stellar mass (M_stellar) and star formation rate (SFR) as SNR_(Ia)(z) = A \u00d7 M_(stellar)(z) + B \u00d7 SFR(z), yields the coefficients A = (1.9 \u00b1 0.1) \u00d7 10^(\u20131)4 SNe yr^(\u20131) M^(\u20131)_\u2609 and B = (3.3 \u00b1 0.2) \u00d7 10^(\u20134) SNe yr^(\u20131) (M_\u2609 yr^(\u20131))^(\u20131). More general two-component models also fit the data well, but single Gaussian or exponential DTDs provide significantly poorer matches. Finally, we split the SNLS sample into two populations by the light-curve width (stretch), and show that the general behavior in the rates of faster-declining SNe Ia (0.8 \u2264 s < 1.0) is similar, within our measurement errors, to that of the slower objects (1.0 \u2264 s < 1.3) out to z ~ 0.8.", "date": "2012-08", "date_type": "published", "publication": "Astronomical Journal", "volume": "144", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 59", "id_number": "CaltechAUTHORS:20120824-150657127", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120824-150657127", "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": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Royal Society" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-6256/144/2/59", "primary_object": { "basename": "Perrett2012p19283Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/8d9zc-b0g08/files/Perrett2012p19283Astron_J.pdf" }, "pub_year": "2012", "author_list": "Perrett, K. and Neill, J. D." }, { "id": "https://authors.library.caltech.edu/records/98ebq-gcb58", "eprint_id": 32666, "eprint_status": "archive", "datestamp": "2023-08-22 05:59:02", "lastmod": "2023-10-18 15:58:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Lou-Yu-Qing", "name": { "family": "Lou", "given": "Yu-Qing" } }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "Classical Novae in Andromeda: Light Curves from the Palomar Transient Factory and GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "globular clusters: general; novae, cataclysmic variables; surveys", "note": "\u00a9 2012 The American Astronomical Society.\nReceived 2012 January 12; accepted 2012 April 16; published 2012 June 5.\nWe thank the referee, Dr. Massimo Della Valle, for very helpful comments and suggestions to improve the manuscript. We thank Marina Orio and Sumin Tang for valuable discussions. We thank the Weizmann Monitoring Team (A. Gal-Yam, I. Arcavi, D. Polishook, A. Sternberg, O. Yaron, D. Xu) for daily monitoring of transient candidates from the PTF discovery stream. M.M.K. acknowledges support from the Hubble Fellowship and the Carnegie-Princeton Fellowship. S.B.C wishes to acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, National Aeronautics and Space Administration (NASA)/Swift grant NNX10AI21G, NASA/Fermi grant NNX1OA057G, and National Science Foundation (NSF) grant AST\u20130908886. This research was supported in part by Tsinghua Center for Astrophysics (THCA), by the National Natural Science Foundation of China (NSFC) grants 10373009, 10533020, and 11073014 at Tsinghua University, by the Ministry of Science and Technology (MOST) under State Key Development Program for Basic Research grant 2012CB821800, by the Tsinghua University Initiative Scientific Research Program, by the SRFDP 20050003088, 200800030071, and 20110002110008, and by the Yangtze Endowment from the Ministry of Education at Tsinghua University. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources and data storage for PTF. 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\nPublished - Cao2012p18931Astrophys_J.pdf
", "abstract": "We present optical light curves of 29 novae in M31 during the 2009 and 2010 observing seasons of the Palomar Transient Factory (PTF). The dynamic and rapid cadences in PTF monitoring of M31, from one day to ten minutes, provide excellent temporal coverage of nova light curves, enabling us to record the photometric evolution of M31 novae in unprecedented detail. We also detect eight of these novae in the near-ultraviolet (UV) band with the Galaxy Evolution Explorer (GALEX) satellite. Novae M31N 2009-10b and M31N 2010-11a show prominent UV emission peaking a few days prior to their optical maxima, possibly implying aspherical outbursts. Additionally, our blueshifted spectrum of the recent outburst of PT And (M31N 2010-12a) indicates that it is a recurrent nova in M31 and not a dwarf nova in the Milky Way as was previously assumed. Finally, we systematically searched for novae in all confirmed globular clusters (GCs) of M31 and found only M31N 2010-10f associated with Bol 126. The specific nova rate in the M31 GC system is thus about one per year, which is not enhanced relative to the rate outside the GC system.", "date": "2012-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "752", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No 133", "id_number": "CaltechAUTHORS:20120724-100019191", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120724-100019191", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10373009" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10533020" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11073014" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "2012CB821800" }, { "agency": "Tsinghua University Initiative Scientific Research Program" }, { "agency": "SRFDP", "grant_number": "20050003088" }, { "agency": "SRFDP", "grant_number": "200800030071" }, { "agency": "SRFDP", "grant_number": "20110002110008" }, { "agency": "Ministry of Education Yangtze Endowment" }, { "agency": "Tsinghua Center for Astrophysics (THCA)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/752/2/133", "primary_object": { "basename": "Cao2012p18931Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/98ebq-gcb58/files/Cao2012p18931Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Cao, Yi; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/vsqbk-svg65", "eprint_id": 31777, "eprint_status": "archive", "datestamp": "2023-08-19 10:56:38", "lastmod": "2023-10-17 21:08:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "An ultraviolet\u2013optical flare from the tidal disruption of a helium-rich stellar core", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy", "note": "\u00a9 2012 Macmillan Publishers Limited.\nReceived 8 November 2011; accepted 23 February 2012.\nPublished online 2 May 2012.\n\nWe thank H. Tananbaum for approving our Chandra Director's Discretionary Time request. We are grateful to G. Lodato for providing the tidal disruption event models in tabular form, and to S. Moran for running software to calculate the host-galaxy K-corrections. We thank R. E. Williams for discussions on the line emission in the spectra. S.G. was supported by NASA through a Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by AURA Inc. for NASA. Partial support for this work was provided by the National Science Foundation. The PS1 survey has 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 institutes, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Inc. and the National Central University of Taiwan, and by NASA under a grant issued through the Planetary Science Division of the NASA Science Mission Directorate. We acknowledge NASA's support for construction, operation, and science analysis of the GALEX mission, which was developed in cooperation with Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Some of the observations reported here were obtained at the MMT Observatory, which is a joint facility of the Smithsonian Institution and the University of Arizona, and at the Liverpool Telescope, which is operated with financial support from the UK Science and Technology Facilities Council. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. R.J.F. is a Clay Fellow. Author Contributions: S.G. designed the observations and the transient detection pipeline for the GALEX TDS, and measured the ultraviolet photometry of PS1-10jh. K.F. and J.D.N coordinated, and D.C.M. facilitated, the GALEX TDS observations. A.R. designed the PhotPipe transient detection pipeline hosted by Harvard/CfA for the PS1 Medium Deep Survey (MDS), and measured the optical photometry of PS1-10jh. R.C. designed, implemented and analysed the MMT optical spectroscopy observations, and contributed to the operation of PhotPipe and the visual inspection of transient alerts. E.B. proposed and facilitated the MMT observations. M.E.H., G.N., D.S. and R.J.F. contributed to the operation of PhotPipe and the visual inspection of transient alerts. P.J.C., R.J.F., G.H.M., L.C. and A.S. contributed to the MMT observations. S.J.S. designed, and K.S. operated, the transient pipeline for PS1 MDS hosted by Queen's University Belfast. C.W.S., J.L.T. and W.M.W.-V. facilitated the transient pipelines for PS1 MDS. W.S.B., K.C.C., T.G., J.N.H., N.K., R.-P.K., E.A.M., J.S.M., P.A.P., C.W.S. and J.L.T. helped build the PS1 system. S.G. requested the Director's Discretionary Time Chandra X-ray observation and analysed the data. A.L. obtained the Liverpool Telescope optical imaging observations and analysed the data, and stimulated discussions on the nature of the SED of PS1-10jh. S.G. analysed and modelled the multicolour light curve and the SED of PS1-10jh. T.H. and C.N. stimulated discussions on the nature of the disrupted star. The paper was organized and written by S.G., and all authors provided feedback on the manuscript.\n\nSubmitted - 1205.0252.pdf
Supplemental Material - nature10990-s1.pdf
", "abstract": "The flare of radiation from the tidal disruption and accretion of a star can be used as a marker for supermassive black holes that otherwise lie dormant and undetected in the centres of distant galaxies. Previous candidate flares have had declining light curves in good agreement with expectations, but with poor constraints on the time of disruption and the type of star disrupted, because the rising emission was not observed. Recently, two 'relativistic' candidate tidal disruption events were discovered, each of whose extreme X-ray luminosity and synchrotron radio emission were interpreted as the onset of emission from a relativistic jet. Here we report a luminous ultraviolet\u2013optical flare from the nuclear region of an inactive galaxy at a redshift of 0.1696. The observed continuum is cooler than expected for a simple accreting debris disk, but the well-sampled rise and decay of the light curve follow the predicted mass accretion rate and can be modelled to determine the time of disruption to an accuracy of two days. The black hole has a mass of about two million solar masses, modulo a factor dependent on the mass and radius of the star disrupted. On the basis of the spectroscopic signature of ionized helium from the unbound debris, we determine that the disrupted star was a helium-rich stellar core.", "date": "2012-05-10", "date_type": "published", "publication": "Nature", "volume": "485", "number": "7397", "publisher": "Nature Publishing Group", "pagerange": "217-220", "id_number": "CaltechAUTHORS:20120601-115631407", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120601-115631407", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/nature10990", "primary_object": { "basename": "1205.0252.pdf", "url": "https://authors.library.caltech.edu/records/vsqbk-svg65/files/1205.0252.pdf" }, "related_objects": [ { "basename": "nature10990-s1.pdf", "url": "https://authors.library.caltech.edu/records/vsqbk-svg65/files/nature10990-s1.pdf" } ], "pub_year": "2012", "author_list": "Gezari, S.; Forster, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/xsptx-ddd06", "eprint_id": 31488, "eprint_status": "archive", "datestamp": "2023-08-19 10:42:04", "lastmod": "2023-10-17 16:37:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riemer-S\u00f8rensen-S", "name": { "family": "Riemer-S\u00f8rensen", "given": "Signe" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "WiggleZ Dark Energy Survey: Cosmological neutrino mass constraint from blue high-redshift galaxies", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Physical Society. Received 21 December 2011; published 23 April 2012. S. R. S. acknowledges financial support from The Danish Council for Independent Research|Natural\nSciences. We acknowledge financial support from the\nAustralian Research Council through Discovery Project\nGrant Nos. DP0772084 and DP1093738. This research\nwas supported by CAASTRO: [46] GALEX (the Galaxy\nEvolution Explorer) is a NASA Small Explorer, launched\nin April 2003. We gratefully acknowledge NASA's support\nfor construction, operation and science analysis for the\nGALEX mission, developed in cooperation with the\nCentre National d'Etudes Spatiales de France and the\nKorean Ministry of Science and Technology. We thank\nthe Anglo-Australian Telescope Allocation Committee\nfor supporting the WiggleZ survey over 9 semesters, and\nwe are very grateful for the dedicated work of the staff of\nthe Australian Astronomical Observatory in the development\nand support of the AAOmega spectrograph, and the\nrunning of the AAT.\n\nPublished - RiemerSorensen2012p18065Phys_Rev_D.pdf
", "abstract": "The absolute neutrino mass scale is currently unknown, but can be constrained by cosmology. The WiggleZ high redshift, star-forming, and blue galaxy sample offers a complementary data set to previous surveys for performing these measurements, with potentially different systematics from nonlinear structure formation, redshift-space distortions, and galaxy bias. We obtain a limit of \u2211m_\u03bd<0.60\u2009\u2009eV (95% confidence) for WiggleZ+Wilkinson\u2009Microwave\u2009Anisotropy\u2009Probe. Combining with priors on the Hubble parameter and the baryon acoustic oscillation scale gives \u2211m_\u03bd<0.29\u2009\u2009eV, which is the strongest neutrino mass constraint derived from spectroscopic galaxy redshift surveys.", "date": "2012-04-23", "date_type": "published", "publication": "Physical Review D", "volume": "85", "number": "8", "publisher": "American Physical Society", "pagerange": "Art. No. 081101", "id_number": "CaltechAUTHORS:20120515-154321243", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120515-154321243", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Danish Council for Independent Research-Natural Sciences" }, { "agency": "Australian Research Council (Australia) Discovery Project", "grant_number": "DP0772084" }, { "agency": "Australian Research Council (Australia) Discovery Project", "grant_number": "DP1093738" }, { "agency": "CAASTRO" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1103/PhysRevD.85.081101", "primary_object": { "basename": "RiemerSorensen2012p18065Phys_Rev_D.pdf", "url": "https://authors.library.caltech.edu/records/xsptx-ddd06/files/RiemerSorensen2012p18065Phys_Rev_D.pdf" }, "pub_year": "2012", "author_list": "Riemer-S\u00f8rensen, Signe; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/cnvkm-vaw08", "eprint_id": 31442, "eprint_status": "archive", "datestamp": "2023-08-22 05:11:47", "lastmod": "2023-10-17 16:35:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Li-I-hui", "name": { "family": "Li", "given": "I. H." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted" } } ] }, "title": "The WiggleZ Dark Energy Survey: Galaxy Evolution at 0.25 \u2264 z \u2264 0.75 Using the Second Red-Sequence Cluster Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: luminosity function, mass function; galaxies: photometry", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 April 20; accepted 2012 January 3; published 2012 February 17.\n\nThe RCS2 data in this paper are based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT\nand CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope\n(CFHT) which is operated by the National Research Council\n(NRC) of Canada, the Institute National des Sciences de\nl'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. I.H.L. thanks the Australian Research Council Linkage International Grant for the early development of this work. I.H.L. and H.K.C.Y. thank the Academia Sinica Institute of Astronomy and Astrophysics, Taiwan, for their hospitality during the early stage of the writing of the paper. The RCS and the research of H.K.C.Y. are supported by grants from the Natural Science and Engineering Research Council of Canada and the Canada Research Chair program. TheWiggleZ team acknowledges financial support from the Australian Research Council through Discovery Project grants. The WiggleZ survey would not have been possible without the dedicated work of the staff of the Anglo-Australian Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT.\n\nPublished - Li2012p18104Astrophys_J.pdf
", "abstract": "We study the evolution of galaxy populations around the spectroscopic WiggleZ sample of star-forming galaxies at 0.25 \u2264 z \u2264 0.75 using the photometric catalog from the Second Red-Sequence Cluster Survey (RCS2). We probe the optical photometric properties of the net excess neighbor galaxies. The key concept is that the marker galaxies and their neighbors are located at the same redshift, providing a sample of galaxies representing a complete census of galaxies in the neighborhood of star-forming galaxies. The results are compared with those using the RCS WiggleZ Spare-Fibre (RCS-WSF) sample as markers, representing galaxies in cluster environments at 0.25 \u2264 z \u2264 0.45. By analyzing the stacked color-color properties of the WiggleZ neighbor galaxies, we find that their optical colors are not a strong function of indicators of star-forming activities such as EW([O II]) or Galaxy Evolution Explorer (GALEX) near-UV luminosity of the markers. The galaxies around the WiggleZ markers exhibit a bimodal distribution on the color-magnitude diagram, with most of them located in the blue cloud. The optical galaxy luminosity functions (GLFs) of the blue neighbor galaxies have a faint-end slope \u03b1 of ~ \u20131.3, similar to that for galaxies in cluster environments drawn from the RCS-WSF sample. The faint-end slope of the GLF for the red neighbors, however, is ~ \u20130.4, significantly shallower than the ~ \u20130.7 found for those in cluster environments. This suggests that the buildup of the faint end of the red sequence in cluster environments is in a significantly more advanced stage than that in the star-forming and lower galaxy density WiggleZ neighborhoods. We find that the red galaxy fraction (f_red) around the star-forming WiggleZ galaxies has similar values from z ~ 0.3 to z ~ 0.6 with f_red ~ 0.28, but drops to f_red ~ 0.20 at z gsim 0.7. This change of f_red with redshift suggests that there is either a higher rate of star-forming galaxies entering the luminosity-limited sample at z \u2273 0.7, or a decrease in the quenching rate of star formation at that redshift. Comparing to that in a dense cluster environment, the f_red of the WiggleZ neighbors is both considerably smaller and has a more moderate change with redshift, pointing to the stronger and more prevalent environmental influences on galaxy evolution in high-density regions.", "date": "2012-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "747", "number": "2", "publisher": "American Astronomical Society", "pagerange": "91", "id_number": "CaltechAUTHORS:20120511-155437070", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120511-155437070", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council Linkage International Grant" }, { "agency": "Academia Sinica Institute of Astronomy and Astrophysics (Taiwan)" }, { "agency": "Natural Science and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chair program" }, { "agency": "Australian Research Council Discovery Project grants" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "COSMOS" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/747/2/91", "primary_object": { "basename": "Li2012p18104Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/cnvkm-vaw08/files/Li2012p18104Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Li, I. H.; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/dvkdk-54b55", "eprint_id": 29076, "eprint_status": "archive", "datestamp": "2023-08-22 04:26:15", "lastmod": "2023-10-24 18:21:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chomiuk-L", "name": { "family": "Chomiuk", "given": "L." }, "orcid": "0000-0002-8400-3705" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Pan-STARRS1 Discovery of Two Ultraluminous Supernovae at z \u2248 0.9", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter; stars: magnetars; supernovae: general; supernovae: individual (PS1-10ky, PS1-10awh)", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 July 3; accepted 2011 September 14; published 2011 November 29. \nWe thank S. Balberg, D. Kasen, B. Metzger, R. Quimby, and R. Stoll for helpful insights. Laura Chomiuk is a Jansky Fellow of the National Radio Astronomy Observatory. Ryan J. Foley is supported by a Clay Fellowship. This discovery was enabled using the PS1 System operated by the PS1 Science Consortium (PS1SC) and its member institutions. The PS1 Surveys have been made possible through the combinations of the Institute for Astronomy at the University of Hawaii, The Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestial Physics, Garching, The Johns Hopkins University, the University of Durham, the University of Edinburgh, the Queen's University of Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Network, and the National Central University of Taiwan. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. The EVLA is run by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc., Gemini Observatory 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 Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva (Argentina). Some of the image processing in this paper was run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. We appreciate the excellent support by the staffs at Gemini, MMT, EVLA, and PS1. We are grateful for access to Gemini under programs GN-2010A-Q-30 and GS-2010B-Q-4 (PI: E. Berger) and GN-2010B-Q-34 (PI: J. Tonry). Partial support for this work was provided by National Science Foundation grants AST-1009749 and AST-0807727. Facilities: PS1(GPC1), MMT (Blue Channel Spectrograph, Hectospec), Gemini:Gillett (GMOS), EVLA, GALEX\n\nPublished - Chomiuk2011p16927Astrophys_J.pdf
", "abstract": "We present the discovery of two ultraluminous supernovae (SNe) at z \u2248 0.9 with the Pan-STARRS1 Medium Deep Survey. These SNe, PS1-10ky and PS1-10awh, are among the most luminous SNe ever discovered, comparable to the unusual transients SN 2005ap and SCP 06F6. Like SN 2005ap and SCP 06F6, they show characteristic high luminosities (M_(bol) \u2248 \u201322.5 mag), blue spectra with a few broad absorption lines, and no evidence for H or He. We have constructed a full multi-color light curve sensitive to the peak of the spectral energy distribution in the rest-frame ultraviolet, and we have obtained time series spectroscopy for these SNe. Given the similarities between the SNe, we combine their light curves to estimate a total radiated energy over the course of explosion of (0.9-1.4) \u00d7 10^(51) erg. We find photospheric velocities of 12,000-19,000 km s^(\u20131) with no evidence for deceleration measured across ~3 rest-frame weeks around light curve peak, consistent with the expansion of an optically thick massive shell of material. We show that, consistent with findings for other ultraluminous SNe in this class, radioactive decay is not sufficient to power PS1-10ky, and we discuss two plausible origins for these events: the initial spin-down of a newborn magnetar in a core-collapse SN, or SN shock breakout from the dense circumstellar wind surrounding a Wolf-Rayet star.", "date": "2011-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "743", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 114", "id_number": "CaltechAUTHORS:20120201-151340323", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120201-151340323", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Clay Fellowship" }, { "agency": "Smithsonian Astrophysical Observatory" }, { "agency": "Harvard University" }, { "agency": "Gemini", "grant_number": "GN-2010A-Q-30" }, { "agency": "Gemini", "grant_number": "GS-2010B-Q-4" }, { "agency": "Gemini", "grant_number": "GN-2010B-Q-34" }, { "agency": "NSF", "grant_number": "AST-1009749" }, { "agency": "NSF", "grant_number": "AST-0807727" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/743/2/114", "primary_object": { "basename": "Chomiuk2011p16927Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/dvkdk-54b55/files/Chomiuk2011p16927Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Chomiuk, L.; Forster, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/z1h2g-06y25", "eprint_id": 29387, "eprint_status": "archive", "datestamp": "2023-08-22 04:17:53", "lastmod": "2023-10-24 22:09:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blake-C", "name": { "family": "Blake", "given": "Chris" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: mapping the distance\u2013redshift\n relation with baryon acoustic oscillations", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; cosmological parameters; distance scale; large-scale structure of Universe", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 August 5. Received 2011 August 4; in original form 2011 July 1. \nArticle first published online: 4 Oct. 2011.\nWe thank the anonymous referee for careful and constructive comments\nthat improved this study.\nWe acknowledge financial support from the Australian Research\nCouncil through Discovery Project grants DP0772084 and\nDP1093738 funding the positions of SB, DP, MP, GP and TMD. SC\nand DC acknowledge the support of the Australian Research Council\nthrough QEII Fellowships. MJD thanks the Gregg Thompson\nDark Energy Travel Fund for financial support.\nWe thank the LasDamas project for making their mock catalogues\npublicly available. In particular EK is much obliged to Cameron\nMcBride for supplying mock catalogues on demand. EK also thanks\nAriel S\u00b4anchez for fruitful lengthy discussions. EK was partially\nsupported by a Google Research Award and NASA Award.\nFB is supported by the Australian Government through the International\nPostgraduate Research Scholarship (IPRS) and by scholarships\nfrom the International Centre for Radio Astronomy Research\n(ICRAR) and the Australian Astronomical Observatory (AAO).\nGALEX is a NASA Small Explorer, launched in 2003 April. We\ngratefully acknowledge NASA's support for construction, operation\nand science analysis for the GALEX mission, developed in cooperation\nwith the Centre National d'Etudes Spatiales of France\nand the Korean Ministry of Science and Technology.\nFinally, the WiggleZ survey would not be possible without the\ndedicated work of the staff of the Australian Astronomical Observatory\nin the development and support of the AAOmega spectrograph,\nand the running of the Anglo-Australian Telescope (AAT).\n\nPublished - Blake2011p17133Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present measurements of the baryon acoustic peak at redshifts z= 0.44, 0.6 and 0.73 in the galaxy correlation function of the final data set of the WiggleZ Dark Energy Survey. We combine our correlation function with lower redshift measurements from the 6-degree Field Galaxy Survey and Sloan Digital Sky Survey, producing a stacked survey correlation function in which the statistical significance of the detection of the baryon acoustic peak is 4.9\u03c3 relative to a zero-baryon model with no peak. We fit cosmological models to this combined baryon acoustic oscillation (BAO) data set comprising six distance\u2013redshift data points, and compare the results with similar cosmological fits to the latest compilation of supernovae (SNe) and cosmic microwave background (CMB) data. The BAO and SNe data sets produce consistent measurements of the equation-of-state w of dark energy, when separately combined with the CMB, providing a powerful check for systematic errors in either of these distance probes. Combining all data sets we determine w=\u22121.03 \u00b1 0.08 for a flat universe, consistent with a cosmological constant model. Assuming dark energy is a cosmological constant and varying the spatial curvature, we find \u03a9_k=\u22120.004 \u00b1 0.006.", "date": "2011-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "418", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1707-1724", "id_number": "CaltechAUTHORS:20120221-102308327", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120221-102308327", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "DP1093738" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" }, { "agency": "Google Research Award" }, { "agency": "NASA" }, { "agency": "Australian Government International Postgraduate Research Scholarship (IPRS)" }, { "agency": "Centre National d'Etudes Spatiales of France" }, { "agency": "Korean Ministry of Science and Technology" }, { "agency": "Australian Astronomical Observatory (AAO)" }, { "agency": "Anglo-Australian Telescope (AAT)" }, { "agency": "International Centre for Radio Astronomy Research (ICRAR)" }, { "agency": "Australian Research Council QEII Fellowships" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2011.19592.x", "primary_object": { "basename": "Blake2011p17133Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/z1h2g-06y25/files/Blake2011p17133Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Blake, Chris; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/3q2wq-nzc16", "eprint_id": 29389, "eprint_status": "archive", "datestamp": "2023-08-22 04:17:58", "lastmod": "2023-10-24 22:09:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blake-C", "name": { "family": "Blake", "given": "Chris" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: measuring the cosmic expansion\n history using the Alcock\u2013Paczynski test and distant supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; dark energy; distance scale", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 August 6. Received 2011 August 4; in original form 2011 July 1. \nArticle first published online: 4 Oct. 2011.\nWe thank the anonymous referee for helpful comments. CB acknowledges\nuseful discussions with Berian James, Juliana Kwan\nand Arman Shafieloo. We acknowledge financial support from\nthe Australian Research Council through Discovery Project grants\nDP0772084 and DP1093738 and Linkage International travel\ngrant LX0881951. SC acknowledges the support of an Australian\nResearch Council QEII Fellowship. MJD and TMD thank the\nGregg Thompson Dark Energy Travel Fund for financial support.\nGALEX (the Galaxy Evolution Explorer) is a NASA Small\nExplorer, launched in 2003 April. We gratefully acknowledge\nNASA's support for construction, operation and science analysis\nfor the GALEX mission, developed in cooperation with the Centre\nNational d'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology.We thank the Anglo-Australian Telescope\nAllocation Committee for supporting theWiggleZ survey over nine\nsemesters, and we are very grateful for the dedicated work of the\nstaff of the Australian Astronomical Observatory in the development\nand support of the AAOmega spectrograph, and the running\nof the AAT.\n\nPublished - Blake2011p17142Mon_Not_R_Astron_Soc.pdf
", "abstract": "Astronomical observations suggest that today's Universe is dominated by a dark energy of unknown physical origin. One of the most notable results obtained from many models is that dark energy should cause the expansion of the Universe to accelerate: but the expansion rate as a function of time has proved very difficult to measure directly. We present a new determination of the cosmic expansion history by combining distant supernovae observations with a geometrical analysis of large-scale galaxy clustering within the WiggleZ Dark Energy Survey, using the Alcock\u2013Paczynski test to measure the distortion of standard spheres. Our result constitutes a robust and non-parametric measurement of the Hubble expansion rate as a function of time, which we measure with 10\u201315 per cent precision in four bins within the redshift range 0.1 < z < 0.9. We demonstrate, in a manner insensitive to the assumed cosmological model, that the cosmic expansion is accelerating. Furthermore, we find that this expansion history is consistent with a cosmological-constant dark energy.", "date": "2011-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "418", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1725-1735", "id_number": "CaltechAUTHORS:20120221-113953988", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120221-113953988", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "DP1093738" }, { "agency": "Linkage International Travel Grant", "grant_number": "LX0881951" }, { "agency": "Australian Research Council QEII Fellowship" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" }, { "agency": "NASA" }, { "agency": "Centre National d'Etudes Spatiales of France" }, { "agency": "Korean Ministry of Science and Technology" }, { "agency": "Anglo-Australian Telescope (AAT) Allocation Committee" }, { "agency": "Australian Astronomical Observatory (AAO)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2011.19606.x", "primary_object": { "basename": "Blake2011p17142Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/3q2wq-nzc16/files/Blake2011p17142Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Blake, Chris; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/nq5ay-r1559", "eprint_id": 28355, "eprint_status": "archive", "datestamp": "2023-08-22 03:58:55", "lastmod": "2023-10-24 17:50:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sahai-R", "name": { "family": "Sahai", "given": "Raghvendra" } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "S\u00e1nchez-Contreras-C", "name": { "family": "S\u00e1nchez Contreras", "given": "Carmen" } } ] }, "title": "Strong Variable Ultraviolet Emission from Y Gem: Accretion Activity in an Asymptotic Giant Branch Star with a Binary Companion?", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; binaries: general; circumstellar matter; stars: AGB and post-AGB; stars: individual (Y Gem, Mira); stars: mass-loss", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 July 15; accepted 2011 August 6; published 2011 September 28. We thank the staff of the Arizona Radio Observatory for\ngranting us observing time. We thank Noam Soker and Joel\nKastner for their valuable comments on an earlier version of\nthis Letter. R.S.'s contribution to the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Financial support was provided by NASA through a Long Term Space Astrophysics and GALEX GO award.\n\nPublished - Sahai2011p16406Astrophys_J_Lett.pdf
", "abstract": "Binarity is believed to dramatically affect the history and geometry of mass loss in asymptotic giant branch (AGB) and post-AGB stars, but observational evidence of binarity is sorely lacking. As part of a project to look for hot binary companions to cool AGB stars using the Galaxy Evolution Explorer archive, we have discovered a late-M star, Y Gem, to be a source of strong and variable UV emission. Y Gem is a prime example of the success of our technique of UV imaging of AGB stars in order to search for binary companions. Y Gem's large and variable UV flux makes it one of the most prominent examples of a late-AGB star with a mass accreting binary companion. The UV emission is most likely due to emission associated with accretion activity and a disk around a main-sequence companion star. The physical mechanism generating the UV emission is extremely energetic, with an integrated luminosity of a few \u00d7 L_\u2609 at its peak. We also find weak CO J = 2-1 emission from Y Gem with a very narrow line profile (FWHM of 3.4 km s^(\u20131)). Such a narrow line is unlikely to arise in an outflow and is consistent with emission from an orbiting, molecular reservoir of radius 300 AU. Y Gem may be the progenitor of the class of post-AGB stars which are binaries and possess disks but no outflows.", "date": "2011-10-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "740", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L39", "id_number": "CaltechAUTHORS:20111207-134126683", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111207-134126683", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "GALEX GO award" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/2041-8205/740/2/L39", "primary_object": { "basename": "Sahai2011p16406Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/nq5ay-r1559/files/Sahai2011p16406Astrophys_J_Lett.pdf" }, "pub_year": "2011", "author_list": "Sahai, Raghvendra; Neill, James D.; et el." }, { "id": "https://authors.library.caltech.edu/records/tkrzj-sxe32", "eprint_id": 25305, "eprint_status": "archive", "datestamp": "2023-08-22 03:27:44", "lastmod": "2023-10-24 15:46:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "SNLS3: Constraints on Dark Energy Combining the Supernova Legacy Survey Three-year Data with Other Probes", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters; cosmology: observations; supernovae: general; surveys", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 April 7; accepted 2011 June 21; published 2011 August 8. This paper is based in part on observations obtained with\nMegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada\u2013France\u2013Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada,\nthe Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. M.S. acknowledges support from the Royal Society. Canadian collaboration members acknowledge support from NSERC and CIAR; French collaboration members from CNRS/IN2P3, CNRS/INSU, and CEA. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. Based in part 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 Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). Based on data from Gemini program IDs: GS-2003B-Q-8, GN-2003B-Q-9, GS-2004A-Q-11, GN-2004A-Q-19, GS-2004B-Q-31, GN-2004B-Q-16, GS-2005A-Q-11, GN-2005A-Q-11, GS-2005BQ-6, GN-2005B-Q-7, GN-2006A-Q-7, and GN-2006B-Q-10.\nBased in part on observations made with ESO Telescopes at\nthe Paranal Observatory under program IDs 171.A-0486 and\n176.A-0589. Some of the data presented herein were obtained\nat 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 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\nPublished - Sullivan2011p15736Astrophys_J.pdf
", "abstract": "We present observational constraints on the nature of dark energy using the Supernova Legacy Survey three-year sample (SNLS3) of Guy et al. and Conley et al. We use the 472 Type Ia supernovae (SNe Ia) in this sample, accounting for recently discovered correlations between SN Ia luminosity and host galaxy properties, and include the effects of all identified systematic uncertainties directly in the cosmological fits. Combining the SNLS3 data with the full WMAP7 power spectrum, the Sloan Digital Sky Survey luminous red galaxy power spectrum, and a prior on the Hubble constant H_0 from SHOES, in a flat universe we find \u03a9_m = 0.269 \u00b1 0.015 and w = \u20131.061^(+0.069)_(\u20130.068) (where the uncertainties include all statistical and SN Ia systematic errors)\u2014a 6.5% measure of the dark energy equation-of-state parameter w. The statistical and systematic uncertainties are approximately equal, with the systematic uncertainties dominated by the photometric calibration of the SN Ia fluxes\u2014without these calibration effects, systematics contribute only a ~2% error in w. When relaxing the assumption of flatness, we find \u03a9_m = 0.271 \u00b1 0.015, \u03a9_k = \u20130.002 \u00b1 0.006, and w = \u20131.069^(+0.091)_(\u20130.092). Parameterizing the time evolution of w as w(a) = w_0 + w_a (1\u2013a) gives w_0 = \u20130.905 \u00b1 0.196, w_a = \u20130.984^(+1.094)_(\u2013 1.097) in a flat universe. All of our results are consistent with a flat, w = \u20131 universe. The size of the SNLS3 sample allows various tests to be performed with the SNe segregated according to their light curve and host galaxy properties. We find that the cosmological constraints derived from these different subsamples are consistent. There is evidence that the coefficient, \u03b2, relating SN Ia luminosity and color, varies with host parameters at >4\u03c3 significance (in addition to the known SN luminosity-host relation); however, this has only a small effect on the cosmological results and is currently a subdominant systematic.", "date": "2011-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "737", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 102", "id_number": "CaltechAUTHORS:20110912-114953536", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110912-114953536", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/737/2/102", "primary_object": { "basename": "Sullivan2011p15736Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/tkrzj-sxe32/files/Sullivan2011p15736Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Sullivan, M.; Ellis, R. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/gasz3-wgv27", "eprint_id": 25278, "eprint_status": "archive", "datestamp": "2023-08-22 03:19:45", "lastmod": "2023-10-24 15:45:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blake-C", "name": { "family": "Blake", "given": "Chris" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z = 0.9", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; cosmological parameters; large-scale structure of Universe", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 April 12. Received 2011 March 26; in original form 2010 December 12. \nArticle first published online: 7 Jun. 2011.\n\n\nWe thank Carlton Baugh, Elise Jennings, Juliana Kwan, David\nParkinson, Will Percival, Roman Scoccimarro and Yong-Seon\nSong for useful comments which influenced and improved the\ndevelopment of this paper. We are particularly grateful to Martin Crocce for providing power spectra for RPT and for helpful comments. We acknowledge financial support from the Australian Research Council through Discovery Project grants funding the positions of SB, MP, GBP and TD. SC acknowledges the support of the Australian Research Council through a QEII Fellowship. MJD and TD thank the Gregg Thompson Dark Energy Travel Fund for financial support. GALEX is a NASA Small Explorer, launched in 2003 April. We\ngratefully acknowledge NASA's support for construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. Finally, the WiggleZ Survey would not be possible without the dedicated work of the staff of the Australian Astronomical Observatory in the development and support of the AAOmega spectrograph, and the running of the AAT.\n\nPublished - Blake2011p15720Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present precise measurements of the growth rate of cosmic structure for the redshift range 0.1 < z < 0.9, using redshift-space distortions in the galaxy power spectrum of the WiggleZ Dark Energy Survey. Our results, which have a precision of around 10 per cent in four\nindependent redshift bins, are well fitted by a flat \u039b cold dark matter (\u039bCDM) cosmological model with matter density parameter \u03a9_m = 0.27. Our analysis hence indicates that this model provides a self-consistent description of the growth of cosmic structure through large-scale\nperturbations and the homogeneous cosmic expansion mapped by supernovae and baryon acoustic oscillations. We achieve robust results by systematically comparing our data with\nseveral different models of the quasi-linear growth of structure including empirical models, fitting formulae calibrated to N-body simulations, and perturbation theory techniques. We extract the first measurements of the power spectrum of the velocity divergence field, P_(\u03b8\u03b8) (k),\nas a function of redshift (under the assumption that P_(g\u03b8) (k) = \u2212 \u221aP_(gg)(k)P_(\u03b8\u03b8) (k), where g is the galaxy overdensity field), and demonstrate that the WiggleZ galaxy\u2013mass cross-correlation is consistent with a deterministic (rather than stochastic) scale-independent bias model for WiggleZ galaxies for scales k < 0.3 h Mpc^(\u22121). Measurements of the cosmic growth rate from\nthe WiggleZ Survey and other current and future observations offer a powerful test of the physical nature of dark energy that is complementary to distance\u2013redshift measures such as supernovae and baryon acoustic oscillations.", "date": "2011-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "415", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2876-2891", "id_number": "CaltechAUTHORS:20110909-135550756", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110909-135550756", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2011.18903.x", "primary_object": { "basename": "Blake2011p15720Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/gasz3-wgv27/files/Blake2011p15720Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Blake, Chris; Forster, Karl; et el." }, { "id": "https://authors.library.caltech.edu/records/cyjvr-1n920", "eprint_id": 24722, "eprint_status": "archive", "datestamp": "2023-08-19 07:31:04", "lastmod": "2023-10-24 14:52:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika T." } }, { "id": "Greer-F", "name": { "family": "Greer", "given": "Frank" } }, { "id": "Hoenk-M-E", "name": { "family": "Hoenk", "given": "Michael E." } }, { "id": "Blacksberg-J", "name": { "family": "Blacksberg", "given": "Jordana" } }, { "id": "Dickie-M-R", "name": { "family": "Dickie", "given": "Matthew R." } }, { "id": "Nikzad-S", "name": { "family": "Nikzad", "given": "Shouleh" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } } ] }, "title": "Ultraviolet antireflection coatings for use in silicon detector design", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 Optical Society of America. \n\nReceived 23 February 2011; revised 25 May 2011; accepted 27 May 2011; posted 31 May 2011 (Doc. ID 142383); published 19 July 2011. \n\nThe research described here was funded in part by a National Aeronautics and Space Administration (NASA) Space Grant. The research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, and was supported in part by internal funding from Columbia University. The authors wish to thank Blake Jacquot, Todd Jones, and Patrick Morrissey for their help and advice in the writing of this paper.\n\nPublished - Hamden2011p15448Appl_Optics.pdf
", "abstract": "We report on the development of coatings for a charged-coupled device (CCD) detector optimized for use in a fixed dispersion UV spectrograph. Because of the rapidly changing index of refraction of Si, single layer broadband antireflection (AR) coatings are not suitable to increase quantum efficiency at all wavelengths of interest. Instead, we describe a creative solution that provides excellent performance over UV wavelengths. We describe progress in the development of a coated CCD detector with theoretical quantum efficiencies (QEs) of greater than 60% at wavelengths from 120 to 300\u2009nm. This high efficiency may be reached by coating a backside-illuminated, thinned, delta-doped CCD with a series of thin film AR coatings. The materials tested include MgF_2 (optimized for highest performance from 120\u2013150\u2009nm), SiO_2 (150\u2013180\u2009nm), Al_2O_3 (180\u2013240\u2009nm), MgO (200\u2013250\u2009nm), and HfO_2 (240\u2013300\u2009nm). A variety of deposition techniques were tested and a selection of coatings that minimized reflectance on a Si test wafer were applied to functional devices. We also discuss future uses and improvements, including graded and multilayer coatings.", "date": "2011-07-20", "date_type": "published", "publication": "Applied Optics", "volume": "50", "number": "21", "publisher": "Optical Society of America", "pagerange": "4180-4188", "id_number": "CaltechAUTHORS:20110808-091608589", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110808-091608589", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Columbia University" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1364/AO.50.004180", "primary_object": { "basename": "Hamden2011p15448Appl_Optics.pdf", "url": "https://authors.library.caltech.edu/records/cyjvr-1n920/files/Hamden2011p15448Appl_Optics.pdf" }, "pub_year": "2011", "author_list": "Hamden, Erika T.; Greer, Frank; et el." }, { "id": "https://authors.library.caltech.edu/records/3tcdr-58962", "eprint_id": 24381, "eprint_status": "archive", "datestamp": "2023-08-22 03:10:52", "lastmod": "2023-10-23 22:37:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Drake-A-J", "name": { "family": "Drake", "given": "A. J." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. S." } }, { "id": "Williams-R", "name": { "family": "Williams", "given": "R." } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "M. J." }, "orcid": "0000-0002-3168-0139" } ] }, "title": "The Discovery and Nature of the Optical Transient CSS100217:102913+404220", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: nuclei; galaxies: stellar content; supernovae: general", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 December 17; accepted 2011 April 26; published 2011 June 22.\nSome of the data presented herein were obtained at the W. M. Keck\nObservatory, which is operated as a scientific partnership among the California\nInstitute of Technology, the University of California, and the National\nAeronautics and Space Administration. The Observatory was made possible\nby the generous financial support of the W. M. Keck Foundation.\n\nBased on observations made with the NASA/ESA Hubble Space Telescope,\nobtained at the Space Telescope Science Institute, which is operated by the\nAssociation of Universities for Research in Astronomy, Inc., under NASA\ncontract NAS 5-26555. These observations are associated with program 12117.\n\n\nWe thank Minjin Kim for help in analyzing the SDSS spectrum.\nThe CRTS survey is supported by the U.S. National Science\nFoundation under grants AST-0909182 and CNS-0540369.\nSupport for program number GO proposal 12117 was provided\nby NASA through a grant from the Space Telescope Science\nInstitute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The work at Caltech was supported in part by the NASA Fermi grant 08-FERMI08-0025, and by the Ajax Foundation. The CSS survey is funded by the National Aeronautics and Space Administration under grant no. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. J.L.P. acknowledges support from NASA through Hubble Fellowship Grant HF-51261.01-A awarded by the STScI, which is operated by AURA, Inc. for NASA, under contract NAS 5-26555. The PQ survey is supported by the U.S. National Science Foundation under Grants AST-0407448 and AST-0407297. Support for M.C. is provided by Proyecto Basal PFB-06/2007, by FONDAP Centro de Astrof\u00edsica 15010003, and by MIDEPLAN Rs Programa Iniciativa Cient\u00edfica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The Expanded Very Large Array is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both the development\nand the operation of the LAT as well as scientific data\nanalysis. These include NASA and DOE in the United States,\nCEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy,\nMEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg\nFoundation, the Swedish Research Council and the National\nSpace Board in Sweden. We thank all the observers at ARIES\nwho provided their valuable time and support for the observations of this event. The UBVRI observations presented here are included by R.R. in partial fulfillment of the requirements for a Ph.D. degree.\n\nPublished - Drake2011p14661Astrophys_J.pdf
Submitted - 1103.5514
", "abstract": "We report on the discovery and observations of the extremely luminous optical transient CSS100217:102913+404220 (CSS100217 hereafter). Spectroscopic observations showed that this transient was coincident with a galaxy at redshift z = 0.147 and reached an apparent magnitude of V ~ 16.3. After correcting for foreground Galactic extinction we determine the absolute magnitude to be M_V = \u201322.7 approximately 45 days after maximum light. Over a period of 287 rest-frame days, this event had an integrated bolometric luminosity of 1.3 \u00d7 10^(52) erg based on time-averaged bolometric corrections of ~15 from V- and R-band observations. Analysis of the pre-outburst Sloan Digital Sky Survey (SDSS) spectrum of the source shows features consistent with a narrow-line Seyfert 1 galaxy. High-resolution Hubble Space Telescope and Keck follow-up observations show that the event occurred within 150 pc of the nucleus of the galaxy, suggesting a possible link to the active nuclear region. However, the rapid outburst along with photometric and spectroscopic evolution are much more consistent with a luminous supernova. Line diagnostics suggest that the host galaxy is undergoing significant star formation. We use extensive follow-up of the event along with archival Catalina Sky Survey NEO search and SDSS data to investigate the three most likely sources of such an event: (1) an extremely luminous supernova, (2) the tidal disruption of a star by the massive nuclear black hole, and (3) variability of the central active galactic nucleus (AGN). We find that CSS100217 was likely an extremely luminous Type IIn supernova and occurred within the range of the narrow-line region of an AGN. We discuss how similar events may have been missed in past supernova surveys because of confusion with AGN activity.", "date": "2011-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "735", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 106", "id_number": "CaltechAUTHORS:20110712-112722577", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110712-112722577", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "NSF", "grant_number": "CNS-0540369" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA", "grant_number": "08-FERMI08-0025" }, { "agency": "Ajax Foundation" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-51261.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-0407448" }, { "agency": "NSF", "grant_number": "AST-0407297" }, { "agency": "Proyecto Basal", "grant_number": "PFB-06/2007" }, { "agency": "FONDAP Centro de Astrofisica", "grant_number": "15010003" }, { "agency": "MIDEPLAN Rs Programa Iniciativa Cientifica Milenio", "grant_number": "P07-021-F" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/735/2/106", "primary_object": { "basename": "1103.5514", "url": "https://authors.library.caltech.edu/records/3tcdr-58962/files/1103.5514" }, "related_objects": [ { "basename": "Drake2011p14661Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/3tcdr-58962/files/Drake2011p14661Astrophys_J.pdf" } ], "pub_year": "2011", "author_list": "Drake, A. J.; Djorgovski, S. G.; et el." }, { "id": "https://authors.library.caltech.edu/records/z8vw5-0vd51", "eprint_id": 23922, "eprint_status": "archive", "datestamp": "2023-08-22 02:53:33", "lastmod": "2023-10-23 20:09:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lemonias-J-J", "name": { "family": "Lemonias", "given": "Jenna J." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David" }, "orcid": "0000-0002-8528-7340" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie A." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" } ] }, "title": "The Space Density of Extended Ultraviolet (XUV) Disks in the Local Universe and Implications for Gas Accretion onto Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: structure; surveys; ultraviolet: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 September 28; accepted 2011 March 10; published 2011 May 6. We thank the anonymous referee for valuable comments that\nsubstantially improved the quality of this paper. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with the\nCentre National d'\u00c9tudes Spatiales (CNES) of France and the \nKorean Ministry of Science and Technology. This work has made extensive use of the MPA/JHU and the NYU SDSS value-added catalogs. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the\nHigher Education Funding Council for England. The SDSSWeb\nsite is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology,\nthe Korean Scientist Group, the Chinese Academy of Sciences\n(LAMOST), Los Alamos National Laboratory, the Max-Planck-\nInstitute for Astronomy (MPIA), the Max-Planck-Institute for\nAstrophysics (MPA), New Mexico State University, Ohio State\nUniversity, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.\nFacilities: GALEX, Sloan\n\nPublished - Lemonias2011p14044Astrophys_J.pdf
", "abstract": "We present results of the first unbiased search for extended ultraviolet (XUV)-disk galaxies undertaken to determine the space density of such galaxies. Our sample contains 561 local (0.001 < z < 0.05) galaxies that lie in the intersection of available Galaxy Evolution Explorer (GALEX) deep imaging (exposure time >1.5 \u00d7 10^4 s) and Sloan Digital Sky Survey DR7 footprints. We explore modifications to the standard classification scheme for our sample that includes both disk- and bulge-dominated galaxies. Visual classification of each galaxy in the sample reveals an XUV-disk frequency of up to 20% for the most nearby portion of our sample. On average over the entire sample (out to z = 0.05) the frequency ranges from a hard limit of 4%-14%. The GALEX imaging allows us to detect XUV disks beyond 100 Mpc. The XUV regions around XUV-disk galaxies are consistently bluer than the main bodies. We find a surprisingly high frequency of XUV emission around luminous red (NUV-r > 5) and green valley (3 < NUV-r < 5) galaxies. The XUV-disk space density in the local universe is >(1.5-4.2) \u00d7 10^(\u20133) Mpc^(\u20133). Using the XUV emission as an indicator of recent gas accretion, we estimate that the cold gas accretion rate onto these galaxies is >(1.7-4.6) \u00d7 10^(\u20133) M_\u2299 Mpc^(\u20133) yr^(\u20131). The number of XUV disks in the green valley and the estimated accretion rate onto such galaxies points to the intriguing possibility that 7%-18% of galaxies in this population are transitioning away from the red sequence.", "date": "2011-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "733", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 74", "id_number": "CaltechAUTHORS:20110607-083832342", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110607-083832342", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "American Museum of Natural History" }, { "agency": "Astrophysical Institute Potsdam" }, { "agency": "University of Basel" }, { "agency": "University of Cambridge" }, { "agency": "Case Western Reserve University" }, { "agency": "University of Chicago" }, { "agency": "Drexel University" }, { "agency": "Fermilab" }, { "agency": "Institute for Advanced Study" }, { "agency": "Japan Participation Group" }, { "agency": "Johns Hopkins University" }, { "agency": "Joint Institute for Nuclear Astrophysics" }, { "agency": "Kavli Institute for Particle Astrophysics and Cosmology" }, { "agency": "Korean Scientist Group" }, { "agency": "Chinese Academy of Sciences" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Max-Planck-Institute for Astrophysics (MPA)" }, { "agency": "New Mexico State University" }, { "agency": "Ohio State University" }, { "agency": "University of Pittsburgh" }, { "agency": "University of Portsmouth" }, { "agency": "Princeton University" }, { "agency": "United States Naval Observatory" }, { "agency": "University of Washington" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/733/2/74", "primary_object": { "basename": "Lemonias2011p14044Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/z8vw5-0vd51/files/Lemonias2011p14044Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Lemonias, Jenna J.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/g5a2y-ews42", "eprint_id": 23284, "eprint_status": "archive", "datestamp": "2023-08-22 02:26:57", "lastmod": "2023-10-23 18:58:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shri R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Jacobsen-J", "name": { "family": "Jacobsen", "given": "Janet" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Green-Y", "name": { "family": "Green", "given": "Yoav" } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "Derek B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Howell-J-L", "name": { "family": "Howell", "given": "Jacob L." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Keliser-I-K-W", "name": { "family": "Kleiser", "given": "Io K. W." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam" }, "orcid": "0000-0001-9515-478X" }, { "id": "Li-Weidong", "name": { "family": "Li", "given": "Weidong" } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Starr-D", "name": { "family": "Starr", "given": "Dan" } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Tendulkar-S-P", "name": { "family": "Tendulkar", "given": "Shriharsh P." }, "orcid": "0000-0003-2548-2926" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } }, { "id": "Kennea-J-A", "name": { "family": "Kennea", "given": "Jamie" }, "orcid": "0000-0002-6745-4790" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "Gustavo" } }, { "id": "Hale-D-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger M." } }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "Jeff" } }, { "id": "Velur-V", "name": { "family": "Velur", "given": "Viswa" } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Henning-J-R", "name": { "family": "Henning", "given": "John" } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "McKenna-D-L", "name": { "family": "McKenna", "given": "Dan" } }, { "id": "Blake-C-H", "name": { "family": "Blake", "given": "Cullen" } } ] }, "title": "PTF 10fqs: A Luminous Red Nova in the Spiral Galaxy Messier 99", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: AGB and post-AGB; stars: mass-loss; supernovae: general; supernovae: individual (PTF 10fqs); surveys", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 July 20; accepted 2011 February 4; published 2011 March 14.\n\nM.M.K. thanks the Gordon and Betty Moore Foundation for\na Hale Fellowship in support of graduate study. The Weizmann Institute PTF participation is supported in part by the Israel Science Foundation via grants to A.G.Y. The Weizmann-Caltech collaborative PTF effort is supported by the US\u2013Israel Binational Science Foundation. A.G.Y. and M.S. are jointly supported by the \"making connections\" Weizmann\u2013UK program. A.G.Y. further acknowledges support by a Marie Curie IRG fellowship and the Peter and Patricia Gruber Award, as well as funding by the Benoziyo Center for Astrophysics and the Yeda-Sela center at the Weizmann Institute. A.V.F.'s group and KAIT are supported by National Science Foundation (NSF) grant AST-0908886, the Sylvia & Jim Katzman Foundation, the Richard & Rhoda Goldman Fund, Gary and Cynthia Bengier, and the TABASGO Foundation; additional funding was provided by NASA through Spitzer grant 1322321, as well as HST grant AR-11248 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. J.S.B. and his group are partially funded by a DOE SciDAC grant. E.O.O. and D.P. are supported by the Einstein fellowship. L.B. is supported by the National Science Foundation under grants PHY 05-51164 and AST 07-07633. We are grateful to the staff of the Gemini Observatory for their promptness and high efficiency in attending to our TOO request. Likewise, we thank the staff of the Very Large Array and the Hobby\u2013Eberly Telescope. We acknowledge the following internet repositories: SEDS (Messier Objects) and GOLDMine (Virgo Cluster), Finally, as always, we are grateful to the librarians who maintain the ADS, the NED, and SIMBAD\ndata systems. The Hobby\u2013Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universit\u00e4t M\u00fcnchen, and Georg-August-Universit\u00e4t G\u00f6ttingen. The HET is named in honor of its principal benefactors,William P. Hobby and Robert E. Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome Optics, who fabricated several optics for the instrument but died before its completion; it is a joint project of the Hobby\u2013Eberly Telescope partnership and the\nInstituto de Astronom\u00eda de la Universidad Nacional Aut\u00f3noma de M\u00e9xico. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. The Expanded Very Large Array is operated by the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - Kasliwal2011p13405Astrophys_J.pdf
", "abstract": "The Palomar Transient Factory (PTF) is systematically charting the optical transient and variable sky. A primary\nscience driver of PTF is building a complete inventory of transients in the local universe (distance less than 200 Mpc). Here, we report the discovery of PTF 10fqs, a transient in the luminosity \"gap\" between novae and supernovae. Located on a spiral arm of Messier 99, PTF 10fqs has a peak luminosity of M_r = \u221212.3, red color (g \u2212 r = 1.0), and is slowly evolving (decayed by 1 mag in 68 days). It has a spectrum dominated by intermediate-width H\u03b1\n(\u2248930 km s^(\u22121)) and narrow calcium emission lines. The explosion signature (the light curve and spectra) is overall\nsimilar to that of M85 OT2006-1, SN 2008S, and NGC 300 OT. The origin of these events is shrouded in mystery\nand controversy (and in some cases, in dust). PTF 10fqs shows some evidence of a broad feature (around 8600 \u00c5)\nthat may suggest very large velocities (\u224810,000 km s^(\u22121)) in this explosion. Ongoing surveys can be expected to find\na few such events per year. Sensitive spectroscopy, infrared monitoring, and statistics (e.g., disk versus bulge) will eventually make it possible for astronomers to unravel the nature of these mysterious explosions.", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 134", "id_number": "CaltechAUTHORS:20110412-115639625", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110412-115639625", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Weizmann Institute" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "TABASGO Foundation" }, { "agency": "NASA", "grant_number": "1322321" }, { "agency": "NASA", "grant_number": "AR-11248" }, { "agency": "NASA", "grant_number": "AR-11248" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "TAPIR" }, { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/730/2/134", "primary_object": { "basename": "Kasliwal2011p13405Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/g5a2y-ews42/files/Kasliwal2011p13405Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Kasliwal, Mansi M.; Kulkarni, Shri R.; et el." }, { "id": "https://authors.library.caltech.edu/records/q85w7-z0767", "eprint_id": 23329, "eprint_status": "archive", "datestamp": "2023-08-22 02:27:40", "lastmod": "2023-10-23 19:00:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Efremova-B-V", "name": { "family": "Efremova", "given": "Boryana V." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David A." }, "orcid": "0000-0002-8528-7340" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "Denis" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Rey-S-C", "name": { "family": "Rey", "given": "Soo-Chang" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } } ] }, "title": "The Recent Star Formation in NGC 6822: An Ultraviolet Study", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 6822); galaxies: stellar content; Local Group; stars: formation; ultraviolet: stars", "note": "\u00a9 2011 American Astronomical Society. Received 2009 April 19; accepted 2011 January 7; published 2011 March 9. We thank Philip Massey for very helpful clarifications on the\ncalibration of the H\u03b1 image, Alin Tolea for initial discussions about the source-contour definition, and the anonymous referee for valuable comments. The GALEX data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is\nprovided by the NASA Office of Space Science via grantNAG5-\n7584 and by other grants and contracts. GALEX (The Galaxy\nEvolution Explorer) is a NASA Small Explorer, launched in\n2003 April. We gratefully acknowledge NASA's support for\nconstruction, operation, and science analysis of the GALEX\nmission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The H\u03b1 image used in this paper was obtained by Massey et al. (2007a) as part of the Survey of Local Group Galaxies Currently Forming Stars and downloaded from http://www.archive.noao.edu/nsa/. S.-C.R. is supported by the NRF of Korea to the Center for Galaxy Evolution Research.\n\nPublished - Efremova2011p13395Astrophys_J.pdf
", "abstract": "We characterize the star formation in the low-metallicity galaxy NGC 6822 over the past few hundred million years, using GALEX far-UV (FUV,1344-1786 \u00c5) and near-UV (NUV, 1771-2831 \u00c5) imaging, and ground-based H alpha imaging. From the GALEX FUV image, we define 77 star-forming (SF) regions with area > 860 pc^2, and surface brightness \u227e 26.8 mag (AB) arcsec^(-2), within 0\u00b0.2 (1.7 kpc) of the center of the galaxy. We estimate the extinction by interstellar dust in each SF region from resolved photometry of the hot\nstars it contains: E(B - V) ranges from the minimum foreground value of 0.22 mag up to 0.66 \u00b1 0.21 mag. The integrated FUV and NUV photometry, compared with stellar population models, yields ages of the SF complexes up to a few hundred Myr, and masses from 2 x 10^2 M_\u2299 to 1.5 x 10^6 M_\u2299. The derived ages and masses strongly depend on the assumed type of interstellar selective extinction, which we find to vary across the galaxy. The total mass of the FUV-defined SF regions translates into an average star formation rate (SFR) of 1.4 x 10^(-2) M_\u2299 yr^(-1) over the past 100 Myr, and SFR = 1.0 x 10^(-2) M_\u2299 yr^(-1) in the most recent 10 Myr. The latter is in agreement with the value that we derive from the H\u03b1 luminosity, SFR = 0.008 M_\u2299 yr^(-1). The SFR in the most recent epoch becomes higher if we add the SFR = 0.02 M_\u2299 yr^(-1) inferred from far-IR measurements, which trace star formation still embedded in dust (age \u227e a few Myr).", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 88", "id_number": "CaltechAUTHORS:20110414-085412903", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110414-085412903", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA", "grant_number": "NAG5-7584" }, { "agency": "National Research Foundation of Korea" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/730/2/88", "primary_object": { "basename": "Efremova2011p13395Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/q85w7-z0767/files/Efremova2011p13395Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Efremova, Boryana V.; Bianchi, Luciana; et el." }, { "id": "https://authors.library.caltech.edu/records/n6sr0-b7953", "eprint_id": 23324, "eprint_status": "archive", "datestamp": "2023-08-22 02:16:49", "lastmod": "2023-10-23 19:00:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Borthakuri-S", "name": { "family": "Borthakuri", "given": "Sanchayeeta" } }, { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik" } }, { "id": "Kauffmann-G", "name": { "family": "Kauffmann", "given": "Guinevere" } }, { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara" } }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "Claus" }, "orcid": "0000-0003-2685-4488" }, { "id": "Sembach-K", "name": { "family": "Sembach", "given": "Ken" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Chris" }, "orcid": "0000-0002-8650-1644" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" } ] }, "title": "Extreme Feedback and the Epoch of Reionization: Clues in the Local Universe", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies: kinematics and dynamics; intergalactic medium", "note": "\u00a9 2011 American Astronomical Society. Received 2010 November 17; accepted 2011 January 19; published 2011 February 23. Based on observations with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The observations are associated with GO programs\n10920, 11107, and 11727.\nFacilities: HST(COS), GALEX, Spitzer\n\nPublished - Heckman2011p13384Astrophys_J.pdf
", "abstract": "The source responsible for reionizing the universe at z > 6 remains uncertain. While an energetically adequate population of star-forming galaxies may be in place, it is unknown whether a large enough fraction of their ionizing radiation can escape into the intergalactic medium. Attempts to measure this escape fraction in intensely star-forming galaxies at lower redshifts have largely yielded upper limits. In this paper, we present new Hubble Space Telescope Cosmic Origins Spectrograph and archival Far-Ultraviolet Spectroscopic Explorer (FUSE) far-UV spectroscopy of a sample of 11 Lyman Break Analogs (LBAs), a rare population of local galaxies that strongly resemble the high-z Lyman Break galaxies. We combine these data with Sloan Digital Sky Survey optical spectra and Spitzer photometry. We also analyze archival FUSE observations of 15 typical UV-bright local starbursts. We find evidence of small covering factors for optically thick neutral gas in three cases. This is based on two independent pieces of evidence: a significant residual intensity in the cores of the strongest interstellar absorption-lines tracing neutral gas and a small ratio of extinction-corrected H\u03b1 to UV plus far-IR luminosities. These objects represent three of the four LBAs that contain a young, very compact (~10^2 pc), and highly massive (~10^9 M_\u2299) dominant central object (DCO). These three objects also differ from the other galaxies in showing a significant amount of blueshifted Ly\u03b1 emission, which may be related to the low covering factor of neutral gas. All four LBAs with DCOs in our sample show extremely high velocity outflows of interstellar gas, with line centroids blueshifted by about 700 km s^(\u20131) and maximum outflow velocities reaching at least 1500 km s^(\u20131). We show that these properties are consistent with an outflow driven by a powerful starburst that is exceptionally compact. We speculate that such extreme feedback may be required to enable the escape of ionizing radiation from star-forming galaxies.", "date": "2011-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 5", "id_number": "CaltechAUTHORS:20110414-085411947", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110414-085411947", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/730/1/5", "primary_object": { "basename": "Heckman2011p13384Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/n6sr0-b7953/files/Heckman2011p13384Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Heckman, Timothy M.; Borthakuri, Sanchayeeta; et el." }, { "id": "https://authors.library.caltech.edu/records/xqt85-7cp06", "eprint_id": 23001, "eprint_status": "archive", "datestamp": "2023-08-19 05:41:09", "lastmod": "2023-10-23 17:47:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "B. Y." } }, { "id": "Wheatley-J-M", "name": { "family": "Wheatley", "given": "J. M." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "GALEX observations of quasar variability in the ultraviolet", "ispublished": "pub", "full_text_status": "public", "keywords": "ultraviolet: galaxies \u2013 quasars: general", "note": "\u00a9 ESO 2011. Received 4 October 2010, Accepted 14 December 2010, Published online 19 January 2011. We particularly acknowledge the dedicated work of the\nGALEX mission operations support staff at JPL/Caltech in Pasadena. Financial\nsupport for this research was provided by the NASA GALEX Guest Investigator\nprogram and NASA grant NAS5-98034 to UC Berkeley. We are indebted to Dr.\nSuvi Gezari who made many suggestions that have greatly improved this paper.\n\nPublished - Welsh2011p13145Astron_Astrophys.pdf
", "abstract": "Aims. Using archival observations recorded over a 5+ year timeframe with the NASA GALaxy Evolution eXplorer (GALEX) satellite, we present a study of the ultraviolet (UV) variability of 4360 quasars of redshifts up to z = 2.5 that have optical counterparts in the Sloan Digital Sky Survey DR5 spectroscopic catalog of Schneider et al. (2007, AJ, 134, 102). The observed changes in both the far UV (FUV: 1350\u22121785 \u00c5) and near UV (NUV: 1770\u22122830 \u00c5) AB magnitudes as a function of time may help differentiate between models of the emission mechanisms thought to operate in these active galaxies.\nMethods. A list of NUV and FUV variable quasars was derived from the UV light-curves of sources with 5 or more observational visits by GALEX that spanned a time-frame > 3 months. By measuring the error in the derived mean UV magnitude from the series of GALEX observations for each source, quasars whose UV variability was greater than the 3-\u03c3 variance from the mean observed value were deemed to be (intrinsically) UV variable. This conservative selection criterion (which was applied to both FUV and NUV observations) resulted in identifying 550 NUV and 371 FUV quasars as being statistically significant UV variable objects.\nResults. Following the work of Vanden Berk et al. (2004, ApJ, 601, 692), we have performed a structure function (SF) analysis of these data to search for possible correlations between UV variability and parameters such as rest frame time-lag, redshift, luminosity and radio loudness. Firstly, we observe that the amplitudes of variability as a function of time-lag for both the NUV and FUV data are far larger than those observed at visible wavelengths. Secondly, the levels of FUV variability are greater than those observed in the NUV for a given value of time-lag. Also, the amplitudes of both the NUV and FUV variability of quasars increase as a function of rest frame time-lag, irrespective of the value of quasar redshift, for time-lags <200 days. For time-lags >300 days there is a pronounced rollover in the NUV SF for all redshift values, which is also observed (with a lower signi\u00decance) in the FUV variability data. Although we find no strong relationship between UV variability and redshift, our data do show that higher redshift quasars appear to be more variable than their low redshift counterparts. Our data also show that, for all values of time-lag, the more luminous quasars tend to be slightly less UV variable, with perhaps the exception of FUV variable quasars for short time-lags. \nAlthough our data sample is small, we find that radio-loud quasars are marginally more variable than radio quiet ones by a factor ~2 in the NUV and by a factor 1 \u2212 3 in the FUV. Therefore, our present observations support the notion in which the radio properties of quasars have a limited influence on the observed UV variability of these objects. In summation, our present analysis favors a quasar model in which UV variability is mainly due to stochastic changes in the underlying continuum level, rather than models that favor gravitational microlensing or discrete-event processes.", "date": "2011-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "527", "publisher": "EDP Sciences", "pagerange": "Art. No. A15", "id_number": "CaltechAUTHORS:20110321-090452720", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110321-090452720", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-98034" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1051/0004-6361/201015865", "primary_object": { "basename": "Welsh2011p13145Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/xqt85-7cp06/files/Welsh2011p13145Astron_Astrophys.pdf" }, "pub_year": "2011", "author_list": "Welsh, B. Y.; Wheatley, J. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/37y1v-krc71", "eprint_id": 23052, "eprint_status": "archive", "datestamp": "2023-08-19 05:37:49", "lastmod": "2023-10-23 17:51:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Perets-H-B", "name": { "family": "Perets", "given": "Hagai B." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Crockett-R-M", "name": { "family": "Crockett", "given": "R. Mark." } }, { "id": "Anderson-J-P", "name": { "family": "Anderson", "given": "Joseph P." }, "orcid": "0000-0003-0227-3451" }, { "id": "James-P-A", "name": { "family": "James", "given": "Phil A." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Leonard-D-C", "name": { "family": "Leonard", "given": "Douglas C." } } ] }, "title": "The Old Environment of the Faint Calcium-rich Supernova SN 2005cz", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: star formation \u2013 H_(II) regions \u2013 stars: formation \u2013 supernovae: general \u2013 supernovae:\nindividual (SN 2005cz) \u2013 white dwarfs", "note": "\u00a9 2011 American Astronomical Society. Received 2010 December 1; accepted 2011 January 18; published 2011 January 31. We gratefully acknowledge NASA, the Centre National\nd'Etudes Spatiales of France, and the Korean Ministry of\nScience and Technology for the development, construction,\noperation, and science analysis of the GALEX (Galaxy Evolution\nExplorer) mission.\n\nPublished - Perets2011p13018Astrophys_J_Lett.pdf
", "abstract": "The supernova SN 2005cz has recently attracted some attention due to the fact that it was spectroscopically similar to type Ib supernovae (SNe Ib), a class that is presumed to result from the core collapse of massive stars, yet it occurred in an elliptical galaxy, where one expects very few massive stars to exist. Two explanations for this remarkable event were put forward. Perets et al. associate SN 2005cz with the class of Ca-rich, faint SNe Ib, which likely result from old double-white-dwarf systems with an He-rich secondary. On the other hand, Kawabata et al. suggest that SN 2005cz is indeed a core-collapse event (in a binary system), albeit of a star at the lower end of the mass range, 10-12 M_\u2299. The existence of this star in its elliptical host is explained as resulting from low-level star formation (SF) activity in that galaxy. Here we present extensive observations of the location of SN 2005cz, sensitive to a variety of SF tracers, including optical spectroscopy, H\u03b1 emission, UV emission, and Hubble Space Telescope photometry. We show that NGC 4589, the host galaxy of SN 2005cz, does not show any signatures of a young stellar population or recent SF activity either close to or far from the location of SN 2005cz.", "date": "2011-02-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "728", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L36", "id_number": "CaltechAUTHORS:20110322-130425655", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110322-130425655", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/2041-8205/728/2/L36", "primary_object": { "basename": "Perets2011p13018Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/37y1v-krc71/files/Perets2011p13018Astrophys_J_Lett.pdf" }, "pub_year": "2011", "author_list": "Perets, Hagai B.; Gal-Yam, Avishay; et el." }, { "id": "https://authors.library.caltech.edu/records/ek4b5-abg28", "eprint_id": 23043, "eprint_status": "archive", "datestamp": "2023-08-22 01:51:57", "lastmod": "2023-10-23 17:50:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran" }, "orcid": "0000-0002-6786-8774" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" } ] }, "title": "The Extreme Hosts of Extreme Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; stars: luminosity function, mass function; stars: massive; supernovae: general", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 September 7; accepted 2010 November 12; published 2010 December 23.\n\nWe gratefully acknowledge the anonymous referee for a careful reading and useful suggestions that improved the presentation of this work. Joint research by A.G. and M.S. is supported by the Weizmann-UK program. A.G. is also supported by grants from the Israeli Science Foundation, an EU FP7 Marie Curie IRG Fellowship, and a research grant from the Peter and Patricia Gruber Awards. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. 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 the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/ The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology,\nthe Korean Scientist Group, the Chinese Academy of Sciences\n(LAMOST), Los Alamos National Laboratory, the Max-Planck-\nInstitute for Astronomy (MPIA), the Max-Planck-Institute for\nAstrophysics (MPA), New Mexico State University, Ohio State\nUniversity, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department\nof Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources and data storage for this\nproject.\n\nPublished - Neill2011p13135Astrophys_J.pdf
", "abstract": "We use GALEX ultraviolet (UV) and optical integrated photometry of the hosts of 17 luminous supernovae (LSNe, having peak M_V < \u201321) and compare them to a sample of 26, 000 galaxies from a cross-match between the SDSS DR4 spectral catalog and GALEX interim release 1.1. We place the LSN hosts on the galaxy NUV \u2013 r versus M_r color-magnitude diagram (CMD) with the larger sample to illustrate how extreme they are. The LSN hosts appear to favor low-density regions of the galaxy CMD falling on the blue edge of the blue cloud toward the low-luminosity end. From the UV-optical photometry, we estimate the star formation history of the LSN hosts. The hosts have moderately low star formation rates (SFRs) and low stellar masses (M_*) resulting in high specific star formation rates (sSFR). Compared with the larger sample, the LSN hosts occupy low-density regions of a diagram plotting sSFR versus M_* in the area having higher sSFR and lower M_*. This preference for low M_*, high sSFR hosts implies that the LSNe are produced by an effect having to do with their local environment. The correlation of mass with metallicity suggests that perhaps wind-driven mass loss is the factor that prevents LSNe from arising in higher-mass, higher-metallicity hosts. The massive progenitors of the LSNe (>100 M_\u2609), by appearing in low-SFR hosts, are potential tests for theories of the initial mass function that limit the maximum mass of a star based on the SFR.", "date": "2011-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "727", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20110322-095700336", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110322-095700336", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Weizmann-UK" }, { "agency": "Israel Science Foundation" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Peter and Patricia Gruber Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/727/1/15", "primary_object": { "basename": "Neill2011p13135Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/ek4b5-abg28/files/Neill2011p13135Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Neill, James D.; Quimby, Robert; et el." }, { "id": "https://authors.library.caltech.edu/records/1c6q3-ebq87", "eprint_id": 22059, "eprint_status": "archive", "datestamp": "2023-08-22 01:42:03", "lastmod": "2023-10-23 15:38:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Supernova Constraints and Systematic Uncertainties from the First Three Years of the Supernova Legacy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters; cosmology: observations; supernovae: general", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 August 6; accepted 2010 October 22; published 2010 December 13.\n\nThe SNLS collaboration gratefully acknowledges the assistance of Pierre Martin and the CFHT Queued Service Observations team. Jean-Charles Cuillandre and Kanoa Withington were also indispensable in making possible real-time data reduction at CFHT. This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique\n(CNRS) of France, and the University of Hawaii. This work is\nbased in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. Canadian collaboration members acknowledge support fromNSERC and CIAR, French collaboration members from CNRS/IN2P3, CNRS/INSU and CEA, and Portugese members from Funda\u00b8cao para a Ciencia e Tecnologia. We thank D. J. Schlegel for making the updated SDSS calibration available to us prior to publication, and A. Riess, A. Landolt, and R. Kessler for many useful discussions. M. Hicken provided useful feedback about the CfAIII SN sample. We thank R. Bohlin for helping us understand the uncertainties in the STIS SED of Vega, and R. de Jong for clarifying the NICMOS nonlinearity corrections. Finally, we thank the anonymous referee, whose extremely thoughtful and thorough comments greatly improved this paper.\nFacilities: CFHT (MegaCam), Gemini:Gillett (GMOS-N),\nGemini:South (GMOS-S), Keck:I (LRIS), VLT:Antu (FORS2),\nVLT:Kueyen (FORS1)\n\nPublished - Conley2011p12541Astrophys_J_Suppl_S.pdf
", "abstract": "We combine high-redshift Type Ia supernovae from the first three years of the Supernova Legacy Survey (SNLS) with other supernova (SN) samples, primarily at lower redshifts, to form a high-quality joint sample of 472 SNe (123 low-z, 93 SDSS, 242 SNLS, and 14 Hubble Space Telescope). SN data alone require cosmic acceleration at >99.999% confidence, including systematic effects. For the dark energy equation of state parameter (assumed constant out to at least z = 1.4) in a flat universe, we find w = \u20130.91^(+0.16)_(\u20130.20)(stat)^(+0.07)_(\u20130.14)(sys) from SNe only, consistent with a cosmological constant. Our fits include a correction for the recently discovered relationship between host-galaxy mass and SN absolute brightness. We pay particular attention to systematic uncertainties, characterizing them using a systematic covariance matrix that incorporates the redshift dependence of these effects, as well as the shape-luminosity and color-luminosity relationships. Unlike previous work, we include the effects of systematic terms on the empirical light-curve models. The total systematic uncertainty is dominated by calibration terms. We describe how the systematic uncertainties can be reduced with soon to be available improved nearby and intermediate-redshift samples, particularly those calibrated onto USNO/SDSS-like systems.", "date": "2011-01", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "192", "publisher": "American Astronomical Society", "pagerange": "Art. No. 1", "id_number": "CaltechAUTHORS:20110207-162201734", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110207-162201734", "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": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0067-0049/192/1/1", "primary_object": { "basename": "Conley2011p12541Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/1c6q3-ebq87/files/Conley2011p12541Astrophys_J_Suppl_S.pdf" }, "pub_year": "2011", "author_list": "Conley, A.; Ellis, R. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/3ey62-4qb79", "eprint_id": 24179, "eprint_status": "archive", "datestamp": "2023-08-19 04:52:06", "lastmod": "2024-01-13 05:17:34", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lu-Jessica-R", "name": { "family": "Lu", "given": "Jessica R." }, "orcid": "0000-0001-9611-0009" }, { "id": "Clarkson-W-I", "name": { "family": "Clarkson", "given": "Will" } }, { "id": "McCrady-N", "name": { "family": "McCrady", "given": "Nate" } }, { "id": "Ghez-A-M", "name": { "family": "Ghez", "given": "Andrea M." }, "orcid": "0000-0003-3230-5055" }, { "id": "Morris-M-R", "name": { "family": "Morris", "given": "Mark R." }, "orcid": "0000-0002-6753-2066" }, { "id": "Stolte-A", "name": { "family": "Stolte", "given": "Andrea" } }, { "id": "Yelda-S", "name": { "family": "Yelda", "given": "Sylvana" }, "orcid": "0000-0001-5036-4329" }, { "id": "Do-Tuan", "name": { "family": "Do", "given": "Tuan" }, "orcid": "0000-0001-9554-6062" } ] }, "title": "Clarifying our View of Star Formation in Massive Young Clusters with Adaptive Optics", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2011 Astronomical Society of the Pacific. J. R. Lu's support for this work was provided by the California\nInstitute of Technology's Millikan Postdoctoral Fellowship. The W. M. Keck Observatory 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 Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the\nopportunity to conduct observations from this mountain.\n\nPublished - Lu2011p13930Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf
", "abstract": "Observations of massive (> 10^4 M_\u2299), young (<10 Myr) star clusters within our Galaxy allow us to fully sample the upper end of the initial mass function within a single star formation event. Such clusters also reside in a range of environments including the Galactic disk, the Galactic center region, and immediately surrounding the supermassive black hole in our Galactic nucleus. However, studies of\nthese clusters are limited by crowding in the dense cores, strong and variable visible extinction, and confusion between cluster members and contaminating field stars. Using\nKeck laser-guided adaptive optics observations, we obtain high-resolution images and high-precision proper motions to both identify individual cluster members and investigate\nthe kinematic properties of such clusters. As we build up complete proper motion data sets for several massive young clusters, our multi-color near-infrared photometry\nwill yield precise mass functions that can be compared to search for environmental dependencies.", "date": "2011", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "63-71", "id_number": "CaltechAUTHORS:20110623-094921842", "isbn": "978-1-58381-760-5", "book_title": "UP2010: Have Observations Revealed a Variable Upper End of the Initial Mass Function?", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110623-094921842", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech Millikan Fellowship" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." } } ] }, "primary_object": { "basename": "Lu2011p13930Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf", "url": "https://authors.library.caltech.edu/records/3ey62-4qb79/files/Lu2011p13930Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf" }, "pub_year": "2011", "author_list": "Lu, Jessica R.; Clarkson, Will; et el." }, { "id": "https://authors.library.caltech.edu/records/e3bxf-v1w40", "eprint_id": 24158, "eprint_status": "archive", "datestamp": "2023-08-19 04:51:52", "lastmod": "2024-01-13 05:17:28", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Li-Gongjie", "name": { "family": "Li", "given": "Gongjie" }, "orcid": "0000-0001-8308-0808" } ] }, "title": "Extreme Starbursts and the Low Mass IMF", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2011 Astronomical Society of the Pacific.\n\nThe modeling of starbursts and the use of the 4000\u00c5 break to\nconstrain the low mass IMF was done in collaboration with P. Capak (Li et al. 2010).\n\nPublished - Scoville2011p13940Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf
", "abstract": "The temperatures and densities of the interstellar medium (ISM) in starburst galaxies are greatly elevated compared to those in star forming giant molecular clouds (GMCs) in normal galaxies. I review the observed ISM properties in the prototype starburst Arp 200 and then discuss considerations for star formation in such starburst galaxy nuclei. We have also found a previously unrecognized observational constraint on the low mass star populations applicable to these starbursts. Using stellar population synthesis models from Starburst99 with instantaneous and constant starbursts, we identify and quantify spectral diagnostics for stellar populations. The characteristic age of the stellar population dominating the restframe optical (not the younger stars dominating the UV) can be estimated from the 4000\u00c5 break strength (D4000). We find that the presence of the 4000\u00c5 break requires a stellar population older than ~100 Myr (since OB stars would dominate the continuum short of 4000\u00c5 and they exhibit no break). Very importantly, we also find that the initial mass function (IMF) must extend down to a few solar masses if the 4000\u00c5 break is present. Thus, the detection of the 4000\u00c5 break implies an IMF extending to low mass. The strength of the 4000\u00c5 break can be used to constrain the IMF at low stellar masses, while the absence of the feature could be used to identify PopIII stars (which would have low metallicity and probably few low mass stars). The break is, in fact, observed in Arp 220 and in the z = 2 \u2013 7 galaxy SEDs, casting doubt on recent suggestions of top heavy IMFs for high z galaxies and starbursts. The apparent invariance of the IMF is likely due to the fact that the fragmentation scale for stellar mass condensations occurs at very high density on scales of ~100 AU. At this point, the densities will be ~10^(11) per cc and the initial conditions in the galactic GMCs will have been long forgotten. This 100 AU scale corresponds to the point at which solar mass condensations become optical thick in the far infrared and thus separate quasi-statically from the overall collapse \u2013 it is also the typical scale of binary star separations, lending support to the notion that this is the scale for stellar mass fragmentation within collapsing cloud cores.", "date": "2011", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "317-324", "id_number": "CaltechAUTHORS:20110621-120200217", "isbn": "978-1-58381-760-5", "book_title": "UP2010: Have Observations Revealed a Variable Upper End of the Initial Mass Function?", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110621-120200217", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." } } ] }, "primary_object": { "basename": "Scoville2011p13940Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf", "url": "https://authors.library.caltech.edu/records/e3bxf-v1w40/files/Scoville2011p13940Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf" }, "pub_year": "2011", "author_list": "Scoville, N. and Li, Gongjie" }, { "id": "https://authors.library.caltech.edu/records/3gktk-fmb43", "eprint_id": 24170, "eprint_status": "archive", "datestamp": "2023-08-19 04:51:57", "lastmod": "2024-01-13 05:17:30", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie A." } } ] }, "title": "H\u03b1 and UV imaging of Low Surface Brightness Galaxies and Extended UV Disks", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2011 Astronomical Society of the Pacific.\nGALEX is a NASA Small Explorer, launched in 2003 April.\nWe gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - Wyder2011p13941Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf
", "abstract": "GALEX observations have revealed UV emission extending far beyond the optical and H-alpha disks of several nearby spiral galaxies, raising the question of possible massive star deficiency, i.e., deviations from the standard 'universal' stellar initial mass function (IMF) at the upper end, in certain low density environments. We have undertaken an H\u03b1 imaging survey of low surface brightness galaxies observed by GALEX and with existing HI maps with the aim of investigating the variation of the H\u03b1/UV ratio with the local density. Here we present preliminary results for 14 such galaxies observed with the Large Format Camera on the Palomar 200 inch telescope using custom narrow band filters.", "date": "2011", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "235-239", "id_number": "CaltechAUTHORS:20110622-152009146", "isbn": "978-1-58381-760-5", "book_title": "Up2010: Have Observations Revealed a Variable Upper End of the Initial Mass Function?", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110622-152009146", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." } } ] }, "primary_object": { "basename": "Wyder2011p13941Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf", "url": "https://authors.library.caltech.edu/records/3gktk-fmb43/files/Wyder2011p13941Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf" }, "pub_year": "2011", "author_list": "Wyder, Ted K. and Treyer, Marie A." }, { "id": "https://authors.library.caltech.edu/records/381t3-31q06", "eprint_id": 24180, "eprint_status": "archive", "datestamp": "2023-08-19 04:52:11", "lastmod": "2024-01-13 05:17:36", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" } ] }, "title": "Identifying Variations to the IMF at High-z Through Deep Radio Surveys", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2011 Astronomical Society of the Pacific.\n\nI would like to thank the organizers of the UP2010 conferences for\nputting together an exciting and diverse program, as well for letting me be a part of it.\n\nPublished - Murphy2011p13942Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf
", "abstract": "In this article I briefly describe how deep radio surveys may provide a\nmeans to identify variations in the upper end of the initial mass function (IMF) in star-forming\ngalaxies at high redshifts (i.e., z \u2273 3). At such high redshifts, I argue that deep\nradio continuum observations at frequencies \u227310 GHz using next generation facilities\n(e.g., EVLA, MeerKAT, SKA/NAA) will likely provide the most accurate measurements\nfor the ionizing photon rates (star formation rates; SFRs) of normal galaxies\nsince their non-thermal emission should be highly suppressed due to the increased inverse\nCompton (IC) losses from the cosmic microwave background (CMB), leaving\nonly thermal (free-free) emission detectable. Thus, a careful analysis of such observations\nin combination with future ALMA and JWST data, measuring the rest-frame\nfar-infrared and UV emission from the same population of galaxies, may yield the best\nmeans to search for variability in the stellar IMF at such epochs.", "date": "2011", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "361-368", "id_number": "CaltechAUTHORS:20110623-095747177", "isbn": "978-1-58381-760-5", "book_title": "UP2010: Have Observations Revealed a Variable Upper End of the Initial Mass Function?", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110623-095747177", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." } } ] }, "primary_object": { "basename": "Murphy2011p13942Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf", "url": "https://authors.library.caltech.edu/records/381t3-31q06/files/Murphy2011p13942Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf" }, "pub_year": "2011", "author_list": "Murphy, Eric J." }, { "id": "https://authors.library.caltech.edu/records/0xkm6-12e13", "eprint_id": 24182, "eprint_status": "archive", "datestamp": "2023-08-19 04:52:15", "lastmod": "2024-01-13 05:17:38", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" } ] }, "title": "Measuring the Upper End of the Initial Mass Function with Supernovae", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2011 Astronomical Society of the Pacific.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's support for construction,\noperation, and science analysis for the GALEX mission, developed in cooperation\nwith the Centre National d'Etudes Spatiales of France and the Korean Ministry\nof Science and Technology.\nFunding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation,\nthe Participating Institutions, the National Science Foundation, the U.S. Department\nof Energy, the National Aeronautics and Space Administration, the Japanese\nMonbukagakusho, the Max Planck Society, and the Higher Education Funding Council\nfor England. The SDSS Web Site is http://www.sdss.org/.\nThis research has made use of the NASA/IPAC Extragalactic Database (NED)\nwhich is operated by the Jet Propulsion Laboratory, California Institute of Technology,\nunder contract with the National Aeronautics and Space Administration.\n\nPublished - Neill2011p13943Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf
", "abstract": "Supernovae arise from progenitor stars occupying the upper end of the\ninitial mass function. Their extreme brightness allows individual massive stars to be\ndetected at cosmic distances, lending supernovae great potential as tracers of the upper\nend of the IMF and its evolution. Exploiting this potential requires progress in many\nareas of supernova science. These include understanding the progenitor masses that\nproduce various types of supernovae and accurately characterizing the supernova outburst\nand the environment in which it was produced. I present some preliminary work\nidentifying the environmental conditions that produce the most luminous supernovae,\nbelieved to arise from stars with masses greater than 100 M_\u2299. I illustrate that the presence\nof these extreme supernovae in small star-forming dwarfs can be used to test our\nunderstanding of the upper end of the IMF.", "date": "2011", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "329-335", "id_number": "CaltechAUTHORS:20110623-105227213", "isbn": "978-1-58381-760-5", "book_title": "UP2010: Have Observations Revealed a Variable Upper End of the Initial Mass Function?", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110623-105227213", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." } } ] }, "primary_object": { "basename": "Neill2011p13943Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf", "url": "https://authors.library.caltech.edu/records/0xkm6-12e13/files/Neill2011p13943Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf" }, "pub_year": "2011", "author_list": "Neill, James D." }, { "id": "https://authors.library.caltech.edu/records/qegm5-1nh61", "eprint_id": 24172, "eprint_status": "archive", "datestamp": "2023-08-19 04:52:02", "lastmod": "2024-01-13 05:17:32", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-J", "name": { "family": "Cooke", "given": "Jeff" }, "orcid": "0000-0001-5703-2108" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Barton-E-J", "name": { "family": "Barton", "given": "Elizabeth J." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" } ] }, "title": "Type IIn Supernova Detections in z ~ 2 Lyman Break Galaxies: Probing the IMF Directly", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2011 Astronomical Society of the Pacific.\n\nBased on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a\ncollaborative project of NRC and CNRS.\n\nPublished - Cooke2011p13932Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf
", "abstract": "Type IIn supernovae (SNe IIn) exhibit luminous ultraviolet continua during outburst and luminous, long-lived narrow ultraviolet and optical emission lines attributed to circumstellar interaction. These properties have enabled successful detections at z ~ 2 in archival imaging and continued investigations from late-time spectroscopy. Because SNe IIn are believed to have massive (\u227350M_\u2609) progenitors, searches in the well-studied Lyman break galaxy (LBG) host population offer the prospect of testing the form of the high-redshift stellar initial mass function (IMF) in a high density star formation environment directly. I briefly discuss our z ~ 2 photometric detection method targeting LBGs in the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) and present data from the first 6 confirmed z ~ 2 SNe IIn pulled from 30 photometric SN candidates. A comparison of the color and magnitude distributions of the SN host galaxies to that of the full LBG sample finds that z ~ 2 SNe preferentially occur in bluer, fainter galaxies. I conclude with a discussion of an approach that uses the CFHTLS pilot sample to provide a first estimate of the form of the high-redshift IMF. Upcoming deep synoptic imaging surveys will greatly improve z ~ 2 SNe IIn statistics from ~10^5 expected detections and future large aperture space- and ground-based telescopes will have the sensitivities to extend this work to z \u2273 6.", "date": "2011", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "337-344", "id_number": "CaltechAUTHORS:20110622-152037317", "isbn": "978-1-58381-760-5", "book_title": "Up2010: Have Observations Revealed a Variable Upper End of the Initial Mass Function?", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110622-152037317", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Treyer-M", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." } } ] }, "primary_object": { "basename": "Cooke2011p13932Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf", "url": "https://authors.library.caltech.edu/records/qegm5-1nh61/files/Cooke2011p13932Up2010_Have_Observations_Revealed_A_Variable_Upper_End_Of_The_Initial_Mass_Function.pdf" }, "pub_year": "2011", "author_list": "Cooke, Jeff; Sullivan, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/jvef9-dyw39", "eprint_id": 21416, "eprint_status": "archive", "datestamp": "2023-08-22 01:31:43", "lastmod": "2023-10-21 00:01:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "R." } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "G." } }, { "id": "Hale-D", "name": { "family": "Hale", "given": "D." } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "R." } }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "J." } }, { "id": "Velur-V", "name": { "family": "Velur", "given": "V." } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Henning-J", "name": { "family": "Henning", "given": "J." } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "K." } }, { "id": "McKenna-D", "name": { "family": "McKenna", "given": "D." } } ] }, "title": "Supernova PTF 09UJ: A Possible Shock Breakout from a Dense Circumstellar Wind", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (PTF 09uj)", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2010 July 9; accepted 2010 September 27; published 2010 November 12.\nWe thank an anonymous referee for useful comments. E.O.O.\nand D.P. are supported by an Einstein fellowship. S.B.C. and\nA.V.F. acknowledge generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/\nSwift grants NNX09AL08G and NNX10AI21G, and NSF grant\nAST-0908886. A.G. acknowledges support by the Israeli and\nthe US-Israel Binational Science Foundations, an EU/IRG fellowship,\nthe Benoziyo Center for Astrophysics, and the Peter\nand Patricia Gruber Awards. The National Energy Research\nScientific Computing Center, which is supported by the Office\nof Science of the U. S. Department of Energy under Contract\nNo. DE-AC02-05CH11231, provided staff, computational resources,\nand data storage for this project. P.E.N. acknowledges\nsupport from the US Department of Energy Scientific Discovery\nthrough Advanced Computing program under contract DEFG02-\n06ER06-04. J.S.B.'s work on PTF was supported by NSF/\nOIA award AST-0941742 (\"Real-Time Classification of Massive\nTime-Series Data Streams\"). L.B. and K.S. are supported\nby the NSF under grants PHY 05-51164 and AST 07-07633.\n\nPublished - Ofek2010p12144Astrophys_J.pdf
", "abstract": "Type-IIn supernovae (SNe IIn), which are characterized by strong interaction of their ejecta with the surrounding circumstellar matter (CSM), provide a unique opportunity to study the mass-loss history of massive stars shortly before their explosive death. We present the discovery and follow-up observations of an SN IIn, PTF 09uj, detected by the Palomar Transient Factory (PTF). Serendipitous observations by Galaxy Evolution Explorer (GALEX) at ultraviolet (UV) wavelengths detected the rise of the SN light curve prior to the PTF discovery. The UV light curve of the SN rose fast, with a timescale of a few days, to a UV absolute AB magnitude of about \u201319.5. Modeling our observations, we suggest that the fast rise of the UV light curve is due to the breakout of the SN shock through the dense CSM (n \u2248 10^(10) cm^(\u20133)). Furthermore, we find that prior to the explosion the progenitor went through a phase of high mass-loss rate (~0.1 M_\u2299 yr^(\u20131)) that lasted for a few years. The decay rate of this SN was fast relative to that of other SNe IIn.", "date": "2010-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "724", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1396-1401", "id_number": "CaltechAUTHORS:20101217-083631333", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101217-083631333", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX09AL08G" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "NSF", "grant_number": "AST-0941742" }, { "agency": "NASA Einstein Fellowship" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/724/2/1396", "primary_object": { "basename": "Ofek2010p12144Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/jvef9-dyw39/files/Ofek2010p12144Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Ofek, E. O.; Neill, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/7dn08-fg096", "eprint_id": 21703, "eprint_status": "archive", "datestamp": "2023-08-19 04:41:16", "lastmod": "2023-10-21 00:15:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara" } }, { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Law-D-R", "name": { "family": "Law", "given": "David R." }, "orcid": "0000-0002-9402-186X" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Mallery-R-P", "name": { "family": "Mallery", "given": "Ryan" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy H." } } ] }, "title": "The kinematics of ionized gas in lyman-break analogs at z ~ 0.2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: kinematics and dynamics \u2013 galaxies: starburst", "note": "\u00a9 2010 American Astronomical Society. Received 2010 July 16; accepted 2010 September 20; published 2010 November 12. The authors thank Jim Lyke, Al Conrad, Randy Campbell, and\nHien Tran for invaluable assistance with the laser observations.\nWe also thank the anonymous referee for useful comments\nregarding dynamical masses. T.S.G. thanks Brant Robertson for\nuseful discussions concerning theoretical modeling of galaxy\nformation at z ~ 2. We also thank those of Hawaiian ancestry\nfor hospitably allowing telescope operations on the summit of\nMauna Kea.\n\nPublished - Goncalves2010p12146Astrophys_J.pdf
", "abstract": "We present results for 19 \"Lyman-break analogs\" observed with Keck/OSIRIS with an adaptive-optics-assisted\nspatial resolution of less than 200 pc. We detect satellites/companions, diffuse emission, and velocity shear, all\nwith high signal-to-noise ratios. These galaxies present remarkably high velocity dispersion along the line of sight\n(~70 km s^(\u22121)), much higher than standard star-forming spirals in the low-redshift universe. We artificially redshift\nour data to z ~ 2.2 to allow for a direct comparison with observations of high-z Lyman-break galaxies and find\nstriking similarities between both samples. This suggests that either similar physical processes are responsible\nfor their observed properties, or, alternatively, that it is very difficult to distinguish between different mechanisms\noperating in the low- versus high-redshift starburst galaxies based on the available data. The comparison between\nmorphologies in the UV/optical continuum and our kinemetry analysis often shows that neither is by itself sufficient\nto confirm or completely rule out the contribution from recent merger events. We find a correlation between the\nkinematic properties and stellar mass, in that more massive galaxies show stronger evidence for a disk-like structure.\nThis suggests a co-evolutionary process between the stellar mass buildup and the formation of morphological and\ndynamical substructure within the galaxy.", "date": "2010-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "724", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1373-1388", "id_number": "CaltechAUTHORS:20110111-114649643", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110111-114649643", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/724/2/1373", "primary_object": { "basename": "Goncalves2010p12146Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7dn08-fg096/files/Goncalves2010p12146Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Gon\u00e7alves, Thiago S.; Basu-Zych, Antara; et el." }, { "id": "https://authors.library.caltech.edu/records/bvhe7-rzy83", "eprint_id": 20211, "eprint_status": "archive", "datestamp": "2023-08-22 00:48:00", "lastmod": "2023-10-20 22:19:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" } ] }, "title": "GALEX and Pan-STARRS1 Discovery of SN IIP 2010aq: The First Few Days After Shock Breakout in a Red Supergiant Star", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual (SN 2010aq); surveys; ultraviolet: general", "note": "\u00a9 2010 The American Astronomical Society. Received 2010 June 11; accepted 2010 July 23; published 2010 August 12. S.G. thanks I. Rabinak and E. Nakar for kindly providing\ntheir models in the GALEX and PS1 filters, L. Dessart for helpful\ndiscussions, and the anonymous referee for useful comments.\nS.G. was supported by NASA through Hubble Fellowship grant\nHST-HF-01219.01-A awarded by the Space Telescope Science\nInstitute, which is operated by AURA, Inc., for NASA, under\ncontract NAS 5-26555. The PS1 Surveys have been made\npossible through the combinations of the Institute for Astronomy at the University of Hawaii, The Pan-STARRS Project\nOffice, the Max-Planck Society and its participating institutes,\nthe Max Planck Institute for Astronomy, Heidelberg, and the\nMax Planck Institute for Extraterrestrial Physics, Garching,\nThe Johns Hopkins University, the University of Durham, the\nUniversity of Edinburgh, the Queen's University of Belfast, the\nHarvard-Smithsonian Center forAstrophysics, the Las Cumbres\nObservatory Global Network, and the National Central University\nof Taiwan. We gratefully acknowledge NASA's support for\nconstruction, operation, and science analysis for the GALEX\nmission, developed in cooperation with CNES of France and\nthe Korean MOST.\n\nPublished - Gezari2010p11445Astrophys_J_Lett.pdf
", "abstract": "We present the early UV and optical light curve of Type IIP supernova (SN) 2010aq at z = 0.0862, and compare it to analytical models for thermal emission following SN shock breakout in a red supergiant star. SN 2010aq was discovered in joint monitoring between the Galaxy Evolution Explorer (GALEX) Time Domain Survey (TDS) in the NUV and the Pan-STARRS1 Medium Deep Survey (PS1 MDS) in the g, r, i, and z bands. The GALEX and Pan-STARRS1 observations detect the SN less than 1 day after the shock breakout, measure a diluted blackbody temperature of 31, 000 \u00b1 6000 K 1 day later, and follow the rise in the UV/optical light curve over the next 2 days caused by the expansion and cooling of the SN ejecta. The high signal-to-noise ratio of the simultaneous UV and optical photometry allows us to fit for a progenitor star radius of 700 \u00b1 200R_\u2609, the size of a red supergiant star. An excess in UV emission two weeks after shock breakout compared with SNe well fitted by model atmosphere-code synthetic spectra with solar metallicity is best explained by suppressed line blanketing due to a lower metallicity progenitor star in SN 2010aq. Continued monitoring of PS1 MDS fields by the GALEX TDS will increase the sample of early UV detections of Type II SNe by an order of magnitude and probe the diversity of SN progenitor star properties.", "date": "2010-09-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "720", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L77-L81", "id_number": "CaltechAUTHORS:20100929-072734347", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100929-072734347", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01219.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/2041-8205/720/1/L77", "primary_object": { "basename": "Gezari2010p11445Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/bvhe7-rzy83/files/Gezari2010p11445Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Gezari, S.; Forster, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/k0rbs-y5c40", "eprint_id": 19975, "eprint_status": "archive", "datestamp": "2023-08-22 00:47:21", "lastmod": "2023-10-20 22:05:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Loh-Yeong-Shang", "name": { "family": "Loh", "given": "Yeong-Shang" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S\u00e9bastien" } }, { "id": "Scranton-R", "name": { "family": "Scranton", "given": "Ryan" } }, { "id": "Mallery-R-P", "name": { "family": "Mallery", "given": "Ryan P." } }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "St\u00e9phane" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } } ] }, "title": "The UV\u2013optical colour dependence of galaxy clustering in the local universe", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; galaxies: clusters: general; galaxies: elliptical and lenticular; galaxies: evolution", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS.\n\nAccepted 2010 April 22. Received 2010 April 20; in original form 2009 April 8.\nArticle first published online: 17 June 2010.\n\nYSL would like to thank C. Hirata, S. Salim, C. Park, J. Kormendy\nand Z. Zheng for helpful discussions. This work has made extensive\nuse of IDLUTILS8 and Goddard IDL libraries. RMR acknowledges\nsupport from grant GO-11182 from the Space Telescope Science\nInstitute.\nGALEX is a NASA Small Explorer, launched in 2003 April. We\ngratefully acknowledge NASA's support for construction, operation\nand science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France\nand the Korean Ministry of Science and Technology.\nFacilities: GALEX, SDSS\n\nPublished - Loh2010p11322Mon_Not_R_Astron_Soc.pdf
", "abstract": "We measure the UV-optical colour dependence of galaxy clustering in the local Universe. Using the clean separation of the red and blue sequences made possible by the NUV\u2212r colour\u2013magnitude diagram, we segregate the galaxies into red, blue and intermediate 'green' classes. We explore the clustering as a function of this segregation by removing the dependence on luminosity and by excluding edge-on galaxies as a means of a non-model dependent veto of highly extincted galaxies. We find that \u03be(r_p, \u03c0) for both red and green galaxies shows strong redshift-space distortion on small scales \u2013 the 'finger-of-God' effect, with green galaxies having a lower amplitude than is seen for the red sequence, and the blue sequence showing almost no distortion. On large scales, \u03be(r_p, \u03c0) for all three samples show the effect of large-scale streaming from coherent infall. On scales of 1 h^(\u22121) Mpc < r_p < 10 h^(\u22121) Mpc, the projected auto-correlation function w_p(r_p) for red and green galaxies fits a power law with slope \u03b3 ~ 1.93 and amplitude r_0 ~ 7.5 and 5.3, compared with \u03b3 ~ 1.75 and r_0 ~ 3.9 h^(\u22121) Mpc for blue sequence galaxies. Compared to the clustering of a fiducial L* galaxy, the red, green and blue have a relative bias of 1.5, 1.1 and 0.9, respectively. The w_p(r_p) for blue galaxies display an increase in convexity at ~ 1 h^(\u22121) Mpc, with an excess of large-scale clustering. Our results suggest that the majority of blue galaxies are likely central galaxies in less massive haloes, while red and green galaxies have larger satellite fractions, and preferentially reside in virialized structures. If blue sequence galaxies migrate to the red sequence via processes like mergers or quenching that take them through the green valley, such a transformation may be accompanied by a change in environment in addition to any change in luminosity and colour.", "date": "2010-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "407", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "55-70", "id_number": "CaltechAUTHORS:20100915-141422615", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100915-141422615", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-11182" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2010.16908.x", "primary_object": { "basename": "Loh2010p11322Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/k0rbs-y5c40/files/Loh2010p11322Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2010", "author_list": "Loh, Yeong-Shang; Rich, R. Michael; et el." }, { "id": "https://authors.library.caltech.edu/records/h8wza-m8083", "eprint_id": 19751, "eprint_status": "archive", "datestamp": "2023-08-22 00:31:21", "lastmod": "2023-10-20 21:20:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "A." } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Astier-P", "name": { "family": "Astier", "given": "P." } }, { "id": "Balland-C", "name": { "family": "Balland", "given": "C." } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "R. G." } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "D." } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "J." } }, { "id": "Hardin-D", "name": { "family": "Hardin", "given": "D." } }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Pain-R", "name": { "family": "Pain", "given": "R." } }, { "id": "Palanque-Delabrouille-N", "name": { "family": "Palanque-Delabrouille", "given": "N." } }, { "id": "Perrett-K-M", "name": { "family": "Perrett", "given": "K. M." } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "C. J." } }, { "id": "Regnault-N", "name": { "family": "Regnault", "given": "N." } }, { "id": "Rich-J-A", "name": { "family": "Rich", "given": "J." }, "orcid": "0000-0002-5807-5078" }, { "id": "Ruhlmann-Kleider-V", "name": { "family": "Ruhlmann-Kleider", "given": "V." } }, { "id": "Baumont-S", "name": { "family": "Baumont", "given": "S." } }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "E. Y." } }, { "id": "Kronborg-T", "name": { "family": "Kronborg", "given": "T." } }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "C." }, "orcid": "0000-0003-1731-0497" }, { "id": "Perlmutter-S", "name": { "family": "Perlmutter", "given": "S." } }, { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E. S." } } ] }, "title": "The dependence of Type Ia Supernovae luminosities on their host galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; cosmology: observations; distance scale", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS.\n\nAccepted 2010 March 26. Received 2010 March 26; in original form 2010 February 26.\nArticle first published online: 4 May 2010.\n\nMS acknowledges support from the Royal Society. This paper is\nbased in part on observations obtained with MegaPrime/MegaCam,\na joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013\nHawaii Telescope (CFHT) which is operated by the National Research\nCouncil (NRC) of Canada, the Institut National des Sciences\nde l'Univers of the Centre National de la Recherche Scientifique\n(CNRS) of France and the University of Hawaii. This work is\nbased in part on data products produced at the Canadian Astronomy\nData Centre as part of the CFHT Legacy Survey, a collaborative\nproject of NRC and CNRS. Based in part on observations obtained\nwith WIRCam, a joint project of CFHT, Taiwan, Korea, Canada,\nFrance, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which\nis operated by the National Research Council (NRC) of Canada,\nthe Institute National des Sciences de l'Univers of the Centre National\nde la Recherche Scientifique of France, and the University\nof Hawaii. This work is based in part on data products produced at\nTERAPIX, the WIRDS (WIRcam Deep Survey) consortium, and\nthe Canadian Astronomy Data Centre. This research was supported\nby a grant from the Agence Nationale de la Recherche ANR-07-\nBLAN-0228. Canadian collaboration members acknowledge support\nfrom NSERC and CIAR; French collaboration members from\nCNRS/IN2P3, CNRS/INSU and CEA. Based in part on observations\nmade with ESO Telescopes at the Paranal Observatory under\nprogram IDs 171.A-0486 and 176.A-0589. Based in part on\nobservations obtained at the Gemini Observatory, which is operated\nby the Association of Universities for Research in Astronomy,\nInc., under a cooperative agreement with the NSF on behalf of\nthe Gemini partnership: the National Science Foundation (United\nStates), the Science and Technology Facilities Council (United\nKingdom), the National Research Council (Canada), CONICYT\n(Chile), the Australian Research Council (Australia), Ministrio da\nCincia e Tecnologia (Brazil) andMinisterio de Ciencia, Tecnologa e\nInnovacin Productiva (Argentina). The programmes under which\ndata were obtained at the Gemini Observatory are: GS-2003BQ-\n8, GN-2003B-Q-9, GS-2004A-Q-11, GN-2004A-Q-19, GS-\n2004B-Q-31, GN-2004B-Q-16, GS-2005A-Q-11, GN-2005A-11,\nGS-2005B-Q-6, GN-2005B-Q-7, GN-2006A-Q-7 and GN-2006BQ-\n10. Some of the data presented herein were obtained at the W.\nM. Keck Observatory, which is operated as a scientific partnership\namong the California Institute of Technology, the University of California\nand theNational Aeronautics and SpaceAdministration. The\nObservatory was made possible by the generous financial support of\nthe W. M. Keck Foundation. Based on observations made with the\nNASA/ESA Hubble Space Telescope, obtained 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\nPublished - Sullivan2010p11170Mon_Not_R_Astron_Soc.pdf
Supplemental Material - MNR_16731_sm_Table1.zip
", "abstract": "Precision cosmology with Type Ia supernovae (SNe Ia) makes use of the fact that SN Ia luminosities depend on their light-curve shapes and colours. Using Supernova Legacy Survey (SNLS) and other data, we show that there is an additional dependence on the global characteristics of their host galaxies: events of the same light-curve shape and colour are, on average, 0.08 mag (\u22434.0\u03c3) brighter in massive host galaxies (presumably metal-rich) and galaxies with low specific star formation rates (sSFR). These trends do not depend on any assumed cosmological model, and are independent of the SN light-curve width: both fast and slow-declining events show the same trends. SNe Ia in galaxies with a low sSFR also have a smaller slope ('\u03b2') between their luminosities and colours with ~2.7\u03c3 significance, and a smaller scatter on SN Ia Hubble diagrams (at 95 per cent confidence), though the significance of these effects is dependent on the reddest SNe. SN Ia colours are similar between low-mass and high-mass hosts, leading us to interpret their luminosity differences as an intrinsic property of the SNe and not of some external factor such as dust. If the host stellar mass is interpreted as a metallicity indicator using galaxy mass\u2013metallicity relations, the luminosity trends are in qualitative agreement with theoretical predictions. We show that the average stellar mass, and therefore the average metallicity, of our SN Ia host galaxies decreases with redshift. The SN Ia luminosity differences consequently introduce a systematic error in cosmological analyses, comparable to the current statistical uncertainties on parameters such as w, the equation of state of dark energy. We show that the use of two SN Ia absolute magnitudes, one for events in high-mass (metal-rich) galaxies and the other for events in low-mass (metal-poor) galaxies, adequately corrects for the differences. Cosmological fits incorporating these terms give a significant reduction in \u03c7^2 (3.8\u03c3\u20134.5\u03c3); linear corrections based on host parameters do not perform as well. We conclude that all future SN Ia cosmological analyses should use a correction of this (or similar) form to control demographic shifts in the underlying galaxy population.", "date": "2010-08-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "406", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "782-802", "id_number": "CaltechAUTHORS:20100831-152257012", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100831-152257012", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-07-BLAN-0228" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2010.16731.x", "primary_object": { "basename": "MNR_16731_sm_Table1.zip", "url": "https://authors.library.caltech.edu/records/h8wza-m8083/files/MNR_16731_sm_Table1.zip" }, "related_objects": [ { "basename": "Sullivan2010p11170Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/h8wza-m8083/files/Sullivan2010p11170Mon_Not_R_Astron_Soc.pdf" } ], "pub_year": "2010", "author_list": "Sullivan, M.; Conley, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/81pvs-1t832", "eprint_id": 22903, "eprint_status": "archive", "datestamp": "2023-08-22 00:25:36", "lastmod": "2024-01-13 00:12:03", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Tuttle-S-E", "name": { "family": "Tuttle", "given": "Sarah E." } }, { "id": "Vibert-D", "name": { "family": "Vibert", "given": "Didier" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Frank-S", "name": { "family": "Frank", "given": "Stephan" } }, { "id": "Evrard-J", "name": { "family": "Evrard", "given": "Jean" } }, { "id": "Mirc-F", "name": { "family": "Mirc", "given": "Frederi" } } ] }, "title": "FIREBALL: Detector, data acquisition and reduction", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Integral Field Spectroscopy; FIREBALL; Data Reduction; Instrument Calibration", "note": "\u00a9 2010 SPIE. \n\nThe material is based upon work supported by NASA under award No. NNX08AO39G. The FIREBALL team acknowledges the support from CNES, CNRS, and LAM.\n\nPublished - Rahman2010p12882Adaptive_Optics_Systems_Pts_1-3.pdf
", "abstract": "The Faint Intergalactic Redshifted Emission Balloon (FIREBALL) had its first scientific flight in June 2009. The instrument combines microchannel plate detector technology with fiber-fed integral field spectroscopy on an unstable stratospheric balloon gondola platform. This unique combination poses a series of calibration and data reduction challenges that must be addressed and resolved to allow for accurate data analysis. We discuss our approach and some of the methods we are employing to accomplish this task.", "date": "2010-07-30", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 773228", "id_number": "CaltechAUTHORS:20110315-135645488", "isbn": "978-0-8194-8222-8", "book_title": "Space telescopes and instrumentation 2010 : ultraviolet to gamma ray", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-135645488", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AO39G" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Laboratoire d'Astrophysique de Marseille (LAM)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Arnaud-M", "name": { "family": "Arnaud", "given": "Monique" } }, { "id": "Murray-S-S", "name": { "family": "Murray", "given": "Stephen S." } }, { "id": "Takahashi-Tadayuki", "name": { "family": "Takahashi", "given": "T." } } ] }, "doi": "10.1117/12.857862", "primary_object": { "basename": "Rahman2010p12882Adaptive_Optics_Systems_Pts_1-3.pdf", "url": "https://authors.library.caltech.edu/records/81pvs-1t832/files/Rahman2010p12882Adaptive_Optics_Systems_Pts_1-3.pdf" }, "pub_year": "2010", "author_list": "Rahman, Shahinur; Matuszewski, Mateusz; et el." }, { "id": "https://authors.library.caltech.edu/records/v2by3-c7h43", "eprint_id": 22880, "eprint_status": "archive", "datestamp": "2023-08-22 00:25:31", "lastmod": "2024-01-13 00:11:55", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Evrard-J", "name": { "family": "Evrard", "given": "Jean" } }, { "id": "Mirc-F", "name": { "family": "Mirc", "given": "Frederi" } }, { "id": "Grange-R", "name": { "family": "Grange", "given": "Robert" } }, { "id": "Frank-S", "name": { "family": "Frank", "given": "Stephan" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Tuttle-S-E", "name": { "family": "Tuttle", "given": "Sarah E." } }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "McLean-R", "name": { "family": "McLean", "given": "Ryan" } }, { "id": "Chave-R-G", "name": { "family": "Chave", "given": "Robert G." } } ] }, "title": "FIREBALL: Instrument pointing and aspect reconstruction", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Integral field spectroscopy; FIREBALL; Data reduction; Pointing stabilization", "note": "\u00a9 2010 SPIE. \n\nThe material is based upon work supported by NASA under award No. NNX08AO39G. The FIREBALL collaboration also acknowledges support from CNES, LAM and CNRS.\n\nPublished - Matuszewski2010p12885Adaptive_Optics_Systems_Pts_1-3.pdf
", "abstract": "The Faint Intergalactic Redshifted Emission Balloon (FIREBALL) had its first scientific flight in June 2009. The instrument is a 1 meter class balloon-borne telescope equipped with a vacuum-ultraviolet integral field spectrograph intended to detect emission from the inter-galactic medium at redshifts 0.3 < z < 1.0. The scientific goals and the challenging environment place strict constraints on the pointing and tracking systems of the gondola. In this manuscript we briefly review our pointing requirements, discuss the methods and solutions used to meet those requirements, and present the aspect reconstruction results from the first successful scientific flight.", "date": "2010-07-30", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 773229", "id_number": "CaltechAUTHORS:20110315-090952702", "isbn": "978-0-8194-8222-8", "book_title": "Space telescopes and instrumentation 2010: ultraviolet to gamma ray", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-090952702", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AO39G" }, { "agency": "Centre National d'Etudes Spatiales (CNES)" }, { "agency": "Laboratoire d'Astrophysique de Marseille (LAM)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Arnaud-M", "name": { "family": "Arnaud", "given": "Monique" } }, { "id": "Murray-S-S", "name": { "family": "Murray", "given": "Stephen S." } }, { "id": "Takahashi-Tadayuki", "name": { "family": "Takahashi", "given": "T." } } ] }, "doi": "10.1117/12.857869", "primary_object": { "basename": "Matuszewski2010p12885Adaptive_Optics_Systems_Pts_1-3.pdf", "url": "https://authors.library.caltech.edu/records/v2by3-c7h43/files/Matuszewski2010p12885Adaptive_Optics_Systems_Pts_1-3.pdf" }, "pub_year": "2010", "author_list": "Matuszewski, Mateusz; Evrard, Jean; et el." }, { "id": "https://authors.library.caltech.edu/records/6smap-kr842", "eprint_id": 71596, "eprint_status": "archive", "datestamp": "2023-08-19 03:20:26", "lastmod": "2024-01-13 20:17:10", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tuttle-S-E", "name": { "family": "Tuttle", "given": "Sarah E." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Grange-R", "name": { "family": "Grange", "given": "Robert" } }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "Jean-Michel" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "FIREBALL: the first ultraviolet fiber fed spectrograph", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology, Integral Field Spectroscopy, FIREBALL, UV Spectroscopy, Fiber spectrograph, IGM, CGM", "note": "\u00a9 2010 SPIE. \n\nThe material is based upon work supported by NASA under award No. NNX08AO39G. The FIREBALL collaboration also acknowledges support from CNES, LAM and CNRS.\n\nPublished - 773227_1.pdf
", "abstract": "FIREBall (the Faint Intergalactic Redshifted Emission Balloon) is a balloon-borne 1m telescope coupled to an ultraviolet fiber-fed spectrograph. FIREBall is designed to study the faint and diffuse emission of the warm hot intergalactic medium, until now detected primarily in absorption. FIREBall is a pathfinding mission to test new technology and make new constraints on the temperature and density of this gas. FIREBall has flown twice, the most recent flight (June 2009) a fully functioning science flight. Here we describe the spectrograph design, current setup, and calibration measurements from the campaign.", "date": "2010-07-30", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 773227", "id_number": "CaltechAUTHORS:20161028-153125969", "isbn": "978-0-8194-8222-8", "book_title": "Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161028-153125969", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AO39G" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Laboratoire d'Astrophysique de Marseille (LAM)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Arnaud-M", "name": { "family": "Arnaud", "given": "Monique" } }, { "id": "Murray-S-S", "name": { "family": "Murray", "given": "Stephen S." } }, { "id": "Takahashi-Tadayuki", "name": { "family": "Takahashi", "given": "Tadayuki" } } ] }, "doi": "10.1117/12.857877", "primary_object": { "basename": "773227_1.pdf", "url": "https://authors.library.caltech.edu/records/6smap-kr842/files/773227_1.pdf" }, "pub_year": "2010", "author_list": "Tuttle, Sarah E.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/5hvf3-ddd91", "eprint_id": 71624, "eprint_status": "archive", "datestamp": "2023-08-19 03:20:00", "lastmod": "2024-01-13 20:17:30", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Evrard-J", "name": { "family": "Evrard", "given": "Jean" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Matt" } }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } }, { "id": "Tuttle-S-E", "name": { "family": "Tuttle", "given": "Sarah" } }, { "id": "McLean-R", "name": { "family": "McLean", "given": "Ryan" } }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "Jean-Michel" } }, { "id": "Mirc-F", "name": { "family": "Mirc", "given": "Frederi" } }, { "id": "Grange-R", "name": { "family": "Grange", "given": "Robert" } }, { "id": "Chave-R-G", "name": { "family": "Chave", "given": "Robert" } } ] }, "title": "FIREBALL: the Faint Intergalactic medium Redshifted Emission Balloon: overview and first science flight results", "ispublished": "unpub", "full_text_status": "public", "keywords": "Instrumentation, Integral Field Spectroscopy, Ultraviolet", "note": "\u00a9 2010 SPIE The International Society for Optical Engineering. \n\nThe material is based upon work supported by NASA under award No. NNX08AO39G. The FIREBALL collaboration also acknowledges considerable support from CNES, LAM, and CNRS. The FIREBALL flights would not be possible without the many contributions of the Columbia Scientific Ballooning Facility.\n\nPublished - 773205_1.pdf
", "abstract": "FIREBALL (the Faint Intergalactic Redshifted Emission Balloon) is a balloon-borne 1m telescope coupled to an ultraviolet fiber-fed spectrograph. FIREBALL is designed to study the faint and diffuse emission of the intergalactic medium, until now detected primarily in absorption. FIREBALL is a path finding mission to test new technology and make new constraints on the temperature and density of this gas. We report on the first successful science flight of FIREBALL, in June 2009, which proved every aspect of the complex instrument performance, and provided the strongest measurements and constraints on IGM emission available from any instrument.", "date": "2010-07-29", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 773205", "id_number": "CaltechAUTHORS:20161031-112536885", "isbn": "978-0-8194-8222-8", "book_title": "Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161031-112536885", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AO39G" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Laboratoire d'Astrophysique de Marseille (LAM)" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory", "value": "Space Astrophysics Laboratory" } ] }, "contributors": { "items": [ { "id": "Arnaud-M", "name": { "family": "Arnaud", "given": "Monique" } }, { "id": "Murray-S-S", "name": { "family": "Murray", "given": "Stephen S." } }, { "id": "Takahashi-Tadayuki", "name": { "family": "Takahashi", "given": "Tadayuki" } } ] }, "doi": "10.1117/12.857850", "primary_object": { "basename": "773205_1.pdf", "url": "https://authors.library.caltech.edu/records/5hvf3-ddd91/files/773205_1.pdf" }, "pub_year": "2010", "author_list": "Milliard, Bruno; Martin, D. Christopher; et el." }, { "id": "https://authors.library.caltech.edu/records/43x1q-h9720", "eprint_id": 22819, "eprint_status": "archive", "datestamp": "2023-08-22 00:23:27", "lastmod": "2024-01-13 00:11:20", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Chris" }, "orcid": "0000-0002-8650-1644" }, { "id": "Moore-A", "name": { "family": "Moore", "given": "Anna" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } }, { "id": "Adkins-S-M", "name": { "family": "Adkins", "given": "Sean" } }, { "id": "Epps-H-W", "name": { "family": "Epps", "given": "Harland" } } ] }, "title": "The Keck Cosmic Web Imager", "ispublished": "unpub", "full_text_status": "public", "keywords": "Instrumentation; Integral Field Spectroscopy; Visible", "note": "\u00a9 2010 SPIE. \n\nThe W. M. Keck Observatory 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 material is based in part upon work supported by AURA through the National Science Foundation under Scientific Program Order No.5 as issued for support of the Telescope Systems Instrumentation Program (TSIP), in accordance with Proposal No. AST-0335461 submitted by AURA.\n\nPublished - Martin2010p12894Adaptive_Optics_Systems_Pts_1-3.pdf
", "abstract": "We are designing the Keck Cosmic Web Imager (KCWI) as a new facility instrument for the Keck II telescope at the W. M. Keck Observatory (WMKO). KCWI is based on the Cosmic Web Imager (CWI), an instrument that has recently had first light at the Hale Telescope. KCWI is a wide-field integral-field spectrograph (IFS) optimized for precision sky limited spectroscopy of low surface brightness phenomena. KCWI will feature high throughput, and flexibility in field of view (FOV), spatial sampling, bandpass, and spectral resolution. KCWI will provide full wavelength coverage (0.35 to 1.05 \u03bcm) using optimized blue and red channels. KCWI will provide a unique and complementary capability at WMKO (optical band integral field spectroscopy) that is directly connected to one of the Observatory's strategic goals (faint object, high precision spectroscopy), at a modest cost and on a competitive time scale, made possible by its simple concept and the prior demonstration of CWI.", "date": "2010-07-19", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 77350M", "id_number": "CaltechAUTHORS:20110311-080931295", "isbn": "978-0-81948-225-9", "book_title": "Ground-based and airborne instrumentation for astronomy III", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110311-080931295", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0335461" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } }, { "id": "Ramsay-S-K", "name": { "family": "Ramsay", "given": "Suzanne K." } }, { "id": "Takami-Hideki", "name": { "family": "Takami", "given": "Hideki" } } ] }, "doi": "10.1117/12.858227", "primary_object": { "basename": "Martin2010p12894Adaptive_Optics_Systems_Pts_1-3.pdf", "url": "https://authors.library.caltech.edu/records/43x1q-h9720/files/Martin2010p12894Adaptive_Optics_Systems_Pts_1-3.pdf" }, "pub_year": "2010", "author_list": "Martin, Chris; Moore, Anna; et el." }, { "id": "https://authors.library.caltech.edu/records/mayvg-nmp79", "eprint_id": 23147, "eprint_status": "archive", "datestamp": "2023-08-22 00:20:53", "lastmod": "2024-01-13 05:13:51", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Mateusz" } }, { "id": "Chang-Daphne", "name": { "family": "Chang", "given": "Daphne" } }, { "id": "Crabill-R-M", "name": { "family": "Crabill", "given": "Robert M." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna M." }, "orcid": "0000-0002-2894-6936" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } } ] }, "title": "The Cosmic Web Imager: An integral field spectrograph for the Hale Telescope at Palomar Observatory: Instrument design and first results", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Integral Field Spectroscopy; VPH Gratings; Cosmic Web Imager", "note": "\u00a9 2010 SPIE. \n\nThis material is based upon work supported by Caltech and the NSF Under Award No. AST-0505381. We extend special thanks to the wonderful staff at Palomar Observatory and the talented and caring people at Caltech Optical Observatories.\n\nPublished - Matuszewski2010p12888Adaptive_Optics_Systems_Pts_1-3.pdf
", "abstract": "We describe the Cosmic Web Imager (CWI), a UV-VIS integral field spectrograph designed for the Hale 200\" telescope at the Palomar Observatory. CWI has been built specifically for the observation of diffuse radiation. The instrument field of view is 60\" x 40\" with spectral resolving power of R ~5000 and seeing limited spatial resolution. It utilizes volume phase holographic gratings and is intended to cover the spectral range 3800\u00c5 to 9500\u00c5 with an instantaneous bandwidth of ~450\u00c5. CWI saw first light in July 2009, and conducted its first successful scientific observations in May 2010.", "date": "2010-07-14", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 77350P", "id_number": "CaltechAUTHORS:20110329-084157258", "isbn": "978-0-81948-225-9", "book_title": "Ground-Based and Airborne Instrumentation for Astronomy III", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110329-084157258", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0505381" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } }, { "id": "Ramsay-S-K", "name": { "family": "Ramsay", "given": "Suzanne K." } }, { "id": "Takami-Hideki", "name": { "family": "Takami", "given": "Hideki" } } ] }, "doi": "10.1117/12.856644", "primary_object": { "basename": "Matuszewski2010p12888Adaptive_Optics_Systems_Pts_1-3.pdf", "url": "https://authors.library.caltech.edu/records/mayvg-nmp79/files/Matuszewski2010p12888Adaptive_Optics_Systems_Pts_1-3.pdf" }, "pub_year": "2010", "author_list": "Matuszewski, Mateusz; Chang, Daphne; et el." }, { "id": "https://authors.library.caltech.edu/records/9ywtt-d6d76", "eprint_id": 19121, "eprint_status": "archive", "datestamp": "2023-08-22 00:19:00", "lastmod": "2023-10-20 19:23:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Botticella-M-T", "name": { "family": "Botticella", "given": "M. T." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" } ] }, "title": "Supernova 2009kf: An Ultraviolet Bright Type IIP Supernova Discovered with Pan-STARRS 1 and GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: evolution; supernovae: general; supernovae: individual (2009kf)", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2010 January 29; accepted 2010 May 12; published 2010 June 16.\nThe PS1 Surveys have been made possible through contributions\nof the Institute for Astronomy at the University of Hawaii\nin Manoa, the Pan-STARRS Project Office, the Max-Planck Society\nand its participating institutes, the Max Planck Institute\nfor Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial\nPhysics, Garching, Johns Hopkins University, the\nUniversity of Durham, the University of Edinburgh, the Queens\nUniversity Belfast, the Harvard-Smithsonian Center for Astrophysics,\nand the Los Cumbres Observatory Global Telescope\nNetwork, Incorporated. This work is also based on observations\ncollected at LT, WHT and NOT (La Palma), and Gemini\n(Hawaii). This work, conducted as part of the award \"Understanding\nthe lives of massive stars from birth to supernovae\"\n(S.J.S.) made under the European Heads of Research Councils\nand European Science Foundation EURYI Awards scheme, see\nwww.esf.org/euryi. M.T.B. thanks E. Cappellaro, L. Zampieri,\nand S. Benetti for helpful discussions. S.M. and E.K. acknowledge\nsupport from the Academy of Finland (project:8120503).\n\nPublished - Botticella2010p10816Astrophys_J_Lett.pdf
", "abstract": "We present photometric and spectroscopic observations of a luminous Type IIP Supernova (SN) 2009kf discovered by the Pan-STARRS 1 (PS1) survey and also detected by the Galaxy Evolution Explorer. The SN shows a plateau in its optical and bolometric light curves, lasting approximately 70 days in the rest frame, with an absolute magnitude of M_V = -18.4 mag. The P-Cygni profiles of hydrogen indicate expansion velocities of 9000 km s^(-1) at 61 days after discovery which is extremely high for a Type IIP SN. SN 2009kf is also remarkably bright in the near-ultraviolet (NUV) and shows a slow evolution 10-20 days after optical discovery. The NUV and optical luminosity at these epochs can be modeled with a blackbody with a hot effective temperature (T ~ 16,000 K) and a large radius (R ~ 1 \u00d7 10^(15) cm). The bright bolometric and NUV luminosity, the light curve peak and plateau duration, the high velocities, and temperatures suggest that 2009kf is a Type IIP SN powered by a larger than normal explosion energy. Recently discovered high-z SNe (0.7 < z < 2.3) have been assumed to be IIn SNe, with the bright UV luminosities due to the interaction of SN ejecta with a dense circumstellar medium. UV-bright SNe similar to SN 2009kf could also account for these high-z events, and its absolute magnitude M_(NUV) = -21.5 \u00b1 0.5 mag suggests such SNe could be discovered out to z ~ 2.5 in the PS1 survey.", "date": "2010-07-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "717", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L52-L56", "id_number": "CaltechAUTHORS:20100720-100110749", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100720-100110749", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Academy of Finland", "grant_number": "8120503" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/2041-8205/717/1/L52", "primary_object": { "basename": "Botticella2010p10816Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/9ywtt-d6d76/files/Botticella2010p10816Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Botticella, M. T.; Neill, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/t2se2-sb605", "eprint_id": 18879, "eprint_status": "archive", "datestamp": "2023-08-22 00:06:39", "lastmod": "2023-10-20 19:09:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hester-J-A", "name": { "family": "Hester", "given": "Janice A." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" } ] }, "title": "IC 3418: Star Formation in a Turbulent Wake", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (Virgo); galaxies: individual (IC 3418); ultraviolet: galaxies", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2010 February 22; accepted 2010 May 6; published 2010 May 19.\n\nThis research has made use of the GOLD Mine Database\nand of the NASA/IPAC Extragalactic Database (NED) which is\noperated by the Jet Propulsion Laboratory, California Institute\nof Technology, under contract with the National Aeronautics\nand Space Administration. The authors thank L. Cortese for\nhelpful comments.\n\nPublished - Hester2010p10549Astrophys_J_Lett.pdf
", "abstract": "Galaxy Evolution Explorer observations of IC 3418, a low surface brightness galaxy in the Virgo Cluster, revealed a striking 17 kpc UV tail of bright knots and diffuse emission. H\u03b1 imaging confirms that star formation is ongoing in the tail. IC 3418 was likely recently ram pressure stripped on its first pass through Virgo. We suggest that star formation is occurring in molecular clouds that formed in IC 3418's turbulent stripped wake. Tides and ram pressure stripping (RPS) of molecular clouds are both disfavored as tail formation mechanisms. The tail is similar to the few other observed star-forming tails, all of which likely formed during RPS. The tails' morphologies reflect the forces present during their formation and can be used to test for dynamical coupling between molecular and diffuse gas, thereby probing the origin of the star-forming molecular gas.", "date": "2010-06-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "716", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L14-L18", "id_number": "CaltechAUTHORS:20100630-140822183", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100630-140822183", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/2041-8205/716/1/L14", "primary_object": { "basename": "Hester2010p10549Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/t2se2-sb605/files/Hester2010p10549Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Hester, Janice A.; Seibert, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/ah7xc-x8c07", "eprint_id": 21015, "eprint_status": "archive", "datestamp": "2023-08-19 02:48:26", "lastmod": "2024-01-13 00:06:53", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "The GALEX Extended Mission: Surveying UV Tracers of the Hidden Side of Galaxy Evolution", "ispublished": "unpub", "full_text_status": "public", "keywords": "dark matter, star formation, galaxies, red shift", "note": "\u00a9 2010 American Institute of Physics.\nIssue Date: 8 June 2010.\nGALEX is a NASA Small Explorer, launched in April 2003.We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - Martin2010p11966Aip_Conf_Proc.pdf
", "abstract": "The Galaxy Evolution Explorer (GALEX) continues its surveys of the ultraviolet sky. GALEX surveys have supported the following galaxy evolution investigations: calibrating UV as a star formation rate tracer, using wide and deep surveys to measure star formation history, studying the evolution of dust extinction and metallicity, selecting and analyzing galaxies in transitory states, finding local analogs to Lyman Break Galaxies, probing and time-dating star formation in a wide variety of physical regimes. Our continuing mission is focussed on relating star formation history and galaxy evolution paths to the properties of dark matter halos and their assembly history, and on beginning to relate the evolution of galaxies to that of black holes and the intergalactic medium. GALEX has proven that the UV is an ideal band to find and map star formation in low mass, low density objects, and potentially in primordial gas. With future UV missions it may be possible to map emission from the intergalactic and circum-galactic medium, and make a definitive connection between galaxy evolution and the cooling, accretion, heating, and enrichment of gas in the cosmic web.", "date": "2010-06-08", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "103-114", "id_number": "CaltechAUTHORS:20101124-095102724", "isbn": "978-0-7354-0786-2", "book_title": "Hunting for the dark : the hidden side of galaxy formation", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101124-095102724", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Debattista-V-P", "name": { "family": "Debattista", "given": "Victor P." } }, { "id": "Popescu-C-C", "name": { "family": "Popescu", "given": "Cristina C." } } ] }, "corp_creators": { "items": [ "GALEX Science Team" ] }, "doi": "10.1063/1.3458462", "primary_object": { "basename": "Martin2010p11966Aip_Conf_Proc.pdf", "url": "https://authors.library.caltech.edu/records/ah7xc-x8c07/files/Martin2010p11966Aip_Conf_Proc.pdf" }, "pub_year": "2010", "author_list": "Martin, D. Christopher" }, { "id": "https://authors.library.caltech.edu/records/fakfs-49934", "eprint_id": 17602, "eprint_status": "archive", "datestamp": "2023-08-21 23:24:40", "lastmod": "2023-10-20 00:03:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "R. A." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T. M." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "A." } }, { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "T." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" } ] }, "title": "Morphologies of Local Lyman Break Galaxy Analogs. II. A Comparison with Galaxies at z \u2243 2\u20134 in ACS and WFC3 Images of the Hubble Ultra Deep Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; early universe; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 2 (2010 February 20); received 2009 November 6; accepted for publication 2010 January 6;\npublished 2010 January 25.\n\nWe are grateful to Xu Kong for providing us with the source\nlist of BzK galaxies in the HUDF from Kong et al. (2008).\nWe thank Guinevere Kauffmann, Qi Guo, and Eyal Neistein\nfor sharing their insight on the different gas accretion modes.\nWe thank Lee Armus, Brant Robertson, James Bullock, Marc\nRafelski, and Jeff Cooke for very useful comments to a previous\nversion of this paper submitted to the e-print archive.\nBased on observations made with the NASA/ESA HST,\nwhich is operated by the Association of Universities for Research\nin Astronomy, Inc., under NASA contract NAS 5-26555.\nThese observations are associated with programs 10920, 11107, and 11563.\n\nPublished - Overzier2010p7132Astrophys_J.pdf
", "abstract": "Previous work has shown that Lyman break galaxies (LBGs) display a range in structures (from single and compact to more clumpy and extended) that is different from typical local star-forming galaxies. Recently, we have introduced a sample of rare, nearby (z < 0.3) starburst galaxies that appear to be good analogs of LBGs. These \"Lyman break analogs\" (LBAs) provide an excellent training set for understanding starbursts at different redshifts. We present an application of this by comparing the rest-frame ultraviolet (UV) and optical morphologies of 30 LBAs with those of galaxies at z ~ 2-4 in the Hubble Ultra Deep Field. We compare LBAs with star-forming sBzK galaxies at z ~ 2, and LBGs at z ~ 3-4 at the same intrinsic UV luminosity (L_(UV) \u2273 0.3L^*_(z=3)). The UV/optical colors and sizes of LBAs and LBGs are very similar, while the BzK galaxies are somewhat redder and larger. LBAs lie along a mass-metallicity relation that is offset from that of typical local galaxies, but similar to that seen at z ~ 2. There is significant overlap between the morphologies (G, C, A, and M_(20)) of the local and high-redshift samples, although the high-redshift samples are somewhat less concentrated and clumpier than the LBAs. Based on their highly asymmetric morphologies, we find that in the majority of LBAs the starbursts appear to be triggered by interactions/mergers. When the images of the LBAs are degraded to the same sensitivity and linear resolution as the images of LBGs and BzK galaxies, we find that these relatively faint asymmetric features are no longer detectable. This effect is particularly severe in the rest-frame UV. It has been suggested that high-redshift galaxies experience intense bursts unlike anything seen in the local universe, possibly due to cold flows and instabilities. In part, this is based on the fact that the majority (~70%) of LBGs do not show morphological signatures of interactions or mergers. Our results suggest that this evidence is insufficient, since a large fraction of such signatures would likely have been missed in current observations of galaxies at z ~ 2-4. This leaves open the possibility that clumpy accretion and mergers remain important in driving the evolution of these starbursts, together with rapid gas accretion through other means.", "date": "2010-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "710", "number": "2", "publisher": "American Astronomical Society", "pagerange": "979-991", "id_number": "CaltechAUTHORS:20100225-165613498", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100225-165613498", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/710/2/979", "primary_object": { "basename": "Overzier2010p7132Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/fakfs-49934/files/Overzier2010p7132Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Overzier, R. A.; Heckman, T. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/gtntv-sn183", "eprint_id": 17444, "eprint_status": "archive", "datestamp": "2023-08-21 23:16:11", "lastmod": "2023-10-19 23:53:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Drinkwater-M-J", "name": { "family": "Drinkwater", "given": "Michael J." } }, { "id": "Jurek-R-J", "name": { "family": "Jurek", "given": "Russell J." } }, { "id": "Blake-C", "name": { "family": "Blake", "given": "Chris" } }, { "id": "Woods-D", "name": { "family": "Woods", "given": "David" } }, { "id": "Pimbblet-K-A", "name": { "family": "Pimbblet", "given": "Kevin A." } }, { "id": "Glazebrook-K", "name": { "family": "Glazebrook", "given": "Karl" } }, { "id": "Sharp-R", "name": { "family": "Sharp", "given": "Rob" } }, { "id": "Pracy-M-B", "name": { "family": "Pracy", "given": "Michael B." } }, { "id": "Brough-S", "name": { "family": "Brough", "given": "Sarah" }, "orcid": "0000-0002-9796-1363" }, { "id": "Colless-M", "name": { "family": "Colless", "given": "Matthew" }, "orcid": "0000-0001-9552-8075" }, { "id": "Couch-W-J", "name": { "family": "Couch", "given": "Warrick J." } }, { "id": "Croom-S-M", "name": { "family": "Croom", "given": "Scott M." }, "orcid": "0000-0003-2880-9197" }, { "id": "Davis-T-M", "name": { "family": "Davis", "given": "Tamara M." } }, { "id": "Forbes-D", "name": { "family": "Forbes", "given": "Duncan" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Gilbank-D-G", "name": { "family": "Gilbank", "given": "David G." } }, { "id": "Gladders-M", "name": { "family": "Gladders", "given": "Michael" } }, { "id": "Jelliffe-B", "name": { "family": "Jelliffe", "given": "Ben" } }, { "id": "Jones-N", "name": { "family": "Jones", "given": "Nick" } }, { "id": "Li-I-hui", "name": { "family": "Li", "given": "I-hui" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry" }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Poole-G-B", "name": { "family": "Poole", "given": "Gregory B." } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wisnioski-E", "name": { "family": "Wisnioski", "given": "Emily" } }, { "id": "Wyder-T", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Yee-H-K-C", "name": { "family": "Yee", "given": "H. K. C." } } ] }, "title": "The WiggleZ Dark Energy Survey: survey design and first data release", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: high-redshift; galaxies: photometry; galaxies: starburst; cosmology: observations; ultraviolet: galaxies", "note": "\u00a9 2009 The Authors. Journal compilation \u00a9 2009 RAS.\n\nAccepted 2009 September 21; received 2009 September 19; in original form 2009 July 13.\n\nThis project would not be possible without the superb\nAAOmega/2dF facility provided by the Anglo-Australian Observatory\n(AAO).We wish to thank all the AAO staff for their support,\nespecially the night assistants, support astronomers and Russell\nCannon (who greatly assisted with the quality control of the 2dF\nsystem).\nWe also wish to thank Alejandro Dubrovsky for writing software\nused to check the guide star and blank sky positions, Maksym\nBernyk and David Barnes for help with the data base construction,\nPeter Jensen and Max Spolaor for assistance with the redshift\nmeasurements, Michael Stanley for help with the selection of new\nGALEX positions andMichael Cooper for providingDEEP2 spectra\nfor the comparison in Section 5.2.2.\nWe wish to acknowledge financial support from The Australian\nResearch Council (grants DP0772084 and LX0881951 directly\nfor the WiggleZ project, and grant LE0668442 for programming\nsupport), Swinburne University of Technology, The University of\nQueensland, the AAO and The Gregg Thompson Dark Energy\nTravel Fund.\nGALEX is a NASA Small Explorer, launched in 2003 April. We\ngratefully acknowledgeNASA's support for construction, operation\nand science analysis for the GALEX mission, developed in cooperation\nwith the Centre National d'Etudes Spatiales of France\nand the Korean Ministry of Science and Technology.\nFunding for the SDSS and SDSS-II has been provided by the Alfred\nP. Sloan Foundation, the Participating Institutions, the National\nScience Foundation, the U.S. Department of Energy, the National\nAeronautics and Space Administration, the Japanese Monbukagakusho,\ntheMax Planck Society and theHigher Education Funding\nCouncil for England. The SDSS website is http://www.sdss.org/.\nThe RCS2 survey is based on observations obtained with\nMegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA,\nat the CFHT which is operated by the National Research Council\n(NRC) of Canada, the Institut National des Sciences de l'Univers\n(CNRS) of France and the University of Hawaii. The RCS2 survey\nis supported by grants to HKCY from the Canada Research Chair\nprogramme and the Discovery programme of the Natural Science\nand Engineering Research Council of Canada.\n\nPublished - Drinkwater2010p6976Mon_Not_R_Astron_Soc.pdf
", "abstract": "The WiggleZ Dark Energy Survey is a survey of 240 000 emission-line galaxies in the distant Universe, measured with the AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope (AAT). The primary aim of the survey is to precisely measure the scale of baryon acoustic oscillations (BAO) imprinted on the spatial distribution of these galaxies at look-back times of 4\u20138 Gyr.\n\nThe target galaxies are selected using ultraviolet (UV) photometry from the Galaxy Evolution Explorer satellite, with a flux limit of NUV < 22.8 mag . We also require that the targets are detected at optical wavelengths, specifically in the range 20.0 < r < 22.5 mag . We use the Lyman break method applied to the UV colours, with additional optical colour limits, to select high-redshift galaxies. The galaxies generally have strong emission lines, permitting reliable redshift measurements in relatively short exposure times on the AAT. The median redshift of the galaxies is z_(med)= 0.6 . The redshift range containing 90 per cent of the galaxies is 0.2 < z < 1.0 .\n\nThe survey will sample a volume of ~1 Gpc^3 over a projected area on the sky of 1000 deg^2, with an average target density of 350 deg^(\u22122). Detailed forecasts indicate that the survey will measure the BAO scale to better than 2 per cent and the tangential and radial acoustic wave scales to approximately 3 and 5 per cent, respectively. Combining the WiggleZ constraints with existing cosmic microwave background measurements and the latest supernova data, the marginalized uncertainties in the cosmological model are expected to be \u03c3(\u03a9_m) = 0.02 and \u03c3(w) = 0.07 (for a constant w model). The WiggleZ measurement of w will constitute a robust, precise and independent test of dark energy models.\n\nThis paper provides a detailed description of the survey and its design, as well as the spectroscopic observations, data reduction and redshift measurement techniques employed. It also presents an analysis of the properties of the target galaxies, including emission-line diagnostics which show that they are mostly extreme starburst galaxies, and Hubble Space Telescope images, which show that they contain a high fraction of interacting or distorted systems. In conjunction with this paper, we make a public data release of data for the first 100 000 galaxies measured for the project.", "date": "2010-01-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "401", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1429-1452", "id_number": "CaltechAUTHORS:20100210-104344933", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100210-104344933", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council", "grant_number": "DP0772084" }, { "agency": "Australian Research Council", "grant_number": "LX0881951" }, { "agency": "Australian Research Council", "grant_number": "LE0668442" }, { "agency": "Swinburne University of Technology" }, { "agency": "The University of Queensland" }, { "agency": "AAO" }, { "agency": "Gregg Thompson Dark Energy Travel Fund" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1111/j.1365-2966.2009.15754.x", "primary_object": { "basename": "Drinkwater2010p6976Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/gtntv-sn183/files/Drinkwater2010p6976Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2010", "author_list": "Drinkwater, Michael J.; Jurek, Russell J.; et el." }, { "id": "https://authors.library.caltech.edu/records/x0j8q-46843", "eprint_id": 22891, "eprint_status": "archive", "datestamp": "2023-08-21 23:03:15", "lastmod": "2024-01-13 00:11:57", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna M." }, "orcid": "0000-0002-2894-6936" }, { "id": "Ahmed-S", "name": { "family": "Ahmed", "given": "Sara" } }, { "id": "Ashley-M-C-B", "name": { "family": "Ashley", "given": "Michael C. B." } }, { "id": "Barreto-M-K", "name": { "family": "Barreto", "given": "Max K." } }, { "id": "Cui-Xiangqun", "name": { "family": "Cui", "given": "Xiangqun" } }, { "id": "Delacroix-A", "name": { "family": "Delacroix", "given": "Alex" } }, { "id": "Feng-LongLong", "name": { "family": "Feng", "given": "LongLong" } }, { "id": "Gong-Xuefei", "name": { "family": "Gong", "given": "Xuefei" } }, { "id": "Lawrence-J", "name": { "family": "Lawrence", "given": "Jon" } }, { "id": "Luong-van-D-M", "name": { "family": "Luong-van", "given": "Daniel M." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Riddle-R-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Rowley-N", "name": { "family": "Rowley", "given": "Nicole" } }, { "id": "Shang-Zhaohui", "name": { "family": "Shang", "given": "Zhaohui" } }, { "id": "Storey-J-W-V", "name": { "family": "Storey", "given": "John W. V." } }, { "id": "Tothill-N-F-H", "name": { "family": "Tothill", "given": "Nick F. H." } }, { "id": "Travouillon-T", "name": { "family": "Travouillon", "given": "Tony" } }, { "id": "Wang-Lifan", "name": { "family": "Wang", "given": "Lifan" } }, { "id": "Yang-Huigen", "name": { "family": "Yang", "given": "Huigen" } }, { "id": "Yang-Ji", "name": { "family": "Yang", "given": "Ji" } }, { "id": "Zhou-Xu", "name": { "family": "Zhou", "given": "Xu" } }, { "id": "Zhu-Zhengxi", "name": { "family": "Zhu", "given": "Zhengxi" } } ] }, "title": "Gattini 2010: Cutting Edge Science at the Bottom of the World", "ispublished": "unpub", "full_text_status": "public", "keywords": "Gattini; Dome A; PLATO observatory; Antarctic wide field surveys; cosmic web; site testing; cloud cover; aurora; night sky brightness", "note": "\u00a9 2010 SPIE.\n\nThis research is supported by the Chinese PANDA International Polar Year project and the Polar Research Institute of\nChina. The authors wish to thank all the members of the 20081200912010 PRIC Dome A expeditions for their heroic\nefforts in reaching the site and for providing invaluable assistance to the expedition astronomers in setting up the\nPLATO observatory and its associated instrument suite. This research is financially supported by the US National\nScience Foundation and the United States Antarctic Program. The operation of PLATO at Dome A is supported by the\nAustralian Research Council, the Australian Antarctic Division, and the University of New South Wales.\n\nPublished - Moore2010p12880Adaptive_Optics_Systems_Pts_1-3.pdf
", "abstract": "The high altitude Antarctic sites of Dome A and the South Pole offer intriguing locations for future large scale optical astronomical\n Observatories. The Gattini project was created to measure the optical\n sky brightness, large area cloud cover and aurora of the winter-time\n sky above such high altitude Antarctic sites. The Gattini-DomeA camera\n was installed on the PLATO instrument module as part of the Chinese-led\n traverse to the highest point on the Antarctic plateau in January 2008.\n This single automated wide field camera contains a suite of Bessel\n photometric filters (B, V, R) and a long-pass red filter for the\n detection and monitoring of OH emission. We have in hand one complete\n winter-time dataset (2009) from the camera that was recently returned\n in April 2010.\n The Gattini-South Pole UV camera is a wide-field optical camera that in\n 2011 will measure for the first time the UV properties of the\n winter-time sky above the South Pole dark sector. This unique dataset\n will consist of frequent images taken in both broadband U and B filters\n in addition to high resolution (R similar to 5000) long slit\n spectroscopy over a narrow bandwidth of the central field. The camera\n is a proof of concept for the 2m-class Antarctic Cosmic Web Imager\n telescope, a dedicated experiment to directly detect and map the\n redshifted lyman alpha fluorescence or Cosmic Web emission we believe\n possible due to the unique geographical qualities of the site.\n We present the current status of both projects.", "date": "2010", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 77331S", "id_number": "CaltechAUTHORS:20110315-091730089", "isbn": "978-0-81948-223-5", "book_title": "Ground-based and airborne telescopes III", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-091730089", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chinese PANDA International Polar Year project" }, { "agency": "Polar Research Institute of China (PRIC)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Stepp-L-M", "name": { "family": "Stepp", "given": "Larry M." } }, { "id": "Gilmozzi-R", "name": { "family": "Gilmozzi", "given": "Roberto" } }, { "id": "Hall-H-J", "name": { "family": "Hall", "given": "Helen J." } } ] }, "doi": "10.1117/12.858187", "primary_object": { "basename": "Moore2010p12880Adaptive_Optics_Systems_Pts_1-3.pdf", "url": "https://authors.library.caltech.edu/records/x0j8q-46843/files/Moore2010p12880Adaptive_Optics_Systems_Pts_1-3.pdf" }, "pub_year": "2010", "author_list": "Moore, Anna M.; Ahmed, Sara; et el." }, { "id": "https://authors.library.caltech.edu/records/8erbq-p0k35", "eprint_id": 20645, "eprint_status": "archive", "datestamp": "2023-08-21 22:59:52", "lastmod": "2024-01-13 00:05:39", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "Quenching Star Formation in the Green Valley: The Mass Flux at Intermediate Redshifts", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: general", "note": "\u00a9 2010 International Astronomical Union.\n\nPublished - Goncalves2010p11741Ages_Of_Stars.pdf
", "abstract": "We have obtained several hundred very deep spectra with DEIMOS/Keck in order\nto estimate the galactic mass flux density at intermediate redshifts (0.6 < z < 0.9) from the\n\"blue cloud\" to the red sequence across the so-called \"green valley\", the intermediate region in\nthe color-magnitude plot between those two populations. We use spectral indices (specifically\nD_n (4000) and H_(\u03b4,A)) to determine star formation histories. Together with an independent measurement\nof number density of galaxies in each bin of the color-magnitude plot, one can infer\nthe rate at which galaxies from a given sample are transiting through that bin. Measuring this\nvalue for all magnitude values, studies at lower redshift determined that the mass flux density\nin the green valley is comparable to both the mass build-up rate of the red sequence and the\nmass loss rate from the blue cloud. We show preliminary results for our intermediate redshift\nsample.", "date": "2010", "date_type": "published", "publisher": "Cambridge University Press", "place_of_pub": "Cambridge [England]", "pagerange": "261-264", "id_number": "CaltechAUTHORS:20101103-090116060", "isbn": "9780521764841", "book_title": "Stellar populations : planning for the next decade : proceedings of the 262th [sic] symposium of the International Astronomical Union held in Rio de Janeiro, Brasil, August 3-7, 2009", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101103-090116060", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Bruzual-Alfonzo-G-R", "name": { "family": "Bruzual-Alfonzo", "given": "Gustavo Ramon" } }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } } ] }, "doi": "10.1017/S1743921310002887", "primary_object": { "basename": "Goncalves2010p11741Ages_Of_Stars.pdf", "url": "https://authors.library.caltech.edu/records/8erbq-p0k35/files/Goncalves2010p11741Ages_Of_Stars.pdf" }, "pub_year": "2010", "author_list": "Gon\u00e7alves, Thiago S. and Martin, D. Christopher" }, { "id": "https://authors.library.caltech.edu/records/4y57r-j9v31", "eprint_id": 76872, "eprint_status": "archive", "datestamp": "2023-08-19 00:53:58", "lastmod": "2023-10-25 16:56:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Conley-A", "name": { "family": "Conley", "given": "Alex" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } } ] }, "title": "The Local Hosts of Type Ia Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 supernovae: general", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2009 July 13; accepted 2009 November 4; published 2009 December 4.\n\nJ.N. would like to thank Fillipo Mannucci, Dan Maoz, Massimo Della Valle, and Patrizia Braschi, the organizers of the 2008 May SN Ia rates conference in Florence, Italy where a preliminary version of this work was presented and discussed. We acknowledge the useful comments by the anonymous referee.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology.\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\nFunding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/.\n\nThe SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck Institute for Astronomy (MPIA), the Max-Planck Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.\n\nPublished - Neill_2009_ApJ_707_1449.pdf
Submitted - 0911.0690.pdf
", "abstract": "We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1 Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^(10) M\u2609, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population. A low host extinction subsample hints at a residual trend in peak luminosity with host age, after correcting for light-curve shape, giving the appearance that older hosts produce less-extincted SNe Ia on average. This has implications for cosmological fitting of SNe Ia, and suggests that host age could be useful as a parameter in the fitting. Converting host mass to metallicity and computing ^(56)Ni mass from the supernova light curves, we find that our local sample is consistent with a model that predicts a shallow trend between stellar metallicity and the ^(56)Ni mass that powers the explosion, but we cannot rule out the absence of a trend. We measure a correlation between ^(56)Ni mass and host age in the local universe that is shallower and not as significant as that seen at higher redshifts. The details of the age-^(56)Ni mass correlations at low and higher redshift imply a luminosity-weighted age threshold of ~3 Gyr for SN Ia hosts, above which they are less likely to produce SNe Ia with ^(56)Ni masses above ~0.5 M\u2609.", "date": "2009-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "707", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1449-1465", "id_number": "CaltechAUTHORS:20170424-145706380", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170424-145706380", "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)" }, { "agency": "NASA" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.1088/0004-637X/707/2/1449", "primary_object": { "basename": "0911.0690.pdf", "url": "https://authors.library.caltech.edu/records/4y57r-j9v31/files/0911.0690.pdf" }, "related_objects": [ { "basename": "Neill_2009_ApJ_707_1449.pdf", "url": "https://authors.library.caltech.edu/records/4y57r-j9v31/files/Neill_2009_ApJ_707_1449.pdf" } ], "pub_year": "2009", "author_list": "Neill, J. D.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/41psc-yz579", "eprint_id": 16919, "eprint_status": "archive", "datestamp": "2023-08-21 22:45:42", "lastmod": "2023-10-19 22:39:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sheen-Yun-Kyeong", "name": { "family": "Sheen", "given": "Yun-Kyeong" } }, { "id": "Jeong-Hyunjin", "name": { "family": "Jeong", "given": "Hyunjin" } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Ferreras-I", "name": { "family": "Ferreras", "given": "Ignacio" } }, { "id": "Lotz-J-M", "name": { "family": "Lotz", "given": "Jennifer M." }, "orcid": "0000-0003-3130-5643" }, { "id": "Olsen-Knut-A-G", "name": { "family": "Olsen", "given": "Knut A. G." }, "orcid": "0000-0002-7134-8296" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Barnes-S-A", "name": { "family": "Barnes", "given": "Sydney" } }, { "id": "Park-Jang-Hyun", "name": { "family": "Park", "given": "Jang-Hyun" } }, { "id": "Ree-Chang-H", "name": { "family": "Ree", "given": "Chang H." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friendman-P-G", "name": { "family": "Friendman", "given": "Peter G." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "Tidal Dwarf Galaxies Around a Post-merger Galaxy, NGC 4922", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; galaxies: individual (NGC 4922); galaxies: interactions; galaxies: starburst; ultraviolet: galaxies", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 6 (2009 December); received 2009 July 28; accepted for publication 2009 October 9; published 2009 November 5.\n\nWe are indebted to Giuseppe Gavazzi and Alessandro Boselli\nfor supporting our use of the GALEX data made public after\ntheir guest investigation acquired them but prior to their use.\nWe thank the anonymous referee for various clarifications. This\nresearch was supported by Basic Science Research Program\nthrough the National Research Foundation of Korea (NRF)\nfunded by the Ministry of Education, Science and Technology\n(Doyak 20090078756). S.K.Y. also acknowledges support from\nKorea Astronomy and Space Science Institute. We have used\nthe GALEX UV data obtained from the Multimission Archive\nat the Space Telescope Science Institute (MAST). GALEX is\noperated for NASA by the California Institute of Technology\nunder NASA contract NAS5-98034. We are grateful to the\nLowell Observatory for granting observing time and hospitality during our visit.\n\nPublished - Sheen2009p6482Astron_J.pdf
", "abstract": "One possible channel for the formation of dwarf galaxies involves birth in the tidal tails of interacting galaxies. We report the detection of a bright UV tidal tail and several young tidal dwarf galaxy (TDG) candidates in the post-merger galaxy NGC 4922 in the Coma cluster. Based on a two-component population model (combining young and old stellar populations), we find that the light of tidal tail predominantly comes from young stars (a few Myr old). The Galaxy Evolution Explorer ultraviolet data played a critical role in the parameter (age and mass) estimation. Our stellar mass estimates of the TDG candidates are ~10^(6\u20137) M_\u2609, typical for dwarf galaxies.", "date": "2009-12", "date_type": "published", "publication": "Astronomical Journal", "volume": "138", "number": "6", "publisher": "American Astronomical Society", "pagerange": "1911-1916", "id_number": "CaltechAUTHORS:20091209-093951716", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091209-093951716", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Science and Technology (Korea)", "grant_number": "Doyak 20090078756" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NASA", "grant_number": "NAS5-98034" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-6256/138/6/1911", "primary_object": { "basename": "Sheen2009p6482Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/41psc-yz579/files/Sheen2009p6482Astron_J.pdf" }, "pub_year": "2009", "author_list": "Sheen, Yun-Kyeong; Jeong, Hyunjin; et el." }, { "id": "https://authors.library.caltech.edu/records/7hqe0-5m943", "eprint_id": 16790, "eprint_status": "archive", "datestamp": "2023-08-21 22:43:13", "lastmod": "2023-10-19 22:33:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik A." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Tremonti-C-A", "name": { "family": "Tremonti", "given": "Christy" } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara" } }, { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Ptak-A", "name": { "family": "Ptak", "given": "Andy" }, "orcid": "0000-0001-5655-1440" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Ford-H-C", "name": { "family": "Ford", "given": "Holland C." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry" }, "orcid": "0000-0002-1576-1676" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" } ] }, "title": "Local Lyman Break Galaxy Analogs: The Impact of Massive Star-Forming Clumps on the Interstellar Medium and the Global Structure of Young, Forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: bulges; galaxies: high-redshift; galaxies: peculiar; galaxies: starburst", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 1 (2009 November 20); received 2009 June 18; accepted for publication 2009 October 7;\npublished 2009 October 28.\n\nWe are very grateful to Frederic Bournaud, Rychard\nBouwens, Jarle Brinchmann, Bruce Elmegreen, Guinevere\nKauffmann, Lisa Kewley, Isa Oliveira, Francesco Shankar, and\nthe anonymous referee for useful suggestions and discussions.\nWe thank Brent Groves for generating the optically thin models\nreferred to in Section 4. We thank Anne Pellerin for her help\nwith the WFPC2 reductions. We thank the support staff at ESO\nParanal for their assistance with the FLAMES observations.\n\nPublished - Overzier2009p6414Astrophys_J.pdf
", "abstract": "We report on the results of Hubble Space Telescope optical and UV imaging, Spitzer mid-IR photometry, and optical spectroscopy of a sample of 30 low-redshift (z ~ 0.1 to 0.3) galaxies chosen from the Sloan Digital Sky Survey and Galaxy Evolution Explorer surveys to be accurate local analogs of the high-redshift Lyman break galaxies. The Lyman break analogs (LBAs) are similar in stellar mass, metallicity, dust extinction, star formation rate (SFR), physical size, and gas velocity dispersion, thus enabling a detailed investigation of many processes that are important in star-forming galaxies at high redshift. The main optical emission-line properties of LBAs, including evidence for outflows, are also similar to those typically found at high redshift. This indicates that the conditions in their interstellar medium are comparable. In the UV, LBAs are characterized by complexes of massive clumps of star formation, while in the optical they most often show evidence for (post-)mergers and interactions. In six cases, we find a single extremely massive (up to several \u00d710^9 M_\u2609) compact (radius ~10^2 pc) dominant central object (DCO). The DCOs are preferentially found in LBAs with the highest mid-IR luminosities (L_(24 \u03bcm) = 10^(10.3)-10^(11.2) L_\u2609) and correspondingly high SFRs (15-100 M_\u2609 yr^(\u20131)). We show that the massive star-forming clumps (including the DCOs) have masses much larger than the nuclear super star clusters seen in normal late-type galaxies. However, the DCOs do have masses, sizes, and densities similar to the excess light/central cusps seen in typical elliptical galaxies with masses similar to the LBA galaxies. We suggest that the DCOs form in the present-day examples of the dissipative mergers at high redshift that are believed to have produced the central cusps in local ellipticals (consistent with the disturbed optical morphologies of the LBAs). More generally, the properties of the LBAs are consistent with the idea that instabilities in a gas-rich disk lead to very massive star-forming clumps that eventually coalesce to form a spheroid. Finally, we comment on the apparent lack of energetically significant active galactic nuclei in the DCOs. We speculate that the DCOs are too young at present to grow a supermassive black hole because they are still in a supernova-dominated outflow phase (age less than 50 Myr).", "date": "2009-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "706", "number": "1", "publisher": "American Astronomical Society", "pagerange": "203-222", "id_number": "CaltechAUTHORS:20091124-113044359", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091124-113044359", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/706/1/203", "primary_object": { "basename": "Overzier2009p6414Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7hqe0-5m943/files/Overzier2009p6414Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Overzier, Roderik A.; Heckman, Timothy M.; et el." }, { "id": "https://authors.library.caltech.edu/records/r85nt-hx563", "eprint_id": 15881, "eprint_status": "archive", "datestamp": "2023-08-21 21:51:39", "lastmod": "2023-10-19 17:19:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rey-Soo-Chang", "name": { "family": "Rey", "given": "Soo-Chang" } }, { "id": "Sohn-Sangmo-T", "name": { "family": "Sohn", "given": "Sangmo T." } }, { "id": "Beasley-M-A", "name": { "family": "Beasley", "given": "Michael A." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Yoon-Suk-Jin", "name": { "family": "Yoon", "given": "Suk-Jin" } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Kang-Yongbeom", "name": { "family": "Kang", "given": "Yongbeom" } }, { "id": "Lee-Kyeongsook", "name": { "family": "Lee", "given": "Kyeongsook" } }, { "id": "Chung-Chul", "name": { "family": "Chung", "given": "Chul" } }, { "id": "Lee-Sang-Yoon", "name": { "family": "Lee", "given": "Sang-Yoon" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jose" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } } ] }, "title": "Probing the intermediate-age globular clusters in NGS 5128 from ultraviolet observations", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 5128); galaxies: star clusters; globular clusters: general; ultraviolet: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2009 May 12, accepted for publication 2009 June 12\nPublished 2009 June 29. \n\nWe thank Sugata Kaviraj for useful suggestions on the\nmanuscript. This work was supported by the Korea Research\nFoundation Grant funded by the Korean Government\n(MOEHRD; KRF-2005-202-C00158) and the Korea Science\nand Engineering Foundation (KOSEF) through the Astrophysical\nResearch Center for the Structure and Evolution of the\nCosmos (ARCSEC). GALEX (Galaxy Evolution Explorer) is a\nNASA Small Explorer, launched in 2003 April. We gratefully\nacknowledge NASA's support for construction, operation, and\nscience analysis for the GALEX mission, developed in cooperation\nwith the Centre National d'Etudes Spatiales of France and\nthe Korean Ministry of Science and Technology.\n\nPublished - Rey2009p5117Astrophys_J_Lett.pdf
", "abstract": "We explore the age distribution of the globular cluster (GC) system of the nearby elliptical galaxy NGC 5128\nusing ultraviolet (UV) photometry from GALEX observations, with UV\u2013optical colors used as the age indicator.\nMost GCs in NGC 5128 follow the general trends of GCs in M31 and the Milky Way in the UV\u2013optical color\u2013\ncolor diagram, which indicates that the majority of GCs in NGC 5128 are old similar to the age range of old\nGCs in M31 and the Milky Way. A large fraction of spectroscopically identified intermediate-age GC (IAGC)\ncandidates with ~3\u20138 Gyr are not detected in the far-UV (FUV) passband. Considering the nature of intermediate age\npopulations being faint in the FUV passband, we suggest that many of the spectroscopically identified IAGCs\nmay be truly intermediate in age. This is in contrast to the case of M31 where a large fraction of spectroscopically\nsuggested IAGCs are detected in FUV and therefore may not be genuine IAGCs but rather older GCs with\ndeveloped blue horizontal branch stars. Our UV photometry strengthens the results previously suggesting the\npresence of GC and stellar subpopulation with intermediate age in NGC 5128. The existence of IAGCs strongly\nindicates the occurrence of at least one more major star formation episode after a starburst at high redshift.", "date": "2009-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "700", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L11-L15", "id_number": "CaltechAUTHORS:20090916-115854862", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090916-115854862", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Korea Research Foundation", "grant_number": "KRF-2005-202-C00158" }, { "agency": "Korea Science and Engineering Foundation" }, { "agency": "Astrophysical Research Center for the Structure and Evolution of the Cosmos (ARCSEC)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/700/1/L11", "primary_object": { "basename": "Rey2009p5117Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/r85nt-hx563/files/Rey2009p5117Astrophys_J_Lett.pdf" }, "pub_year": "2009", "author_list": "Rey, Soo-Chang; Sohn, Sangmo T.; et el." }, { "id": "https://authors.library.caltech.edu/records/9prk2-bxw73", "eprint_id": 14844, "eprint_status": "archive", "datestamp": "2023-08-20 02:16:31", "lastmod": "2023-10-18 19:57:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara R." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S\u00e9bastien" } }, { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Tim" } }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "Michel" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd A." } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Studying Large- and Small-Scale Environments of Ultraviolet Luminous Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution galaxies: halos galaxies: interactions galaxies: starburst methods: statistical", "note": "\u00a9 2009. The American Astronomical Society. Received 2008 September 13; accepted 2009 March 26; published 2009 June 23. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with\nthe Centre National d'Etudes Spatiales of France and the Korean\nMinistry of Science and Technology. The HST COSMOS\nprogram was supported through NASA grant HST-GO-\n09822. More information on the COSMOS survey is available at\nhttp://www.astro.caltech.edu/cosmos. We thank Michael Blanton\nfor access to the IDL kcorrect (version 4.1.4) analysis package.\nThis work has greatly benefitted from the careful comments\nand suggestions made by the anonymous referee. A.R.B. gratefully\nrecognizes Ian McGreer and Andrei Mesinger for their\ncontributions to this analysis, and David Hogg for insightful discussions.\n\nPublished - BasuZych2009p4712Astrophys_J.pdf
", "abstract": "Studying the environments of 0.4 < z < 1.2 ultraviolet (UV)-selected galaxies, as examples of extreme star-forming galaxies (with star formation rates (SFRs) in the range of 3-30 M_\u2609 yr^(\u20131)), we explore the relationship between high rates of star formation, host halo mass, and pair fractions. We study the large- and small-scale environments of local ultraviolet luminous galaxies (UVLGs) by measuring angular correlation functions. We cross-correlate these systems with other galaxy samples: a volume-limited sample (ALL), a blue luminous galaxy sample, and a luminous red galaxy (LRG) sample. We determine the UVLG comoving correlation length to be r_0 = 4.8^(+11.6)_(\u20132.4) h^(\u20131) Mpc at z = 1.0, which is unable to constrain the halo mass for this sample. However, we find that UVLGs form close (separation <30 kpc) pairs with the ALL sample, but do not frequently form pairs with LRGs. A rare subset of UVLGs, those with the highest FUV surface brightnesses, are believed to be local analogs of high-redshift Lyman break galaxies (LBGs) and are called Lyman break analogs (LBAs). LBGs and LBAs share similar characteristics (i.e., color, size, surface brightness, specific SFRs, metallicities, and dust content). Recent Hubble Space Telescope images of z ~ 0.2 LBAs show disturbed morphologies, signs of mergers and interactions. UVLGs may be influenced by interactions with other galaxies and we discuss this result in terms of other high star-forming, merging systems.", "date": "2009-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "699", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1307-1320", "id_number": "CaltechAUTHORS:20090806-102256755", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090806-102256755", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" }, { "agency": "NASA", "grant_number": "HST-GO-09822" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/699/2/1307", "primary_object": { "basename": "BasuZych2009p4712Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/9prk2-bxw73/files/BasuZych2009p4712Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Basu-Zych, Antara R.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/74sya-8j842", "eprint_id": 15355, "eprint_status": "archive", "datestamp": "2023-08-21 21:39:36", "lastmod": "2023-10-18 21:42:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Tim" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Eracleous-M", "name": { "family": "Eracleous", "given": "Michael" }, "orcid": "0000-0002-3719-940X" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Gon\u00e7alves-T-S", "name": { "family": "Gon\u00e7alves", "given": "Thiago S." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Chris" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "Luminous Thermal Flares from Quiescent Supermassive Black Holes", "ispublished": "pub", "full_text_status": "public", "keywords": "black hole physics; galaxies: nuclei; ultraviolet: ISM; X-rays: galaxies", "note": "\u00a9 2009. The American Astronomical Society. Received 2008 December 15; accepted 2009 April 14; published 2009 May 29.\nWe thank the anonymous referee for their helpful comments.\nS.G. was supported by NASA through Hubble Fellowship grant\nHST-HF-01219.01-A awarded by the Space Telescope Science\nInstitute, which is operated by the Association of Universities\nfor Research in Astronomy, Inc., for NASA, under contract\nNAS 5-26555, and in part by Chandra grant G07- 8112X. We\ngratefully acknowledge NASA's support for construction, operation,\nand science analysis for the GALEX mission, developed\nin cooperation with Centre National d'Etudes Spatiales\nof France and the Korean Ministry of Science and Technology.\nSome of the data presented were obtained at the W. M.\nKeck Observatory, which is operated as a scientific partnership\namong the California Institute of Technology, the University of\nCalifornia, and NASA. The Observatory was make possible by\nthe generous financial support of the W. M. Keck Foundation.\nThe analysis pipeline used to reduce the DEIMOS data was\ndeveloped at UC Berkeley with support from NSF grant AST-\n0071048. The Hobby-Eberly Telescope (HET) is a joint project\nof the University of Texas at Austin, the Pennsylvania State University,\nStanford University, Ludwig-Maximillians-Universit\u00e4t\nM\u00fcnchen, and Georg-August-Universit\u00e4t G\u00f6ttingen. The HET\nis named in honor of its principal benefactors,William P. Hobby\nand Robert E. Eberly. The Marcario Low-Resolution Spectrograph\nis named for Mike Marcario of High Lonesome Optics,\nwho fabricated several optics for the instrument but died before\nits completion; it is a joint project of the Hobby\u2013Eberly\nTelescope partnership and the Instituto de Astronom\u00eda de la\nUniversidad Nacional Aut\u03ccnoma de M\u00e9xico.\n\nPublished - Gezari2009p4601Astrophys_J.pdf
", "abstract": "A dormant supermassive black hole lurking in the center of a galaxy will be revealed when a star passes close enough to be torn apart by tidal forces, and a flare of electromagnetic radiation is emitted when the bound fraction of the stellar debris falls back onto the black hole and is accreted. Although the tidal disruption of a star is a rare event in a galaxy,\u224810^(\u20134) yr^(\u20131), observational candidates have emerged in all-sky X-ray and deep ultraviolet (UV) surveys in the form of luminous UV/X-ray flares from otherwise quiescent galaxies. Here we present the third candidate tidal disruption event discovered in the Galaxy Evolution Explorer (GALEX) Deep Imaging Survey: a 1.6 \u00d7 10^(43) erg s^(\u20131) UV/optical flare from a star-forming galaxy at z = 0.1855. The UV/optical spectral energy distribution (SED) during the peak of the flare measured by GALEX and Palomar Large Field Camera imaging can be modeled as a single temperature blackbody with T_(bb) = 1.7 \u00d7 10^5 K and a bolometric luminosity of 3 \u00d7 10^(45) erg s^(\u20131), assuming an internal extinction with E(B \u2013 V)_(gas) = 0.3. The Chandra upper limit on the X-ray luminosity during the peak of the flare, L_X (2 \u2013 10 keV)<10^(41) erg s^(\u20131), is 2 orders of magnitude fainter than expected from the ratios of UV to X-ray flux density observed in active galaxies. We compare the light curves and broadband properties of all three tidal disruption candidates discovered by GALEX, and find that (1) the light curves are well fitted by the power-law decline expected for the fallback of debris from a tidally disrupted solar-type star and (2) the UV/optical SEDs can be attributed to thermal emission from an envelope of debris located at roughly 10 times the tidal disruption radius of a \u224810^7 M_\u2609 central black hole. We use the observed peak absolute optical magnitudes of the flares (\u201317.5>M_g > \u2013 18.9) to predict the detection capabilities of upcoming optical synoptic surveys.", "date": "2009-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "698", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1367-1379", "id_number": "CaltechAUTHORS:20090827-112314953", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090827-112314953", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-HF-01219.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Chandra", "grant_number": "G07- 8112X" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-0071048" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/698/2/1367", "primary_object": { "basename": "Gezari2009p4601Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/74sya-8j842/files/Gezari2009p4601Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Gezari, Suvi; Heckman, Tim; et el." }, { "id": "https://authors.library.caltech.edu/records/5shns-74157", "eprint_id": 15415, "eprint_status": "archive", "datestamp": "2023-08-20 02:06:12", "lastmod": "2023-10-18 21:45:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S\u00e9bastien" } }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "St\u00e9phane" } }, { "id": "Arag\u03ccn-Calvo-M-A", "name": { "family": "Arag\u03ccn-Calvo", "given": "Miguel A." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Peter-F-G", "name": { "family": "Peter", "given": "Friedman G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Spatial Clustering from GALEX-SDSS Samples: Star Formation History and Large-Scale Clustering", "ispublished": "pub", "full_text_status": "public", "keywords": "ultraviolet: galaxies", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2008 December 8; accepted 2009 April 21; published 2009 June 4. \n\nWe thank Ching-Wa Yip for useful discussions. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASAs support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d(tm)Etudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - Heinis2009p4610Astrophys_J.pdf
", "abstract": "We measure the projected spatial correlation function w_p (r_p ) from a large sample combining Galaxy Evolution Explorer ultraviolet imaging with the Sloan Digital Sky Survey spectroscopic sample. We study the dependence of the clustering strength for samples selected on (NUV \u2013 r)_(abs) color, specific star formation rate (SSFR), and stellar mass. We find that there is a smooth transition in the clustering of galaxies as a function of this color from weak clustering among blue galaxies to stronger clustering for red galaxies. The clustering of galaxies within the \"green valley\" has an intermediate strength, and is consistent with that expected from galaxy groups. The results are robust to the correction for dust extinction. The comparison with simple analytical modeling suggests that the halo occupation number increases with older star formation epochs. When splitting according to SSFR, we find that the SSFR is a more sensitive tracer of environment than stellar mass.", "date": "2009-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "698", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1838-1851", "id_number": "CaltechAUTHORS:20090828-130619755", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090828-130619755", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/698/2/1838", "primary_object": { "basename": "Heinis2009p4610Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/5shns-74157/files/Heinis2009p4610Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Heinis, S\u00e9bastien; Budav\u00e1ri, Tam\u00e1s; et el." }, { "id": "https://authors.library.caltech.edu/records/axpa8-8kq87", "eprint_id": 15619, "eprint_status": "archive", "datestamp": "2023-08-21 21:26:34", "lastmod": "2023-10-19 14:39:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "The Star Formation Law at Low Surface Density", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: irregular; galaxies: ISM; galaxies: spiral; ultraviolet: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 October 2; accepted 2009 February 24; published 2009 April 27. \n\nWe thank Joannah Hinz, Samuel Boissier, Robert Kennicutt, and Mark Krumholz for helpful discussions. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology.\n\nPublished - Wyder2009p2578Astrophys_J.pdf
", "abstract": "We investigate the nature of the star formation law at low gas surface densities using a sample of 19 low surface brightness (LSB) galaxies with existing H I maps in the literature, UV imaging from the Galaxy Evolution Explorer satellite, and optical images from the Sloan Digital Sky Survey. All of the LSB galaxies have (NUV \u2013 r) colors similar to those for higher surface brightness star-forming galaxies of similar luminosity indicating that their average star formation histories are not very different. Based upon four LSB galaxies with both UV and far-infrared (FIR) data, we find FIR/UV ratios significantly less than 1, implying low amounts of internal UV extinction in LSB galaxies. We use the UV images and H I maps to measure the star formation rate (SFR) and hydrogen gas surface density within the same region for all the galaxies. The LSB galaxy star formation rate surface densities lie below the extrapolation of the power law fit to the SFR surface density as a function of the total gas density for higher surface brightness galaxies. Although there is more scatter, the LSB galaxies also lie below a second version of the star formation law in which the SFR surface density is correlated with the gas density divided by the orbital time in the disk. The downturn seen in both star formation laws is consistent with theoretical models that predict lower star formation efficiencies in LSB galaxies due to the declining molecular fraction with decreasing density.", "date": "2009-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "696", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1834-1853", "id_number": "CaltechAUTHORS:20090904-124126138", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090904-124126138", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/696/2/1834", "primary_object": { "basename": "Wyder2009p2578Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/axpa8-8kq87/files/Wyder2009p2578Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Wyder, Ted K.; Martin, D. Christopher; et el." }, { "id": "https://authors.library.caltech.edu/records/3bpzr-2mh11", "eprint_id": 18227, "eprint_status": "archive", "datestamp": "2023-08-21 21:24:43", "lastmod": "2024-01-12 23:39:38", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" } ] }, "title": "The GALEX View of Supernova Hosts", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: evolution; supemovae: general", "note": "\u00a9 2009 American Institute of Physics.\n\nIssue Date: 3 May 2009.\n\nWe acknowledge the use of the NASA Extragalactic Database and the Infra-Red Science Archive and their vital contribution to this work.\n\nPublished - Neill2009p8067Probing_Stellar_Populations_Out_To_The_Distant_Universe.pdf
", "abstract": "We exploit the accumulating, high-quality, multi-wavelength imaging data of nearby supernova (SN) hosts to explore the relationship between SN production and host galaxy evolution. The Galaxy Evolution Explorer (GALEX, [1]) provides ultraviolet (UV) imaging in two bands, complementing data in the optical and infra-red (IR). We compare host properties, derived from spectral energy distribution (SED) fitting, with nearby, well-observed SN Ia light curve properties. We also explore where the hosts of different types of SNe fall relative to the red and blue sequences on the galaxy UV-optical color-magnitude diagram (CMD, [2]). We conclude that further exploration and larger samples will provide useful results for constraining the progenitors of SNe.", "date": "2009-05-03", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "New York, NY", "pagerange": "528-531", "id_number": "CaltechAUTHORS:20100510-152057423", "isbn": "978-0-7354-0648-3", "book_title": "Probing Stellar Populations Out to the Distant Universe: CEFALU 2008, Proceedings of the International Conference", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100510-152057423", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1063/1.3141604", "primary_object": { "basename": "Neill2009p8067Probing_Stellar_Populations_Out_To_The_Distant_Universe.pdf", "url": "https://authors.library.caltech.edu/records/3bpzr-2mh11/files/Neill2009p8067Probing_Stellar_Populations_Out_To_The_Distant_Universe.pdf" }, "pub_year": "2009", "author_list": "Neill, James D.; Sullivan, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/cj5cf-1h258", "eprint_id": 14134, "eprint_status": "archive", "datestamp": "2023-08-21 21:10:32", "lastmod": "2023-10-18 16:09:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S\u00e9bastien" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alexander S." } }, { "id": "Nieto-Santisteban-M", "name": { "family": "Nieto-Santisteban", "given": "Mar\u00eda" } }, { "id": "Gupchup-J", "name": { "family": "Gupchup", "given": "Jayant" } }, { "id": "Shiao-B", "name": { "family": "Shiao", "given": "Bernie" } }, { "id": "Smith-M", "name": { "family": "Smith", "given": "Myron" }, "orcid": "0000-0002-3321-1432" }, { "id": "Chang-R", "name": { "family": "Chang", "given": "Ruixiang" } }, { "id": "Kauffmann-G", "name": { "family": "Kauffmann", "given": "Guinevere" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } } ] }, "title": "GALEX\u2013SDSS catalogs for statistical studies", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; methods: statistical; surveys; ultraviolet: general", "note": "\u00a9 2009. The American Astronomical Society.\nReceived 2008 August 14; accepted 2009 January 5; published 2009 March 24.\nGALEX is a NASA Small Explorer. We acknowledge NASA's\nsupport for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. This research has made use of data obtained from and software provided by the US National Virtual Observatory, which is sponsored by the National Science Foundation. T.B. gratefully acknowledges support from the Gordon and Betty Moore Foundation via GBMF 554.\n\nPublished - Budavari2009p1375Astrophys_J.pdf
", "abstract": "We present a detailed study of the Galaxy Evolution Explorer's (GALEX) photometric catalogs with special focus\non the statistical properties of the All-sky and Medium Imaging Surveys. We introduce the concept of primaries to\nresolve the issue of multiple detections and follow a geometric approach to define clean catalogs with well understood selection functions. We cross-identify the GALEX sources (GR2+3) with Sloan Digital Sky Survey (SDSS; DR6)\nobservations, which indirectly provides an invaluable insight into the astrometric model of the UV sources and\nallows us to revise the band merging strategy. We derive the formal description of the GALEX footprints as well as\ntheir intersections with the SDSS coverage along with analytic calculations of their areal coverage. The crossmatch catalogs are made available for the public. We conclude by illustrating the implementation of typical selection criteria in SQL for catalog subsets geared toward statistical analyses, e.g., correlation and luminosity function studies.", "date": "2009-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "694", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1281-1292", "id_number": "CaltechAUTHORS:20090501-142926332", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090501-142926332", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF 554" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/694/2/1281", "primary_object": { "basename": "Budavari2009p1375Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/cj5cf-1h258/files/Budavari2009p1375Astrophys_J.pdf" }, "pub_year": "2009", "author_list": "Budav\u00e1ri, Tam\u00e1s; Heinis, S\u00e9bastien; et el." }, { "id": "https://authors.library.caltech.edu/records/g904j-7dv15", "eprint_id": 15314, "eprint_status": "archive", "datestamp": "2023-08-20 00:57:51", "lastmod": "2023-10-18 21:39:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David A." }, "orcid": "0000-0002-8528-7340" }, { "id": "Donovan-J", "name": { "family": "Donovan", "given": "Jennifer" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" } ] }, "title": "Massive star formation within the Leo 'primordial' ring", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2009 Nature Publishing Group. \n\nReceived 3 November 2008; Accepted 13 January 2009. \n\nGALEX is a NASA Small Explorer, launched in April 2003. We gratefully acknowledge NASA's support of the construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales, France, and the Korean Ministry of Science and Technology. This research draws upon data provided by B. Millis as distributed by the National Optical Astronomy Observatory (NOAO) Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy under a cooperative agreement with the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research made use of NASA's Astrophysics Data System.", "abstract": "Few intergalactic, plausibly primordial clouds of neutral atomic hydrogen (H I) have been found in the local Universe, suggesting that such structures have either dispersed, become ionized or produced a stellar population on gigayear timescales. The Leo ring1,2, a massive (M_(HI)<1.8x10^9M_\u2299, M_\u2299 denoting the solar mass), 200-kpc-wide structure orbiting the galaxies M105 and NGC3384 with a 4-Gyr period, is a candidate primordial cloud. Despite repeated atttempts3,4, it has previously been seen only from HI emission, suggesting the absence of a stellar population. Here we report the detection of ultraviolet light from gaseous substructures of the Leo ring, which we attribute to recent massive star formation. The ultraviolet colour of the detected complexes is blue, implying the onset of a burst of star formation or continuous star formation of moderate (~10^8-yr) duration. Measured ultraviolet\u2013visible photometry favours models with low metallicity (Z=Z_\u2299/50\u2013Z_\u2299/5, Z_\u2299 denoting the solar metallicity), that is, a low proportion of elements heavier than helium, although spectroscopic confirmation is needed. We speculate that the complexes are dwarf galaxies observed during their formation, but distinguished by their lack of a dark matter component5. In this regard, they resemble tidal dwarf galaxies, although without the enrichment preceding tidal stripping. If structures like the Leo ring were common in the early Universe, they may have produced a large, yet undetected, population of faint, metal-poor, halo-lacking dwarf galaxies.", "date": "2009-02-19", "date_type": "published", "publication": "Nature", "volume": "457", "number": "7232", "publisher": "Nature Publishing Group", "pagerange": "990-993", "id_number": "CaltechAUTHORS:20090826-105346060", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090826-105346060", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/nature07780", "pub_year": "2009", "author_list": "Thilker, David A.; Donovan, Jennifer; et el." }, { "id": "https://authors.library.caltech.edu/records/1tttg-dnp32", "eprint_id": 16337, "eprint_status": "archive", "datestamp": "2023-08-22 12:46:00", "lastmod": "2023-10-19 22:07:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "id": "Dessart-L", "name": { "family": "Dessart", "given": "Luc" } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "St\u00e9phane" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Woosley-S-E", "name": { "family": "Woosley", "given": "S. E." } }, { "id": "Hillier-D-J", "name": { "family": "Hillier", "given": "D. John" } }, { "id": "Bazin-G", "name": { "family": "Bazin", "given": "Gurvan" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Le-Du-J", "name": { "family": "Le Du", "given": "J\u00e9r\u00e9my" } }, { "id": "Mazure-A", "name": { "family": "Mazure", "given": "Alain" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "radiative transfer; stars: atmospheres; supernovae: general; ultraviolet: ISM", "note": "\u00a9 2008 The American Astronomical Society.\nPrint publication: Issue 2 (2008 August 20)\nReceived 2008 April 7, accepted for publication 2008 July 8\nPublished 2008 July 31.\nWe thank the anonymous referee for their helpful comments.\nL. D. acknowledges support for this work from the SciDAC\nprogram of the DOE, under grants DE-FC02-01ER41184 and\nDE-FC02-06ER41452, and from the NSF under grant AST-\n0504947. S. W. acknowledges support from the SciDAC under\ngrant DE-FC02-06ER41438 and also by NASA under grant\nNNG05GG28G. S. G. and S. B. thank Bruno Milliard for his\nsupport during this study. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with CNES of France\nand the Korean MOST. Based on observations obtained with\nMegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA,\nat the CFHT, which is operated by the NRC of Canada,\nthe INSU of the CNRS of France, and the University of Hawaii.\nThis work is based in part on data products produced at TERAPIX\nand the CADC as part of the CFHT Legacy Survey, a\ncollaborative project of NRC and CNRS. Based on observations\nmade with the ESO telescopes at the La Silla or Paranal Observatories\nunder proposal IDs 171.A-0486 and 176.A-0589.\n\nPublished - GEZapjl08.pdf
", "abstract": "We report the serendipitous detection by GALEX of fast (<1 day) rising (\u22731 mag) UV emission from two Type\nII plateau (II-P) supernovae (SNe) at z = 0.185 and 0.324 discovered by the Supernova Legacy Survey. Optical\nphotometry and VLT spectroscopy 2 weeks after the GALEX detections link the onset of UV emission to the time\nof shock breakout. Using radiation hydrodynamics and non-LTE radiative transfer simulations, and starting from a\nstandard red supergiant (RSG; Type II-P SN progenitor) star evolved self-consistently from the main sequence to\niron core collapse, we model the shock breakout phase and the 55 hr that follow. The small scale height of our\nRSG atmosphere model suggests that the breakout signature is a thermal soft X-ray burst (\u03bbpeak ~ 90 \u00c5) with a peak\nduration of \u227e2000 s. Longer durations are possible but require either an extended and tenuous nonstandard envelope\nor an unusually dense RSG wind with M ~ 10^(-3)M_\u2609yr^(-1). The GALEX observations miss the peak of the luminous (M_(FUV)\u2248 \u2212 20), UV burst but unambiguously capture the rise of the emission and a subsequent 2 day long plateau. \nThe postbreakout, UV-bright plateau is a prediction of our model in which the shift of the peak of the spectral\nenergy distribution (SED) from \u223c100 to \u223c1000 \u00c5 and the ejecta expansion both counteract the decrease in bolometric luminosity from \u223c10^(11) to ~ 10^9 L_\u2609 over that period. Based on the observed detection efficiency of our study, we \nmake predictions for the breakout detection rate of the GALEX Time Domain Survey.", "date": "2008-08-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "683", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L131-L134", "id_number": "CaltechAUTHORS:20091013-202239042", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091013-202239042", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-FC02-01ER41184" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FC02-06ER41452" }, { "agency": "NSF", "grant_number": "AST-0504947" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FC02-06ER41438" }, { "agency": "NASA", "grant_number": "NNG05GG28G" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" }, { "agency": "European Southern Observatory - La Silla or Paranal Observatories", "grant_number": "171.A-0486" }, { "agency": "European Southern Observatory - La Silla or Paranal Observatories", "grant_number": "176.A-0589" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/591647", "primary_object": { "basename": "GEZapjl08.pdf", "url": "https://authors.library.caltech.edu/records/1tttg-dnp32/files/GEZapjl08.pdf" }, "pub_year": "2008", "author_list": "Gezari, Suvi; Dessart, Luc; et el." }, { "id": "https://authors.library.caltech.edu/records/de1xv-ggg78", "eprint_id": 75799, "eprint_status": "archive", "datestamp": "2023-08-19 23:08:53", "lastmod": "2024-01-13 20:27:14", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tuttle-S-E", "name": { "family": "Tuttle", "given": "Sarah E." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Grange-R", "name": { "family": "Grange", "given": "Robert" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Rahman-S", "name": { "family": "Rahman", "given": "Shahinur" } }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "Jean-Michel" } }, { "id": "McLean-R", "name": { "family": "McLean", "given": "Ryan" } }, { "id": "Tajiri-Gordon", "name": { "family": "Tajiri", "given": "Gordon" } }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "M." } } ] }, "title": "The FIREBall fiber-fed UV spectrograph", "ispublished": "unpub", "full_text_status": "public", "keywords": "UV, fiber, IFU, spectroscopy, astronomical instrumentation, galaxy evolution, balloon-borne instrument", "note": "\u00a9 2008 SPIE. \n\nThe authors would like to thank Victoria Johnston, David Stenning, and Eve LoCastro for their hard work in the lab. The crew at CSBF was fantastic and make launching a balloon seem (almost) easy.\n\nPublished - 70141T_1-1.pdf
", "abstract": "FIREBall (Faint Intergalactic Redshifted Emission Balloon) had a successful first engineering flight in July of 2007 from Palestine, Texas. Here we detail the design and construction of the spectrograph. FIREBall consists of a 1m telescope coupled to a fiber-fed ultraviolet spectrograph flown on a short duration balloon. The spectrograph is designed to map hydrogen and metal line emission from the intergalactic medium at several redshifts below z=1, exploiting a small window in atmospheric oxygen absorption at balloon altitudes. The instrument is a wide-field IFU fed by almost 400 fibers. The Offner mount spectrograph is designed to be sensitive in the 195-215nm window accessible at our altitudes of 35-40km. We are able to observe Ly\u03b1, as well as OVI and CIV doublets, from 0.3 < z < 0.9. Observations of UV bright B stars and background measurements allow characterization of throughput for the entire system and will inform future flights.", "date": "2008-07-09", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 70141T", "id_number": "CaltechAUTHORS:20170406-103359612", "isbn": "978-0-8194-7224-3", "book_title": "Ground-based and airborne instrumentation for astronomy II", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170406-103359612", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } }, { "id": "Casali-M-M", "name": { "family": "Casali", "given": "Mark M." } } ] }, "doi": "10.1117/12.789836", "primary_object": { "basename": "70141T_1-1.pdf", "url": "https://authors.library.caltech.edu/records/de1xv-ggg78/files/70141T_1-1.pdf" }, "pub_year": "2008", "author_list": "Tuttle, Sarah E.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/w9880-ger04", "eprint_id": 12393, "eprint_status": "archive", "datestamp": "2023-09-14 16:44:37", "lastmod": "2023-10-23 20:42:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "Jean-Michel" } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "P\u00e9roux-C", "name": { "family": "P\u00e9roux", "given": "C\u00e9line" }, "orcid": "0000-0002-4288-599X" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jose" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Ly alpha-emitting galaxies at 0.2 < z < 0.35 from GALEX spectroscopy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: ISM; galaxies: luminosity function, mass function; galaxies: starburst; ultraviolet: galaxies", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 November 5; accepted 2008 March 1. \n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. 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 NASA.\n\nPublished - DEHapj08.pdf
", "abstract": "We have used the GALEX (Galaxy Evolution Explorer) spectroscopic survey mode, with a resolution of similar to 8 angstrom in the far-ultraviolet (FUV; 1350-1750 angstrom) and similar to 20 angstrom in the near-ultraviolet (NUV; 1950-2750 angstrom) for a systematic search of Ly alpha-emitting galaxies at low redshift. Our aim is to fill a gap between high-redshift surveys and a small set of objects studied in detail in the nearby universe. A blind search of 7018 spectra extracted in five deep exposures (5.65 deg(2)) has resulted in 96 Ly alpha-emitting galaxy candidates in the FUV domain after accounting for broad-line AGNs. The Ly alpha equivalent widths (EWs) are consistent with stellar population model predictions and show no trends as a function of UV color or UV luminosity, with the exception of a possible decrease in the most luminous objects that may be due to small-number statistics. The objects' distribution in EW is similar to that at z similar to 3, but their fraction among star-forming galaxies is smaller. Avoiding uncertain candidates, a subsample of 66 objects in the range 0.2 < z < 0.35 has been used to build a Ly alpha luminosity function (LF). The incompleteness due to objects with significant Ly alpha emission but a UV continuum too low for spectral extraction has been evaluated. A comparison with H alpha LFs in the same redshift domain is consistent with an average Ly alpha/H alpha of similar to 1 in about 15% of the star-forming galaxies. A comparison with high-redshift Ly alpha LFs implies an increase of the Ly alpha luminosity density by a factor of about 16 from z similar to 0.3 to z similar to 3. By comparison with the factor of 5 increase in the UV luminosity density in the same redshift range, this suggests an increase of the average Ly alpha escape fraction with redshift.", "date": "2008-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "680", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1072-1082", "id_number": "CaltechAUTHORS:DEHapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:DEHapj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Centre National d'Etudes Spatiales (France)" }, { "agency": "Korean Ministry of Science and Technology" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/587953", "primary_object": { "basename": "DEHapj08.pdf", "url": "https://authors.library.caltech.edu/records/w9880-ger04/files/DEHapj08.pdf" }, "pub_year": "2008", "author_list": "Deharveng, Jean-Michel; Small, Todd; et el." }, { "id": "https://authors.library.caltech.edu/records/9bxzb-jd590", "eprint_id": 14247, "eprint_status": "archive", "datestamp": "2023-08-22 11:32:49", "lastmod": "2023-10-18 16:26:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik A." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Kauffmann-G", "name": { "family": "Kauffmann", "given": "Guinevere" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara" } }, { "id": "Lotz-J-M", "name": { "family": "Lotz", "given": "Jennifer" }, "orcid": "0000-0003-3130-5643" }, { "id": "Aloisi-A", "name": { "family": "Aloisi", "given": "Alessandra" }, "orcid": "0000-0003-4137-882X" }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phanie" } }, { "id": "Hoopes-C-G", "name": { "family": "Hoopes", "given": "C." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry" }, "orcid": "0000-0002-1576-1676" } ] }, "title": "Hubble Space Telescope morphologies of local Lyman break galaxy analogs. I. evidence for starbursts triggered by merging", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; early universe; galaxies: high-redshift; galaxies: starburst", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 September 18, accepted for publication 2007 December 21.\nThis paper has benefited from discussions and helpful comments from numerous friends and colleagues. We thank Casey Papovich, Masami Ouchi, and Isa Oliveira for carefully reading through the manuscript. We further thank Rychard Bouwens, Nick Cross, Ricardo Demarco, Marijn Franx, Lisa Kewley, Cheng Li, Crystal Martin, Alessandro Rettura, Samir Salim, Christi Tremonti, Arjen van der Wel, and Andrew Zirm for discussion of various parts of this paper. R. A. O. thanks Gabrelle Saurage for her excellent support during observations at APO.\nBased on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with program 10920. Based on observations obtained with the Apache Point Observatory (APO) 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium.\n\nPublished - OVEapj08b.pdf
", "abstract": "Heckman and coworkers used the GALEX UV imaging survey to show that there exists a rare population of nearby compact UV-luminous galaxies (UVLGs) that closely resemble high-redshift Lyman break galaxies (LBGs). We present HST images in the UV, optical, and H\u03b1 and resimulate them at the depth and resolution of the GOODS/UDF fields to show that the morphologies of UVLGs are also similar to those of LBGs. Our sample of eight LBG analogs thus provides detailed insight into the connection between star formation and LBG morphology. Faint tidal features or companions can be seen in all of the rest-frame optical images, suggesting that the starbursts are the result of a merger or interaction. The UV/optical light is dominated by unresolved (~100-300 pc) super starburst regions (SSBs). A detailed comparison with the galaxies Haro 11 and VV 114 at z = 0.02 indicates that the SSBs themselves consist of diffuse stars and (super) star clusters. The structural features revealed by the new HST images occur on very small physical scales and are thus not detectable in images of high-redshift LBGs, except in a few cases where they are magnified by gravitational lensing. We propose, therefore, that LBGs are mergers of gas-rich, relatively low-mass (M_* ~ 10^(10) M\u2609) systems, and that the mergers trigger the formation of SSBs. If galaxies at high redshifts are dominated by SSBs, then the faint-end slope of the luminosity function is predicted to have slope \u03b1 ~ 2. Our results are the most direct confirmation to date of models that predict that the main mode of star formation in the early universe was highly collisional.", "date": "2008-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "677", "number": "1", "publisher": "American Astronomical Society", "pagerange": "37-62", "id_number": "CaltechAUTHORS:20090517-213718284", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090517-213718284", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/529134", "primary_object": { "basename": "OVEapj08b.pdf", "url": "https://authors.library.caltech.edu/records/9bxzb-jd590/files/OVEapj08b.pdf" }, "pub_year": "2008", "author_list": "Overzier, Roderik A.; Heckman, Timothy M.; et el." }, { "id": "https://authors.library.caltech.edu/records/dazfr-rqw98", "eprint_id": 14238, "eprint_status": "archive", "datestamp": "2023-08-22 11:31:10", "lastmod": "2023-10-18 16:25:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Graham-M-L", "name": { "family": "Graham", "given": "M. L." }, "orcid": "0000-0002-9154-3136" }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "C. J." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Gwyn-S-D-J", "name": { "family": "Gwyn", "given": "S. D. J." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "E. Y." } }, { "id": "Astier-P", "name": { "family": "Astier", "given": "P." } }, { "id": "Balam-D", "name": { "family": "Balam", "given": "D." } }, { "id": "Balland-C", "name": { "family": "Balland", "given": "C." } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "R. G." } }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "A." } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "D." } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "J." } }, { "id": "Hardin-D", "name": { "family": "Hardin", "given": "D." } }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Pain-R", "name": { "family": "Pain", "given": "R." } }, { "id": "Perrett-K-M", "name": { "family": "Perrett", "given": "K." } }, { "id": "Regnault-N", "name": { "family": "Regnault", "given": "N." } }, { "id": "Baumont-S", "name": { "family": "Baumont", "given": "S." } }, { "id": "Le-Du-J", "name": { "family": "Le Du7", "given": "J." } }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "C." }, "orcid": "0000-0003-1731-0497" }, { "id": "Perlmutter-S", "name": { "family": "Perlmutter", "given": "S." } }, { "id": "Ripoche-P", "name": { "family": "Ripoche", "given": "P." } }, { "id": "Suzuki-Naoyuki", "name": { "family": "Suzuki", "given": "N." } }, { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E. S." } }, { "id": "Zhang-T", "name": { "family": "Zhang", "given": "T." } } ] }, "title": "Type Ia supernovae rates and galaxy clustering from the CFHT supernova legacy survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies; clusters; general; supernovae", "note": "We gratefully acknowledge the CFHT Queued Service Observations\nteam, Olivier Ilbert and Henry McCracken for\nearly access to and correspondence regarding their photometric\nredshift galaxy catalog, Lisbeth Olsen for early access the\noptical cluster catalog, Jon Willis and Dan Maoz for helpful\nconversations, and our anonymous referee for constructive\ncorrespondence. This paper is based on observations obtained\nwith MegaPrime/MegaCam, a joint project of CFHT and\nCEA/DAPNIA, at the CFHT, which is operated by the National\nResearch Council of Canada, the Institut National des Science\nde l'Univers of the Centre National de la Recherche Scientifique\n(CNRS) of France, and the University of Hawaii. This\npaper is also based on spectroscopic observations obtained at\nthe Gemini Observatory which is operated by the Association\nof Universities for Research in Astronomy, Inc., under a cooperative\nagreement with the NSF on behalf of the Gemini\npartnership; the Very Large Telescope at the European Southern\nObservatory in Paranal, Chile; theW. M. Keck Observatory\nwhich is operated as a scientific partnership among the California\nInstitute of Technology, the University of California, and\nthe National Aeronautics and Space Administration; and the\n6.5 m Magellan Telescopes located at Las Campanas Observatory,\nChile. This work is based in part on data products from the\nCanadian Astronomy Data Centre as part of the CFHT Legacy\nSurvey, a collaborative project of NRC and CNRS. This work\nhas been supported by NSERC and the University of Victoria.\nFacilities: CFHT.\n\nPublished - GRAaj08.pdf
", "abstract": "The Canada-France-Hawaii Telescope Supernova Legacy Survey (CFHT SNLS) has created a large homogeneous database of intermediate redshift (0.2 < z < 1.0) type Ia supernovae (SNe Ia). The SNLS team has shown that correlations exist between SN Ia rates, properties, and host galaxy star-formation rates (SFRs). The SNLS SN Ia database has now been combined with a photometric redshift galaxy catalog and an optical galaxy cluster catalog to investigate the possible influence of galaxy clustering on the SN Ia rate, over and above the expected effect due to the dependence of SFR on clustering through the morphology-density relation. We identify three cluster SNe Ia, plus three additional possible cluster SNe Ia, and find the SN Ia rate per unit mass in clusters at intermediate redshifts is consistent with the rate per unit mass in field early-type galaxies and the SN Ia cluster rate from low-redshift cluster targeted surveys. We also find the number of SNe Ia in cluster environments to be within a factor of 2 of expectations from the two-component SN Ia rate model.", "date": "2008-04-04", "date_type": "published", "publication": "Astronomical Journal", "volume": "135", "number": "4", "publisher": "American Astronomical Society", "pagerange": "1343-1349", "id_number": "CaltechAUTHORS:20090515-133448742", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090515-133448742", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Research Council of Canada" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "University of Hawaii" }, { "agency": "NSF" }, { "agency": "European Southern Observatory (ESO)" }, { "agency": "W. M. Keck Observatory" }, { "agency": "Caltech" }, { "agency": "NASA" }, { "agency": "Las Campanas Observatory" }, { "agency": "Canadian Astronomy Data Centre" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "University of Victoria" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-6256/135/4/1343", "primary_object": { "basename": "GRAaj08.pdf", "url": "https://authors.library.caltech.edu/records/dazfr-rqw98/files/GRAaj08.pdf" }, "pub_year": "2008", "author_list": "Graham, M. L.; Pritchet, C. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/8bm2z-6h076", "eprint_id": 14180, "eprint_status": "archive", "datestamp": "2023-08-22 11:30:11", "lastmod": "2023-10-18 16:19:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Bazin-G", "name": { "family": "Bazin", "given": "G." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Halpern-J-P", "name": { "family": "Halpern", "given": "J. P." } }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S. G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } } ] }, "title": "UV/optical detections of candidate tidal disruption events by GALEX and CFHTLS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: g nuclei; ultraviolet: galaxies; X-rays: galaxies", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 August 14; accepted 2007 December 25.\nWe thank our anonymous referee for their insightful comments\nthat helped us improve our paper. We are grateful for the\npublic database of SN candidates produced by the Supernova\nLegacy Survey, which has been very useful for this study. S. G.\nwas supported in part by the Volontariat International-CNES of\nFrance and through Chandra grant G06-7099X issued by the\nChandra X-Ray Observatory, which is operated by the Smithsonian\nAstrophysical Observatory for and on behalf of NASA.\nWe gratefully acknowledge NASA's support for construction,\noperation, and science analysis for the GALEX mission, developed\nin cooperation with Centre National d'Etudes Spatiales of\nFrance and the Korean Ministry of Science and Technology.\nBased on observations obtained with MegaPrime/MegaCam,\na joint project of CFHT and CEA/DAPNIA, at the Canada-\nFrance-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National de Sciences de l'Univers of the Centre National de la\nRecherche Scientifique (CNRS) of France, and the University\nof Hawaii. This work is based in part on data products produced\nat TERAPIX and the Canadian Astronomy Data Centre\nas part of the CFHT Legacy Survey, a collaborative project of\nNRC and CNRS. This paper makes use of photometric redshifts\nproduced jointly by Terapix and the VVDS teams, and\nthe CENCOS interface (http://cencosw.oamp.fr) was used for\ndata retrieval and analyses.\n\nPublished - GEZapj08.pdf
", "abstract": "We present two luminous UV/optical flares from the nuclei of apparently inactive early-type galaxies at z = 0.37 and 0.33 that have the radiative properties of a flare from the tidal disruption of a star. In this paper we report the second candidate tidal disruption event discovery in the UV by the GALEX Deep Imaging Survey and present simultaneous optical light curves from the CFHTLS Deep Imaging Survey for both UV flares. The first few months of the UV/optical light curves are well fitted with the canonical t^(\u22125/3) power-law decay predicted for emission from the fallback of debris from a tidally disrupted star. Chandra ACIS X-ray observations during the flares detect soft X-ray sources with T_(bb) = (2\u20135) \u00d7 10^5 K or \u0393 > 3 and place limits on hard X-ray emission from an underlying AGN down to L_X(2\u201310 keV) \u227e 10^41 ergs s^\u22121. Blackbody fits to the UV/optical spectral energy distributions of the flares indicate peak flare luminosities of \u2273 10^44-10^45 ergs s^\u22121. The temperature, luminosity, and light curves of both flares are in excellent agreement with emission from a tidally disrupted main-sequence star onto a central black hole of several times 10^7 M\u2299. The observed detection rate of our search over ~2.9 deg^2 of GALEX Deep Imaging Survey data spanning from 2003 to 2007 is consistent with tidal disruption rates calculated from dynamical models, and we use these models to make predictions for the detection rates of the next generation of optical synoptic surveys.", "date": "2008-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "676", "number": "2", "publisher": "American Astronomical Society", "pagerange": "944-969", "id_number": "CaltechAUTHORS:20090507-125659445", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090507-125659445", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Chandra X-Ray Observatory", "grant_number": "G06-7099X" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/529008", "primary_object": { "basename": "GEZapj08.pdf", "url": "https://authors.library.caltech.edu/records/8bm2z-6h076/files/GEZapj08.pdf" }, "pub_year": "2008", "author_list": "Gezari, S.; Basa, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/80qqb-jn307", "eprint_id": 16870, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:21", "lastmod": "2023-10-19 22:37:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David A." }, "orcid": "0000-0002-8528-7340" }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Meurer-G-R", "name": { "family": "Meurer", "given": "Gerhardt" }, "orcid": "0000-0002-0163-2507" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Ferguson-A-M-N", "name": { "family": "Ferguson", "given": "Annette M. N." } }, { "id": "Mu\u0144oz-Mateos-J-C", "name": { "family": "Mu\u0144oz-Mateos", "given": "Juan Carlos" } }, { "id": "Madsen-G-J", "name": { "family": "Madsen", "given": "Greg J." } }, { "id": "Hameed-S", "name": { "family": "Hameed", "given": "Salman" } }, { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2007 April 30; accepted for publication 2007 September 11. \n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003April.We gratefully acknowledgeNASA's\nsupport for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. A. G. d. P. is financed by the MAGPOP EU Marie Curie Research Training Network and partially by the Spanish Programma Nacional de Astronom\u0131\u00b4a y Astrof\u0131\u00b4sica under grants AYA2003-01676 and AYA2006-02358.\nThis research has made use of the NASA/IPAC Extragalactic\nDatabase (NED). We acknowledge the use of the HyperLeda\ndatabase ( http:// leda.univ-lyon1.fr). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under US Government grant NAGW-2166. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. Some images presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities\nfor Research in Astronomy, Inc., under NASA contract NAS5-\n26555. Support for MAST for non-HST data is provided by the\nNASA Office of Space Science via grant NAG5-7584 and by\nother grants and contracts. This research has made use of the NASA/IPAC Infrared Science Archive. This publication makes use of data products from the Two Micron All Sky Survey.\nFacilities: GALEX, CTIO:2MASS, FLWO:2MASS, Sloan, PO:1.2m, UKST\n\nPublished - THIapjss07a.pdf
", "abstract": "We have initiated a search for extended ultraviolet disk (XUV-disk) galaxies in the local universe. Here we compare GALEX UV and visible-NIR images of 189 nearby (D < 40 Mpc) S0-Sm galaxies included in the GALEX Atlas of Nearby Galaxies and present the first catalog of XUV-disk galaxies. We find that XUV-disk galaxies are surprisingly common but have varied relative (UV/optical) extent and morphology. Type 1 objects (\u227320% incidence) have structured, UV-bright/optically faint emission features in the outer disk, beyond the traditional star formation threshold. Type 2 XUV-disk galaxies (~10% incidence) exhibit an exceptionally large, UV-bright/optically low surface brightness (LSB) zone having blue UV\u2013K_s outside the effective extent of the inner, older stellar population, but not reaching extreme galactocentric distance. If the activity occurring in XUV-disks is episodic, a higher fraction of present-day spirals could be influenced by such outer disk star formation. Type 1 disks are associated with spirals of all types, whereas Type 2 XUV-disks are predominantly found in late-type spirals. Type 2 XUV-disks are forming stars quickly enough to double their (currently low) stellar mass in the next Gyr (assuming a constant star formation rate). XUV-disk galaxies of both types are systematically more gas-rich than the general galaxy population. Minor external perturbation may stimulate XUV-disk incidence, at least for Type 1 objects. XUV-disks are the most actively evolving galaxies growing via inside-out disk formation in the current epoch, and may constitute a segment of the galaxy population experiencing significant, continued gas accretion from the intergalactic medium or neighboring objects.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "538-571", "id_number": "CaltechAUTHORS:20091203-140520449", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091203-140520449", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/523853", "primary_object": { "basename": "THIapjss07a.pdf", "url": "https://authors.library.caltech.edu/records/80qqb-jn307/files/THIapjss07a.pdf" }, "pub_year": "2007", "author_list": "Thilker, David A.; Bianchi, Luciana; et el." }, { "id": "https://authors.library.caltech.edu/records/4drye-pfq50", "eprint_id": 17451, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:40", "lastmod": "2023-10-19 23:54:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S\u00e9bastien" } }, { "id": "Blaizot-J", "name": { "family": "Blaizot", "given": "J\u00e9r\u00e9my" } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "St\u00e9phane" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Laget-M", "name": { "family": "Laget", "given": "Michel" } }, { "id": "Viton-M", "name": { "family": "Viton", "given": "Maurice" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" } ] }, "title": "Clustering Properties of Rest-Frame UV-Selected Galaxies. I. the Correlation Length Derived from GALEX Data in the Local Universe", "ispublished": "pub", "full_text_status": "public", "keywords": "stars : formation; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 August 22; accepted 2007 October 16.\nIt is with great pleasure that we thank Jean-Michel Deharveng\nfor support and discussions. GALEX (Galaxy Evolution Explorer)\nis a NASA Small Explorer, launched in 2003 April. We gratefully\nacknowledge NASA's support for construction, operation, and\nscience analysis for the GALEX mission, developed in cooperation\nwith the Centre National d'Etudes Spatiales of France and\nthe Korean Ministry of Science and Technology.\n\nPublished - MILapjss07.pdf
", "abstract": "We present the first measurements of the angular correlation function of galaxies selected in the far (1530 \u00c5) and near (2310 \u00c5) ultraviolet from the GALEX survey fields overlapping SDSS DR5 in low Galactic extinction regions. The area used covers 120 deg^2 (GALEX Medium Imaging Survey) down to magnitude AB = 22, yielding a total of 100,000 galaxies. The mean correlation length is ~3.7 \u00b1 0.6 Mpc, and no significant trend is seen for this value as a function of the limiting apparent magnitude or between the GALEX bands. This estimate is close to that found from samples of blue galaxies in the local universe selected in the visible and similar to that derived at z \u2243 3 for LBGs with similar rest frame selection criteria. This result supports models that predict antibiasing of star-forming galaxies at low redshift and brings an additional clue to the downsizing of star formation at z < 1.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "494-502", "id_number": "CaltechAUTHORS:20100211-100214164", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-100214164", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/524658", "primary_object": { "basename": "MILapjss07.pdf", "url": "https://authors.library.caltech.edu/records/4drye-pfq50/files/MILapjss07.pdf" }, "pub_year": "2007", "author_list": "Milliard, Bruno; Heinis, S\u00e9bastien; et el." }, { "id": "https://authors.library.caltech.edu/records/2tyef-r7q04", "eprint_id": 20103, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:52", "lastmod": "2023-10-20 22:13:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S\u00e9bastien" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" } ] }, "title": "Clustering Properties of Rest-Frame UV-Selected Galaxies. II. Migration of Star Formation Sites with Cosmic Time from GALEX and CFHTLS", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: formation; ultraviolet: galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 August 22; accepted 2007 May 31.\n\nWe thank Christian Marinoni for stimulating discussions. GALEX\n(Galaxy Evolution Explorer) is a NASA Small Explorer, launched in\n2003 April. We gratefully acknowledge NASA's support for construction,\noperation, and science analysis for the GALEX mission, developed\nin cooperation with the Centre National d'Etudes Spatiales\nof France and the Korean Ministry of Science and Technology.\nThis study is also based on observations obtained with\nMegaPrime/MegaCam, a joint project of the Canada-France-\nHawaii Telescope (CFHT) and CEA/DAPNIA, at CFHT, which\nis operated by the National Research Council (NRC) of Canada,\nthe Institut National des Science de l'Univers of the Centre National\nde la Recherche Scientifique (CNRS) of France, and the\nUniversity of Hawaii. This work is based in part on data products\nproduced at TERAPIX and the Canadian Astronomy Data Centre\nas part of the CFHT Legacy Survey, a collaborative project of\nNRC and CNRS.\n\nPublished - HEIapjss07.pdf
", "abstract": "We analyze the clustering properties of ultraviolet-selected galaxies by using GALEX-SDSS data at z < 0.6 and CFHTLS deep u' imaging at z ~ 1. These data sets provide a unique basis at z \u2264 1 which can be directly compared with high-redshift samples built with similar selection criteria. We discuss the dependence of the correlation function parameters (r_0 and \u03b4) on the ultraviolet luminosity, as well as the linear bias evolution. We find that the bias parameter shows a gradual decline from high (b_8 \u2273 2) to low redshift (b_8 \u2243 0.79_(\u22120.08)^(+0.1)). When accounting for the fraction of the star formation activity enclosed in the different samples, our results suggest that the bulk of star formation migrated from high-mass dark matter halos at z > 2 (10^(12) M_\u2299 \u2264 M_(min) \u2264 10^(13) M_\u2299, located in high-density regions) to less massive halos at low redshift (M_(min) \u2264 10^(12) M_\u2299, located in low-density regions). This result extends the \"downsizing\" picture (shift of the star formation activity from high stellar mass systems at high z to low stellar mass at low z) to the dark matter distribution.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "503-511", "id_number": "CaltechAUTHORS:20100923-113018914", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100923-113018914", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/520580", "primary_object": { "basename": "HEIapjss07.pdf", "url": "https://authors.library.caltech.edu/records/2tyef-r7q04/files/HEIapjss07.pdf" }, "pub_year": "2007", "author_list": "Heinis, S\u00e9bastien; Wyder, Ted K.; et el." }, { "id": "https://authors.library.caltech.edu/records/vg2dj-krq39", "eprint_id": 16865, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:11", "lastmod": "2023-10-19 22:37:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Treyer-M", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Johnson-B", "name": { "family": "Johnson", "given": "Ben" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Wyder-T", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Extinction-corrected Star Formation Rates Empirically Derived from Ultraviolet-Optical Colors", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; surveys; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2007 April 24; accepted for publication 2007 July 19.\n\nThe authors thank their anonymous referee, whose many comments greatly improved this paper. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for its construction, operation, and science analysis, as well as the cooperation of the French Centre National d'Etudes Spatiales and the Korean Ministry of Science and Technology.\n\nPublished - TREapjss07.pdf
", "abstract": "Using a sample of galaxies from the Sloan Digital Sky Survey spectroscopic catalog with measured star formation rates (SFRs) and ultraviolet (UV) photometry from the GALEX Medium Imaging Survey, we derived empirical linear correlations between the SFR to UV luminosity ratio and the UV\u2013optical colors of blue-sequence galaxies. The relations provide a simple prescription to correct UV data for dust attenuation that best reconciles the SFRs derived from UV and emission-line data. The method breaks down for the red-sequence population as well as for very blue galaxies such as the local \"supercompact\" UV luminous galaxies and the majority of high-redshift Lyman break galaxies, which form a low-attenuation sequence of their own.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "256-266", "id_number": "CaltechAUTHORS:20091203-110549888", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091203-110549888", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/521794", "primary_object": { "basename": "TREapjss07.pdf", "url": "https://authors.library.caltech.edu/records/vg2dj-krq39/files/TREapjss07.pdf" }, "pub_year": "2007", "author_list": "Treyer, Marie; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/6h0f8-mtg72", "eprint_id": 18050, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:14", "lastmod": "2023-10-20 15:32:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "Jean-Michel" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "GALEX UV Color Relations for Nearby Early-Type Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: photometry; galaxies: stellar content; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 May 4; accepted 2006 July 20.\n\nWe wish to acknowledge Jakob Walcher for kindly extracting\nfor us useful data from stochastic realizations of star formation\nmodels. GALEX (Galaxy Evolution Explorer) is a NASA Small\nExplorer, launched in 2003 April. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with the\nCentre National d'Etudes Spatiales of France and the Korean\nMinistry of Science and Technology. The grating, window, and\naspheric corrector were supplied by France. We acknowledge\nthe dedicated team of engineers, technicians, and administrative\nstaff from JPL/Caltech; Orbital Sciences Corporation; University\nof California, Berkeley; Laboratory Astrophysique Marseille;\nand the other institutions who made this mission possible. This\nwork was partly supported by grant R01-2006-000-10716-0 (SKY)\nfrom the Basic Research Program of the Korea Science and Engineering\nFoundation. A. G. d. P. is financed by the MAGPOP EU\nMarie Curie Research Training Network.\n\nFacilities: GALEX\n\nPublished - DONapjss07.pdf
", "abstract": "We use GALEX/optical photometry to construct color-color relationships for early-type galaxies sorted by morphological type. We have matched objects in the GALEX GR1 public release and the first IR1.1 internal release, with the RC3 early-type galaxies having a morphological type -5.5 \u2264 T < \u2212 1.5, with mean error on T < 1.5 and mean error on (B \u2212 V)_T < 0.05. After visual inspection of each match, we are left with 130 galaxies with reliable GALEX pipeline photometry in the far-UV and near-UV bands. This sample is divided into ellipticals (-5.5 \u2264 T < \u2212 3.5) and lenticulars (-3.5 \u2264 T < \u2212 1.5). After correction for Galactic extinction, the color-color diagrams FUV \u2212 NUV versus (B \u2212 V)_(Tc) are plotted for the two subsamples. We find a tight anticorrelation between the FUV \u2212 NUV and (B \u2212 V)_(Tc) colors for ellipticals, with the UV color getting bluer when the (B \u2212 V)_(Tc) gets redder. This relationship very likely is an extension of the color-metallicity relationship in the GALEX NUV band. We suspect that the main source of the correlation is metal line blanketing in the NUV band. The FUV \u2212 NUV versus B \u2212 V correlation has larger scatter for lenticular galaxies; we speculate that this reflects the presence of low-level star formation. If the latter objects (i.e., those that are blue both in FUV \u2212 NUV and in B \u2212 V) are interpreted as harboring recent star formation activity, this would be the case for a few percent (~4%) of ellipticals and ~15% of lenticulars; this would mean about 10% of early-type galaxies have residual star formation in our full sample of 130 early-type galaxies. We also plot FUV \u2212 NUV versus the Mg_2 index and central velocity dispersion. We find a tight anticorrelation between FUV \u2212 NUV and the Mg_2 index; we suspect that this reflects blanketing in the NUV band being correlated with overall metallicity. We find a marginal anticorrelation of FUV \u2212 V_T with Mg_2 for elliptical galaxies.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "597-606", "id_number": "CaltechAUTHORS:20100422-120941446", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100422-120941446", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2006-000-10716-0" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516643", "primary_object": { "basename": "DONapjss07.pdf", "url": "https://authors.library.caltech.edu/records/6h0f8-mtg72/files/DONapjss07.pdf" }, "pub_year": "2007", "author_list": "Donas, Jos\u00e9; Deharveng, Jean-Michel; et el." }, { "id": "https://authors.library.caltech.edu/records/b52a4-nt324", "eprint_id": 16729, "eprint_status": "archive", "datestamp": "2023-08-22 10:33:50", "lastmod": "2023-10-19 22:30:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. Kevin" }, "orcid": "0000-0002-1588-6700" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David" }, "orcid": "0000-0003-4401-0430" }, { "id": "Buat-V", "name": { "family": "Buat", "given": "Veronique" } }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "Michael" } }, { "id": "Babbedge-T", "name": { "family": "Babbedge", "given": "Thomas" } }, { "id": "Iglesias-P\u00e1ramo-J", "name": { "family": "Iglesias-P\u00e1ramo", "given": "Jorge" } }, { "id": "Takeuchi-Tsutomu-T", "name": { "family": "Takeuchi", "given": "Tsutomu T." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "Fan" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Gonzalez-Solares-E", "name": { "family": "Gonzalez-Solares", "given": "Eduardo" } }, { "id": "Lonsdale-C-J", "name": { "family": "Lonsdale", "given": "Carol" }, "orcid": "0000-0003-0898-406X" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Smith-Gene", "name": { "family": "Smith", "given": "Gene" } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "IR and UV Galaxies at z = 0.6: Evolution of Dust Attenuation and Stellar Mass as Revealed by SWIRE and GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: active; galaxies: evolution; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2006 April 10; accepted 2006 December 4.\n\nGALEX (Galaxy Evolution Explorer ) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with the\nCentre National d'Etudes Spatiales of France and the Korean Ministry\nof Science and Technology. Support for this work, part of the\nSpitzer Space Telescope Legacy Science Program, was provided\nby NASA through an award issued by JPL under NASA contract\n1407. This publication makes use of data products from the Two\nMicron All Sky Survey, which is a joint project of the University\nof Massachusetts and the Infrared Processing and Analysis\nCenter/California Institute of Technology, funded by NASA and\nNSF.\n\nPublished - XUCapjss07.pdf
", "abstract": "We study dust attenuation and stellar mass of z ~ 0.6 star-forming galaxies using new SWIRE observations in IR and GALEX observations in UV. Two samples are selected from the SWIRE and GALEX source catalogs in the SWIRE/GALEX field ELAIS-N1-00 (\u03a9 = 0.8 deg^2). The UV-selected sample has 600 galaxies with photometric redshift (hereafter photo-z) 0.5 \u2264 z \u2264 0.7 and NUV \u2264 23.5 (corresponding to L_(FUV) \u2265 10^(9.6) L_\u2609). The IR-selected sample contains 430 galaxies with f_(24 \u03bcm) \u2265 0.2 mJy (L_(dust) \u2265 10^(10.8) L_\u2609) in the same photo-z range. It is found that the mean L_(dust)/L_(FUV) ratios of the z = 0.6 UV galaxies are consistent with that of their z = 0 counterparts of the same L_(FUV). For IR galaxies, the mean L_(dust)/L_(FUV) ratios of the z = 0.6 LIRGs (L_(dust) ~ 10^(11) L_\u2609) are about a factor of 2 lower than local LIRGs, whereas z = 0.6 ULIRGs (L_(dust) ~ 10^(12) L_\u2609) have the same mean L_(dust)/L_(FUV) ratios as their local counterparts. This is consistent with the hypothesis that the dominant component of LIRG population has changed from large, gas-rich spirals at z > 0.5 to major mergers at z = 0. The stellar mass of z = 0.6 UV galaxies of L_(FUV) \u2264 10^(10.2) L_\u2609 is about a factor of 2 less than their local counterparts of the same luminosity, indicating growth of these galaxies. The mass of z = 0.6 UV luminous galaxies (UVLGs: L_(FUV) > 10^(10.2) L_\u2609) and IR-selected galaxies, which are nearly exclusively LIRGs and ULIRGs, is the same as their local counterparts.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "432-440", "id_number": "CaltechAUTHORS:20091117-111643880", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-111643880", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516641", "primary_object": { "basename": "XUCapjss07.pdf", "url": "https://authors.library.caltech.edu/records/b52a4-nt324/files/XUCapjss07.pdf" }, "pub_year": "2007", "author_list": "Xu, C. Kevin; Shupe, David; et el." }, { "id": "https://authors.library.caltech.edu/records/0ddag-5k140", "eprint_id": 17457, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:45", "lastmod": "2023-10-19 23:54:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mallery-R-P", "name": { "family": "Mallery", "given": "Ryan P." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung" } } ] }, "title": "Keck DEIMOS Spectroscopy of a GALEX UV-Selected Sample from the Medium Imaging Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : active; galaxies : high-redshift; galaxies : starburst; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 January 25; accepted 2006 July 25.\nGALEX is a NASA Small Explorer, launched in 2003 April.\nWe gratefully acknowledge NASA's support for construction,\noperation, and science analysis for the GALEX mission, developed\nin cooperation with the Centre National d'Etudes Spatiales\nof France and the Korean Ministry of Science and Technology.\nThe authors wish to recognize and acknowledge the very significant\ncultural role and reverence that the summit of Mauna\nKea has always had within the indigenous Hawaiian community.\nWe are most fortunate to have the opportunity to conduct observations\nfrom this mountain. The analysis pipeline used to\nreduce the DEIMOS data was developed at University of California,\nBerkeley, with support from NSF grant AST 00-71048.\nThe authors thank an anonymous referee for extremely helpful\ncomments.\nFacilities: GALEX, Keck:II.\n\nPublished - MALapjss07a.pdf
", "abstract": "We report results from a pilot program to obtain spectroscopy for objects detected in the Galaxy Evolution Explorer (GALEX) Medium Imaging Survey (MIS). Our study examines the properties of galaxies detected by GALEX fainter than the Sloan Digital Sky Survey (SDSS) spectroscopic survey. This is the first study to extend the techniques of Salim and coworkers to estimate stellar masses, star formation rates (SFRs), and the b (star formation history) parameter for star-forming galaxies out to z ~ 0.7. We obtain redshifts for 50 GALEX MIS sources reaching NUV = 23.9 (AB mag) having counterparts in the SDSS Data Release 4 (DR4). Of our sample, 43 are star-forming galaxies with z < 0.7, 3 have emission-line ratios indicative of active galactic nuclei with z < 0.7, and 4 objects with z > 1 are QSOs, 3 of which are not previously cataloged. We compare our sample to a much larger sample of ~50,000 matched GALEX/SDSS galaxies with SDSS spectroscopy; while our survey is shallow, the optical counterparts to our sources reach ~3 mag fainter in SDSS r than the SDSS spectroscopic sample. We use emission-line diagnostics for the galaxies to determine that the sample contains mostly star-forming galaxies. The galaxies in the sample populate the blue sequence in the NUV \u2212 r versus Mr color-magnitude diagram. The derived stellar masses of the galaxies range from 10^8 to 10^(11) M_\u2299, and derived SFRs are between 10^(\u22121) and 10^2 M_\u2299 yr^(\u22121). Our sample has SFRs, luminosities, and velocity dispersions that are similar to the samples of faint compact blue galaxies studied previously in the same redshift range by Koo and collaborators, Guzm\u00e1n and collaborators, and Phillips and collaborators. However, our sample is ~2 mag fainter in surface brightness than the compact blue galaxies. We find that the star formation histories for a majority of the galaxies are consistent with a recent starburst within the last 100 Myr.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "471-481", "id_number": "CaltechAUTHORS:20100211-112458004", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-112458004", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 00-71048" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516638", "primary_object": { "basename": "MALapjss07a.pdf", "url": "https://authors.library.caltech.edu/records/0ddag-5k140/files/MALapjss07a.pdf" }, "pub_year": "2007", "author_list": "Mallery, Ryan P.; Rich, R. Michael; et el." }, { "id": "https://authors.library.caltech.edu/records/c9yh3-b1y96", "eprint_id": 17464, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:50", "lastmod": "2023-10-19 23:55:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mallery-R-P", "name": { "family": "Mallery", "given": "Ryan P." } }, { "id": "Kewley-L-J", "name": { "family": "Kewley", "given": "Lisa J." }, "orcid": "0000-0001-8152-3943" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } }, { "id": "Tremonti-C-A", "name": { "family": "Tremonti", "given": "Christy" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung" } } ] }, "title": "Nitrogen Production in Starburst Galaxies Detected by GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : abundances; galaxies : fundamental parameters; galaxies : starburst; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 October 13; accepted 2007 April 5.\nGALEX is a NASA Small Explorer, launched in 2003 April.\nWe gratefully acknowledge NASA's support for construction, operation,\nand science analysis for the GALEX mission, developed in\ncooperation with the CNES of France and the Korean Ministry of\nScience and Technology. Funding for the creation and distribution\nof the SDSS Archive has been provided by the Alfred P. Sloan\nFoundation, the Participating Institutions, NASA, NSF, DoE,\nMonbukagakusho, and the Max Planck Society.\nFacilities: GALEX.\n\nPublished - MALapjss07b.pdf
", "abstract": "We investigate the production of nitrogen in star-forming galaxies with ultraviolet (UV) radiation detected by the Galaxy Evolution Explorer Satellite (GALEX). We use a sample of 8745 GALEX emission-line galaxies matched to the Sloan Digital Sky Survey (SDSS) spectroscopic sample. We derive both gas-phase oxygen and nitrogen abundances for the sample and apply stellar population synthesis models to derive stellar masses and star formation histories of the galaxies. We compare oxygen abundances derived using three different diagnostics. We derive the specific star formation rates of the galaxies by modeling the seven-band GALEX+SDSS photometry. We find that galaxies that have log (SFR/M_*) \u2273 \u2212 10.0 typically have values of log (N/O) ~ 0.05 dex less than galaxies with log (SFR/M_*) \u227e \u2212 10.0 and similar oxygen abundances.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "482-493", "id_number": "CaltechAUTHORS:20100212-094447213", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100212-094447213", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/518833", "primary_object": { "basename": "MALapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/c9yh3-b1y96/files/MALapjss07b.pdf" }, "pub_year": "2007", "author_list": "Mallery, Ryan P.; Kewley, Lisa J.; et el." }, { "id": "https://authors.library.caltech.edu/records/j5awf-89828", "eprint_id": 17404, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:36", "lastmod": "2023-10-19 23:51:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kauffmann-G", "name": { "family": "Kauffmann", "given": "Guinevere" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "Stephane" } }, { "id": "Hoopes-C-G", "name": { "family": "Hoopes", "given": "Charles G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick F." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Ongoing Formation of Bulges and Black Holes in the Local Universe: New Insights from GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : active; galaxies : bulges; galaxies : elliptical and lenticular, cD; galaxies : formation", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 July 18; accepted 2006 September 13.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with the Centre\nNational d'Etudes Spatiales (CNES) of France and the Korean\nMinistry of Science and Technology. Funding for the creation\nand distribution of the SDSS Archive has been provided by the\nAlfred P. Sloan Foundation, the Participating Institutions, the\nNational Aeronautics and Space Administration, the National\nScience Foundation, the US Department of Energy, the Japanese\nMonbukagakusho, and the Max Planck Society. The SDSS Web\nsite is http://www.sdss.org. The SDSS is managed by the Astrophysical\nResearch Consortium for the Participating Institutions.\nThe Participating Institutions are the University of Chicago,\nFermilab, the Institute for Advanced Study, the Japan Participation\nGroup, the Johns Hopkins University, the Korean Scientist\nGroup, Los Alamos National Laboratory, the Max Planck\nInstitute for Astronomy, the Max Planck Institute for Astrophysics,\nNew Mexico State University, the University of Pittsburgh,\nthe University of Portsmouth, Princeton University, the US Naval\nObservatory, and the University of Washington.\n\nPublished - KAUapjss07.pdf
", "abstract": "We analyze a volume-limited sample of massive bulge-dominated galaxies with data from both the Sloan Digital Sky Survey and the Galaxy Evolution Explorer (GALEX) satellite. The galaxies have central velocity dispersions greater than 100 km s^(\u22121) and stellar surface mass densities that lie above the value where galaxies transition from actively star-forming to passive systems. The sample is limited to redshifts 0.03 < z < 0.07. At these distances, the SDSS spectra sample the light from the bulge-dominated central regions of the galaxies. The GALEX NUV data provide high sensitivity to low rates of global star formation in these systems. Our sample of bulge-dominated galaxies exhibits a much larger dispersion in NUV \u2212 r color than in optical g \u2212 r color. The dispersion increases for galaxies with smaller central velocity dispersions, and nearly all of the galaxies with bluer NUV \u2212 r colors are active galactic nuclei (AGNs). Both GALEX images and SDSS color profiles demonstrate that the excess UV light is nearly always associated with an extended disk. When comparing fiber-based estimates of stellar age to global ones, we find that galaxies with red outer regions almost never have a young bulge or a strong AGN. Galaxies with blue outer regions have bulges and black holes that span a wide range in age and accretion rate. Galaxies with young bulges and strongly accreting black holes almost always have blue outer disks. The black hole growth rate correlates much more strongly with the age of the stars in the bulge than in the disk. Our suggested scenario is one in which the source of gas that builds the bulge and black hole is a low-mass reservoir of cold gas in the disk. The presence of this gas is a necessary but not sufficient condition for bulge and black hole growth. Some mechanism must transport this gas inward in a time variable way. The disk gas itself is likely to be the result of the accretion of gas from an external source. As the gas in the disk is converted into stars, galaxies will turn red, but further inflow can bring them back into the blue NUV \u2212 r sequence.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "357-376", "id_number": "CaltechAUTHORS:20100205-135117202", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100205-135117202", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516647", "primary_object": { "basename": "KAUapjss07.pdf", "url": "https://authors.library.caltech.edu/records/j5awf-89828/files/KAUapjss07.pdf" }, "pub_year": "2007", "author_list": "Kauffmann, Guinevere; Heckman, Timothy M.; et el." }, { "id": "https://authors.library.caltech.edu/records/sw8er-eaf44", "eprint_id": 18044, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:09", "lastmod": "2023-10-20 15:31:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V\u00e9ronique" } }, { "id": "Cortese-L", "name": { "family": "Cortese", "given": "Luca" }, "orcid": "0000-0002-7422-9823" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "Denis" } }, { "id": "Mu\u0144oz-Mateos-J-C", "name": { "family": "Mu\u0144oz-Mateos", "given": "Juan Carlos" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Radial Variation of Attenuation and Star Formation in the Largest Late-Type Disks Observed with GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: spiral; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 April 20; accepted 2006 July 28.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'E\u00b4 tudes Spatiales of France and the Korean Ministry of\nScience and Technology. A. G. d. P. is partially financed by the\nSpanish Programa Nacional de Astronom\u0131\u00b4a y Astrof \u0131\u00b4sica under\ngrant AYA2003-01676. We also thank the MAGPOP network\nfor its support, and the referee for very constructive comments.\nFacilities: GALEX\n\nPublished - BOIapjss07.pdf
", "abstract": "For a sample of 43 nearby, late-type galaxies, we have investigated the radial variation of both the current star formation rate and the dust-induced UV light attenuation. To do this we have cross-correlated IRAS images and GALEX observations for each of these galaxies and compiled observations of the gas (CO and H I) and metal-abundance gradients found in the literature. We find that attenuation correlates with metallicity. We then use the UV profiles, corrected for attenuation, to study several variants of the Schmidt law and conclude that our results are compatible with a simple law similar to the one of Kennicutt extending smoothly to lower surface densities, but with considerable scatter. We do not detect an abrupt break in the UV light at the threshold radius derived from H\u03b1 data (at which the H\u03b1 profile shows a break and beyond which only a few H II regions are usually found). We interpret the H\u03b1 sudden break not as a change in the star formation regime (as often suggested), but as the vanishingly small number of ionizing stars corresponding to low levels of star formation.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "524-537", "id_number": "CaltechAUTHORS:20100421-122451071", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100421-122451071", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Programa Nacional de Astronom\u00eda y Astrof\u00edsica", "grant_number": "AYA2003-01676" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516642", "primary_object": { "basename": "BOIapjss07.pdf", "url": "https://authors.library.caltech.edu/records/sw8er-eaf44/files/BOIapjss07.pdf" }, "pub_year": "2007", "author_list": "Boissier, Samuel; Gil de Paz, Armando; et el." }, { "id": "https://authors.library.caltech.edu/records/cnv2r-r7224", "eprint_id": 18086, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:33", "lastmod": "2023-10-20 15:34:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Rodriguez-Merino-L", "name": { "family": "Rodriguez-Merino", "given": "Lino" } }, { "id": "Viton-M", "name": { "family": "Viton", "given": "Maurice" } }, { "id": "Laget-M", "name": { "family": "Laget", "given": "Michel" } }, { "id": "Efremova-B-V", "name": { "family": "Efremova", "given": "Boryana" } }, { "id": "Herald-J-E", "name": { "family": "Herald", "given": "James" } }, { "id": "Conti-A", "name": { "family": "Conti", "given": "Alberto" } }, { "id": "Shiao-Bernie", "name": { "family": "Shiao", "given": "Bernie" } }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Thakar-A-R", "name": { "family": "Thakar", "given": "A." } }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Rey-Soo-Chang", "name": { "family": "Rey", "given": "Soo-Chang" } }, { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David" }, "orcid": "0000-0002-8528-7340" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Statistical Properties of the GALEX-SDSS Matched Source Catalogs, and Classification of the UV Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: stellar content; quasars: general; stars: statistics; surveys; ultraviolet: stars; white dwarfs", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 July 21; accepted 2006 October 26.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis of\nthe GALEX mission, developed in cooperation with the Centre\nNational d'Etudes Spatiales of France and the Korean Ministry\nof Science and Technology. We are grateful to John Hutchings,\nWei Zheng, and Gordon Richards for discussions about QSO\nissues and clarifications about the QSO SDSS catalogs and templates, to Alessandro Bressan for providing the yet unpublished SSP models and for extremely useful discussions, and (with Olga Vega) for assistance in calculations of the galaxy template, to Paula Szkody and Knox Long for illuminating discussions about CVs and for the CV templates.\nFacilities: GALEX, Sloan\n\nPublished - BIAapjss07.pdf
", "abstract": "We use the Galaxy Evolution Explorer (GALEX) Medium and All-Sky Imaging Survey (MIS and AIS) data from the first public data release (GR1), matched to the Sloan Digital Sky Survey (SDSS) DR3 catalog, to perform source classification. The GALEX surveys provide photometry in far- and near-UV bands and the SDSS in five optical bands (u, g, r, i, z). The GR1/DR3 overlapping areas are 363 (86) deg^2 for the GALEX AIS (MIS), for sources within the 0.5\u00b0 central area of the GALEX fields. Our sample covers mostly |b| > 30\u00b0 Galactic latitudes. We present statistical properties of the GALEX-SDSS matched sources catalog, containing >2 \u00d7 10^6 objects detected in at least one UV band. We classify the matched sources by comparing the seven-band photometry to model colors constructed for different classes of astrophysical objects. For sources with photometric errors <0.3 mag, the corresponding typical AB-magnitude limits are m_(FUV) ~ 21.5, m_(NUV) ~ 22.5 for AIS, and m_(FUV) ~ 24, m_(NUV) ~ 24.5 for MIS. At AIS depth, the number of Galactic and extragalactic objects are comparable, but the latter predominate in the MIS. On the basis of our stellar models, we estimate the GALEX surveys detect hot white dwarfs throughout the Milky Way halo (down to a radius of 0.04 R_\u2609 at MIS depth), providing an unprecedented improvement in the Galactic WD census. Their observed surface density is consistent with Milky Way model predictions. We also select low-redshift QSO candidates, extending the known QSO samples to lower magnitudes, and providing z \u2248 1 candidates for detailed z \u2248 1 follow-up investigations. SDSS optical spectra available for a large subsample confirm the classification for the photometrically selected candidates with 97% purity for single hot stars, \u224845% (AIS) or 31% (MIS) for binaries containing a hot star and a cooler companion, and about 85% for QSOs.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "659-672", "id_number": "CaltechAUTHORS:20100430-103413888", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100430-103413888", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516648", "primary_object": { "basename": "BIAapjss07.pdf", "url": "https://authors.library.caltech.edu/records/cnv2r-r7224/files/BIAapjss07.pdf" }, "pub_year": "2007", "author_list": "Bianchi, Luciana; Rodriguez-Merino, Lino; et el." }, { "id": "https://authors.library.caltech.edu/records/ghrgp-29r85", "eprint_id": 16739, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:00", "lastmod": "2023-10-19 22:31:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Arnouts-S", "name": { "family": "Arnouts", "given": "Stephane" } }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "The Calibration and Data Products of GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "space vehicles; surveys; telescopes; ultraviolet : general", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 December 8; accepted 2007 May 16.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology.\nFacilities: GALEX\n\nPublished - MORapjss07.pdf
", "abstract": "We describe the calibration status and data products pertaining to the GR2 and GR3 data releases of the Galaxy Evolution Explorer (GALEX). These releases have identical pipeline calibrations that are significantly improved over the GR1 data release. GALEX continues to survey the sky in the far-ultraviolet (FUV, ~154 nm) and near-ultraviolet (NUV, ~232 nm) bands, providing simultaneous imaging with a pair of photon-counting, microchannel plate, delay line readout detectors. These 1.25\u00b0 field of view detectors are well suited to ultraviolet observations because of their excellent red rejection and negligible background. A dithered mode of observing and photon list output pose complex requirements on the data processing pipeline, entangling detector calibrations, and aspect reconstruction algorithms. Recent improvements have achieved photometric repeatability of 0.05 and 0.03 m_(AB) in the FUV and NUV, respectively. We have detected a long-term drift of order 1% FUV and 6% NUV over the mission. Astrometric precision is of order 0.5\" rms in both bands. In this paper we provide the GALEX user with a broad overview of the calibration issues likely to be confronted in the current release. Improvements are likely as the GALEX mission continues into an extended phase with a healthy instrument, no consumables, and increased opportunities for guest investigations.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "682-697", "id_number": "CaltechAUTHORS:20091118-092117490", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091118-092117490", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/520512", "primary_object": { "basename": "MORapjss07.pdf", "url": "https://authors.library.caltech.edu/records/ghrgp-29r85/files/MORapjss07.pdf" }, "pub_year": "2007", "author_list": "Morrissey, Patrick; Conrow, Tim; et el." }, { "id": "https://authors.library.caltech.edu/records/fh896-54351", "eprint_id": 16749, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:05", "lastmod": "2023-10-19 22:31:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Wheatley-J-M", "name": { "family": "Wheatley", "given": "Jonathan M." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Browne-S-E", "name": { "family": "Browne", "given": "Stanley E." } }, { "id": "West-A-A", "name": { "family": "West", "given": "Andrew A." } }, { "id": "Siegmund-O-H-W", "name": { "family": "Siegmund", "given": "Oswald H. W." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } } ] }, "title": "The Detection of M Dwarf UV Flare Events in the GALEX Data Archives", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: variables: other; ultraviolet: stars", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2006 March 24; accepted for publication 2006 May 12.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003April.We gratefully acknowledgeNASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology.We acknowledge the dedicated team of\nengineers, technicians, and administrative staff fromJPL/Caltech,\nOrbital Sciences Corporation, University of California, Berkeley,\nLaboratoire d'Astrophysique de Marseille, and the other institutions\nwho made this mission possible. Financial support for this\nresearch was provided by the NASA GALEX Guest Investigator\nscience program. This publicationmakes use of data products from\nthe SIMBAD database, operated at CDS, Strasbourg, France.\nFacilities: GALEX\n\nPublished - WELapjss07.pdf
", "abstract": "We present the preliminary results from implementing a new software tool that enables inspection of time-tagged photon data for the astronomical sources contained within individual GALEX ultraviolet (UV) images of the sky. We have inspected the photon data contained within 1802 GALEX images to reveal rapid, short-term (\u2272500 s) UV source variability in the form of stellar \"flares.\" The mean associated change in near-UV (NUV) magnitude due to this flaring activity is 2.7 \u00b1 0.3 mag. A list of 49 new UV variable star candidates is presented, together with their associated Sloan Digital Sky Survey (SDSS) photometric magnitudes. From these data we can associate the main source of these UV flare events with magnetic activity on M dwarf stars. Photometric parallaxes have been determined for 32 of these sources, placing them at distances ranging from approximately 25 to 1000 pc. The average UV flare energy for these flare events is 2.5 \u00d7 10^(30) ergs, which is of a similar energy to that of U-band, X-ray, and EUV flares observed on many local M dwarf stars. We have found that stars of classes M0 to M5 flare with energies spanning a far larger range and with an energy approximately 5 times greater than those of later (M6 to M8) spectral type.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "673-681", "id_number": "CaltechAUTHORS:20091118-114325154", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091118-114325154", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516640", "primary_object": { "basename": "WELapjss07.pdf", "url": "https://authors.library.caltech.edu/records/fh896-54351/files/WELapjss07.pdf" }, "pub_year": "2007", "author_list": "Welsh, Barry Y.; Wheatley, Jonathan M.; et el." }, { "id": "https://authors.library.caltech.edu/records/78ds1-0za93", "eprint_id": 18057, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:20", "lastmod": "2023-10-20 15:32:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hoopes-C-G", "name": { "family": "Hoopes", "given": "Charles G." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Tremonti-C-A", "name": { "family": "Tremonti", "given": "Christy A." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } }, { "id": "Kauffmann-G", "name": { "family": "Kauffmann", "given": "Guinevere" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "The Diverse Properties of the Most Ultraviolet-Luminous Galaxies Discovered by GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 June 6; accepted 2006 September 7.\n\nWe thank the referee, Michael Strauss, for providing very\nhelpful comments that greatly improved the paper. GALEX is a\nNASA Small Explorer launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and\nscientific analysis for the GALEX mission. Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the participating institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.\nFacilities: GALEX, Sloan\n\nPublished - HOOapjss07.pdf
", "abstract": "We report on the properties of a sample of ultraviolet-luminous galaxies (UVLGs) selected by matching the Galaxy Evolution Explorer (GALEX) All-Sky Imaging and Medium Imaging Surveys with the Sloan Digital Sky Survey third data release. The overlap between these two surveys is roughly 450 deg^2. Of 25,362 galaxies (with SDSS spectroscopy) in the range 0.0 < z < 0.3 detected by GALEX, there are 215 galaxies with L > 2 \u00d7 10^(10) L_\u2609 at 1530 \u00c5 (observed wavelength). The properties of this population are well correlated with ultraviolet surface brightness. We find that the galaxies with low UV surface brightness are primarily large spiral systems with a mixture of old and young stellar populations, while the high surface brightness galaxies consist primarily of compact starburst systems, with an approximate boundary at a surface brightness of I_(1530) = 10^8 L_\u2609 kpc^(\u22122). The large galaxies appear to be the high-luminosity tail of the galaxy star formation function and owe their large luminosity to their large surface area. In terms of the behavior of surface brightness with luminosity, size with luminosity, the mass-metallicity relation, and other parameters, the compact UVLGs clearly depart from the trends established by the full sample of galaxies. The subset of compact UVLGs with the highest surface brightness (I_(1530) > 10^9 L_\u2609 kpc^(\u22122); \"supercompact UVLGs\") have characteristics that are remarkably similar to Lyman break galaxies at higher redshift. They are much more luminous (and thus have much higher star formation rates) than typical local ultraviolet-bright starburst galaxies and blue compact dwarf galaxies. They have metallicities that are systematically lower than normal galaxies of the same stellar mass, indicating that they are less chemically evolved. In all these respects, they are the best local analogs for Lyman break galaxies.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "441-456", "id_number": "CaltechAUTHORS:20100423-135206576", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100423-135206576", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516644", "primary_object": { "basename": "HOOapjss07.pdf", "url": "https://authors.library.caltech.edu/records/78ds1-0za93/files/HOOapjss07.pdf" }, "pub_year": "2007", "author_list": "Hoopes, Charles G.; Heckman, Timothy M.; et el." }, { "id": "https://authors.library.caltech.edu/records/6ghkb-dg080", "eprint_id": 17710, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:44", "lastmod": "2023-10-20 00:10:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "K." }, "orcid": "0000-0001-5464-0888" }, { "id": "Kaviraj-S", "name": { "family": "Kaviraj", "given": "S." } }, { "id": "Khochfar-S", "name": { "family": "Khochfar", "given": "S." } }, { "id": "Yoon-Suk-Jin", "name": { "family": "Yoon", "given": "S.-J." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "S. K." } }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "J." } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "T." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "L." }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "J." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Y.-W." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "A." } } ] }, "title": "The Effect of Environment on the Ultraviolet Color-Magnitude Relation of Early-Type Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2005 November 2; accepted for publication 2005 December 28.\n\nSpecial thanks are given to M. Bernardi, who kindly supplied\nher early-type galaxy catalog, which provided us with a great insight\non our catalog generation. We warmly thank C. Wolf for making\nthe COMBO-17 S11 field image available to us. We would also\nlike to thank E. Gawiser, L. Miller, S. Rawlings, J. Silk, R. Davies,\nI. Jorgensen, M. Sarzi, J. Magorrian, S. Salim, M. Urry, and\nK. Kotera for helpful comments and discussions.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's support\nfor construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry\nof Science and Technology. This work was supported by grant\nR01-2006-000-10716-0 from the Basic Research Program of the\nKOSEF and Yonsei University Research Fund to the corresponding\nauthor (S. K. Yi).\n\nPublished - SCHAapjss07.pdf
", "abstract": "We use GALEX near-UV (NUV) photometry of a sample of early-type galaxies selected in the SDSS (Sloan Digital Sky Survey) to study the UV color-magnitude relation (CMR). NUV \u2212 r color is an excellent tracer of even small amounts (~1% mass fraction) of recent (\u22721 Gyr) star formation, and so the NUV \u2212 r CMR allows us to study the effect of environment on the recent star formation history. We analyze a volume-limited sample of 839 visually inspected early-type galaxies in the redshift range 0.05 < z < 0.10 brighter than M_r of \u201321.5 with any possible emission-line or radio-selected active galactic nuclei (AGNs) removed to avoid contamination. We find that contamination by AGN candidates and late-type interlopers highly bias any study of recent star formation in early-type galaxies and that, after removing those, our lower limit to the fraction of massive early-type galaxies showing signs of recent star formation is roughly 30% \u00b1 3% . This suggests that residual star formation is common even among the present day early-type galaxy population. We find that the fraction of UV-bright early-type galaxies is 25% higher in low-density environments. However, the density effect is clear only in the lowest density bin. The blue galaxy fraction for the subsample of the brightest early-type galaxies, however, shows a very strong density dependence, in the sense that the blue galaxy fraction is lower in a higher density region.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "512-523", "id_number": "CaltechAUTHORS:20100309-143017549", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100309-143017549", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2006-000-10716-0" }, { "agency": "Yonsei University" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516631", "primary_object": { "basename": "SCHAapjss07.pdf", "url": "https://authors.library.caltech.edu/records/6ghkb-dg080/files/SCHAapjss07.pdf" }, "pub_year": "2007", "author_list": "Schawinski, K.; Kaviraj, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/bzn8v-vpc70", "eprint_id": 17465, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:58", "lastmod": "2023-10-19 23:55:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Joe-Young-H", "name": { "family": "Joe", "given": "Young H." } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David" }, "orcid": "0000-0002-8528-7340" }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Rey-Soo-Chang", "name": { "family": "Rey", "given": "Soo-Chang" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung" } } ] }, "title": "The GALEX Ultraviolet Atlas of Nearby Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "atlases; galaxies : evolution; galaxies : fundamental parameters; galaxies : photometry; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society\nReceived 2006 January 6; accepted 2006 March 15.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology. A. G. d. P. is partially financed by the\nMAGPOP EU Marie Curie Research Training Network and the\nSpanish Programa Nacional de Astronom\u0131\u00b4a y Astrof\u0131\u00b4sica under\ngrant AYA2003-01676. We thank Cren Frayer and Olga Pevunova\nfor preparing the online version of the Atlas. We are also thankful to\nthe referee for his/her valuable comments which helped to improve\nthe paper.\nFacilities: GALEX.\n\nPublished - PAZapjss07.pdf
", "abstract": "We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; \u03bb_(eff) = 1516 \u00c5) and near-ultraviolet (NUV; \u03bb_(eff) = 2267 \u00c5) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe. From the surface brightness profiles obtained we have computed asymptotic magnitudes, colors, and luminosities, along with the concentration indices C31 and C42. We have also morphologically classified the UV surface brightness profiles according to their shape. This data set has been complemented with archival optical, near-infrared, and far-infrared fluxes and colors. We find that the integrated (FUV \u2212 K) color provides robust discrimination between elliptical and spiral/irregular galaxies and also among spiral galaxies of different subtypes. Elliptical galaxies with brighter K-band luminosities (i.e., more massive) are redder in (NUV \u2212 K) color but bluer in (FUV \u2212 NUV) (a color sensitive to the presence of a strong UV upturn) than less massive ellipticals. In the case of the spiral/irregular galaxies our analysis shows the presence of a relatively tight correlation between the (FUV \u2212 NUV) color (or, equivalently, the slope of the UV spectrum, \u03b2) and the total infrared-to-UV ratio. The correlation found between (FUV \u2212 NUV) color and K-band luminosity (with lower luminosity objects being bluer than more luminous ones) can be explained as due to an increase in the dust content with galaxy luminosity. The images in this Atlas along with the profiles and integrated properties are publicly available through a dedicated Web page.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "185-255", "id_number": "CaltechAUTHORS:20100212-095356894", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100212-095356894", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship" }, { "agency": "Programa Nacional de Astronom\u0131a y Astrof\u0131sica", "grant_number": "AYA2003-01676" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516636", "primary_object": { "basename": "PAZapjss07.pdf", "url": "https://authors.library.caltech.edu/records/bzn8v-vpc70/files/PAZapjss07.pdf" }, "pub_year": "2007", "author_list": "Gil de Paz, Armando; Boissier, Samuel; et el." }, { "id": "https://authors.library.caltech.edu/records/gg4zj-k9291", "eprint_id": 18060, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:25", "lastmod": "2023-10-20 15:33:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Takeuchi-Tsutomu-T", "name": { "family": "Takeuchi", "given": "T. T." } }, { "id": "Iglesias-P\u00e1ramo-J", "name": { "family": "Iglesias-P\u00e1ramo", "given": "J." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "L." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "J." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T. M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Y.-W." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S." } }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "A. S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "B." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "S. K." } } ] }, "title": "The Local Universe as Seen in the Far-Infrared and Far-Ultraviolet: A Global Point of View of the Local Recent Star Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: photometry; galaxies: stellar content; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2006 June 9; accepted 2006 September 25.\n\nWe thank the anonymous referee for her/ his very useful and\nextensive comments. GALEX (the Galaxy Evolution Explorer) is\na NASA Small Explorer, launched in 2003 April. We gratefully\nacknowledge NASA's support for the construction, operation,\nand scientific analysis for the GALEX mission, developed in cooperation\nwith the Centre National d'Etudes Spatiales of France\nand the Korean Ministry of Science and Technology.V. B., D. B.,\nand J. I.-P. gratefully acknowledge CNES and ''Programme National\nGalaxie'' support for the scientific analysis for the GALEX\nmission. T. T. T. has been supported by a Japan Society for the\nPromotion of Science Fellowship for Research Abroad for the\nearly phase of this project, and later by the 21st Century Center\nof Excellence Program ''Exploring New Science by Bridging\nParticle-Matter Hierarchy'' at Tohoku University. This research\nhas made use of the NASA/IPAC Extragalactic Database, which\nis operated by the Jet Propulsion Laboratory/California Institute\nof Technology, under contract with the National Aeronautics and Space Administration. We also acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr).\n\nPublished - BUAapjss07.pdf
", "abstract": "We select far-infrared (FIR: 60 \u03bcm) and far-ultraviolet (FUV: 530 \u00c5) samples of nearby galaxies in order to discuss the biases encountered by monochromatic surveys (FIR or FUV). Very different volumes are sampled by each selection, and much care is taken to apply volume corrections to all the analyses. The distributions of the bolometric luminosity of young stars are compared for both samples: they are found to be consistent with each other for galaxies of intermediate luminosities, but some differences are found for high (>5 \u00d7 10^(10) L_\u2609) luminosities. The shallowness of the IRAS survey prevents us from securing a comparison at low luminosities (<2 \u00d7 10^9 L_\u2609). The ratio of the total infrared (TIR) luminosity to the FUV luminosity is found to increase with the bolometric luminosity in a similar way for both samples up to 5 \u00d7 10^(10) L_\u2609. Brighter galaxies are found to have a different behavior according to their selection: the L_(TIR)/L_(FUV) ratio of the FUV-selected galaxies brighter than 5 \u00d7 10^(10) L_\u2609 reaches a plateau, whereas L_(TIR)/L_(FUV) continues to increase with the luminosity of bright galaxies selected in FIR. The volume-averaged specific star formation rate (SFR per unit galaxy stellar mass, SSFR) is found to decrease toward massive galaxies within each selection. The mean values of the SSFR are found to be larger than those measured for optical and NIR-selected samples over the whole mass range for the FIR selection, and for masses larger than 10^(10) M_\u2609 for the FUV selection. Luminous and massive galaxies selected in FIR appear as active as galaxies with similar characteristics detected at z ~ 0.7.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "404-414", "id_number": "CaltechAUTHORS:20100423-135341806", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100423-135341806", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science" }, { "agency": "Tohoku University" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516645", "primary_object": { "basename": "BUAapjss07.pdf", "url": "https://authors.library.caltech.edu/records/gg4zj-k9291/files/BUAapjss07.pdf" }, "pub_year": "2007", "author_list": "Buat, V.; Takeuchi, T. T.; et el." }, { "id": "https://authors.library.caltech.edu/records/nrj8f-m0023", "eprint_id": 17735, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:54", "lastmod": "2023-10-20 00:11:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ree-Chang-H", "name": { "family": "Ree", "given": "Chang H." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Yoon-Suk-Jin", "name": { "family": "Yoon", "given": "Suk-Jin" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "Jean-Michel" } }, { "id": "Sohn-Young-Jong", "name": { "family": "Sohn", "given": "Young-Jong" } }, { "id": "Kaviraj-Sugata", "name": { "family": "Kaviraj", "given": "Sugata" } }, { "id": "Rhee-Jonghwan", "name": { "family": "Rhee", "given": "Jonghwan" } }, { "id": "Sheen-Yun-Kyeong", "name": { "family": "Sheen", "given": "Yun-Kyeong" } }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "Kevin" }, "orcid": "0000-0001-5464-0888" }, { "id": "Rey-Soo-Chang", "name": { "family": "Rey", "given": "Soo-Chang" } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Rhee-Jaehyon", "name": { "family": "Rhee", "given": "Jaehyon" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } } ] }, "title": "The Look-back Time Evolution of Far-Ultraviolet Flux from the Brightest Cluster Elliptical Galaxies at z < 0.2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: stellar content; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2006 September 14; accepted for publication 2007 March 15.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with the Centre\nNational d'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology. Yonsei University participation was supported\nby the Creative Research Initiative Program of MOST/KOSEF. We are grateful to Marc Sarzi for providing his spectral\nfitting code, adapted for use on SDSS spectra. S. K. Y. acknowledges\nsupport by grant R01-2006-000-10716-0 from the\nBasic Research Program of the Korea Science and Engineering\nFoundation.\n\nPublished - REEapjss07.pdf
", "abstract": "We present the GALEX UV photometry of the elliptical galaxies in Abell clusters at moderate redshifts (z < 0.2) for the study of the look-back time evolution of the UV upturn phenomenon. The brightest elliptical galaxies (M_r \u2272 \u221222) in 12 remote clusters are compared with the nearby giant elliptical galaxies of comparable optical luminosity in the Fornax and Virgo clusters. The sample galaxies presented here appear to be quiescent without signs of massive star formation or strong nuclear activity and show smooth, extended profiles in their UV images, indicating that the far-UV (FUV) light is mostly produced by hot stars in the underlying old stellar population. Compared to their counterparts in nearby clusters, the FUV flux of cluster giant elliptical galaxies at moderate redshifts fades rapidly with ~2 Gyr of look-back time, and the observed pace in FUV \u2212 V color evolution agrees reasonably well with the prediction from the population synthesis models where the dominant FUV source is hot horizontal-branch stars and their progeny. A similar amount of color spread (~1 mag) in FUV \u2212 V exists among the brightest cluster elliptical galaxies at z ~ 0.1, as observed among the nearby giant elliptical galaxies of comparable optical luminosity.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "607-618", "id_number": "CaltechAUTHORS:20100315-113445648", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100315-113445648", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministry of Science and Technology (Korea)" }, { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2006-000-10716-0" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/518125", "primary_object": { "basename": "REEapjss07.pdf", "url": "https://authors.library.caltech.edu/records/nrj8f-m0023/files/REEapjss07.pdf" }, "pub_year": "2007", "author_list": "Ree, Chang H.; Lee, Young-Wook; et el." }, { "id": "https://authors.library.caltech.edu/records/c1v2e-b7t06", "eprint_id": 18042, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:04", "lastmod": "2023-10-20 15:31:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "P\u00e9rez-Gonz\u00e1lez-P-G", "name": { "family": "P\u00e9rez-Gonz\u00e1lez", "given": "Pablo G." }, "orcid": "0000-0003-4528-5639" }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "Benjamin" } }, { "id": "Wolf-C", "name": { "family": "Wolf", "given": "Christian" }, "orcid": "0000-0002-4569-016X" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Meisenheimer-K", "name": { "family": "Meisenheimer", "given": "Klaus" } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "George" }, "orcid": "0000-0003-2303-6519" } ] }, "title": "The Star Formation and Extinction Coevolution of UV-Selected Galaxies over 0.05 < z < 1.2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2007 January 21; accepted 2007 July 27.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology.\nFacilities: GALEX, Sloan\n\nPublished - MARapjss07b.pdf
", "abstract": "We use a new stacking technique to obtain mean mid-IR and far-IR to far-UV flux ratios over the rest-frame near-UV, near-IR color-magnitude diagram. We employ COMBO-17 redshifts and COMBO-17 optical, GALEX far- and near-UV, and Spitzer IRAC and MIPS mid-IR photometry. This technique permits us to probe the infrared excess (IRX), the ratio of far-IR to far-UV luminosity, and the specific star formation rate (SSFR) and their coevolution over 2 orders of magnitude of stellar mass and over redshift 0.1 < z < 1.2. We find that the SSFR and the characteristic mass (M_0) above which the SSFR drops increase with redshift (downsizing). At any given epoch, the IRX is an increasing function of mass up to M_0. Above this mass the IRX falls, suggesting gas exhaustion. In a given mass bin below M_0, the IRX increases with time in a fashion consistent with enrichment. We interpret these trends using a simple model with a Schmidt-Kennicutt law and extinction that tracks gas density and enrichment. We find that the average IRX and SSFR follow a galaxy age parameter \u03be, which is determined mainly by the galaxy mass and time since formation. We conclude that blue-sequence galaxies have properties which show simple, systematic trends with mass and time such as the steady buildup of heavy elements in the interstellar media of evolving galaxies and the exhaustion of gas in galaxies that are evolving off the blue sequence. The IRX represents a tool for selecting galaxies at various stages of evolution.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "415-431", "id_number": "CaltechAUTHORS:20100421-122354466", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100421-122354466", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/522088", "primary_object": { "basename": "MARapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/c1v2e-b7t06/files/MARapjss07b.pdf" }, "pub_year": "2007", "author_list": "Martin, D. Christopher; Small, Todd; et el." }, { "id": "https://authors.library.caltech.edu/records/nw3kf-sn393", "eprint_id": 17546, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:18", "lastmod": "2023-10-19 23:59:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "Benjamin D." } }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie A." } }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Hoopes-C-G", "name": { "family": "Hoopes", "given": "Charles" } }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "Michel" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd A." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex. S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung" } } ] }, "title": "The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; surveys; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2007 August 2; accepted for publication 2007 October 16.\n\nD. S. gratefully acknowledges discussions with Eric Bell and\nMichael Blanton and the hospitality of the Max Planck Institut fu\u00a8r Astronomie in Heidelberg and the Aspen Center for Physics. This work has made extensive use of the idlutils, kcorrect, and Goddard IDL libraries, as well as the MPA/JHU and the\nNYU SDSS value-added catalogs. GALEX (Galaxy Evolution\nExplorer) is a NASA Small Explorer, launched in April 2003.\nWe gratefully acknowledge NASA's support for the construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology.\nFacilities: GALEX\n\nPublished - SCHIapjss07b.pdf
", "abstract": "We use the UV-optical color magnitude diagram in combination with spectroscopic and photometric measurements derived from the SDSS spectroscopic sample to measure the distribution of galaxies in the local universe (z < 0.25) and their physical properties as a function of specific star formation rate (SFR/M_*) and stellar mass (M_*). Throughout this study our emphasis is on the properties of galaxies on and off of a local \"star-forming sequence.\" We discuss how the physical characteristics of galaxies along this sequence are related to scaling relations typically derived for galaxies of different morphological types. We find, among other trends, that our measure of the star formation rate surface density, \u03a3_(SFR), is nearly constant along this sequence. We discuss this result and implications for galaxies at higher redshift. For the first time, we report on measurements of the local UV luminosity function versus galaxy structural parameters, as well as inclination. We also split our sample into disk-dominated and bulge-dominated subsamples using the i-band Sersic index and find that disk-dominated galaxies occupy a very tight locus in SFR/M_* vs. M_* space, while bulge-dominated galaxies display a much larger spread of SFR/M_* at fixed stellar mass. A significant fraction of galaxies with SFR/M_* and \u03a3_(SFR) above those on the \"star-forming sequence\" are bulge-dominated. We can use our derived distribution functions to ask whether a significant fraction of these galaxies may be experiencing a final episode of star formation (possibly induced by a merger or other burst), soon to be quenched, by determining whether this population can explain the growth rate of the non-star-forming galaxies on the \"red sequence.\" We find that this is a plausible scenario for bulge-dominated galaxies near the characteristic transition mass under reasonable assumptions regarding quenching timescales. Similarly, we use this technique to estimate the rate of mergers/starbursts that take galaxies off of the star-forming sequence and show that the implied merger rates are consistent with local measurements.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "315-341", "id_number": "CaltechAUTHORS:20100222-095205221", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-095205221", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/524659", "primary_object": { "basename": "SCHIapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/nw3kf-sn393/files/SCHIapjss07b.pdf" }, "pub_year": "2007", "author_list": "Schiminovich, David; Wyder, Ted K.; et el." }, { "id": "https://authors.library.caltech.edu/records/n4fsm-t4108", "eprint_id": 16731, "eprint_status": "archive", "datestamp": "2023-08-22 10:33:55", "lastmod": "2023-10-19 22:31:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Budav\u00e1ri-T", "name": { "family": "Budav\u00e1ri", "given": "Tam\u00e1s" } }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie A." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "The UV-Optical Galaxy Color-Magnitude Diagram. I. Basic Properties", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; galaxies: luminosity function, mass function; galaxies: statistics; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2006 November 14, accepted for publication 2007 June 26.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology.\nFacilities: GALEX\n\nPublished - WYDapjss07.pdf
", "abstract": "We have analyzed the bivariate distribution of galaxies as a function of ultraviolet-optical colors and absolute magnitudes in the local universe. The sample consists of galaxies with redshifts and optical photometry from the Sloan Digital Sky Survey (SDSS) main galaxy sample matched with detections in the near-ultraviolet (NUV) and far-ultraviolet (FUV) bands in the Medium Imaging Survey being carried out by the Galaxy Evolution Explorer (GALEX) satellite. In the (NUV \u2212 r)_(0.1) versus M_(r,0.1) galaxy color-magnitude diagram, the galaxies separate into two well-defined blue and red sequences. The (NUV \u2212 r)_(0.1) color distribution at each M_(r,0.1) is not well fit by the sum of two Gaussians due to an excess of galaxies in between the two sequences. The peaks of both sequences become redder with increasing luminosity, with a distinct blue peak visible up to M_(r,0.1) ~ \u2212 23. The r_(0.1)-band luminosity functions vary systematically with color, with the faint-end slope and characteristic luminosity gradually increasing with color. After correcting for attenuation due to dust, we find that approximately one-quarter of the color variation along the blue sequence is due to dust, with the remainder due to star formation history and metallicity. Finally, we present the distribution of galaxies as a function of specific star formation rate and stellar mass. The specific star formation rates imply that galaxies along the blue sequence progress from low-mass galaxies with star formation rates that increase somewhat with time to more massive galaxies with a more or less constant star formation rate. Above a stellar mass of ~10^(10.5) M_\u2609, galaxies with low ratios of current to past averaged star formation rate begin to dominate.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "293-314", "id_number": "CaltechAUTHORS:20091117-113251451", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-113251451", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/521402", "primary_object": { "basename": "WYDapjss07.pdf", "url": "https://authors.library.caltech.edu/records/n4fsm-t4108/files/WYDapjss07.pdf" }, "pub_year": "2007", "author_list": "Wyder, Ted K.; Martin, D. Christopher; et el." }, { "id": "https://authors.library.caltech.edu/records/afscw-jj304", "eprint_id": 17473, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:08", "lastmod": "2023-10-19 23:55:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "The UV-Optical Galaxy Color-Magnitude Diagram. III. Constraints on Evolution from the Blue to the Red Sequence", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : evolution; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 February 27; accepted 2006 June 18.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology. We also thank the referee for excellent\ncomments.\nFacilities: GALEX.\n\nPublished - MARapjss07a.pdf
", "abstract": "We introduce a new quantity, the mass flux density of galaxies evolving from the blue sequence to the red sequence. We propose a simple technique for constraining this mass flux using the volume-corrected number density in the extinction-corrected UV-optical color-magnitude distribution, the stellar age indexes H\u03b4_A and D_n(4000), and a simple prescription for spectral evolution using a quenched star formation history. We exploit the excellent separation of red and blue sequences in the NUV \u2212 r band Hess function. The final value we measure, \u03c1_T = 0.033 M_\u2299 yr^(\u22121) Mpc^(\u22123), is strictly speaking an upper limit due to the possible contributions of bursting, composite, and extincted galaxies. However, it compares favorably with estimates of the average mass flux that we make based on the red luminosity function evolution derived from the DEEP2 and COMBO-17 surveys, \u03c1_R = +0.034 M_\u2299 yr^(\u22121) Mpc^(\u22123). We find that the blue sequence mass has remained roughly constant since z = 1 (\u03c1_B \u2243 0.01 M_\u2299 yr^(\u22121) Mpc^(\u22123)), but the average on-going star formation of \u03c1_(SF) \u2243 0.037 M_\u2299 yr^(\u22121) Mpc^(\u22123) over 0 < z < 1 is balanced by mass flux off the blue sequence. We explore the nature of the galaxies in the transition zone with particular attention to the frequency and impact of active galactic nuclei (AGNs). The AGN fraction peaks in the transition zone. We find circumstantial, albeit weak evidence that the quench rates are higher in higher luminosity AGNs.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "342-356", "id_number": "CaltechAUTHORS:20100212-150837678", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100212-150837678", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516639", "primary_object": { "basename": "MARapjss07a.pdf", "url": "https://authors.library.caltech.edu/records/afscw-jj304/files/MARapjss07a.pdf" }, "pub_year": "2007", "author_list": "Martin, D. Christopher; Wyder, Ted K.; et el." }, { "id": "https://authors.library.caltech.edu/records/na1bh-wj762", "eprint_id": 16358, "eprint_status": "archive", "datestamp": "2023-08-22 10:33:30", "lastmod": "2023-10-19 22:08:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Basu-Zych-A-R", "name": { "family": "Basu-Zych", "given": "Antara R." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "Benjamin D." } }, { "id": "Hoopes-C-G", "name": { "family": "Hoopes", "given": "Charles" } }, { "id": "Overzier-R-A", "name": { "family": "Overzier", "given": "Roderik" } }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie A." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd A." } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung" } } ] }, "title": "The Young and the Dustless: Interpreting Radio Observations of Ultraviolet-Luminous Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : starburst; radio continuum : galaxies; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 February 7; accepted 2007 June 18.\nGALEX (Galaxy Evolution Explorer) is a NASA small explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's support\nfor construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology. We thank Michael Blanton for access\nto the IDL kcorrect (ver. 4.1.4) analysis package.We recognize\nthat funding for the SDSS archive has been provided by the\nAlfred P. Sloan Foundation, the Participating Institutions, the\nNational Aeronautics and Space Administration, the National\nScience Foundation, the US Department of Energy, the Japanese\nMonbukagakusho, and the Max Planck Society.\n\nPublished - BASapjss07.pdf
", "abstract": "Ultraviolet-luminous galaxies (UVLGs) have been identified as intensely star-forming nearby galaxies. A subset of these, the supercompact UVLGs, are believed to be local analogs of high-redshift Lyman break galaxies. Here we investigate the radio continuum properties of this important population for the first time. We have observed 42 supercompact UVLGs with the VLA, all of which have extensive coverage in the UV/optical by GALEX and SDSS. Our analysis includes comparison samples of multiwavelength data from the Spitzer First Look Survey and from the SDSS-GALEX matched catalogs. In addition we have Spitzer MIPS data for 24 of our galaxies and find that they fall on the radio-FIR correlation of normal star-forming galaxies. We find that our galaxies have lower radio to UV ratios and lower Balmer decrements than other local galaxies with similar (high) star formation rates. Optical spectra show they have lower D_n(4000) and H\u03b4_A indices, higher H\u03b2 emission-line equivalent widths, and higher [O III]5007/H\u03b2 emission-line ratios than normal star-forming galaxies. Comparing these results to galaxy spectral evolution models we conclude that supercompact UVLGs are distinguished from normal star-forming galaxies firstly by their high specific star formation rates. Moreover, compared to other types of galaxies with similar star formation rates, they have significantly less dust attenuation. In both regards they are similar to Lyman break galaxies. This suggests that the process that causes star formation in the supercompact UVLGs differs from other local star-forming galaxies, but may be similar to Lyman break galaxies.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "457-470", "id_number": "CaltechAUTHORS:20091016-084254435", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091016-084254435", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Jaqpanese Monbukagakusho" }, { "agency": "Max Planck Society" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/521146", "primary_object": { "basename": "BASapjss07.pdf", "url": "https://authors.library.caltech.edu/records/na1bh-wj762/files/BASapjss07.pdf" }, "pub_year": "2007", "author_list": "Basu-Zych, Antara R.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/whk45-c8s65", "eprint_id": 17716, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:49", "lastmod": "2023-10-20 00:10:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "St\u00e9phane" } }, { "id": "Brinchmann-J", "name": { "family": "Brinchmann", "given": "Jarle" } }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "Benjamin D." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Mallery-R-P", "name": { "family": "Mallery", "given": "Ryan" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "UV Star Formation Rates in the Local Universe", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: fundamental parameters; surveys; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2006 December 22; accepted for publication 2007 April 25.\n\nWe thank Janice C. Lee for insightful comments and helpful\ndiscussions. We thank the referee for numerous valuable suggestions.\nWe also thank Alessandro Boselli and Michael Blanton.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's support\nfor construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre\nNational d'Etudes Spatiales of France and the Korean Ministry\nof Science and Technology. Funding for the Sloan Digital Sky\nSurvey (SDSS) and SDSS-II has been provided by the Alfred P.\nSloan Foundation, the Participating Institutions, the National\nScience Foundation, the U.S. Department of Energy, the National\nAeronautics and Space Administration, the Japanese\nMonbukagakusho, and theMax Planck Society, and the Higher\nEducation Funding Council for England. This research has made\nuse of NASA's Astrophysics Data System.\nFacilities: GALEX, Sloan\n\nPublished - SALapjss07.pdf
", "abstract": "We measure star formation rates (SFRs) of \u224850,000 optically selected galaxies in the local universe (z \u2248 0.1)\u2014from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (ultraviolet) and SDSS photometry to a library of dust-attenuated population synthesis models. For star-forming galaxies, our UV-based SFRs compare remarkably well with those from SDSS-measured emission lines (H\u03b1). Deviations from perfect agreement are shown to be due to differences in the dust attenuation estimates. In contrast to H\u03b1 measurements, UV provides reliable SFRs for galaxies with weak H\u03b1, and where H\u03b1 is contaminated with AGN emission (1/2 of the sample). Using full-SED SFRs, we calibrate a simple prescription that uses GALEX far- and near-UV magnitudes to produce dust-corrected SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGNs, (2) those hosting an AGN, and (3) galaxies without H\u03b1 emission. We find that the three have distinct star formation histories, with AGNs lying intermediate between the star-forming and the quiescent galaxies. Star-forming galaxies without an AGN lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. On the other hand, weak AGNs, while also massive, have lower SFRs, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent galaxies via strong and weak AGNs. We confirm that some galaxies with no H\u03b1 show signs of star formation in the UV. We derive a cosmic star formation density at z = 0.1 with significantly smaller total error than previous measurements.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "267-292", "id_number": "CaltechAUTHORS:20100310-103408116", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100310-103408116", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/519218", "primary_object": { "basename": "SALapjss07.pdf", "url": "https://authors.library.caltech.edu/records/whk45-c8s65/files/SALapjss07.pdf" }, "pub_year": "2007", "author_list": "Salim, Samir; Rich, R. Michael; et el." }, { "id": "https://authors.library.caltech.edu/records/1qcby-fc616", "eprint_id": 17552, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:25", "lastmod": "2023-10-19 23:59:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kaviraj-S", "name": { "family": "Kaviraj", "given": "S." } }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "K." }, "orcid": "0000-0001-5464-0888" }, { "id": "Devriendt-J-E-G", "name": { "family": "Devriendt", "given": "J. E. G." }, "orcid": "0000-0002-8140-0422" }, { "id": "Ferreras-I", "name": { "family": "Ferreras", "given": "I." } }, { "id": "Khochfar-S", "name": { "family": "Khochfar", "given": "S." } }, { "id": "Yoon-Suk-Jin", "name": { "family": "Yoon", "given": "S.-J." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "S. K." } }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "J.-M." } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "T." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "L." }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "J." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Y.-W." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "A." } } ] }, "title": "UV-Optical Colors as Probes of Early-Type Galaxy Evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 January 4; accepted 2006 September 11.\nWe are grateful to the anonymous referee for various clarifications.\nWe warmly thank Chris Wolf for providing high-resolution\nCOMBO-17 images, which formed an integral part of our morphological\nclassification process. We also thank Mariangela\nBernardi for her generous help in the initial stages of this project, for providing the DR2 versions of her SDSS early-type catalog\nprior to publication, and many interesting discussions. We are\ngrateful to Jeremy Blaizot for his extensive help with the GALICS\nmodel and to Andre\u00b4s Jorda\u00b4n, Joseph Silk, Roger Davies, and\nAndrew Benson for many useful comments regarding this work.\nS. K. acknowledges PPARC graduate D Phil scholarship PPA/S/S/\n2002/03532. This work was supported by grant R01-2006-000-\n10716-0 from the Basic Research Program of the Korea Science & Engineering Foundation and Yonsei University Research Fund\n(2005) to S. K. Y.\n\nPublished - KAVapjss07.pdf
", "abstract": "We have studied ~2100 early-type galaxies in the SDSS DR3 which have been detected by the GALEX Medium Imaging Survey (MIS), in the redshift range 0 < z < 0.11. Combining GALEX UV photometry with corollary optical data from the SDSS, we find that, at a 95% confidence level, at least ~30% of galaxies in this sample have UV to optical colors consistent with some recent star formation within the last Gyr. In particular, galaxies with an NUV \u2212 r color less than 5.5 are very likely to have experienced such recent star formation, taking into account the possibility of a contribution to NUV flux from the UV upturn phenomenon. We find quantitative agreement between the observations and the predictions of a semianalytical \u039bCDM hierarchical merger model and deduce that early-type galaxies in the redshift range 0 < z < 0.11 have ~1%-3% of their stellar mass in stars less than 1 Gyr old. The average age of this recently formed population is ~300-500 Myr. We also find that \"monolithically\" evolving galaxies, where recent star formation can be driven solely by recycled gas from stellar mass loss, cannot exhibit the blue colors (NUV \u2212 r < 5.5) seen in a significant fraction (~30%) of our observed sample.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "619-642", "id_number": "CaltechAUTHORS:20100222-105254739", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-105254739", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Particle Physics and Astronomy Research Council (PPARC)", "grant_number": "PPA/S/S/2002/03532" }, { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2006-000-10716-0" }, { "agency": "Yonsei University" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/516633", "primary_object": { "basename": "KAVapjss07.pdf", "url": "https://authors.library.caltech.edu/records/1qcby-fc616/files/KAVapjss07.pdf" }, "pub_year": "2007", "author_list": "Kaviraj, S.; Schawinski, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/j39p1-ybg60", "eprint_id": 16869, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:16", "lastmod": "2023-10-19 22:37:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "David A." }, "orcid": "0000-0002-8528-7340" }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Braun-R", "name": { "family": "Braun", "given": "Robert" } }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "Denis" } }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Ultraviolet and Infrared Diagnostics of Star Formation and Dust in NGC 7331", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: individual (NGC 7331); infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December); received 2006 July 17; accepted for publication 2006 September 26.\n\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April.We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology. Support for this work, part of the Spitzer\nSpace Telescope Legacy Science Program,was provided by NASA\nthrough contract 1224769 issued by the Jet Propulsion Laboratory\n(JPL), California Institute of Technology, under NASA contract\n1407. This research has made use of the NASA/IPAC Extragalactic\nDatabase (NED) which is operated by JPL, California\nInstitute of Technology, under contract withNASA. This research\nhas made use of NASA's Astrophysics Data System.\n\nPublished - THIapjss07b.pdf
", "abstract": "We present images of NGC 7331 obtained with GALEX and Spitzer, tracing UV and IR signatures of star formation. NGC 7331's morphology at 8-850 \u03bcm is dominated by a central dust ring. This structure is a vigorous site of star formation (hosting one-third of the present activity) but remains inconspicuous in our GALEX UV imagery. Radial profile analysis and photometry for discrete UV- and UV+IR-selected substructures indicate a decline in UV extinction with increasing galactocentric distance, although highly attenuated star-forming regions can be found throughout the disk. UV-optical surface brightness profiles suggest a recent birthrate parameter (b_8) that is highest in the outer part of the disk, even though the local star formation intensity peaks in the ring. Bolometric luminosity and UV attenuation are correlated in substructures on 0.4 kpc scales, with a relationship similar to that established for starburst galaxies. The distribution of substructures in L(IR)/L(FUV), L_\u03bb(FUV)/L_\u03bb(NUV) space suggests that the majority of the disk is best characterized by Milky Way-type dust, with the exception of sources in the star-forming ring. As found by Calzetti et al. in M51, the observed 8 and 24 \u03bcm luminosity for substructures in NGC 7331 are correlated, showing a decline in L_\u03bd(8 \u03bcm)/L_\u03bd(24 \u03bcm) with increasing luminosity. We demonstrate the dependence of L_\u03bd(8 \u03bcm)/L_\u03bd(24 \u03bcm) on the local extinction-corrected H\u03b1 surface brightness (hence current \u03a3_(SFR)). A power law of slope 1.64 (1.87) accurately describes the Schmidt-law relation versus \u03a3_(H_2) (\u03a3_(gas)) for molecular-dominated environments. The same locations show no correlation between \u03a3_(SFR) and \u03a3_(HI). For atomic-dominated regions above an apparent local star formation threshold, we found a trend for increasing \u03a3_(SFR) at higher \u03a3_(HI) , although the Schmidt-law correlation with molecular-only surface density persists in areas dominated by atomic gas.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "572-596", "id_number": "CaltechAUTHORS:20091203-140413022", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091203-140413022", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "JPL" }, { "agency": "Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516646", "primary_object": { "basename": "THIapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/j39p1-ybg60/files/THIapjss07b.pdf" }, "pub_year": "2007", "author_list": "Thilker, David A.; Boissier, Samuel; et el." }, { "id": "https://authors.library.caltech.edu/records/vecsc-4ev31", "eprint_id": 17472, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:03", "lastmod": "2023-10-19 23:55:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "Benjamin D." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Treyer-M-A", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jose" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Ultraviolet through Infrared Spectral Energy Distributions from 1000 SDSS Galaxies: Dust Attenuation", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies : evolution; galaxies : fundamental parameters; infrared : galaxies; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 August 2; accepted 2007 September 3.\nB. D. J. would like to thank A. Basu-Zych, S. Salim, A. Boselli,\nS. Boissier, and L. Cortese for comments that improved the paper.\nB. D. J. was supported by NASA GSRP grant NNG-05GO43H.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge NASA's\nsupport for construction, operation, and science analysis for the\nGALEX mission, developed in cooperation with the Centre National\nd'Etudes Spatiales of France and the Korean Ministry of\nScience and Technology. This work is based in part on observations\nmade with the Spitzer Space Telescope, which is operated\nby the Jet Propulsion Laboratory, California Institute of Technology,\nunder a contract with NASA. In particular, the publicly\navailable Spitzer data obtained by the SWIRE team have been\nessential to this work. Funding for the SDSS and SDSS-II has\nbeen provided by the Alfred P. Sloan Foundation, the Participating\nInstitutions, the National Science Foundation, the Department\nof Energy, the National Aeronautics and Space Administration,\nthe Japanese Monbukagakusho, the Max Planck Society, and the\nHigher Education Funding Council for England. The SDSS Web\nsite is http://www.sdss.org. The SDSS is managed by the Astrophysical\nResearch Consortium for the Participating Institutions.\nThe Participating Institutions are the American Museum of Natural History,\nAstrophysical Institute Potsdam, University of Basel,\nUniversity of Cambridge, Case Western Reserve University, University\nof Chicago, Drexel University, Fermilab, the Institute for\nAdvanced Study, the Japan Participation Group, Johns Hopkins\nUniversity, the Joint Institute for Nuclear Astrophysics, the Kavli\nInstitute for Particle Astrophysics and Cosmology, the Korean\nScientist Group, the Chinese Academy of Sciences (LAMOST),\nLos Alamos National Laboratory, the Max Planck Institute for\nAstronomy (MPIA), the Max Planck Institute for Astrophysics\n(MPA), New Mexico State University, Ohio State University,\nUniversity of Pittsburgh, University of Portsmouth, Princeton\nUniversity, the United States Naval Observatory, and the University\nof Washington.\n\nPublished - JOHapjss07b.pdf
", "abstract": "The meaningful comparison of models of galaxy evolution to observations is critically dependent on the accurate treatment of dust attenuation. To investigate dust absorption and emission in galaxies we have assembled a sample of ~1000 galaxies with UV through IR photometry from GALEX, SDSS, and Spitzer, and optical spectroscopy from SDSS. The ratio of IR to UV emission (IRX) is used to constrain the dust attenuation in galaxies. We use the 4000 \u00c5 break as a robust and useful, although coarse, indicator of star formation history (SFH). We examine the relationship between IRX and the UV spectral slope (a common attenuation indicator at high redshift) and find little dependence of the scatter on D_n(4000). We construct average UV through far-IR spectral energy distributions (SEDs) for different ranges of IRX, D_n(4000), and stellar mass (M_*) to show the variation of the entire SED with these parameters. When binned simultaneously by IRX, D_n(4000), and M_* these SEDs allow us to determine a low-resolution average attenuation curve for different ranges of M_*. The attenuation curves thus derived are consistent with a \u03bb^(\u22120.7) attenuation law, and we find no significant variations with M_*. Finally, we show the relationship between IRX and the global stellar mass surface density and gas-phase metallicity. Among star-forming galaxies we find a strong correlation between IRX and stellar mass surface density, even at constant metallicity, a result that is closely linked to the well-known correlation between IRX and star formation rate.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "392-403", "id_number": "CaltechAUTHORS:20100212-135026966", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100212-135026966", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Graduate Student Research Fellowship", "grant_number": "NNG-05GO43H" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/522960", "primary_object": { "basename": "JOHapjss07b.pdf", "url": "https://authors.library.caltech.edu/records/vecsc-4ev31/files/JOHapjss07b.pdf" }, "pub_year": "2007", "author_list": "Johnson, Benjamin D.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/edv3h-2c472", "eprint_id": 20005, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:46", "lastmod": "2023-10-20 22:07:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "Benjamin D." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Treyer-M", "name": { "family": "Treyer", "given": "Marie" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } } ] }, "title": "Ultraviolet, Optical, and Infrared Constraints on Models of Stellar Populations and Dust Attenuation", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: evolution; galaxies: fundamental parameters; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2007 February 26; accepted 2007 August 30.\n\nThe anonymous referee provided extremely useful comments that resulted in substantial improvements to the paper. B. D. J. thanks S. Salim, A. Boselli, S. Boissier, and L. Cortese for helpful comments. B. D. J. was supported by NASA GSRP grant NNG- 05GO43H. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. This work is based in part on observationsmade with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. In particular, the publicly available Spitzer data obtained by the SWIRE team have been essential to this work. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, the Astrophysical Institute Potsdam, the University of Basel, the University of Cambridge, Case Western Reserve University, the University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max Planck Institute for Astronomy (MPIA), the Max Planck Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, the University of Pittsburgh, the University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.\n\nPublished - JOHapjss07a.pdf
", "abstract": "The color of galaxies is a fundamental property, easily measured, that constrains models of galaxies and their evolution. Dust attenuation and star formation history (SFH) are the dominant factors affecting the color of galaxies. Here we explore the empirical relation between SFH, attenuation, and color for a wide range of galaxies, including early types. These galaxies have been observed by GALEX, SDSS, and Spitzer, allowing the construction of measures of dust attenuation from the ratio of infrared (IR) to ultraviolet (UV) flux and measures of SFH from the strength of the 4000 \u00c5 break. The empirical relation between these three quantities is compared to models that separately predict the effects of dust and SFH on color. This comparison demonstrates the quantitative consistency of these simple models with the data and hints at the power of multiwavelength data for constraining these models. The UV color is a strong constraint; we find that a Milky Way extinction curve is disfavored, and that the UV emission of galaxies with large 4000 \u00c5 break strengths is likely to arise from evolved populations. We perform fits to the relation between SFH, attenuation, and color. This relation links the production of starlight and its absorption by dust to the subsequent reemission of the absorbed light in the IR. Galaxy models that self-consistently treat dust absorption and emission as well as stellar populations will need to reproduce these fitted relations in the low-redshift universe.", "date": "2007-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "173", "number": "2", "publisher": "American Astronomical Society", "pagerange": "377-391", "id_number": "CaltechAUTHORS:20100917-094457903", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100917-094457903", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Graduate Student Research Fellowship", "grant_number": "NNG-05GO43H" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/522932", "primary_object": { "basename": "JOHapjss07a.pdf", "url": "https://authors.library.caltech.edu/records/edv3h-2c472/files/JOHapjss07a.pdf" }, "pub_year": "2007", "author_list": "Johnson, Benjamin D.; Schiminovich, David; et el." }, { "id": "https://authors.library.caltech.edu/records/bd25f-z8615", "eprint_id": 17555, "eprint_status": "archive", "datestamp": "2023-08-22 10:29:05", "lastmod": "2023-10-19 23:59:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Iglesias-P\u00e1ramo-J", "name": { "family": "Iglesias-P\u00e1ramo", "given": "J." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Hern\u00e1ndez-Fern\u00e1ndez-J", "name": { "family": "Hern\u00e1ndez-Fern\u00e1ndez", "given": "J." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Takeuchi-Tsutomu-T", "name": { "family": "Takeuchi", "given": "T. T." } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D." }, "orcid": "0000-0003-4401-0430" }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Babbedge-T", "name": { "family": "Babbedge", "given": "T." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "T." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Gonz\u00e1lez-Solares-E", "name": { "family": "Gonz\u00e1lez-Solares", "given": "E." } }, { "id": "Lonsdale-C-J", "name": { "family": "Lonsdale", "given": "C." }, "orcid": "0000-0003-0898-406X" }, { "id": "Smith-Gene", "name": { "family": "Smith", "given": "G." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T. A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S. G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "L." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "J." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T. M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Y.-W." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "A. S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "B. Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "S. K." } } ] }, "title": "UV to IR SEDs of UV-Selected Galaxies in the ELAIS Fields: Evolution of Dust Attenuation and Star Formation Activity from z = 0.7 to 0.2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : evolution; surveys; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 February 28; accepted 2007 July 21.\nWe thank the anonymous referee for his/her interesting comments\nand suggestions that helped to improve the former version\nof this manuscript. Thanks are also given to Steve Donegan for\nhis careful reading and English revision of the text. This paper\nhas benefited from interesting discussions with G. L. Granato\nand L. Silva. GALEX (Galaxy Evolution Explorer) is a NASA Small\nExplorer, launched in 2003 April. We gratefully acknowledge\nNASA's support for the construction, operation, and science\nanalysis for the GALEX mission, developed in cooperation with\nthe Centre National d'Etudes Spatiales of France and the Korean\nMinistry of Science and Technology. Support for this work, part\nof the Spitzer Space Telescope Legacy Science Program, was\nprovided by NASA through an award issued by JPL under\nNASA contract 1407. This article is based on observations made\nwith the Isaac Newton Telescope, operated on the island of La\nPalma by the Isaac Newton Group at the Spanish Observatorio\nde El Roque de los Muchachos. This work has been partially\nfunded by the projects AYA 2004-08260-C03-02 of the Spanish\nPNAYA and TIC114 of the Junta de Andaluc\u0131\u00b4a. T. T. T. has been\nsupported by Program for Improvement of Research Environment\nfor Young Researchers from Special Coordination Funds\nfor Promoting Science and Technology (SCF) commissioned by\nthe Ministry of Education, Culture, Sports, Science, and Technology\n(MEXT) of Japan.\n\nPublished - IGLapj07.pdf
", "abstract": "We study the ultraviolet to far-infrared (hereafter UV-to-IR) SEDs of a sample of intermediate-redshift (0.2 \u2264 z \u2264 0.7) UV-selected galaxies from the ELAIS N1 and ELAIS N2 fields by fitting a multi-wavelength data set to a library of GRASIL templates. Star formation related properties of the galaxies are derived from the library of models by using Bayesian statistics. We find a decreasing presence of galaxies with low attenuation and low total luminosity as redshift decreases, which does not hold for high total luminosity galaxies. In addition, the dust attenuation of low-mass galaxies increases as redshift decreases, and this trend seems to disappear for galaxies with M_* \u2265 10^(11) M_\u2299. This result is consistent with a mass-dependent evolution of the dust-to-gas ratio, which could be driven by a mass-dependent efficiency of star formation in star-forming galaxies. The specific star formation rates (SSFR) decrease with increasing stellar mass at all redshifts, and for a given stellar mass the SSFR decreases with decreasing redshift. The differences in the slope of the M^*-SSFR relation found between this work and others at similar redshift could be explained by the adopted selection criteria of the samples, which for a UV-selected sample, favors blue, star-forming galaxies.", "date": "2007-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "670", "number": "1", "publisher": "American Astronomical Society", "pagerange": "279-294", "id_number": "CaltechAUTHORS:20100222-135706376", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-135706376", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Plan Nacional de Astronom\u00eda y Astrof\u00edsica", "grant_number": "AYA 2004-08260-C03-02" }, { "agency": "Junta de Andaluc\u0131a", "grant_number": "TIC114" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/521867", "primary_object": { "basename": "IGLapj07.pdf", "url": "https://authors.library.caltech.edu/records/bd25f-z8615/files/IGLapj07.pdf" }, "pub_year": "2007", "author_list": "Iglesias-P\u00e1ramo, J.; Buat, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/xcv6q-j4v13", "eprint_id": 16705, "eprint_status": "archive", "datestamp": "2023-08-22 09:52:16", "lastmod": "2023-10-19 22:29:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "M. A." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Sasaki-S-S", "name": { "family": "Sasaki", "given": "S. S." } }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mellier-Y", "name": { "family": "Mellier", "given": "Y." } }, { "id": "Bertin-E", "name": { "family": "Bertin", "given": "E." } }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T. A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S G." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "L." } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "J." } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "T. M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Y.-W." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "A. S." } }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "B. Y." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "S. K." } } ] }, "title": "Deep GALEX Imaging of the COSMOS HST Field: A First Look at the Morphology of z ~ 0.7 Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; surveys", "note": "\u00a9 2009 American Astronomical Society. \n\nReceived 2006 July 28; accepted 2007 January 9. \n\nThe COSMOS HST Treasury program was supported through NASA grant HST-GO-09822. We wish to thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 70 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/~cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. The COSMOS Science meeting in 2005 May was supported in part by the NSF through grant OISE-0456439.\n\n GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. \n\nFacilities: HST(ACS), GALEX, Subaru, CFHT, KPNO:2.1m, CTIO:1.5m \n\nBased on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS 5-26555; and with the NASA Galaxy Evolution Explorer (GALEX); also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation; the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX, and the University of Hawaii.\n\nPublished - ZAMapjss07.pdf
", "abstract": "We present a study of the morphological nature of redshift z ~ 0.7 star-forming galaxies using a combination of HST ACS, GALEX, and ground-based images of the COSMOS field. Our sample consists of 8146 galaxies, 5777 of which are detected in the GALEX near-ultraviolet band (2310 \u00c5 or ~1360 \u00c5 rest frame) down to a limiting magnitude of 25.5 (AB), and all of which have a brightness of F814W(HST) < 23 mag and photometric redshifts in the range 0.55 < z < 0.8. We make use of the UV to estimate star formation rates, correcting for the effect of dust using the UV slope, and of the ground-based multiband data to calculate masses. For all galaxies in our sample, we compute, from the ACS F814W images, their concentration (C), asymmetry (A), and clumpiness (S), as well as their Gini coefficient (G) and the second moment of the brightest 20% of their light (M_20). We observe a bimodality in the galaxy population in asymmetry and in clumpiness, although the separation is most evident when either of those parameters is combined with a concentration-like parameter (C, G, or M_20). We further show that this morphological bimodality has a strong correspondence with the FUV-g color bimodality and conclude that UV-optical color predominantly evolves concurrently with morphology. We observe many of the most star-forming galaxies to have morphologies approaching that of early-type galaxies, and we interpret this as evidence that strong starburst events are linked to bulge growth and constitute a process through which galaxies can be brought from the blue to the red sequence while simultaneously modifying their morphology accordingly. We conclude that the red sequence has continued growing at z \u2272 0.7. We also observe z ~ 0.7 galaxies to have physical properties similar to that of local galaxies, except for higher star formation rates. Whence we infer that the dimming of star-forming galaxies is responsible for most of the evolution in star formation rate density since that redshift, although our data are also consistent with a mild number evolution.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "468-493", "id_number": "CaltechAUTHORS:20091113-115202257", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091113-115202257", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-09822" }, { "agency": "NSF", "grant_number": "OISE-0456439" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/516593", "primary_object": { "basename": "ZAMapjss07.pdf", "url": "https://authors.library.caltech.edu/records/xcv6q-j4v13/files/ZAMapjss07.pdf" }, "pub_year": "2007", "author_list": "Zamojski, M. A.; Schiminovich, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/sbv21-73k87", "eprint_id": 18091, "eprint_status": "archive", "datestamp": "2023-08-22 09:47:58", "lastmod": "2024-01-12 23:38:59", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Balam-D", "name": { "family": "Balam", "given": "D." } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "C. J." } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Perrett-K-M", "name": { "family": "Perrett", "given": "K." } }, { "id": "Astier-P", "name": { "family": "Astier", "given": "P." } }, { "id": "Aubourg-\u00c9", "name": { "family": "Aubourg", "given": "\u00c9." } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "R. G." } }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "A." } }, { "id": "Fabbro-S", "name": { "family": "Fabbro", "given": "S." } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "D." } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "J." } }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I." }, "orcid": "0000-0002-2960-978X" }, { "id": "Pain-R", "name": { "family": "Pain", "given": "R." } }, { "id": "Palanque-Delabrouille-N", "name": { "family": "Palanque-Delabrouille", "given": "N." } }, { "id": "Regnault-N", "name": { "family": "Regnault", "given": "N." } }, { "id": "Rich-J", "name": { "family": "Rich", "given": "J." } }, { "id": "Taillet-R", "name": { "family": "Taillet", "given": "R." } }, { "id": "Aldering-G-S", "name": { "family": "Aldering", "given": "G." } }, { "id": "Antilogus-P", "name": { "family": "Antilogus", "given": "P." } }, { "id": "Arsenijevic-V", "name": { "family": "Arsenijevic", "given": "V." } }, { "id": "Balland-C", "name": { "family": "Balland", "given": "C." } }, { "id": "Baumont-S", "name": { "family": "Baumont", "given": "S." } }, { "id": "Bronder-J", "name": { "family": "Bronder", "given": "J." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Filiol-M", "name": { "family": "Filiol", "given": "M." } }, { "id": "Gon\u00e7alves-A-C", "name": { "family": "Gon\u00e7alves", "given": "A. C." } }, { "id": "Hardin-D", "name": { "family": "Hardin", "given": "D." } }, { "id": "Kowalski-M", "name": { "family": "Kowalski", "given": "M." } }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "C." }, "orcid": "0000-0003-1731-0497" }, { "id": "Lusset-V", "name": { "family": "Lusset", "given": "V." } }, { "id": "Mouchet-M", "name": { "family": "Mouchet", "given": "M." } }, { "id": "Mour\u00e3o-A-M", "name": { "family": "Mour\u00e3o", "given": "A." } }, { "id": "Perlmutter-S", "name": { "family": "Perlmutter", "given": "S." } }, { "id": "Ripoche-P", "name": { "family": "Ripoche", "given": "P." } }, { "id": "Schlegel-D-J", "name": { "family": "Schlegel", "given": "D." }, "orcid": "0000-0002-5042-5088" }, { "id": "Tao-C", "name": { "family": "Tao", "given": "C." } } ] }, "title": "The Supernova Type Ia Rate Evolution with SNLS", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; supernovae: general", "note": "\u00a9 2007 American Institute of Physics. \n\nIssue Date: 21 August 2007. \n\nThe authors wish to 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 grateful for our opportunity to conduct observations on this mountain. We acknowledge invaluable assistance from the CFHT Queued Service Observations team, led by P. Martin (CFHT). Our research would not be possible without the assistance of the support staff at CFHT, especially l-C. Cuillandre. The real-time pipelines for supernovae detection run on computers integrated in the CFHT computing system, and are very efficiently installed, maintained and monitored by K. Withington (CFHT). We also heavily rely on the real-time Elixir pipeline which is operated and monitored by l-C. Cuillandre, E. Magnier and K. Withington. We are grateful to L. Simard (CADC) for setting up the image delivery system and his kind and efficient responses to our suggestions for improvements. The Canadian collaboration members acknowledge support from NSERC and CIAR; French collaboration members from CNRS/IN2P3, CNRS/INSU, PNC and CEA. This work was supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the US Department of Energy. The France-Berkeley Fund provided additional collaboration support. We are indebted to A. Hopkins and 1 Beacom for providing us with a draft of their work on SFH prior to its publication. The views expressed in this article are those of the author and do not reflect the official policy or position of the United States Air Force, Department of Defense, or the U.S. Government.\n\nPublished - NEIaipcp07.pdf
", "abstract": "We present a progress report on a project to derive the evolution of the volumetric supernova Type Ia rate from the Supernova Legacy Survey. Our preliminary estimate of the rate evolution divides the sample from Neill et al. into two redshift bins: 0.2 < z < 0.4, and 0.4 < z < 0.6. We extend this by adding a bin from the sample analyzed in Sullivan et al. in the range 0.6 < z < 0.75 from the same time period. We compare the derived trend with previously published rates and a supernova Type Ia production model having two components: one component associated closely with star formation and an additional component associated with host galaxy mass. Our observed trend is consistent with this model, which predicts a rising SN Ia rate out to at least z = 2.", "date": "2007-08-21", "date_type": "published", "publisher": "American Institute of Physics", "id_number": "CaltechAUTHORS:20100430-103548753", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100430-103548753", "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": "Canadian Institute for Advanced Research" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Programme National Galaxies et Cosmologie (PNCG)" }, { "agency": "Commissariat \u00e0 l'\u00c9nergie Atomique (CEA)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "France-Berkeley Fund" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1063/1.2774890", "primary_object": { "basename": "NEIaipcp07.pdf", "url": "https://authors.library.caltech.edu/records/sbv21-73k87/files/NEIaipcp07.pdf" }, "pub_year": "2007", "author_list": "Neill, James D.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/gvtj3-qnk05", "eprint_id": 55875, "eprint_status": "archive", "datestamp": "2023-08-19 20:46:44", "lastmod": "2023-10-20 23:21:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Welsh-B-Y", "name": { "family": "Welsh", "given": "Barry Y." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Wheatley-J-M", "name": { "family": "Wheatley", "given": "Jonathan M." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } } ] }, "title": "A turbulent wake as a tracer of 30,000 years of Mira's mass loss history", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 Macmillan Publishers Limited. \n\nReceived 30 March; accepted 11 June 2007.\n\nWe thank B. Cenko, S. Browne, S. Kulkarni and F. Harrison for assistance in obtaining optical data, and M. Shara and P. Szkody for comments. This work was supported by the National Aeronautics and Space Administration.\n\nSupplemental Material - nature06003-s1.pdf
", "abstract": "Mira is one of the first variable stars ever discovered and it is the prototype (and also the nearest example) of a class of low-to-intermediate-mass stars in the late stages of stellar evolution. These stars are relatively common and they return a large fraction of their original mass to the interstellar medium (ISM) (ref. 2) through a processed, dusty, molecular wind. Thus stars in Mira's stage of evolution have a direct impact on subsequent star and planet formation in their host galaxy. Previously, the only direct observation of the interaction between Mira-type stellar winds and the ISM was in the infrared. Here we report the discovery of an ultraviolet-emitting bow shock and turbulent wake extending over 2 degrees on the sky, arising from Mira's large space velocity and the interaction between its wind and the ISM. The wake is visible only in the far ultraviolet and is consistent with an unusual emission mechanism whereby molecular hydrogen is excited by turbulent mixing of cool molecular gas and shock-heated gas. This wind wake is a tracer of the past 30,000 years of Mira's mass-loss history and provides an excellent laboratory for studying turbulent stellar wind\u2013ISM interactions.", "date": "2007-08-16", "date_type": "published", "publication": "Nature", "volume": "448", "number": "7155", "publisher": "Nature Publishing Group", "pagerange": "780-783", "id_number": "CaltechAUTHORS:20150318-084131649", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150318-084131649", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/nature06003", "primary_object": { "basename": "nature06003-s1.pdf", "url": "https://authors.library.caltech.edu/records/gvtj3-qnk05/files/nature06003-s1.pdf" }, "pub_year": "2007", "author_list": "Martin, D. Christopher; Seibert, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/8bns4-3mv73", "eprint_id": 18017, "eprint_status": "archive", "datestamp": "2023-08-22 09:16:37", "lastmod": "2023-10-20 15:30:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Hudson-M-J", "name": { "family": "Hudson", "given": "Michael J." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "Alex" } } ] }, "title": "The Peculiar Velocities of Local Type Ia Supernovae and Their Impact on Cosmology", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; large-scale structure of universe; supernovae: general", "note": "\u00a9 2007 American Astronomical Society.\n\nReceived 2007 March 5; accepted 2007 April 12; published 2007 May 11.\n\nPublished - NEIapjl07.pdf
", "abstract": "We quantify the effect of Type Ia supernova (SN Ia) peculiar velocities on the derivation of cosmological parameters. The published distant and local SNe Ia used for the Supernova Legacy Survey first-year cosmology report form the sample for this study. While previous work has assumed that the local SNe are at rest in the CMB frame (the no-flow assumption), we test this assumption by applying peculiar velocity corrections to the local SNe using three different flow models. The models are based on the IRAS PSCz galaxy redshift survey, have varying \u03b2 = \u03a9^(0.6)_m/b, and reproduce the Local Group motion in the CMB frame. These data sets are then fit for w, \u03a9_m, and \u03a9_\u039b using flatness or \u039bCDM and a BAO prior, and the \u03c7^2 statistic is used to examine the effect of the velocity corrections on the quality of the fits. The most favored model is the \u03b2 = 0.5 model, which produces a fit significantly better than the no-flow assumption, consistent with previous peculiar velocity studies. By comparing the no-flow assumption with the favored models, we derive the largest potential systematic error in w caused by ignoring peculiar velocities, \u0394w = +0.04. For \u03a9_\u039b the potential error is \u0394\u03a9_\u039b = -0.04, and for \u03a9_m the potential error is \u0394\u03a9_m < +0.01. The favored flow model (\u03b2 = 0.5) produces the following cosmological parameters: w = -1.08^(+0.09)_(-0.08), \u03a9_m = 0.27^(+0.02)_(-0.02) assuming a flat cosmology, and \u03a9_\u039b = 0.80^(0.08)_(-0.07) and \u03a9_m = 0.27^(+0.02)_(-0.02) for a w = -1 (\u039bCDM) cosmology.", "date": "2007-06-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "661", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L123-L126", "id_number": "CaltechAUTHORS:20100419-103646871", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100419-103646871", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/518808", "primary_object": { "basename": "NEIapjl07.pdf", "url": "https://authors.library.caltech.edu/records/8bns4-3mv73/files/NEIapjl07.pdf" }, "pub_year": "2007", "author_list": "Neill, James D.; Hudson, Michael J.; et el." }, { "id": "https://authors.library.caltech.edu/records/6zyf7-2y325", "eprint_id": 16728, "eprint_status": "archive", "datestamp": "2023-08-22 09:05:39", "lastmod": "2023-10-19 22:30:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "Armando" }, "orcid": "0000-0001-6150-2854" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "Samuel" }, "orcid": "0000-0002-9091-2366" }, { "id": "Thilker-D", "name": { "family": "Thilker", "given": "David" } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "Luciana" } }, { "id": "S\u00e1nchez-Contreras-C", "name": { "family": "S\u00e1nchez Contreras", "given": "Carmen" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Timothy M." } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung" } } ] }, "title": "Chemical and Photometric Evolution of Extended Ultraviolet Disks: Optical Spectroscopy of M83 (NGC 5236) and NGC 4625", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : abundances; galaxies : evolution; H ii regions; techniques : spectroscopic; ultraviolet : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 July 28; accepted 2007 February 11.\nGALEX (Galaxy Evolution Explorer) is a NASA Small Explorer,\nlaunched in 2003 April. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with the\nCentre National d'Etudes Spatiales of France and the Korean\nMinistry of Science and Technology. We thank the anonymous\nreferee for his/her constructive comments that have considerably\nimproved the content of the paper. A. G. d. P. is financed by the\nMAGPOP EU Marie Curie Research Training Network and partially\nby the Spanish Programa Nacional de Astronom\u0131\u00b4a y Astrof\u0131sica under grant AYA2003-01676. We thank Judith Cohen\nfor kindly providing her H\u03b1 filter for COSMIC. We are also\nthankful to Sergio Gonzalez and Wojtek Krzeminski for carrying\nout the imaging observations at the Las Campanas 40 inch\ntelescope.\n\n\nFacilities: GALEX, Magellan:Baade (IMACS), Hale (COSMIC),\nSwope (Direct CCD).\n\nPublished - PAZapj07.pdf
", "abstract": "We present the results from the analysis of optical spectra of 31 H\u03b1-selected regions in the extended UV (XUV) disks of M83 (NGC 5236) and NGC 4625 recently discovered by GALEX. The spectra were obtained using IMACS at the Las Campanas Observatory 6.5 m Magellan I telescope and COSMIC at the Palomar 200 inch (5 m) telescope, respectively, for M83 and NGC 4625. The line ratios measured indicate nebular oxygen abundances (derived from the R23 parameter) of the order of Z_\u2299/5-Z_\u2299/10. For most emission-line regions analyzed the line fluxes and ratios measured are best reproduced by models of photoionization by single stars with masses in the range 20-40 M_\u2299 and oxygen abundances comparable to those derived from the R23 parameter. We find indications for a relatively high N/O abundance ratio in the XUV disk of M83. Although the metallicities derived imply that these are not the first stars formed in the XUV disks, such a level of enrichment could be reached in young spiral disks only 1 Gyr after these first stars would have formed. The amount of gas in the XUV disks allows maintaining the current level of star formation for at least a few Gyr.", "date": "2007-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "661", "number": "1", "publisher": "American Astronomical Society", "pagerange": "115-134", "id_number": "CaltechAUTHORS:20091117-105737404", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-105737404", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship" }, { "agency": "Programa Nacional de Astronom\u00eda y Astrof\u0131sica", "grant_number": "AYA2003-01676" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/513730", "primary_object": { "basename": "PAZapj07.pdf", "url": "https://authors.library.caltech.edu/records/6zyf7-2y325/files/PAZapj07.pdf" }, "pub_year": "2007", "author_list": "Gil de Paz, Armando; Madore, Barry F.; et el." }, { "id": "https://authors.library.caltech.edu/records/0zs77-rwq98", "eprint_id": 11402, "eprint_status": "archive", "datestamp": "2023-08-22 09:00:25", "lastmod": "2023-10-16 23:46:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Noeske-K-G", "name": { "family": "Noeske", "given": "K. G." } }, { "id": "Weiner-B-J", "name": { "family": "Weiner", "given": "B. J." } }, { "id": "Faber-S-M", "name": { "family": "Faber", "given": "S. M." }, "orcid": "0000-0003-4996-214X" }, { "id": "Papovich-C", "name": { "family": "Papovich", "given": "C." }, "orcid": "0000-0001-7503-8482" }, { "id": "Koo-David-C", "name": { "family": "Koo", "given": "D. C." }, "orcid": "0000-0003-3385-6799" }, { "id": "Somerville-R-S", "name": { "family": "Somerville", "given": "R. S." } }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "K." }, "orcid": "0000-0001-9742-3138" }, { "id": "Conselice-C-J", "name": { "family": "Conselice", "given": "C. J." }, "orcid": "0000-0003-1949-7638" }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "J. A." }, "orcid": "0000-0001-8684-2222" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "A. L." } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Lotz-J-M", "name": { "family": "Lotz", "given": "J. M." }, "orcid": "0000-0003-3130-5643" }, { "id": "Primack-J-R", "name": { "family": "Primack", "given": "J. R." }, "orcid": "0000-0001-5091-5098" }, { "id": "Barmby-P", "name": { "family": "Barmby", "given": "P." }, "orcid": "0000-0003-2767-0090" }, { "id": "Cooper-M-C", "name": { "family": "Cooper", "given": "M. C." }, "orcid": "0000-0003-1371-6019" }, { "id": "Davis-M-E-Astro", "name": { "family": "Davis", "given": "M." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Guhathakurta-P", "name": { "family": "Guhathakurta", "given": "P." }, "orcid": "0000-0001-8867-4234" }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J." } }, { "id": "Kassin-S-A", "name": { "family": "Kassin", "given": "S. A." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Phillips-A-C", "name": { "family": "Phillips", "given": "A. C." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "T. A." } }, { "id": "Willmer-C-N-A", "name": { "family": "Willmer", "given": "C. N. A." } }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" } ] }, "title": "Star Formation in AEGIS Field Galaxies since z = 1.1: The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galactic evolution; galaxy formation; high-redshift galaxies; starburst", "note": "\u00a9 2007. The American Astronomical Society. \n\nReceived 2006 June 4; accepted 2007 January 31; published 2007 April 2. \n\nSee the survey summary Letter (Davis et al. 2007) for full acknowledgments. This work is based on observations with the W.M. Keck Telescope, the Hubble Space Telescope, the Galaxy Evolution Explorer, the Canada-France-Hawaii Telescope, and the Palomar Observatory, and was supported by NASA and NSF grants. We wish to recognize the cultural role that the summit of Mauna Kea has within the Hawaiian community. 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. Support for this work was provided by NASA through contract numbers 1256790, 960785, and 1255094 issued by JPL/Caltech. We wish to thank the referee for very valuable comments, and D. Elbaz and J. Lee for helpful discussions. K.G.N. acknowledges support from the Aspen Center for Physics. \n\n[J.A.N. and A.L.C. were] Hubble Fellow[s]. \n\n[J.M.L. was a] Leo Goldberg Fellow, National Optical Astronomy Observatory.\n\nPublished - NOEapjl07a.pdf
", "abstract": "We analyze star formation (SF) as a function of stellar mass (M\u2609) and redshift z in the All-Wavelength Extended Groth Strip International Survey. For 2905 field galaxies, complete to 10^10(10^10.8 )M at z < 0.7(1), with Keck\nspectroscopic redshifts out to z = 1.1, we compile SF rates (SFRs) from emission lines, GALEX, and Spitzer MIPS 24 \u00b5m photometry, optical-NIR M* measurements, and HST morphologies. Galaxies with reliable signs of SF form a distinct \"main sequence\" (MS), with a limited range of SFRs at a given M* and z (1 \u03c3 \u227e \u00b10.3 dex), and log (SFR) approximately proportional to log M*. The range of log (SFR) remains constant to z > 1, while the MS as a whole moves to higher SFR as z increases. The range of the SFR along the MS constrains the amplitude of episodic variations of SF and the effect of mergers on the SFR. Typical galaxies spend \u223c67%(95%) of their lifetime since z = 1 within a factor of \u227e2(4) of their average SFR at a given M* and z. The dominant mode of the evolution of SF since z \u223c 1 is apparently a gradual decline of the average SFR in most individual galaxies, not a decreasing frequency of starburst episodes, or a decreasing factor by which SFRs are enhanced in starbursts. LIRGs at z \u223c 1 seem to mostly reflect the high SFR typical for massive galaxies at that epoch. The smooth MS may reflect that the same set of few physical processes governs SF prior to additional quenching processes. A gradual process like gas exhaustion may play a dominant role.", "date": "2007-05-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "660", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L43-L46", "id_number": "CaltechAUTHORS:NOEapjl07a", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:NOEapjl07a", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1256790" }, { "agency": "NASA", "grant_number": "960785," }, { "agency": "NASA", "grant_number": "1255094" }, { "agency": "NSF" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "National Optical Astronomy Observatory (NOAO)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/517926", "primary_object": { "basename": "NOEapjl07a.pdf", "url": "https://authors.library.caltech.edu/records/0zs77-rwq98/files/NOEapjl07a.pdf" }, "pub_year": "2007", "author_list": "Noeske, K. G.; Weiner, B. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/2f3e3-wjh52", "eprint_id": 16631, "eprint_status": "archive", "datestamp": "2023-08-22 09:01:04", "lastmod": "2023-10-19 22:26:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Davis-M-E-Astro", "name": { "family": "Davis", "given": "M." } }, { "id": "Guhathakurta-P", "name": { "family": "Guhathakurta", "given": "P." }, "orcid": "0000-0001-8867-4234" }, { "id": "Konidaris-N-P", "name": { "family": "Konidaris", "given": "N. P." }, "orcid": "0000-0003-1905-2815" }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "J. A." }, "orcid": "0000-0001-8684-2222" }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Biggs-A-D", "name": { "family": "Biggs", "given": "A. D." }, "orcid": "0000-0002-1117-9961" }, { "id": "Barmby-P", "name": { "family": "Barmby", "given": "P." }, "orcid": "0000-0003-2767-0090" }, { "id": "Bundy-K-A", "name": { "family": "Bundy", "given": "K." }, "orcid": "0000-0001-9742-3138" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "A. L." } }, { "id": "Conselice-C-J", "name": { "family": "Conselice", "given": "C. J." }, "orcid": "0000-0003-1949-7638" }, { "id": "Cooper-M-C", "name": { "family": "Cooper", "given": "M. C." }, "orcid": "0000-0003-1371-6019" }, { "id": "Croton-D-J", "name": { "family": "Croton", "given": "D. J." }, "orcid": "0000-0002-5009-512X" }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "P. R. M." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Faber-S-M", "name": { "family": "Faber", "given": "S. M." }, "orcid": "0000-0003-4996-214X" }, { "id": "Fang-T", "name": { "family": "Fang", "given": "T." } }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Georgakakis-A", "name": { "family": "Georgakakis", "given": "A." } }, { "id": "Gerke-B-F", "name": { "family": "Gerke", "given": "B. F." } }, { "id": "Goss-W-M", "name": { "family": "Goss", "given": "W. M." } }, { "id": "Gwyn-S-D-J", "name": { "family": "Gwyn", "given": "S." }, "orcid": "0000-0001-8221-8406" }, { "id": "Harker-J", "name": { "family": "Harker", "given": "J." } }, { "id": "Hopkins-A-M", "name": { "family": "Hopkins", "given": "A. M." }, "orcid": "0000-0002-6097-2747" }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Kassin-S-A", "name": { "family": "Kassin", "given": "S. A." } }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "E. N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Koo-David-C", "name": { "family": "Koo", "given": "D. C." }, "orcid": "0000-0003-3385-6799" }, { "id": "Laird-E-S", "name": { "family": "Laird", "given": "E. S." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lin-Lin", "name": { "family": "Lin", "given": "L." }, "orcid": "0000-0001-6860-9566" }, { "id": "Lotz-J-M", "name": { "family": "Lotz", "given": "J. M." }, "orcid": "0000-0003-3130-5643" }, { "id": "Marshall-P-J", "name": { "family": "Marshall", "given": "P. J." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Metevier-A-J", "name": { "family": "Metevier", "given": "A. J." } }, { "id": "Moustakas-L-A", "name": { "family": "Moustakas", "given": "L. A." }, "orcid": "0000-0003-3030-2360" }, { "id": "Nandra-K", "name": { "family": "Nandra", "given": "K." }, "orcid": "0000-0002-7150-9192" }, { "id": "Noeske-K-G", "name": { "family": "Noeske", "given": "K. G." } }, { "id": "Papovich-C", "name": { "family": "Papovich", "given": "C." }, "orcid": "0000-0001-7503-8482" }, { "id": "Phillips-A-C", "name": { "family": "Phillips", "given": "A. C." } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. M." }, "orcid": "0000-0003-0427-8387" }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Salim-S", "name": { "family": "Salim", "given": "S." }, "orcid": "0000-0003-2342-7501" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Simard-L", "name": { "family": "Simard", "given": "L." } }, { "id": "Smail-Ian-R", "name": { "family": "Smail", "given": "I." }, "orcid": "0000-0003-3037-257X" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "T. A." } }, { "id": "Weiner-B-J", "name": { "family": "Weiner", "given": "B. J." } }, { "id": "Willmer-C-N-A", "name": { "family": "Willmer", "given": "C. N. A." } }, { "id": "Willner-S-P", "name": { "family": "Willner", "given": "S. P." }, "orcid": "0000-0002-9895-5758" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "E. L." }, "orcid": "0000-0001-5058-1593" }, { "id": "Yan-Renbin", "name": { "family": "Yan", "given": "R." } } ] }, "title": "The All-Wavelength Extended Groth Strip International Survey (AEGIS) Data Sets", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: photometry; infrared: galaxies; radio continuum: galaxies; surveys; ultraviolet: galaxies; X-rays: galaxies", "note": "\u00a9 2007 American Astronomical Sociey. \n\nReceived 2006 June 23, accepted for publication 2007 March 8.\nPublished 2007 April 13. \n\nThis research has made use of NASA's Astrophysics Data System Bibliographic Services. The authors wish to 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. A. L. C. and J. A. N. are supported by NASA through Hubble fellowship grants HF-01182 and HF-01165 awarded by STScI, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. J. M. L. acknowledges support from the NOAO Leo Goldberg Fellowship, NASA/STScI grants GO-10134 and AR-10675, NASA NAG5-11513 grant to P. Madau, and a Calspace grant to D. C. Koo. L. A. M.'s work was carried out at JPL/Caltech, under a contract with NASA. S. A. K. would like to thank Eddie Bergeron for assistance with reducing and calibrating the NICMOS data.\n\nPublished - DAVapjl07a.pdf
", "abstract": "In this the first of a series of Letters, we present a panchromatic data set in the Extended Groth Strip region of the sky. Our survey, the All-Wavelength Extended Groth Strip International Survey (AEGIS), aims to study the physical properties and evolutionary processes of galaxies at z ~ 1. It includes the following deep, wide-field imaging data sets: Chandra/ACIS X-ray, GALEX ultraviolet, CFHT/MegaCam Legacy Survey optical, CFHT/CFH12K optical, Hubble Space Telescope/ACS optical and NICMOS near-infrared, Palomar/WIRC near-infrared, Spitzer/IRAC mid-infrared, Spitzer/MIPS far-infrared, and VLA radio continuum. In addition, this region of the sky has been targeted for extensive spectroscopy using the Deep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II 10 m telescope. Our survey is compared to other large multiwavelength surveys in terms of depth and sky coverage.", "date": "2007-05-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "660", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L1-L6", "id_number": "CaltechAUTHORS:20091109-151802988", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091109-151802988", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HF-01182" }, { "agency": "NASA", "grant_number": "HF-01165" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "NASA", "grant_number": "GO-10134" }, { "agency": "NASA", "grant_number": "AR-10675" }, { "agency": "NASA", "grant_number": "NAG5-11513" }, { "agency": "California Space Grant Consortium" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/517931", "primary_object": { "basename": "DAVapjl07a.pdf", "url": "https://authors.library.caltech.edu/records/2f3e3-wjh52/files/DAVapjl07a.pdf" }, "pub_year": "2007", "author_list": "Davis, M.; Guhathakurta, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/g573c-x9x65", "eprint_id": 17386, "eprint_status": "archive", "datestamp": "2023-08-22 08:25:15", "lastmod": "2023-10-23 19:33:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "A." }, "orcid": "0000-0001-6150-2854" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Hanson-H-M", "name": { "family": "Hanson", "given": "H. M." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Bianchi-L", "name": { "family": "Bianchi", "given": "L." } }, { "id": "Block-M", "name": { "family": "Block", "given": "M." } }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "S." }, "orcid": "0000-0002-9091-2366" }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Cannon-J-M", "name": { "family": "Cannon", "given": "J. M." } }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "C." }, "orcid": "0000-0003-2685-4488" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "A." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "M. J." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "M. W." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Sosey-M-L", "name": { "family": "Sosey", "given": "M. L." } }, { "id": "Thilker-D-A", "name": { "family": "Thilker", "given": "D. A." }, "orcid": "0000-0002-8528-7340" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" } ] }, "title": "An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: photometry; infrared: galaxies; infrared: ISM; ultraviolet: galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 September 25; accepted 2006 October 20.\nSupport for this work, part of the Spitzer Space Telescope Legacy\nScience Program, was provided by NASA through contract\n1224769 issued by the Jet Propulsion Laboratory, California\nInstitute of Technology under NASA contract 1407. A. G. d. P. is\nfinanced by the MAGPOP EU Marie Curie Research Training\nNetwork and the Spanish Programa Nacional de Astronom\u0131a y\nAstrof\u0131sica under grant AYA2003-01676. We are thankful for\nthe hard work put in by the instrument teams and the Spitzer\nScience Center. We gratefully acknowledge NASA's support for\nconstruction, operation, and science analysis for the GALEX mission,\ndeveloped in cooperation with the Centre National d'Etudes\nSpatiales of France and the Korean Ministry of Science and Technology.\nThis research has made use of the NASA/IPAC Extragalactic\nDatabase, which is operated by JPL/Caltech, under\ncontract with NASA. This publication makes use of data products\nfrom the Two Micron All Sky Survey, which is a joint project\nof the University of Massachusetts and IPAC/Caltech, funded\nby NASA and the National Science Foundation.\n\nErratum: \"An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies\" (ApJ, 655, 863 [2007])\nD. A. Dale et al. 2008 ApJ 672 735 doi:10.1086/523847\n\nPublished - DALapj07.pdf
Erratum - 0004-637X_672_1_735.pdf
", "abstract": "The ultraviolet-to-radio continuum spectral energy distributions are presented for all 75 galaxies in the Spitzer Infrared Nearby Galaxies Survey (SINGS). A principal component analysis of the sample shows that most of the sample's spectral variations stem from two underlying components, one representative of a galaxy with a low infrared-to-ultraviolet ratio and one representative of a galaxy with a high infrared-to-ultraviolet ratio. The influence of several parameters on the infrared-to-ultraviolet ratio is studied (e.g., optical morphology, disk inclination, far-infrared color, ultraviolet spectral slope, and star formation history). Consistent with our understanding of normal star-forming galaxies, the SINGS sample of galaxies in comparison to more actively star-forming galaxies exhibits a larger dispersion in the infrared-to-ultraviolet versus ultraviolet spectral slope correlation. Early-type galaxies, exhibiting low star formation rates and high optical surface brightnesses, have the most discrepant infrared-to-ultraviolet correlation. These results suggest that the star formation history may be the dominant regulator of the broadband spectral variations between galaxies. Finally, a new discovery shows that the 24 \u03bcm morphology can be a useful tool for parameterizing the global dust temperature and ultraviolet extinction in nearby galaxies. The dust emission in dwarf/irregular galaxies is clumpy and warm accompanied by low ultraviolet extinction, while in spiral galaxies there is typically a much larger diffuse component of cooler dust and average ultraviolet extinction. For galaxies with nuclear 24 \u03bcm emission, the dust temperature and ultraviolet extinction are relatively high compared to disk galaxies.", "date": "2007-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "655", "number": "2", "publisher": "American Astronomical Society", "pagerange": "863-884", "id_number": "CaltechAUTHORS:20100204-095108624", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100204-095108624", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Programa Nacional de Astronom\u0131a y Astrof\u0131sica", "grant_number": "AYA2003-01676" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/510362", "primary_object": { "basename": "0004-637X_672_1_735.pdf", "url": "https://authors.library.caltech.edu/records/g573c-x9x65/files/0004-637X_672_1_735.pdf" }, "related_objects": [ { "basename": "DALapj07.pdf", "url": "https://authors.library.caltech.edu/records/g573c-x9x65/files/DALapj07.pdf" } ], "pub_year": "2007", "author_list": "Dale, D. A.; Gil de Paz, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/fyxa2-mre93", "eprint_id": 75881, "eprint_status": "archive", "datestamp": "2023-08-22 08:02:47", "lastmod": "2023-10-25 15:23:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Beers-T-C", "name": { "family": "Beers", "given": "Timothy C." }, "orcid": "0000-0003-4573-6233" }, { "id": "Flynn-C", "name": { "family": "Flynn", "given": "Chris" } }, { "id": "Rossi-S", "name": { "family": "Rossi", "given": "Silvia" } }, { "id": "Sommer-Larsen-J", "name": { "family": "Sommer-Larsen", "given": "Jesper" } }, { "id": "Wilhelm-R", "name": { "family": "Wilhelm", "given": "Ronald" } }, { "id": "Marsteller-B", "name": { "family": "Marsteller", "given": "Brian" } }, { "id": "Lee-Young-Sun", "name": { "family": "Lee", "given": "Young Sun" } }, { "id": "De-Lee-N", "name": { "family": "De Lee", "given": "Nathan" }, "orcid": "0000-0002-3657-0705" }, { "id": "Krugler-J", "name": { "family": "Krugler", "given": "Julie" } }, { "id": "Deliyannis-C-P", "name": { "family": "Deliyannis", "given": "Constantine P." } }, { "id": "Simmons-A-T", "name": { "family": "Simmons", "given": "Andrew T." } }, { "id": "Mills-E", "name": { "family": "Mills", "given": "Elisabeth" } }, { "id": "Zickgraf-F-J", "name": { "family": "Zickgraf", "given": "Franz-Josef" } }, { "id": "Holmberg-J", "name": { "family": "Holmberg", "given": "Johan" } }, { "id": "\u00d6nehag-A", "name": { "family": "\u00d6nehag", "given": "Anna" } }, { "id": "Eriksson-A", "name": { "family": "Eriksson", "given": "Anders" } }, { "id": "Terndrup-D-M", "name": { "family": "Terndrup", "given": "Donald M." } }, { "id": "Salim-S", "name": { "family": "Salim", "given": "Samir" }, "orcid": "0000-0003-2342-7501" }, { "id": "Andersen-J", "name": { "family": "Andersen", "given": "Johannes" } }, { "id": "Nordstr\u00f6m-B", "name": { "family": "Nordstr\u00f6m", "given": "Birgitta" } }, { "id": "Frebel-A", "name": { "family": "Frebel", "given": "Anna" }, "orcid": "0000-0002-2139-7145" }, { "id": "Rhee-Jaehyon", "name": { "family": "Rhee", "given": "Jaehyon" } } ] }, "title": "Broadband UBVR_CI_C photometry of horizontal-branch and metal-poor candidates from the HK and Hamburg/ESO surveys. I", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: early-type; stars: horizontal-branch; stars: Population II; techniques: photometric", "note": "\u00a9 2007. The American Astronomical Society. \n\nReceived 2006 July 28; accepted 2006 September 13. \n\nWe are thankful to the ESO/Danish 1.5 m, WIYN 0.9 m, NOAO, and MDM time assignment committees for awards of the significant amounts of telescope time required for this project, and for the patience to await the results. We are also grateful for the excellent support that we received at the telescopes.\n\n T. C. B., Y. L., B. M., and N. D. acknowledge partial support from grants AST 00-98508, AST 00-98549, AST 02-05815, AST 04-06784, and PHY 02-16783, Physics Frontier Centers/JINA: Joint Institute for Nuclear Astrophysics, awarded by the US National Science Foundation. J. K. acknowledges partial support from the Honors College at Michigan State University, in the form of a Professorial Assistantship. C. F. acknowledges partial support from the Danish National Research Foundation and the Carlberg Foundation. S. R. acknowledges partial support from the Brazilian institutions FAPESP, CNPq, and Capes. C. P. D. acknowledges partial support from grant AST 02-06202, awarded by the US National Science Foundation. D. T. and S. S. acknowledge partial support from grant AST 02-05789, awarded by the US National Science Foundation, and from the Ohio State Program for the Enhancement of Graduate Studies (PEGS). J. A. and B. N. thank the Carlsberg Foundation and the Swedish and Danish Natural Science Research Councils for partial financial support of this work. N. C. acknowledges partial support from the Deutsche Forschungsgemeinschaft through grants Ch 214/3 and Re 353/44. N. C. is a research fellow of the Royal Swedish Academy of Sciences supported by a grant from the Knut and Alice Wallenberg Foundation. A. F. acknowledges partial support from grant DP0342613, awarded by the Australian Research Council.\n\nPublished - pdf.pdf
", "abstract": "We report broadband UBV and/or BVR_CI_C CCD photometry for a total of 1857 stars in the thick-disk and halo populations of the Galaxy. The majority of our targets were selected as candidate field horizontal-branch or other A-type stars (FHB/A, N = 576), or candidate low-metallicity stars (N = 1221), from the HK and Hamburg/ESO objective-prism surveys. Similar data for a small number of additional stars from other samples are also reported. These data are being used for several purposes. In the case of the FHB/A candidates they are used to accurately separate the lower gravity FHB stars from various higher gravity A-type stars, a subsample that includes the so-called blue metal poor stars, halo and thick-disk blue stragglers, main-sequence A-type dwarfs, and Am and Ap stars. These data are also being used to derive photometric distance estimates to high-velocity hydrogen clouds in the Galaxy and for improved measurements of the mass of the Galaxy. Photometric data for the metal-poor candidates are being used to refine estimates of stellar metallicity for objects with available medium-resolution spectroscopy, to obtain distance estimates for kinematic analyses, and to establish initial estimates of effective temperature for analysis of high-resolution spectroscopy of the stars for which this information now exists.", "date": "2007-01", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "168", "number": "1", "publisher": "American Astronomical Society", "pagerange": "128-139", "id_number": "CaltechAUTHORS:20170408-134142943", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-134142943", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 00-98508" }, { "agency": "NSF", "grant_number": "AST 00-98549" }, { "agency": "NASA", "grant_number": "AST 02-05815" }, { "agency": "NSF", "grant_number": "AST 04-06784" }, { "agency": "NSF", "grant_number": "PHY 02-16783" }, { "agency": "Michigan State University" }, { "agency": "Danish National Research Foundation" }, { "agency": "Carlsberg Foundation" }, { "agency": "Funda\u00e7\u00e3o de Amparo \u00e0 Pesquisa do Estado de S\u00e3o Paulo (FAPESP)" }, { "agency": "Conselho Nacional de Desenvolvimento Cient\u00edfico e Tecnol\u00f3gico (CNPq)" }, { "agency": "Coordena\u00e7\u00e3o de Aperfei\u00e7oamento de Pessoal de N\u00edvel Superior (CAPES)" }, { "agency": "NSF", "grant_number": "AST 02-06202" }, { "agency": "NSF", "grant_number": "AST 02-05789" }, { "agency": "Ohio State Program for the Enhancement of Graduate Studies (PEGS)" }, { "agency": "Swedish Natural Science Research Council" }, { "agency": "Danish Natural Science Research Council" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Ch 214/3" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Re 353/44" }, { "agency": "Royal Swedish Academy of Sciences" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Australian Research Council", "grant_number": "DP0342613" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/509324", "primary_object": { "basename": "pdf.pdf", "url": "https://authors.library.caltech.edu/records/fyxa2-mre93/files/pdf.pdf" }, "pub_year": "2007", "author_list": "Beers, Timothy C.; Flynn, Chris; et el." }, { "id": "https://authors.library.caltech.edu/records/t07nv-vw254", "eprint_id": 13695, "eprint_status": "archive", "datestamp": "2023-08-22 07:48:55", "lastmod": "2023-10-18 00:05:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "B." } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Halpern-J-P", "name": { "family": "Halpern", "given": "J. P." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P." }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "S. G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } } ] }, "title": "Ultraviolet detection of the tidal disruption of a star by a supermassive black hole", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: nuclei; ultraviolet: galaxies", "note": "\u00a9 2006 The American Astronomical Society.\nReceived 2006 August 24; accepted 2006 October 6; published 2006 December 1.\nWe thank the anonymous referee for helpful comments, including\nthe suggestion to add a discussion of the radius of the\nflare emission. We thank C. L. Slesnick for carrying out our\ntarget-of-opportunity observation with the Double Spectrograph\non the Palomar 200 inch telescope, V. Villar for the two dimensional\nbulge/disk composition of the AEGIS HST ACS\nimage, and S. M. Moran for measurement of the stellar velocity\ndispersion of the AEGIS DEEP2 DEIMOS spectrum. S. G. was\nsupported in part by the Volontariat International-CNES of\nFrance, and through Chandra Grant Award G06-7099X issued\nby the Chandra X-ray Observatory, which is operated by the\nSAO for and on behalf of NASA. We gratefully acknowledge\nNASA's support for construction, operation, and science analysis\nfor the GALEX mission, developed in cooperation with\nCNES and the Korean Ministry of Science and Technology.\nThe AEGIS collaboration acknowledges support from the\nNASA/ESA HST grant GO-10134 for the Extended Groth Strip\nobservations, obtained at STScI, which is operated by AURA,\nInc., under a NASA contract. The AEGIS collaboration also\nacknowledges support from the NSF grant AST 05-07483 for\nthe DEEP2 survey observations with DEIMOS at the W. M.\nKeck Observatory. This work is based on observations obtained\nwith MegaPrime/MegaCam, a joint project of CFHT and CEA/\nDAPNIA, at the CFHT which is operated by the NRC of Canada,\nthe CNRS of France, and the University of Hawaii. This\nwork is also based in part on data products produced at TERAPIX\nand the Canadian Astronomy Data Centre as part of the\nCFHT Legacy Survey, a collaborative project of NRC and\nCNRS.\n\nPublished - GEZapjl06.pdf
", "abstract": "A supermassive black hole in the nucleus of a galaxy will be revealed when a star passes close enough to be torn apart by tidal forces and a flare of radiation is emitted by the stream of stellar debris that plunges into the black hole. Since common active galactic nuclei have accreting black holes that can also produce flares, a convincing demonstration that a stellar tidal disruption has occurred generally begins with a \"normal\" galaxy that has no evidence of prior nuclear activity. Here we,report a luminous UV flare from an elliptical galaxy at z=0.37 in the Groth field of the GALEX Deep Imaging Survey that has no evidence of a Seyfert nucleus from optical spectroscopy and X-ray imaging obtained during the flare. Multiwavelength data collected at the time of the event, and for 2 years following, allow us to constrain, for the first time, the spectral energy distribution of a candidate tidal disruption flare from optical through X-rays. The luminosity and temperature of the radiation and the decay curve of the flare are in excellent agreement with theoretical predictions for the tidal disruption of a star, and provide the strongest empirical evidence for a stellar disruption event to date.", "date": "2006-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "653", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L25-L28", "id_number": "CaltechAUTHORS:GEZapjl06", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:GEZapjl06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/European Space Agency Hubble Space Telescope", "grant_number": "GO-10134" }, { "agency": "NSF", "grant_number": "AST 05-07483" }, { "agency": "Chandra grant award", "grant_number": "G06-7099X" }, { "agency": "Volontariat International-CNES" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/509918", "primary_object": { "basename": "GEZapjl06.pdf", "url": "https://authors.library.caltech.edu/records/t07nv-vw254/files/GEZapjl06.pdf" }, "pub_year": "2006", "author_list": "Gezari, S.; Martin, D. C.; et el." }, { "id": "https://authors.library.caltech.edu/records/cfvmq-n3728", "eprint_id": 22349, "eprint_status": "archive", "datestamp": "2023-08-22 07:12:33", "lastmod": "2023-10-23 15:52:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Boissier-S", "name": { "family": "Boissier", "given": "S." }, "orcid": "0000-0002-9091-2366" }, { "id": "Cortese-L", "name": { "family": "Cortese", "given": "L." }, "orcid": "0000-0002-7422-9823" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "A." }, "orcid": "0000-0001-6150-2854" }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" } ] }, "title": "The fate of spiral galaxies in clusters: The star formation history of the anemic Virgo cluster galaxy NGC 4569", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (Virgo); galaxies: individual (NGC 4569-M90); galaxies: interactions; ultraviolet: galaxies", "note": "\u00a9 2006 The American Astronomical Society. Received 2006 June 8; accepted 2006 July 13. \nGALEX is a NASA Small Explorer, launched in 2003 April.\nWe gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales (CNES) of France and the Korean Ministry of Science and Technology.\nWe thank G. Gavazzi and N. Prantzos for their long-term\ncollaboration in the subjects studied in this paper. S. B. thanks the CNES for its funding through GALEX-Marseille. We wish to thank B. Vollmer and J. Kenney for their valuable comments, and the GALEX SODA team for their help with the data reduction.\n\nPublished - BOSapj06.pdf
", "abstract": "We present a new method for studying the star formation history of late-type cluster galaxies undergoing gas starvation or a ram pressure stripping event by combining bidimensional multifrequency observations with multizone models of galactic chemical and spectrophotometric evolution. This method is applied to the Virgo Cluster anemic galaxy NGC 4569. We extract radial profiles from recently obtained UV GALEX images at 1530 and 2310 \u00c5, from visible and near-IR narrow (H\u03b1) and broadband images at different wavelengths (u, B, g, V, r, i, z, J, H, and K), from Spitzer IRAC and MIPS images, and from atomic and molecular gas maps. The model in the absence of interaction (characterized by its rotation velocity and spin parameter) is constrained by the unperturbed H-band light profile and by the H\u03b1 rotation curve. We can reconstruct the observed total gas radial density profile and the light surface brightness profiles at all wavelengths in a ram pressure stripping scenario by making simple assumptions about the gas removal process and the orbit of NGC 4569 inside the cluster. The observed profiles cannot be reproduced by simply stopping gas infall, thus mimicking starvation. Gas removal is required, which is more efficient in the outer disk, inducing radial quenching in the star formation activity, as observed and reproduced by the model. This observational result, consistent with theoretical predictions that a galaxy cluster-IGM interaction is able to modify structural disk parameters without gravitational perturbations, is discussed in the framework of the origin of lenticular galaxies in clusters", "date": "2006-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "651", "number": "2", "publisher": "American Astronomical Society", "pagerange": "811-821", "id_number": "CaltechAUTHORS:20110217-101826211", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110217-101826211", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/507766", "primary_object": { "basename": "BOSapj06.pdf", "url": "https://authors.library.caltech.edu/records/cfvmq-n3728/files/BOSapj06.pdf" }, "pub_year": "2006", "author_list": "Boselli, A.; Boissier, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/5y2z8-chj48", "eprint_id": 22464, "eprint_status": "archive", "datestamp": "2023-08-22 06:53:48", "lastmod": "2023-10-23 16:03:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Conley-A-J", "name": { "family": "Conley", "given": "A." } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Howes-A", "name": { "family": "Howes", "given": "A." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Astier-P", "name": { "family": "Astier", "given": "P." } }, { "id": "Balam-D", "name": { "family": "Balam", "given": "D." } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "R. G." } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "D." } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "J." } }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I." }, "orcid": "0000-0002-2960-978X" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Pain-R", "name": { "family": "Pain", "given": "R." } }, { "id": "Perrett-K-M", "name": { "family": "Perrett", "given": "K." } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "C. J." } }, { "id": "Regnault-N", "name": { "family": "Regnault", "given": "N." } }, { "id": "Rich-J-A", "name": { "family": "Rich", "given": "J. A." }, "orcid": "0000-0002-5807-5078" }, { "id": "Taillet-R", "name": { "family": "Taillet", "given": "R." } }, { "id": "Aubourg-\u00c9", "name": { "family": "Aubourg", "given": "\u00c9." } }, { "id": "Bronder-J", "name": { "family": "Bronder", "given": "J." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Fabbro-S", "name": { "family": "Fabbro", "given": "S." } }, { "id": "Filiol-M", "name": { "family": "Filiol", "given": "M." } }, { "id": "Le-Borgne-D", "name": { "family": "Le Borgne", "given": "D." } }, { "id": "Palanque-Delabrouille-N", "name": { "family": "Palanque-Delabrouille", "given": "N." } }, { "id": "Perlmutter-S", "name": { "family": "Perlmutter", "given": "S." } }, { "id": "Ripoche-P", "name": { "family": "Ripoche", "given": "P." } } ] }, "title": "The Rise Time of Type Ia Supernovae from the Supernova Legacy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology : observations; supernovae : general", "note": "\u00a9 2006 The American Astronomical Society. Received 2006 March 28; accepted 2006 July 16. \nBased on observations obtained with MegaPrime/MegaCam, a joint project\nof the Canada-France-Hawaii Telescope (CFHT) and CEA/DAPNIA, at CFHT,\nwhich is operated by the National Research Council (NRC) of Canada, the Institut\nNational des Sciences de l'Univers of the Centre National de la Recherche Scientifique\n(CNRS) of France, and the University of Hawaii. This work is based in\npart on data products produced at the Canadian Astronomy Data Centre as part of\nthe CFHT Legacy Survey, a collaborative project of NRC and CNRS.\n\nThe authors would like to recognize the very significant cultural role and reverence that the summit of Mauna Kea has within the indigenous community of Hawai'i. We are grateful for our opportunity\nto conduct observations from this mountain. We would\nalso like to thank Peter Nugent and Peter H\u00f6flich for useful discussions. We gratefully acknowledge the assistance of Pierre Martin and the CFHT Queued Service Observations team. Jean-Charles Cuillandre and Kanoa Washington were particularly indispensable in making possible real-time data reduction at CFHT. Canadian collaboration members acknowledge support from NSERC and CIAR; French members from CNRS/IN2P3, CNRS/INSU, and CEA. This research has 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. The views expressed in this article are those of the authors and do not reflect the official position of the United States Air Force, Department of Defense, or US Government.\n\nPublished - CONaj06.pdf
", "abstract": "We compare the rise times of nearby and distant Type Ia supernovae (SNe Ia) as a test for evolution using 73 high-redshift spectroscopically confirmed SNe Ia from the first 2 years of the 5 year Supernova Legacy Survey (SNLS) and published observations of nearby SNe. Because of the \"rolling\" search nature of the SNLS, our measurement is\napproximately 6 times more precise than previous studies, allowing for a more sensitive test of evolution between nearby and distant SNe. Adopting a simple t(2) early-time model (as in previous studies), we find that the rest-frame B rise times for a fiducial SN Ia at high and low redshift are consistent, with values 19.10_(-0.17)^(+0.18) (stat) \u00b1\n0.2(syst) and 19.58_(-0.19)^(+0.22) days, respectively; the statistical significance of this difference is only 1.4 \u03c3. The errors represent the uncertainty in the mean rather than any variation between individual SNe. We also compare subsets of our high-redshift data set based on decline rate, host galaxy star formation rate, and redshift,\nfinding no substantive evidence for any subsample dependence.", "date": "2006-10", "date_type": "published", "publication": "Astronomical Journal", "volume": "132", "number": "4", "publisher": "American Astronomical Society", "pagerange": "1707-1713", "id_number": "CaltechAUTHORS:20110224-082839144", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110224-082839144", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/507788", "primary_object": { "basename": "CONaj06.pdf", "url": "https://authors.library.caltech.edu/records/5y2z8-chj48/files/CONaj06.pdf" }, "pub_year": "2006", "author_list": "Conley, A.; Howell, D. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/q0xx0-5fr30", "eprint_id": 56454, "eprint_status": "archive", "datestamp": "2023-08-19 18:38:03", "lastmod": "2023-10-23 15:25:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "Alexander J." } }, { "id": "Le-Borgne-D", "name": { "family": "Le Borgne", "given": "Damien" } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "Raymond G." } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "Julien" } }, { "id": "Balam-D", "name": { "family": "Balam", "given": "David" } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "Stephane" } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "Dominique" } }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "Isobel M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "Eric Y." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Pain-R", "name": { "family": "Pain", "given": "Reynald" } }, { "id": "Perrett-K-M", "name": { "family": "Perrett", "given": "Kathryn M." } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "Christopher J." } } ] }, "title": "The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2006 Nature Publishing Group. \n\nReceived 7 April; accepted 18 July 2006. \n\nSNLS relies on observations with MegaCam, a joint project\nof CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT). We used data products from the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey. Some data were obtained at the W. M. Keck Observatory. We acknowledge support from NSERC, NERSC, CIAR, CNRS/IN2P3, CNRS/INSU, CEA and the DOE.\n\nSupplemental Material - nature05103-s1.pdf
", "abstract": "The accelerating expansion of the Universe, and the need for dark energy, were inferred from observations of type Ia supernovae. There is a consensus that type Ia supernovae are thermonuclear explosions that destroy carbon\u2013oxygen white dwarf stars that have accreted matter from a companion star, although the nature of this companion remains uncertain. These supernovae are thought to be reliable distance indicators because they have a standard amount of fuel and a uniform trigger: they are predicted to explode when the mass of the white dwarf nears the Chandrasekhar mass of 1.4 solar masses (M_\u2609). Here we show that the high-redshift supernova SNLS-03D3bb has an exceptionally high luminosity and low kinetic energy that both imply a super-Chandrasekhar-mass progenitor. Super-Chandrasekhar-mass supernovae should occur preferentially in a young stellar population, so this may provide an explanation for the observed trend that overluminous type Ia supernovae occur only in 'young' environments. As this supernova does not obey the relations that allow type Ia supernovae to be calibrated as standard candles, and as no counterparts have been found at low redshift, future cosmology studies will have to consider possible contamination from such events.", "date": "2006-09-21", "date_type": "published", "publication": "Nature", "volume": "443", "number": "7109", "publisher": "Nature Publishing Group", "pagerange": "308-311", "id_number": "CaltechAUTHORS:20150408-073732428", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150408-073732428", "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": "National Energy Research Scientific Computing Center (NERSC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/nature05103", "primary_object": { "basename": "nature05103-s1.pdf", "url": "https://authors.library.caltech.edu/records/q0xx0-5fr30/files/nature05103-s1.pdf" }, "pub_year": "2006", "author_list": "Howell, D. Andrew; Sullivan, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/r1xq8-38020", "eprint_id": 7150, "eprint_status": "archive", "datestamp": "2023-08-22 06:29:58", "lastmod": "2023-10-16 20:44:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Le-Borgne-D", "name": { "family": "Le Borgne", "given": "D." } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "C. J." } }, { "id": "Hodsman-A", "name": { "family": "Hodsman", "given": "A." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "R. G." } }, { "id": "Astier-P", "name": { "family": "Astier", "given": "P." } }, { "id": "Aubourg-E", "name": { "family": "Aubourg", "given": "E." } }, { "id": "Balam-D", "name": { "family": "Balam", "given": "D." } }, { "id": "Basa-S", "name": { "family": "Basa", "given": "S." } }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "A." } }, { "id": "Fabbro-S", "name": { "family": "Fabbro", "given": "S." } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "D." } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "J." } }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Taillet-R", "name": { "family": "Taillet", "given": "R." } }, { "id": "Baumont-S", "name": { "family": "Baumont", "given": "S." } }, { "id": "Bronder-J", "name": { "family": "Bronder", "given": "J." } }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Filiol-M", "name": { "family": "Filiol", "given": "M." } }, { "id": "Lusset-V", "name": { "family": "Lusset", "given": "V." } }, { "id": "Perlmutter-S", "name": { "family": "Perlmutter", "given": "S." } }, { "id": "Ripoche-P", "name": { "family": "Ripoche", "given": "P." } }, { "id": "Tao-C", "name": { "family": "Tao", "given": "C." } } ] }, "title": "Rates and properties of Type Ia supernovae as a function of mass and star formation in their host galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "distance scale \u2014 galaxies: evolution \u2014 supernovae: general \u2014 surveys", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2006 February 6; accepted 2006 May 17. The SNLS collaboration gratefully acknowledges the assistance of Pierre Martin and the CFHT Queued Service Observations team. Jean-Charles Cuillandre and Kanoa Withington were also indispensable in making possible real-time data reduction at CFHT. We thank Lars Bildsten and Evan Scannapieco for useful discussions, and Andrew Hopkins for providing a copy of Hopkins & Beacom (2006) prior to submission. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. Canadian collaboration members acknowledge support from NSERC and CIAR; French collaboration members from CNRS/IN2P3, CNRS/INSU, and CEA. 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. The views expressed in this article are those of the authors and do not reflect the official policy or position of the United States Air Force, Department of Defense, or the US government.\n\nPublished - SULapj06.pdf
", "abstract": "We show that Type Ia supernovae (SNe Ia) are formed within both very young and old stellar populations, with observed rates that depend on the stellar mass and mean star formation rates (SFRs) of their host galaxies. Models in which the SN Ia rate depends solely on host galaxy stellar mass are ruled out with >99% confidence. Our analysis is based on 100 spectroscopically confirmed SNe Ia, plus 24 photometrically classified events, all from the Supernova Legacy Survey (SNLS) and distributed over 0.2 < z < 0.75. We estimate stellar masses and SFRs for the SN Ia host galaxies by fitting their broadband spectral energy distributions with the galaxy spectral synthesis code P\u00c9GASE.2. We show that the SN Ia rate per unit mass is proportional to the specific SFR of the parent galaxies\u2014more vigorously star-forming galaxies host more SNe Ia per unit stellar mass, broadly equivalent to the trend of increasing SN Ia rate in later type galaxies seen in the local universe. Following earlier suggestions for a simple \"two-component\" model approximating the SN Ia rate, we find bivariate linear dependencies of the SN Ia rate on both the stellar masses and the mean SFRs of the host systems. We find that the SN Ia rate can be well represented as the sum of 5.3 \u00b1 1.1 \u00d7 10 to the -14 SNe yr to the -1 M(.)to the -1 and 3.9 \u00b1 0.7 \u00d7 10 to the -4 SNe yr to the -1 (M(.) yr to the -1)to the -1 of star formation. We also demonstrate a dependence of distant SN Ia light-curve shapes on star formation in the host galaxy, similar to trends observed locally. Passive galaxies, with no star formation, preferentially host faster declining/dimmer SNe Ia, while brighter events are found in systems with ongoing star formation.", "date": "2006-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "648", "number": "2", "publisher": "American Astronomical Society", "pagerange": "868-883", "id_number": "CaltechAUTHORS:SULapj06", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SULapj06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "primary_object": { "basename": "SULapj06.pdf", "url": "https://authors.library.caltech.edu/records/r1xq8-38020/files/SULapj06.pdf" }, "pub_year": "2006", "author_list": "Sullivan, M.; Le Borgne, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/r34yy-7h677", "eprint_id": 24580, "eprint_status": "archive", "datestamp": "2023-08-22 06:26:21", "lastmod": "2023-10-23 23:29:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" } ] }, "title": "The Type Ia Supernova Rate at z \u2248 0.5 from the Supernova Legacy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; supernovae: general", "note": "\u00a9 2006 The American Astronomical Society. Received 2006 January 23; accepted 2006 May 1. \n\nBased on observations obtained with MegaPrime/MegaCam, a joint project of the Canada-France-Hawaii Telescope (CFHT) and CEA/DAPNIA, at CFHT, which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This work is also based on observations obtained at the European Southern Observatory using the Very Large Telescope on the Cerro Paranal (ESO Large Program 171.A-0486), and on observations (programs GN-2004A-Q-19, GS-2004A-Q-11, GN-2003B-Q-9, and GS-2003B-Q-8) obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). This work is also based on observations 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 Mauna Kea has always had within the indigenous Hawaiian community. We are grateful for our opportunity to conduct observations on this mountain. We acknowledge invaluable assistance from the CFHT Queued Service Observations team, led by P. Martin (CFHT). Our research would not be possible without the assistance of the support staff at CFHT, especially J.-C. Cuillandre. The real-time pipelines for supernova detection run on computers integrated in the CFHT computing system and are very efficiently installed, maintained, and monitored by K. Withington (CFHT). We also heavily rely on the real-time Elixir pipeline, which is operated and monitored by J.-C. Cuillandre, E.Magnier, and K. Withington. We are grateful to L. Simard (CADC) for setting up the image delivery system and his kind and efficient responses to our suggestions for improvements. The Canadian collaboration members acknowledge support from NSERC and CIAR and the French collaboration members from CNRS/ IN2P3, CNRS/INSU, PNC, and CEA. This work was supported in part by the Director, Office of Science, Office of High Energy and Nuclear Physics, of the US Department of Energy. The France-Berkeley Fund provided additional collaboration support. S. Fabbro and A. C. Gon\u00e7alves acknowledge support from FCT, Portugal, under grants SFRH/BPD/14682/2003 and SFRH/BPD/11641/2002, respectively. We are indebted to A. Hopkins and J. Beacom for providing us with a draft of their work on SFH prior to its publication. The views expressed in this article are those of the authors and do not reflect the official policy or position of the United States Air Force, the Department of Defense, or the US Government.\n\nPublished - NEIaj06.pdf
", "abstract": "We present a measurement of the distant Type Ia supernova (SN Ia) rate derived from the first 2 yr of the Canada-France-Hawaii Telescope Supernova Legacy Survey. We observed four 1\u00b0 \u00d7 1\u00b0 fields with a typical temporal frequency of (\u0394t) ~ 4 observer-frame days over time spans of 158-211 days per season for each field, with breaks during the full Moon. We used 8-10 m class telescopes for spectroscopic follow-up to confirm our candidates and determine their redshifts. Our starting sample consists of 73 spectroscopically verified SNe Ia in the redshift range 0.2 < z < 0.6. We derive a volumetric SN Ia rate of r_V((z) = 0:47) [0:42^(+0:13)-(-0:09)(syst:) \u00b1 0:06(stat:)]x 10^-4 yr^-1 Mpc^3, assuming h = 0:7, \u03a9_m = 0:3, and a flat cosmology. Using recently published galaxy luminosity functions derived in our redshift range, we derive a SN Ia rate per unit luminosity of r_L((z) = 0:47) = 0:154^(+0:048)_(-0:033)(syst:)^(+0:039)_(-0:031)(stat:) SN units. Using our rate alone, we place an upper limit on the component of SN Ia production that tracks the cosmic star\nformation history of 1 SN Ia per 10^3 M_\u2609 of stars formed. Our rate and other rates from surveys using spectroscopic\nsample confirmation display only a modest evolution out to z = 0:55.", "date": "2006-09", "date_type": "published", "publication": "Astronomical Journal", "volume": "132", "number": "3", "publisher": "American Astronomical Society", "pagerange": "1126-1145", "id_number": "CaltechAUTHORS:20110728-095419527", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110728-095419527", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSERC and CIAR" }, { "agency": "CNRS/IN2P3 (France)" }, { "agency": "CNRS/INSU (France)" }, { "agency": "PNC (Frace)" }, { "agency": "CEA (France)" }, { "agency": "Office of High Energy and Nuclear Physics" }, { "agency": "Department of Energy (DOE)" }, { "agency": "France-Berkeley Fund" }, { "agency": "FCT (Portugal)", "grant_number": "SFRH/BPD/14682/2003" }, { "agency": "FCT (Portugal)", "grant_number": "SFRH/BPD/11641/2002" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/505532", "primary_object": { "basename": "NEIaj06.pdf", "url": "https://authors.library.caltech.edu/records/r34yy-7h677/files/NEIaj06.pdf" }, "pub_year": "2006", "author_list": "Neill, J. D. and Ellis, R. S." }, { "id": "https://authors.library.caltech.edu/records/2173j-t6j63", "eprint_id": 56222, "eprint_status": "archive", "datestamp": "2023-08-19 18:28:05", "lastmod": "2023-10-23 15:10:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "Kevin" }, "orcid": "0000-0001-5464-0888" }, { "id": "Khochfar-S", "name": { "family": "Khochfar", "given": "Sadegh" } }, { "id": "Kaviraj-Sugata", "name": { "family": "Kaviraj", "given": "Sugata" } }, { "id": "Yi-Sukyoung-K", "name": { "family": "Yi", "given": "Sukyoung K." } }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "Alessandro" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Conrow-T", "name": { "family": "Conrow", "given": "Tim" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neff-S-G", "name": { "family": "Neff", "given": "Susan G." } }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "Mark" }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Bianchi-L-C", "name": { "family": "Bianchi", "given": "Luciana" }, "orcid": "0000-0001-7746-5461" }, { "id": "Donas-J", "name": { "family": "Donas", "given": "Jos\u00e9" } }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Tim" } }, { "id": "Lee-Young-Wook", "name": { "family": "Lee", "given": "Young-Wook" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Milliard-B", "name": { "family": "Milliard", "given": "Bruno" } }, { "id": "Rich-R-M", "name": { "family": "Rich", "given": "R. Michael" }, "orcid": "0000-0003-0427-8387" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } } ] }, "title": "Suppression of star formation in early-type galaxies by feedback from supermassive black holes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2006 Nature Publishing Group.\n\nReceived 15 December 2005; accepted 15 May 2006.\n\nWe thank J. Magorrian for discussions and comments. GALEX is a NASA Small Explorer, launched in April 2003. We acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'\u00c9tudes Spatiales of France and the Korean Ministry of Science and Technology. This work was supported by the Basic Research Program of the Korea Science & Engineering Foundation (S.K.Y.). Author Contributions K.S., S. Khochfar, S. Kaviraj and S.K.Y. performed the data sampling, analysis, interpretation, model construction, and writing of the manuscript. A.B. supplied the Virgo galaxy data, and the rest of the authors contributed to the data acquisition using the GALEX satellite.\n\nSupplemental Material - nature04934-s1.pdf
", "abstract": "Detailed high-resolution observations of the innermost regions of nearby galaxies have revealed the presence of supermassive black holes. These black holes may interact with their host galaxies by means of 'feedback' in the form of energy and material jets; this feedback affects the evolution of the host and gives rise to observed relations between the black hole and the host. Here we report observations of the ultraviolet emissions of massive early-type galaxies. We derive an empirical relation for a critical black-hole mass (as a function of velocity dispersion) above which the outflows from these black holes suppress star formation in their hosts by heating and expelling all available cold gas. Supermassive black holes are negligible in mass compared to their hosts but nevertheless seem to play a critical role in the star formation history of galaxies.", "date": "2006-08-24", "date_type": "published", "publication": "Nature", "volume": "442", "number": "7105", "publisher": "Nature Publishing Group", "pagerange": "888-891", "id_number": "CaltechAUTHORS:20150330-162345264", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150330-162345264", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Korea Science and Engineering Foundation" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1038/nature04934", "primary_object": { "basename": "nature04934-s1.pdf", "url": "https://authors.library.caltech.edu/records/2173j-t6j63/files/nature04934-s1.pdf" }, "pub_year": "2006", "author_list": "Schawinski, Kevin; Khochfar, Sadegh; et el." }, { "id": "https://authors.library.caltech.edu/records/g4yz9-9d833", "eprint_id": 24033, "eprint_status": "archive", "datestamp": "2023-08-22 06:16:33", "lastmod": "2023-10-23 20:15:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "Kevin C." }, "orcid": "0000-0002-1588-6700" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Small-T", "name": { "family": "Small", "given": "Todd" } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } } ] }, "title": "Ultraviolet and Far-Infrared-selected Star-forming Galaxies at z = 0: Differences and Overlaps", "ispublished": "pub", "full_text_status": "public", "keywords": "dust: extinction; galaxies: active; galaxies: luminosity function, mass function; galaxies: starburst; infrared: galaxies; stars: formation; ultraviolet: galaxies", "note": "\u00a9 2006 The American Astronomical Society. Received 2005 December 22; accepted 2006 April 3. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the South Korean Ministry\nof Science and Technology. We thank an anonymous referee for\nvery constructive comments. 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\nPublished - XUCapj06.pdf
", "abstract": "We study two samples of local galaxies, one UV (GALEX) selected and the other FIR (IRAS) selected, to address the question of whether UV and FIR surveys see two sides (\"bright\" and \"dark\") of the star formation of the same population of galaxies or two different populations of star-forming galaxies. No significant difference between the L_(tot) (=L_(60) + L_(FUV)) luminosity functions of the UV and FIR samples is found. In addition, after the correction for the \"Malmquist bias\" (bias for flux-limited samples), the FIR-to-UV ratio versus L_(tot) relations of the two samples are consistent with each other. In the range of 9 \u227e log(L_(tot)/L_\u2299) \u227e 12, both can be approximated by a simple linear relation of log(L_(60)/L_(FUV)) = log(L_(tot)/L_\u2299) - 9.66. These are consistent with the hypothesis that the two samples represent the same population of star-forming galaxies, and their well-documented differences in L_(tot) and in FIR-to-UV ratio are due only to the selection effect. A comparison between the UV luminosity functions shows marginal evidence for a population of faint UV galaxies missing in the FIR-selected sample. The contribution from these \"FIR-quiet\" galaxies to the overall UV population is insignificant, given that the K-band luminosity functions (i.e., the stellar mass functions) of the two samples do not show any significant difference.", "date": "2006-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "646", "number": "2", "publisher": "American Astronomical Society", "pagerange": "834-840", "id_number": "CaltechAUTHORS:20110616-113836578", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110616-113836578", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/504974", "primary_object": { "basename": "XUCapj06.pdf", "url": "https://authors.library.caltech.edu/records/g4yz9-9d833/files/XUCapj06.pdf" }, "pub_year": "2006", "author_list": "Xu, Kevin C.; Barlow, Tom A.; et el." }, { "id": "https://authors.library.caltech.edu/records/w05qq-dcb44", "eprint_id": 6750, "eprint_status": "archive", "datestamp": "2023-08-22 06:03:27", "lastmod": "2023-10-16 20:30:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter" }, "orcid": "0000-0002-3389-0586" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard" }, "orcid": "0000-0001-7782-7071" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Leonard-D-C", "name": { "family": "Leonard", "given": "Douglas C." } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Astier-P", "name": { "family": "Astier", "given": "Pierre" } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "Raymond G." } }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "Alex" } }, { "id": "Fabbro-S", "name": { "family": "Fabbro", "given": "Sebastien" } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "Dominique" } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Pain-R", "name": { "family": "Pain", "given": "Reynald" } }, { "id": "Perrett-K-M", "name": { "family": "Perrett", "given": "Kathy" } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "Chris J." } }, { "id": "Regnault-N", "name": { "family": "Regnault", "given": "Nicolas" } } ] }, "title": "Toward a cosmological Hubble diagram for Type II-P supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "distance scale; supernovae", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2005 April 12; accepted 2006 March 20. \n\nBased on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of the NRC and CNRS. 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. 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 Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. P. E. N. acknowledges support from NASA ATP and LTSA grants. R. S. E. acknowledges financial support from the Department of Energy (DOE). A. G. acknowledges support by NASA through Hubble Fellowship grant HST-HF-01158.01-A, awarded by STScI, which is operated by AURA, Inc., for NASA, under contract NAS5-26555. D. C. L. is supported by a National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship under award AST 04-01479. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US DOE, under contract DE-AC03-76SF00098. We thank them for a generous allocation of computing time.\n\nPublished - NUGapj06.pdf
", "abstract": "We present the first high-redshift Hubble diagram for Type II-P supernovae (SNe II-P) based on five events at redshift up to z ~ 0.3. This diagram was constructed using photometry from the Canada-France-Hawaii Telescope Supernova Legacy Survey and absorption-line spectroscopy from the Keck Observatory. The method used to measure distances to these supernovae is based on recent work by Hamuy & Pinto and exploits a correlation between the absolute brightness of SNe II-P and the expansion velocities derived from the minimum of the Fe II \u03bb 5169 P Cygni feature observed during the plateau phases. We present three refinements to this method that significantly improve the practicality of measuring the distances of SNe II-P at cosmologically interesting redshifts. These are an extinction correction measurement based on the V-I colors at day 50, a cross-correlation measurement for the expansion velocity, and the ability to extrapolate such velocities accurately over almost the entire plateau phase. We apply this revised method to our data set of high-redshift SNe II-P and find that the resulting Hubble diagram has a scatter of only 0.26 mag, thus demonstrating the feasibility of measuring the expansion history, with present facilities, using a method independent of that based on supernovae of Type Ia.", "date": "2006-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "645", "number": "2", "publisher": "American Astronomical Society", "pagerange": "841-850", "id_number": "CaltechAUTHORS:NUGapj06", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:NUGapj06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-01158.01-A" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC03-76SF00098" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST 04-01479" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "primary_object": { "basename": "NUGapj06.pdf", "url": "https://authors.library.caltech.edu/records/w05qq-dcb44/files/NUGapj06.pdf" }, "pub_year": "2006", "author_list": "Nugent, Peter; Sullivan, Mark; et el." }, { "id": "https://authors.library.caltech.edu/records/vs31q-z8z81", "eprint_id": 23680, "eprint_status": "archive", "datestamp": "2023-08-22 05:37:01", "lastmod": "2023-10-23 19:51:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Iglesias-P\u00e1ramo-J", "name": { "family": "Iglesias-P\u00e1ramo", "given": "J." } }, { "id": "Xu-K", "name": { "family": "Xu", "given": "K." } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T. A." } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "P. G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "P. F." }, "orcid": "0000-0001-8177-1023" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "D." } }, { "id": "Seibert-M", "name": { "family": "Seibert", "given": "M." }, "orcid": "0000-0002-1143-5515" }, { "id": "Small-T", "name": { "family": "Small", "given": "T." } }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "T. K." } } ] }, "title": "Star Formation in the Nearby Universe: The Ultraviolet and Infrared Points of View", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; surveys; ultraviolet: galaxies", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2005 April 15; accepted 2006 January 10.\n\nGALEX is a NASA Small Explorer, launched in 2003 April.\nWe gratefully acknowledge NASA's support for the construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. 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. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology,\nunder contract with the National Aeronautics and Space\nAdministration. The Lyon Extragalactic Database (LEDA) is\navailable at http://leda.univ-lyon1.fr. T. T. T. has been financially supported by the Japan Society for the Promotion of Science.\n\nPublished - IGLapjss06.pdf
", "abstract": "This work presents the main ultraviolet (UV) and far-infrared (FIR) properties of two samples of nearby galaxies selected from the GALEX (\u03bb = 2315 \u00c5, hereafter NUV) and IRAS (\u03bb = 60 \u03bcm) surveys, respectively. They are built in order to obtain detection at both wavelengths for most of the galaxies. Star formation rate (SFR) estimators based on the UV and FIR emissions are compared. Systematic differences are found between the SFR estimators for individual galaxies based on the NUV fluxes corrected for dust attenuation and on the total IR luminosity. A combined estimator based on NUV and IR luminosities seems to be the best proxy over the whole range of values of SFR. Although both samples present similar average values of the birthrate parameter b, their star-formation-related properties are substantially different: NUV-selected galaxies tend to show larger values of b for lower masses, SFRs, and dust attenuation, supporting previous scenarios of star formation history (SFH). Conversely, about 20% of the FIR-selected galaxies show high values of b, SFR, and NUV attenuation. These galaxies, most of them being LIRGs and ULIRGs, break down the downsizing picture of SFH; however, their relative contribution per unit volume is small in the local universe. Finally, the cosmic SFR density of the local universe is estimated in a consistent way from the NUV and IR luminosities.", "date": "2006-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "164", "number": "1", "publisher": "American Astronomical Society", "pagerange": "38-51", "id_number": "CaltechAUTHORS:20110516-141002586", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110516-141002586", "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)" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1086/502628", "primary_object": { "basename": "IGLapjss06.pdf", "url": "https://authors.library.caltech.edu/records/vs31q-z8z81/files/IGLapjss06.pdf" }, "pub_year": "2006", "author_list": "Iglesias-P\u00e1ramo, J.; Xu, K.; et el." }, { "id": "https://authors.library.caltech.edu/records/bm98x-frx83", "eprint_id": 51986, "eprint_status": "archive", "datestamp": "2023-08-19 14:25:09", "lastmod": "2023-10-18 19:14:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" } ] }, "title": "GALEX and UV Observations", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2004 American Association for the Advancement of Science.", "abstract": "In his article \"Ultraviolet astronomers face loss of vision\" (News Focus, 25 June, p. 1899), Govert Schilling makes the important point that we will soon lose our view of the ultraviolet (UV) sky unless we preserve or replace the few existing UV space missions.", "date": "2004-10-01", "date_type": "published", "publication": "Science", "volume": "306", "number": "5693", "publisher": "American Association for the Advancement of Science", "pagerange": "54-54", "id_number": "CaltechAUTHORS:20141120-073853263", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141120-073853263", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1126/science.306.5693.54c", "pub_year": "2004", "author_list": "Friedman, Peter G. and Martin, D. Christopher" }, { "id": "https://authors.library.caltech.edu/records/s4v8z-def82", "eprint_id": 88311, "eprint_status": "archive", "datestamp": "2023-08-19 11:04:17", "lastmod": "2024-01-14 20:31:24", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jelinsky-P-N", "name": { "family": "Jelinsky", "given": "Patrick" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Malloy-J", "name": { "family": "Malloy", "given": "James" } }, { "id": "Jelinsky-S", "name": { "family": "Jelinsky", "given": "Sharon" } }, { "id": "Siegmund-O-H-W", "name": { "family": "Siegmund", "given": "Oswald" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Chris" }, "orcid": "0000-0002-8650-1644" }, { "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" } }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted" } }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter" } } ] }, "title": "Performance results of the GALEX cross delay line detectors", "ispublished": "unpub", "full_text_status": "public", "keywords": "Microchannel plates, ultraviolet detectors, GALEX, sealed tube", "note": "\u00a9 2003 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe authors would like to thank the GALEX teams at Caltech and JPL. We would also like to thank Darrel Doliber and Joseph Stock for their large contribution in the construction and characterization of the tubes. This work was supported by Caltech under contract #PC251341 and GSFC grant # NAG5-7615.\n\nPublished - 233.pdf
", "abstract": "We describe the performance results for the Galaxy Evolution Explorer (GALEX) far ultraviolet (FUV) and near ultraviolet (NUV) detectors. The detectors were delivered to JPL/Caltech starting in the fall of 2000 and have undergone approximately 1000 hours of pre-flight system-level testing to date. The GALEX detectors are sealed tube micro-channel plate (MCP) delay line readout detectors. They have a 65 mm diameter active area, which will be the largest format on orbit. The FUV detector has a spectral bandpass from 115 - 180 nm and the NUV detector has a bandpass from 165 - 300 nm. We report here on the performance of the detectors before and after integration into the instrument. Characteristics measured include the background count rate and distribution, gain vs. applied high voltage, spatial resolution and linearity, flat fields, and quantum efficiency.", "date": "2003-02-24", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "233-240", "id_number": "CaltechAUTHORS:20180726-153351878", "isbn": "9780819446336", "book_title": "Future EUV/UV and Visible Space Astrophysics Missions and Instrumentation", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180726-153351878", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "PC251341" }, { "agency": "NASA", "grant_number": "NAG5-7615" } ] }, "local_group": { "items": [ { "id": "Space-Astrophysics-Laboratory" } ] }, "contributors": { "items": [ { "id": "Blades-J-C", "name": { "family": "Blades", "given": "J. Chris" } }, { "id": "Siegmund-O-H-W", "name": { "family": "Siegmund", "given": "Oswald H. W." } } ] }, "doi": "10.1117/12.460013", "primary_object": { "basename": "233.pdf", "url": "https://authors.library.caltech.edu/records/s4v8z-def82/files/233.pdf" }, "pub_year": "2003", "author_list": "Jelinsky, Patrick; Morrissey, Patrick; et el." } ]