[ { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/30yrb-yt749", "eprint_status": "archive", "datestamp": "2024-01-19 20:08:50", "lastmod": "2024-01-19 20:08:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Ping", "name": { "family": "Chen", "given": "Ping" }, "orcid": "0000-0003-0853-6427" }, { "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Schulze", "given": "Steve" }, "orcid": "0000-0001-6797-1889" }, { "name": { "family": "Post", "given": "Richard S." }, "orcid": "0000-0003-3244-0337" }, { "name": { "family": "Liu", "given": "Chang" }, "orcid": "0000-0002-7866-4531" }, { "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Das-Kaustav-K", "name": { "family": "Das", "given": "Kaustav K." } }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "name": { "family": "Katz", "given": "Boaz" }, "orcid": "0000-0003-0584-2920" }, { "name": { "family": "Kushnir", "given": "Doron" } }, { "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" }, { "name": { "family": "Liu", "given": "Dezi" }, "orcid": "0000-0002-0409-5719" }, { "name": { "family": "Liu", "given": "Xiangkun" }, "orcid": "0000-0003-0394-1298" }, { "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "name": { "family": "Rose", "given": "Kovi" }, "orcid": "0000-0002-7329-3209" }, { "name": { "family": "Waxman", "given": "Eli" }, "orcid": "0000-0002-9038-5877" }, { "name": { "family": "Yang", "given": "Sheng" }, "orcid": "0000-0002-2898-6532" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" }, { "id": "Zackay-Barak", "name": { "family": "Zackay", "given": "Barak" } }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew J." }, "orcid": "0000-0003-0228-6594" }, { "name": { "family": "Fang", "given": "Yuan" } }, { "name": { "family": "Fynbo", "given": "Johan P. U." }, "orcid": "0000-0002-8149-8298" }, { "id": "Groom-Steven-L", "name": { "family": "Groom", "given": "Steven L." }, "orcid": "0000-0001-5668-3507" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Irani", "given": "Ido" }, "orcid": "0000-0002-7996-8780" }, { "id": "Jegou-du-Laz-Theophile", "name": { "family": "Jegou du Laz", "given": "Theophile" }, "orcid": "0009-0003-6181-4526" }, { "name": { "family": "Liu", "given": "Xiaowei" } }, { "name": { "family": "Mazzali", "given": "Paolo A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Neill-James-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Qin-Yu-Jing", "name": { "family": "Qin", "given": "Yu-Jing" }, "orcid": "0000-0003-3658-6026" }, { "name": { "family": "Riddle", "given": "Reed L." }, "orcid": "0000-0002-0387-370X" }, { "name": { "family": "Sharon", "given": "Amir" }, "orcid": "0009-0000-2102-5811" }, { "name": { "family": "Strotjohann", "given": "Nora L." }, "orcid": "0000-0002-4667-6730" }, { "id": "Wold-Avery", "name": { "family": "Wold", "given": "Avery" }, "orcid": "0000-0002-9998-6732" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "A 12.4-day periodicity in a close binary system after a supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "Multidisciplinary", "note": "
Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law.
\n\nWe thank B. Cenko, Y. Levin, E. Pian, S. Dong, D. Lai, O. Yaron, J. Morag, Y. S. Rimalt and T. Shenar for the discussions. We thank D. J. Thompson for his comments. P.C. and A.G.-Y. thank Y. Beletsky for his assistance with Magellan telescope remote observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC) and the California Institute of Technology (Caltech). SED Machine is based on the work supported by the National Science Foundation under grant no. 1106171. This study is based on observations obtained with the 48-inch Samuel Oschin Telescope and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility (ZTF) project. ZTF is supported by the National Science Foundation under grant no. AST-2034437 and a collaboration that includes Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum and Northwestern University. Operations were conducted by COO, IPAC and the University of Wisconsin. The Gordon and Betty Moore Foundation, through both the Data-Driven Investigator Program and a dedicated grant, provided funding for SkyPortal. This work has used data from the ATLAS project. The ATLAS project is primarily funded to search for near-earth asteroids through NASA grant nos NN12AR55G, 80NSSC18K0284 and 80NSSC18K1575; by-products of the NEO search include images and catalogues from the survey area. This work was partially funded by the Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889 and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory and the Millennium Institute of Astrophysics (MAS), Chile. This study is based on the observations made with the NOT, owned in collaboration with the University of Turku and Aarhus University and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, respectively, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. One of the spectra from NOT was obtained as part of an NBI school in which M. Killi, N. Allen, K. Gould and D. Zhou participated under the leadership of J. Fynbo. This work was supported by the research project grant Understanding the Dynamic Universe funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067. The study is based on the observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 110.25A6. The access for MMT Observatory for part of the MMT/Binospec data was supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). Mephisto is developed at and operated by the South-Western Institute for Astronomy Research of Yunnan University (SWIFAR-YNU), funded by the Yunnan University Development Plan for World-Class University and Yunnan University Development Plan for World-Class Astronomy Discipline. The Australia Telescope Compact Array is part of the ATNF, which is funded by the Australian government for the operation as a national facility managed by the CSIRO. We acknowledge the Gomeroi people as the Traditional Owners of the Observatory site. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant no. 140. S. Schulze acknowledges support from the G.R.E.A.T. research environment, funded by Vetenskapsrådet, the Swedish Research Council, project no. 2016-06012. B.Z. is supported by a research grant from the Willner Family Leadership Institute for the Weizmann Institute of Science, a research grant from the Center for New Scientists at the Weizmann Institute of Science and a research grant from the Ruth and Herman Albert Scholarship Program for New Scientists. A.H. acknowledges the support from the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation (ISF) and support from the ISF grant no. 647/18. This research was supported by grant no. 2018154 from the United States–Israel Binational Science Foundation (BSF). A.H. is especially grateful to the Sir Zelman Cowen Academic Initiatives for their funding and support. D.L., Xiangkun Liu, Y.F. and Xiaowei Liu acknowledge the support from special grants to the Yunnan Technology Leading Talents and Provincial Innovation Team. D.L., Xiangkun Liu, Y.F. and Xiaowei Liu also acknowledge supports from the Science and Technology Champion Project (202005AB160002) and from two team projects—the Innovation Team (202105AE160021) and the Top Team (202305AT350002)—all funded by the Yunnan Revitalization Talent Support Program. J.P.U.F. is supported by the Independent Research Fund Denmark (DFF-4090-00079) and thanks the Carlsberg Foundation for support.
\nAll authors reviewed the paper and contributed to the interpretation and/or data acquisition. P.C. led the studies. P.C. discovered the periodicity and the γ-ray detection, organized the follow-up observations, conducted X-ray and most optical data acquisition, conducted most of the data reduction, performed the data analysis and wrote most of the paper, including creating all the figures. A.G.-Y. contributed to the follow-up data (including observations performed with MMT/BINOSPEC, Magellan/FIRE, Magellan/FIRE, VLT/X-shooter, NuSTAR, Chandra and ATCA) and to the interpretation, wrote the paper and thoroughly reviewed it. J.S. initiated the study, obtained the spectra with SEDM and NOT, helped in developing the ideas in the paper, wrote the paper and thoroughly reviewed it. S.S. contributed to the follow-up observations with NOT and reduced the NOT spectra. R.S.P. performed the follow-up observations with the 0.8-m RC32 telescope at Post Observatory. C.L. contributed to one MMT/Binospec spectrum, reduced the Magellan/FIRE echelle spectra and contributed to the interpretation. E.O.O. contributed to the follow-up observations with NuSTAR. B.K., D.K., E.O.O., E.W. and B.Z. contributed to the interpretation and especially suggested the analysis of Fermi-LAT data. D.L. performed the Mephisto photometry. Xiangkun Liu organized the Mephisto observations. A.H. and K.R. performed the ATCA radio observation and data reduction. K.K.D., Y.Y., M.M.K. and S.R.K. contributed to the P200/DBSP spectra. C.F. contributed to the SEDM photometry. A.A.M. contributed to one MMT/BINOSPEC spectrum. S.Y. contributed to the analysis of light curves with the nickel decay model. J.P.U.F. obtained a spectrum from the NOT. S.R.K., A.J.D., J.D.N., E.C.B., S.L.G., A.W., T.J.d.L., R.L.R., G.H. and R.D. are the ZTF builders. D.L., Xiaowei Liu, Xiangkun Liu and Y.F. contributed to the observation and reduction of Mephisto data. I.I., A.S., N.L.S., P.A.M. and L.Y. contributed to the interpretation. Y.-J.Q. contributed to the observation of DBSP spectra.
\n\nPhotometry and spectroscopy of SN 2022jli will be made available at the WISeREP public database. Facilities that make all their data available in public archives promptly or after a proprietary period include Palomar 48-inch/ZTF, VLT/X-shooter, NuSTAR, Chandra X-ray Observatory and Fermi Gamma-Ray Space Telescope. Data from the ATLAS, Gaia, ASAS-SN and KKO were obtained from public sources. The data used to perform the analysis and produce the figures for this paper are available at a public GitHub repository (https://github.com/AtomyChan/SN2022jli).
\n\nThe codes used to perform the analysis and produce the figures for this paper are available at a public GitHub repository (https://github.com/AtomyChan/SN2022jli).
", "abstract": "Neutron stars and stellar-mass black holes are the remnants of massive star explosions1. Most massive stars reside in close binary systems2, and the interplay between the companion star and the newly formed compact object has been theoretically explored3, but signatures for binarity or evidence for the formation of a compact object during a supernova explosion are still lacking. Here we report a stripped-envelope supernova, SN 2022jli, which shows 12.4-day periodic undulations during the declining light curve. Narrow Hα emission is detected in late-time spectra with concordant periodic velocity shifts, probably arising from hydrogen gas stripped from a companion and accreted onto the compact remnant. A new Fermi-LAT γ-ray source is temporally and positionally consistent with SN 2022jli. The observed properties of SN 2022jli, including periodic undulations in the optical light curve, coherent Hα emission shifting and evidence for association with a γ-ray source, point to the explosion of a massive star in a binary system leaving behind a bound compact remnant. Mass accretion from the companion star onto the compact object powers the light curve of the supernova and generates the γ-ray emission.
\nPublished - Karambelkar_2023_ApJ_948_137.pdf
", "abstract": "Luminous red novae (LRNe) are transients characterized by low luminosities and expansion velocities, and they are associated with mergers or common-envelope ejections in stellar binaries. Intermediate-luminosity red transients (ILRTs) are an observationally similar class with unknown origins, but they are generally believed to be either electron-capture supernovae in super-asymptotic giant branch stars or outbursts in dusty luminous blue variables (LBVs). In this paper, we present a systematic sample of eight LRNe and eight ILRTs detected as part of the Census of the Local Universe (CLU) experiment on the Zwicky Transient Facility (ZTF). The CLU experiment spectroscopically classifies ZTF transients associated with nearby (<150 Mpc) galaxies, achieving 80% completeness for mr < 20 mag. Using the ZTF-CLU sample, we derive the first systematic LRNe volumetric rate of 7.8_(-3.7)^(+6.5) x 10\u207b\u2075 Mpc\u207b\u00b3 yr\u207b\u00b9 in the luminosity range \u221216 \u2264 M\u1d63 \u2264 \u221211 mag. We find that, in this luminosity range, the LRN rate scales as dN/dL \u221d L^(-2.5 \u00b1 0.3) \u2014 significantly steeper than the previously derived scaling of L^(\u22121.4 \u00b1 0.3) for lower-luminosity LRNe (M\u1d65 \u2265 \u221210 mag). The steeper power law for LRNe at high luminosities is consistent with the massive merger rates predicted by binary population synthesis models. We find that the rates of the brightest LRNe (M\u1d63 \u2264 \u221213 mag) are consistent with a significant fraction of them being progenitors of double compact objects that merge within a Hubble time. For ILRTs, we derive a volumetric rate of 2.6_(-1.4)^(+1.8) x 10^\u207b\u2076 Mpc\u207b\u00b3 yr\u207b\u00b9 for M\u1d63 \u2264 \u221213.5 mag, which scales as dN}/dL \u221d L^(-2.5 \u00b1 0.5). This rate is \u223c1%\u20135% of the local core-collapse supernova rate and is consistent with theoretical ECSN rate estimates.", "date": "2023-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "948", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 137", "id_number": "CaltechAUTHORS:20230612-735327000.26", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230612-735327000.26", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "NSF", "grant_number": "AST-2034437" }, { "agency": "ZTF partner institutions" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "016.192.277" }, { "agency": "William and Marina Kast" }, { "agency": "Google" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Sunil Nagaraj" }, { "agency": "Landon Noll" }, { "agency": "Sandy Otellini" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" } ] }, "doi": "10.3847/1538-4357/acc2b9", "primary_object": { "basename": "Karambelkar_2023_ApJ_948_137.pdf", "url": "https://authors.library.caltech.edu/records/mz8a6-0tc05/files/Karambelkar_2023_ApJ_948_137.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Karambelkar, Viraj R.; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zr9he-c2023", "eprint_id": 119058, "eprint_status": "archive", "datestamp": "2023-08-22 18:42:39", "lastmod": "2023-10-24 23:49:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "McKernan-Barry", "name": { "family": "McKernan", "given": "Barry" }, "orcid": "0000-0002-9726-0508" }, { "id": "Ford-K-E-Saavik", "name": { "family": "Ford", "given": "K. E. Saavik" }, "orcid": "0000-0002-5956-851X" }, { "id": "Stern-Daniel", "name": { "family": "Stern", "given": "Daniel" }, "orcid": "0000-0003-2686-9241" }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "Michael" }, "orcid": "0000-0002-8262-2924" }, { "id": "Burdge-Kevin-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Purdum-Josiah-N", "name": { "family": "Purdum", "given": "Josiah" }, "orcid": "0000-0003-1227-3738" }, { "id": "Rosnet-Philippe", "name": { "family": "Rosnet", "given": "Philippe" }, "orcid": "0000-0002-6099-7565" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" } ] }, "title": "A Light in the Dark: Searching for Electromagnetic Counterparts to Black Hole-Black Hole Mergers in LIGO/Virgo O3 with the Zwicky Transient Facility", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nThe authors thank Will Farr and Colm Talbot for very useful discussions about LIGO/Virgo waveform choices and parameterization. M.J.G., B.M., and K.E.S.F. acknowledge the Center for Computational Astrophysics at the Flatiron Institute, New York for their hospitality and support.\n\nThis work was supported in part by the National Science Foundation grant Nos. AST-1815034, AST-1831412, and AST-2108402, the NASA grant No. 16-ADAP16-0232, and Simons Foundation grant No. 533845. The work of D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. M.W.C. is supported by the National Science Foundation with grant Nos. PHY-2010970 and OAC-2117997. P.R. acknowledges the support received from the Agence Nationale de la Recherche of the French government through the program \"Investissements d'Avenir\" (16-IDEX-0001 CAP 20-25).\n\nThis work made use of the Million Quasars Catalogue. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility (ZTF) project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThe ZTF forced-photometry service was funded under the Heising-Simons Foundation grant No. 12540303 (PI: Graham).\n\nPublished - Graham_2023_ApJ_942_99.pdf
", "abstract": "The accretion disks of active galactic nuclei (AGNs) are promising locations for the merger of compact objects detected by gravitational wave (GW) observatories. Embedded within a baryon-rich, high-density environment, mergers within AGNs are the only GW channel where an electromagnetic (EM) counterpart must occur (whether detectable or not). Considering AGNs with unusual flaring activity observed by the Zwicky Transient Facility (ZTF), we describe a search for candidate EM counterparts to binary black hole (BBH) mergers detected by LIGO/Virgo in O3. After removing probable false positives, we find nine candidate counterparts to BBH mergers during O3 (seven in O3a, two in O3b) with a p-value of 0.0019. Based on ZTF sky coverage, AGN geometry, and merger geometry, we expect \u22483(N_(BBH)/83)(f_(AGN)/0.5) potentially detectable EM counterparts from O3, where N_(BBH) is the total number of observed BBH mergers and f_(AGN) is the fraction originating in AGNs. Further modeling of breakout and flaring phenomena in AGN disks is required to reduce our false-positive rate. Two of the events are also associated with mergers with total masses >100 M_\u2299, which is the expected rate for O3 if hierarchical (large-mass) mergers occur in the AGN channel. Candidate EM counterparts in future GW observing runs can be better constrained by coverage of the Southern sky as well as spectral monitoring of unusual AGN flaring events in LIGO/Virgo alert volumes. A future set of reliable AGN EM counterparts to BBH mergers will yield an independent means of measuring cosmic expansion (H\u2080) as a function of redshift.", "date": "2023-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "942", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 99", "id_number": "CaltechAUTHORS:20230206-9587900.11", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230206-9587900.11", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1815034" }, { "agency": "NSF", "grant_number": "AST-1831412" }, { "agency": "NSF", "grant_number": "AST-2108402" }, { "agency": "NASA", "grant_number": "16-ADAP16-0232" }, { "agency": "Simons Foundation", "grant_number": "533845" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "PHY-2010970" }, { "agency": "NSF", "grant_number": "OAC-2117997" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "16-IDEX-0001 CAP 20-25" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" } ] }, "doi": "10.3847/1538-4357/aca480", "primary_object": { "basename": "Graham_2023_ApJ_942_99.pdf", "url": "https://authors.library.caltech.edu/records/zr9he-c2023/files/Graham_2023_ApJ_942_99.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Graham, Matthew J.; McKernan, Barry; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6jqva-j0p89", "eprint_id": 116515, "eprint_status": "archive", "datestamp": "2023-08-22 17:20:07", "lastmod": "2023-10-24 21:07:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Kramer-Emily-A", "name": { "family": "Kramer", "given": "Emily A." }, "orcid": "0000-0003-0457-2519" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "Andrew" } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Groom-Steven-L", "name": { "family": "Groom", "given": "Steven" }, "orcid": "0000-0001-5668-3507" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Discovery of the First Known Asteroid Confined within the Orbit of Venus", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant N0. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW.\n\nFollowing the final acceptance of this paper for publication Dr. Bryce Bolin elected to withdraw his name from the author list. We note that Dr. Bolin played a critical role in this discovery by recognizing the uniqueness of this object in the pipeline output and triggering timely follow-up. We thank him for his contributions to this paper.\n\nThe development of ZMODE and ZSTREAK and the search for asteroids in ZTF data are made possible by NASA grants 80NSSC19K0780 and 80NSSC21K0659. We acknowledge Dr. Robert Hurt's significant contribution to the generation of figures.\n\nThe authors wish to recognize and acknowledge the cultural significance that Palomar Mountain has for the Pauma Band of the Luise\u00f1o Indians, as well as the importance of the night sky to the Luise\u00f1o people. We are most fortunate to have the opportunity to conduct observations of the sky from this mountain.", "abstract": "We report on the discovery by the Zwicky Transient Facility of an asteroid orbiting entirely within the orbit of Venus, the first known example of this orbital class. The asteroid's perihelion is closer to the Sun than the aphelion of Mercury, and its diameter is estimated at about 1.8 km assuming an albedo of 0.2. The object was first observed on 2020 January 4 in four exposures obtained 7 minutes apart during an evening twilight survey. Its IAU-recognized designation is 594913 'Ayl\u00f3'chaxnim.", "date": "2022-08-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "935", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L6", "id_number": "CaltechAUTHORS:20220825-833128900.760", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220825-833128900.760", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NASA", "grant_number": "80NSSC19K0780" }, { "agency": "NASA", "grant_number": "80NSSC21K0659" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/2041-8213/ac8470", "resource_type": "article", "pub_year": "2022", "author_list": "Ip, Wing-Huen; Masci, Frank J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qgqdz-p2n39", "eprint_id": 114943, "eprint_status": "archive", "datestamp": "2023-08-20 07:23:05", "lastmod": "2023-10-24 15:16:05", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stein-Robert-D", "name": { "family": "Stein", "given": "Robert" }, "orcid": "0000-0003-2434-0387" }, { "name": { "family": "Reusch", "given": "Simeon" }, "orcid": "0000-0002-7788-628X" }, { "name": { "family": "Franckowiak", "given": "Anna" }, "orcid": "0000-0002-5605-2219" }, { "name": { "family": "Kowalski", "given": "Marek" }, "orcid": "0000-0001-8594-8666" }, { "name": { "family": "Necker", "given": "Jannis" }, "orcid": "0000-0003-0280-7484" }, { "name": { "family": "Weimann", "given": "Sven" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Ahumada", "given": "Tom\u00e1s" }, "orcid": "0000-0002-2184-6430" }, { "name": { "family": "Amaro Seoane", "given": "Pau" }, "orcid": "0000-0003-3993-3249" }, { "id": "Anand-Shreya-G", "name": { "family": "Anand", "given": "Shreya" }, "orcid": "0000-0003-3768-7515" }, { "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "name": { "family": "Coughlin", "given": "Michael" }, "orcid": "0000-0002-8262-2924" }, { "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew" }, "orcid": "0000-0002-3168-0139" }, { "id": "Groom-Steven-L", "name": { "family": "Groom", "given": "Steven L." }, "orcid": "0000-0001-5668-3507" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Karambelkar-Viraj-R", "name": { "family": "Karambelkar", "given": "Viraj" }, "orcid": "0000-0003-2758-159X" }, { "name": { "family": "Kong", "given": "Albert K. H." }, "orcid": "0000-0002-5105-344X" }, { "name": { "family": "Kool", "given": "Erik C." }, "orcid": "0000-0002-7252-3877" }, { "name": { "family": "Lincetto", "given": "Massimiliano" }, "orcid": "0000-0002-1460-3369" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "name": { "family": "Medford", "given": "Michael S." }, "orcid": "0000-0002-7226-0659" }, { "name": { "family": "Morgan", "given": "Robert" }, "orcid": "0000-0002-7016-5471" }, { "name": { "family": "Nordin", "given": "Jakob" }, "orcid": "0000-0001-8342-6274" }, { "id": "Rodriguez-Hector", "name": { "family": "Rodriguez", "given": "Hector" } }, { "id": "Sharma-Yashvi", "name": { "family": "Sharma", "given": "Yashvi" }, "orcid": "0000-0003-4531-1745" }, { "name": { "family": "van Santen", "given": "Jakob" }, "orcid": "0000-0002-2412-9728" }, { "name": { "family": "van Velzen", "given": "Sjoert" }, "orcid": "0000-0002-3859-8074" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Neutrino follow-up with the Zwicky Transient Facility: Results from the first 24 campaigns", "ispublished": "unpub", "full_text_status": "public", "keywords": "neutrinos \u2013 astroparticle physics \u2013 transients: tidal disruption events \u2013 transients: supernovae \u2013 gamma-ray bursts", "note": "R.S, and A.F. acknowledges support by the Initiative and Networking Fund of the Helmholtz Association through the Young Investigator Group program (A.F.). J.N. and S.R. acknowledges support by the Helmholtz Weizmann Research School on Multimessenger Astronomy, funded through the Initiative and Networking Fund of the Helmholtz Association, DESY, the Weizmann Institute, the Humboldt University of Berlin, and the University of Potsdam. ECK acknowledges support from the G.R.E.A.T research environment funded by Vetenskapsr\u00e5det, the Swedish Research Council, under project number 2016-06012, and support from The Wenner-Gren Foundations. \n\nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and AST-2034437, and a collaboration including Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Lawrence Berkeley National Laboratories, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, France, the University of Warwick, the University of Bochum, and Northwestern University. Operations are conducted by COO, IPAC, and UW. SED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). \n\nThe data presented herein were obtained in part 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\nBased on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT. \n\nThis research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2018, 2013). This research made use of Astroquery (Ginsburg et al. 2019), 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\nDATA AVAILABILITY. The data presented here, and the Python analysis code used to generate the figures and key results, will be provided by the authors upon reasonable request.\n\nSubmitted - 2203.17135.pdf
", "abstract": "The Zwicky Transient Transient Facility (ZTF) performs a systematic neutrino follow-up program, searching for optical counterparts to high-energy neutrinos with dedicated Target-of-Opportunity (ToO) observations. Since first light in March 2018, ZTF has taken prompt observations for 24 high-quality neutrino alerts from the IceCube Neutrino Observatory, with a median latency of 12.2 hours from initial neutrino detection. From two of these campaigns, we have already reported tidal disruption event (TDE) AT2019dsg and likely TDE AT2019fdr as probable counterparts, suggesting that TDEs contribute >7.8% of the astrophysical neutrino flux. We here present the full results of our program through to December 2021. No additional candidate neutrino sources were identified by our program, allowing us to place the first constraints on the underlying optical luminosity function of astrophysical neutrino sources. Transients with optical absolutes magnitudes brighter that -21 can contribute no more than 87% of the total, while transients brighter than -22 can contribute no more than 58% of the total, neglecting the effect of extinction. These are the the first observational constraints on the neutrino emission of bright populations such as superluminous supernovae. None of the neutrinos were coincident with bright optical AGN flares comparable to that observed for TXS 0506+056/IC170922A, suggesting that most astrophysical neutrinos are not produced during such optical flares. We highlight the outlook for electromagnetic neutrino follow-up programs, including the expected potential for the Rubin Observatory.", "date": "2022-06-01", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20220526-173305519", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220526-173305519", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF)" }, { "agency": "Helmholtz Weizmann Research School on Multimessenger Astronomy" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Humboldt University" }, { "agency": "University of Potsdam" }, { "agency": "Swedish Research Council", "grant_number": "2016-06012" }, { "agency": "Wenner-Gren Foundation" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "NSF", "grant_number": "AST-2034437" }, { "agency": "ZTF partner institutions" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" } ] }, "doi": "10.48550/arXiv.2203.17135", "primary_object": { "basename": "2203.17135.pdf", "url": "https://authors.library.caltech.edu/records/qgqdz-p2n39/files/2203.17135.pdf" }, "resource_type": "monograph", "pub_year": "2022", "author_list": "Stein, Robert; Reusch, Simeon; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/sbwhn-7d873", "eprint_id": 112545, "eprint_status": "archive", "datestamp": "2023-08-22 15:19:00", "lastmod": "2023-10-23 22:36:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Tracy-Xi", "name": { "family": "Chen", "given": "Tracy X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Schmitz-Marion", "name": { "family": "Schmitz", "given": "Marion" }, "orcid": "0000-0002-2055-7549" }, { "id": "Mazzarella-Joseph-M", "name": { "family": "Mazzarella", "given": "Joseph M." }, "orcid": "0000-0002-8204-8619" }, { "id": "Wu-Xiuqin", "name": { "family": "Wu", "given": "Xiuqin" }, "orcid": "0000-0002-4788-9236" }, { "id": "van-Eyken-Julian-C", "name": { "family": "van Eyken", "given": "Julian C." }, "orcid": "0000-0003-2192-5371" }, { "name": { "family": "Accomazzi", "given": "Alberto" }, "orcid": "0000-0002-4110-3511" }, { "id": "Akeson-Rachel-L", "name": { "family": "Akeson", "given": "Rachel L." }, "orcid": "0000-0001-9674-1564" }, { "id": "Allen-Mark-G", "name": { "family": "Allen", "given": "Mark" }, "orcid": "0000-0003-2168-0087" }, { "name": { "family": "Beaton", "given": "Rachael" }, "orcid": "0000-0002-1691-8217" }, { "id": "Berriman-G-Bruce", "name": { "family": "Berriman", "given": "G. Bruce" }, "orcid": "0000-0001-8388-534X" }, { "id": "Boyle-Andrew-W", "name": { "family": "Boyle", "given": "Andrew W." }, "orcid": "0000-0001-6037-2971" }, { "name": { "family": "Brouty", "given": "Marianne" }, "orcid": "0000-0002-0944-1211" }, { "id": "Chan-Ben-Hiu-Pan", "name": { "family": "Chan", "given": "Ben H. P." } }, { "id": "Christiansen-Jessie-L", "name": { "family": "Christiansen", "given": "Jessie L." }, "orcid": "0000-0002-8035-4778" }, { "id": "Ciardi-David-R", "name": { "family": "Ciardi", "given": "David R." }, "orcid": "0000-0002-5741-3047" }, { "id": "Cook-David-O", "name": { "family": "Cook", "given": "David" }, "orcid": "0000-0002-6877-7655" }, { "name": { "family": "D'Abrusco", "given": "Raffaele" }, "orcid": "0000-0003-3073-0605" }, { "id": "Ebert-Rick", "name": { "family": "Ebert", "given": "Rick" }, "orcid": "0000-0002-9500-8587" }, { "id": "Frayer-Cren", "name": { "family": "Frayer", "given": "Cren" } }, { "id": "Fulton-Benjamin-J", "name": { "family": "Fulton", "given": "Benjamin J." }, "orcid": "0000-0003-3504-5316" }, { "id": "Gelino-Christopher-R", "name": { "family": "Gelino", "given": "Christopher" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Henderson-Calen-B", "name": { "family": "Henderson", "given": "Calen B." }, "orcid": "0000-0001-8877-9060" }, { "id": "Howell-Justin-H", "name": { "family": "Howell", "given": "Justin" }, "orcid": "0000-0001-6028-8059" }, { "id": "Kim-Joyce", "name": { "family": "Kim", "given": "Joyce" } }, { "name": { "family": "Landais", "given": "Gilles" }, "orcid": "0000-0003-4868-5873" }, { "id": "Lo-Tak", "name": { "family": "Lo", "given": "Tak" } }, { "name": { "family": "Loup", "given": "C\u00e9cile" } }, { "name": { "family": "Madore", "given": "Barry" }, "orcid": "0000-0002-1576-1676" }, { "name": { "family": "Monari", "given": "Giacomo" }, "orcid": "0000-0002-6863-0661" }, { "name": { "family": "Muench", "given": "August" }, "orcid": "0000-0003-0666-6367" }, { "name": { "family": "Oberto", "given": "Ana\u00efs" }, "orcid": "0000-0001-7141-1542" }, { "name": { "family": "Ocvirk", "given": "Pierre" }, "orcid": "0000-0002-8488-504X" }, { "name": { "family": "Peek", "given": "Joshua E. G." }, "orcid": "0000-0003-4797-7030" }, { "name": { "family": "Perret", "given": "Emmanuelle" }, "orcid": "0000-0002-4068-8175" }, { "id": "Pevunova-Olga", "name": { "family": "Pevunova", "given": "Olga" } }, { "name": { "family": "Ramirez", "given": "Solange V." } }, { "id": "Rebull-Luisa-M", "name": { "family": "Rebull", "given": "Luisa" }, "orcid": "0000-0001-6381-515X" }, { "name": { "family": "Shemmer", "given": "Ohad" }, "orcid": "0000-0003-4327-1460" }, { "name": { "family": "Smale", "given": "Alan" }, "orcid": "0000-0001-9207-9796" }, { "id": "Tam-Raymond", "name": { "family": "Tam", "given": "Raymond" } }, { "id": "Terek-Scott", "name": { "family": "Terek", "given": "Scott" } }, { "name": { "family": "Van Orsow", "given": "Doug" }, "orcid": "0000-0001-8405-0264" }, { "name": { "family": "Vannier", "given": "Patricia" } }, { "id": "Wang-Shin-Ywan", "name": { "family": "Wang", "given": "Shin-Ywan" } } ] }, "title": "Best Practices for Data Publication in the Astronomical Literature", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy databases; Astronomical reference materials; Astronomical object identification; Astrometry; Astronomical coordinate systems; Photometry; Observatories; Telescopes", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 June 2; Revised 2022 March 21; Accepted 2022 March 28; Published 2022 May 4. \n\nWe thank Frank Timmes from Arizona State University for his helpful comments to improve this work. We appreciate the endorsement from the following colleagues: \n\n1. Kim Clube, Royal Astronomical Society, UK;\n2. Uta Grothkopf, European Southern Observatory, Germany;\n3. Mark Lacy, National Radio Astronomy Observatory, USA;\n4. Adam Leary, Oxford University Press, UK;\n5. Greg J. Schwarz, American Astronomical Society, USA.\n\nPublished - Chen_2022_ApJS_260_5.pdf
Submitted - 2106.01477.pdf
", "abstract": "We present an overview of best practices for publishing data in astronomy and astrophysics journals. These recommendations are intended as a reference for authors to help prepare and publish data in a way that will better represent and support science results, enable better data sharing, improve reproducibility, and enhance the reusability of data. Observance of these guidelines will also help to streamline the extraction, preservation, integration and cross-linking of valuable data from astrophysics literature into major astronomical databases, and consequently facilitate new modes of science discovery that will better exploit the vast quantities of panchromatic and multidimensional data associated with the literature. We encourage authors, journal editors, referees, and publishers to implement the best practices reviewed here, as well as related recommendations from international astronomical organizations such as the International Astronomical Union for publication of nomenclature, data, and metadata. A convenient Checklist of Recommendations for Publishing Data in the Literature (Appendix A) is included for authors to consult before the submission of the final version of their journal articles and associated data files. We recommend that publishers of journals in astronomy and astrophysics incorporate a link to this document in their Instructions to Authors.", "date": "2022-05", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "260", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 5", "id_number": "CaltechAUTHORS:20211217-233237912", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211217-233237912", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4365/ac6268", "primary_object": { "basename": "2106.01477.pdf", "url": "https://authors.library.caltech.edu/records/sbwhn-7d873/files/2106.01477.pdf" }, "related_objects": [ { "basename": "Chen_2022_ApJS_260_5.pdf", "url": "https://authors.library.caltech.edu/records/sbwhn-7d873/files/Chen_2022_ApJS_260_5.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Chen, Tracy X.; Schmitz, Marion; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/t21jf-jyk53", "eprint_id": 114224, "eprint_status": "archive", "datestamp": "2023-08-20 06:12:34", "lastmod": "2023-10-23 23:25:39", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" }, "orcid": "0000-0002-4749-2984" }, { "id": "Armus-Lee", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Benson-Andrew-J", "name": { "family": "Benson", "given": "Andrew" }, "orcid": "0000-0001-5501-6008" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Faisst-Andreas-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Gonzalez-Anthony-H", "name": { "family": "Gonzalez", "given": "Anthony" }, "orcid": "0000-0002-0933-8601" }, { "id": "Papovich-Casey-J", "name": { "family": "Papovich", "given": "Casey" }, "orcid": "0000-0001-7503-8482" }, { "id": "Ninkov-Zoran", "name": { "family": "Ninkov", "given": "Zoran" } }, { "id": "Robberto-Massimo", "name": { "family": "Robberto", "given": "Massimo" }, "orcid": "0000-0002-9573-3199" }, { "id": "Rose-Randall-J", "name": { "family": "Rose", "given": "Randall J." } }, { "id": "Rose-Thomas", "name": { "family": "Rose", "given": "Thomas" } }, { "id": "Scarlata-Claudia-M", "name": { "family": "Scarlata", "given": "Claudia" }, "orcid": "0000-0002-9136-8876" }, { "id": "Stanford-Specncer-A", "name": { "family": "Stanford", "given": "S. A." }, "orcid": "0000-0003-0122-0841" }, { "id": "Veach-Todd", "name": { "family": "Veach", "given": "Todd" } }, { "id": "Zhai-Zhongxu", "name": { "family": "Zhai", "given": "Zhongxu" }, "orcid": "0000-0001-7984-5476" }, { "id": "Benson-Bradford-A", "name": { "family": "Benson", "given": "Bradford" }, "orcid": "0000-0002-5108-6823" }, { "id": "Bleem-Lindsey-E", "name": { "family": "Bleem", "given": "L. E." }, "orcid": "0000-0001-7665-5079" }, { "id": "Davis-Michael-W", "name": { "family": "Davis", "given": "Michael W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne" } } ] }, "title": "Illuminating Galaxy Evolution at Cosmic Noon with ISCEA: the Infrared Satellite for Cosmic Evolution Astrophysics", "ispublished": "unpub", "full_text_status": "public", "note": "Attribution 4.0 International (CC BY 4.0).\n\nSubmitted - 2112.02387.pdf
", "abstract": "ISCEA (Infrared Satellite for Cosmic Evolution Astrophysics) is a small astrophysics mission whose Science Goal is to discover how galaxies evolved in the cosmic web of dark matter at cosmic noon. Its Science Objective is to determine the history of star formation and its quenching in galaxies as a function of local density and stellar mass when the Universe was 3-5 Gyrs old (1.2 < z < 2.1). ISCEA is designed to test the Science Hypothesis that during the period of cosmic noon, at 1.7 < z < 2.1, environmental quenching is the dominant quenching mechanism for typical galaxies not only in clusters and groups, but also in the extended cosmic web surrounding these structures. ISCEA meets its Science Objective by making a 10% shot noise measurement of star formation rate down to 6 M_\u2299\u2002 yr\u207b\u00b9 using H-\u03b1 out to a radius > 10 Mpc in each of 50 protocluster (cluster and cosmic web) fields at 1.2 < z < 2.1. ISCEA measures the star formation quenching factor in those fields, and galaxy kinematics with a precision < 50 km s\u207b\u00b9 to deduce the 3D spatial distribution in each field. ISCEA will transform our understanding of galaxy evolution at cosmic noon. \n\nISCEA is a small satellite observatory with a 30 cm equivalent diameter aperture telescope with a FoV of 0.32 deg\u00b2, and a multi-object spectrograph with a digital micro-mirror device (DMD) as its programmable slit mask. ISCEA will obtain spectra of 1000 galaxies simultaneously at an effective resolving power of R = 1000, with 2.8\" x 2.8\" slits, over the NIR wavelength range of 1.1 to 2.0 \u00b5m, a regime not accessible from the ground without large gaps in coverage. ISCEA will achieve a pointing accuracy of \u2264 2\" FWHM over 200s. ISCEA will be launched into a Low Earth Orbit, with a prime mission of 2.5 years. ISCEA's space-qualification of DMDs opens a new window for spectroscopy from space, enabling revolutionary advances in astrophysics.", "date": "2022-04-12", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20220411-225157319", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220411-225157319", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.2112.02387", "primary_object": { "basename": "2112.02387.pdf", "url": "https://authors.library.caltech.edu/records/t21jf-jyk53/files/2112.02387.pdf" }, "resource_type": "monograph", "pub_year": "2022", "author_list": "Wang, Yun; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zpgdx-8gs83", "eprint_id": 108539, "eprint_status": "archive", "datestamp": "2023-08-22 15:05:10", "lastmod": "2023-10-23 17:07:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Faisst-Andreas-L", "name": { "family": "Faisst", "given": "Andreas L." }, "orcid": "0000-0002-9382-9832" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga Ram" }, "orcid": "0000-0001-7583-0621" }, { "id": "Fajardo-Acosta-Sergio-B", "name": { "family": "Fajardo-Acosta", "given": "Sergio" }, "orcid": "0000-0001-9309-0102" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "Roberta" }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Benjamin" }, "orcid": "0000-0001-7648-4142" }, { "id": "Stickley-Nathaniel-R", "name": { "family": "Stickley", "given": "Nathaniel" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Weaver-John-R", "name": { "family": "Weaver", "given": "John R." }, "orcid": "0000-0003-1614-196X" }, { "id": "Brammer-Gabriel-B", "name": { "family": "Brammer", "given": "Gabriel" }, "orcid": "0000-0003-2680-005X" }, { "id": "Koekemoer-Anton-M", "name": { "family": "Koekemoer", "given": "Anton M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Miyatake-Hironao", "name": { "family": "Miyatake", "given": "Hironao" }, "orcid": "0000-0001-7964-9766" } ] }, "title": "Joint Survey Processing. I. Compact Oddballs in the COSMOS Field\u2014Low-luminosity Quasars at z > 6?", "ispublished": "pub", "full_text_status": "public", "keywords": "Surveys; Quasars; High-redshift galaxies; Photometry; Astronomical techniques", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 March 8; revised 2022 January 19; accepted 2022 February 28; published 2022 April 13. \n\nWe thank E. Merlin for providing an updated TPhot version and technical support, and the anonymous referee for a constructive feedback on our manuscript. This research is partially funded by the Joint Survey Processing effort at IPAC/Caltech through NASA grant NNN12AA01C. 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. \n\nThe Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the Faint Images of the Radio Sky at Twenty cm (FIRST) program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. \n\nThis paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org. \n\nBased in part on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center at National Astronomical Observatory of Japan. \n\nSoftware: Astropy 3 (Astropy Collaboration et al. 2013, 2018), Tractor (Lang et al. 2016a, 2016b; Weaver et al. 2022), Photutils (Bradley et al. 2019), SExtractor (Bertin & Arnouts 1996), PSFex (Bertin 2011), TPhot (Merlin et al. 2015, 2016), SkyMaker (Bertin 2009).\n\nPublished - Faisst_2022_ApJ_929_66.pdf
Submitted - 2103.09836.pdf
", "abstract": "The faint-end slope of the quasar luminosity function at z \u223c 6 and its implication on the role of quasars in reionizing the intergalactic medium at early times has been an outstanding problem for some time. The identification of faint high-redshift quasars with luminosities of <10^(44.5) erg s\u207b\u00b9 is challenging. They are rare (few per square degree), and the separation of these unresolved quasars from late-type stars and compact star-forming galaxies is difficult from ground-based observations alone. In addition, source confusion becomes significant at >25 mag, with \u223c30% of sources having their flux contaminated by foreground objects when the seeing resolution is \u223c0''.7. We mitigate these issues by performing a pixel-level joint processing of ground and space-based data from Subaru/Hyper-SuprimeCam (HSC) and Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS). We create a deconfused catalog over the 1.64 deg\u00b2 of the COSMOS field, after accounting for spatial varying point-spread functions and astrometric differences between the two data sets. We identify twelve low-luminosity (M_(UV) \u223c \u221221 mag) z > 6 quasar candidates through (i) their red color measured between ACS/F814W and HSC/i band and (ii) their compactness in the space-based data. Nondetections of our candidates in Hubble DASH data argues against contamination from late-type stars. Our constraints on the faint end of the quasar luminosity function at z \u223c 6.4 suggest a negligibly small contribution to reionization compared to the star-forming galaxy population. The confirmation of our candidates and the evolution of number density with redshift could provide better insights into how supermassive galaxies grew in the first billion years of cosmic time.", "date": "2022-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "929", "number": "1", "publisher": "American Physical Society", "pagerange": "Art. No. 66", "id_number": "CaltechAUTHORS:20210323-151326953", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210323-151326953", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNN12AA01C" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/ac59b3", "primary_object": { "basename": "2103.09836.pdf", "url": "https://authors.library.caltech.edu/records/zpgdx-8gs83/files/2103.09836.pdf" }, "related_objects": [ { "basename": "Faisst_2022_ApJ_929_66.pdf", "url": "https://authors.library.caltech.edu/records/zpgdx-8gs83/files/Faisst_2022_ApJ_929_66.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Faisst, Andreas L.; Chary, Ranga Ram; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cbqa1-mky83", "eprint_id": 112310, "eprint_status": "archive", "datestamp": "2023-08-22 11:50:19", "lastmod": "2023-10-23 21:01:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dib-Sami", "name": { "family": "Dib", "given": "Sami" }, "orcid": "0000-0002-8697-9808" }, { "id": "Braine-Jonathan", "name": { "family": "Braine", "given": "Jonathan" }, "orcid": "0000-0003-1740-1284" }, { "id": "Gopinathan-Maheswar", "name": { "family": "Gopinathan", "given": "Maheswar" }, "orcid": "0000-0002-1369-0608" }, { "id": "Lara-L\u00f3pez-Maritza-A", "name": { "family": "Lara-L\u00f3pez", "given": "Maritza A." }, "orcid": "0000-0001-7327-3489" }, { "id": "Kravtsov-Valery-V", "name": { "family": "Kravtsov", "given": "Valery V." }, "orcid": "0000-0002-9799-5889" }, { "id": "Soam-Archana", "name": { "family": "Soam", "given": "Archana" }, "orcid": "0000-0002-6386-2906" }, { "id": "Sharma-Ekta", "name": { "family": "Sharma", "given": "Ekta" } }, { "id": "Zhukovska-Svitlana", "name": { "family": "Zhukovska", "given": "Svitlana" }, "orcid": "0000-0003-2569-3627" }, { "id": "Aouad-Charles", "name": { "family": "Aouad", "given": "Charles" }, "orcid": "0000-0001-6063-0344" }, { "id": "Belinch\u00f3n-Jos\u00e9-Antonio", "name": { "family": "Belinch\u00f3n", "given": "Jos\u00e9 Antonio" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Li-Di", "name": { "family": "Li", "given": "Di" } } ] }, "title": "The structure and characteristic scales of the H\u202fI gas in galactic disks", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: structure / ISM: general / galaxies: structure / galaxies: ISM / radio lines: ISM / turbulence; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 S. Dib et al. 2021. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nOpen Access funding provided by Max Planck Society. \n\nReceived: 15 July 2021 Accepted: 30 September 2021. \n\nThis work is dedicated to the city of Beirut and to its inhabitants for their resilience in the face of adversity. We thank the referee for a careful reading of the paper and for constructive comments. S.D. would like to thank Volker Ossenkopf-Okada for useful discussions on the calculation of the \u0394-variance spectrum and Andreas Schruba and Robert Kennicutt for useful discussions on the star formation rates in nearby galaxies. We also thank Bruce Elmegreen for commenting on an earlier version of this paper and Elias Brinks and Fabian Walter for clarifications on the THINGS data. We thank Oscar Agertz and Florent Renaud for making data from their simulation available. J.A.B. was supported by Comision Nacional de Ciencias Y Tecnologia through Fondecyt Grant No. 11170083.\n\nPublished - aa41803-21.pdf
", "abstract": "The spatial distribution of the H\u202fI gas in galactic disks holds important clues about the physical processes that shape the structure and dynamics of the interstellar medium (ISM). The structure of the ISM could be affected by a variety of perturbations internal and external to the galaxy, and the unique signature of each of these perturbations could be visible in the structure of interstellar gas. In this work, we quantify the structure of the H\u202fI gas in a sample of 33 nearby galaxies taken from the HI Nearby Galaxy Survey (THINGS) using the delta-variance (\u0394-variance) spectrum. The THINGS galaxies display a large diversity in their spectra, but there are a number of recurrent features. In many galaxies, we observe a bump in the spectrum on scales of a few to several hundred parsec. We find the characteristic scales associated with the bump to be correlated with the galactic star formation rate (SFR) for values of the SFR \u22730.5 M_\u2299 yr\u207b\u00b9 and also with the median size of the H\u202fI shells detected in these galaxies. We interpret this characteristic scale as being associated with the effects of feedback from supernova explosions. On larger scales, we observe in most galaxies two self-similar, scale-free regimes. The first regime, on intermediate scales (\u22720.5R\u2082\u2085), is shallow, and the power law that describes this regime has an exponent in the range [0.1\u20131] with a mean value of 0.55 that is compatible with the density field that is generated by supersonic turbulence in the cold phase of the H\u202fI gas. The second power law is steeper, with a range of exponents between 0.5 and 2.3 and a mean value of \u22481.5. These values are associated with subsonic to transonic turbulence, which is characteristic of the warm phase of the H\u202fI gas. The spatial scale at which the transition between the two self-similar regimes occurs is found to be \u22480.5R25, which is very similar to the size of the molecular disk in the THINGS galaxies. Overall, our results suggest that on scales \u22720.5R\u2082\u2085, the structure of the ISM is affected by the effects of supernova explosions. On larger scales (\u22730.5R\u2082\u2085), stellar feedback has no significant impact, and the structure of the ISM is determined by large-scale processes that govern the dynamics of the gas in the warm neutral medium, such as the flaring of the H\u202fI disk at large galactocentric radii and the effects of ram pressure stripping.", "date": "2021-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "655", "publisher": "EDP Sciences", "pagerange": "Art. No. A101", "id_number": "CaltechAUTHORS:20211208-951186000", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211208-951186000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "11170083" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/202141803", "primary_object": { "basename": "aa41803-21.pdf", "url": "https://authors.library.caltech.edu/records/cbqa1-mky83/files/aa41803-21.pdf" }, "resource_type": "article", "pub_year": "2021", "author_list": "Dib, Sami; Braine, Jonathan; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/eg5pz-meb32", "eprint_id": 108632, "eprint_status": "archive", "datestamp": "2023-08-22 10:26:54", "lastmod": "2023-10-23 17:38:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Caiazzo-Ilaria", "name": { "family": "Caiazzo", "given": "Ilaria" }, "orcid": "0000-0002-4770-5388" }, { "id": "Burdge-Kevin-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Fuller-J", "name": { "family": "Fuller", "given": "James" }, "orcid": "0000-0002-4544-0750" }, { "id": "Heyl-Jeremy", "name": { "family": "Heyl", "given": "Jeremy" }, "orcid": "0000-0001-9739-367X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Richer-Harvey-B", "name": { "family": "Richer", "given": "Harvey B." }, "orcid": "0000-0001-9002-8178" }, { "id": "Schwab-Josiah", "name": { "family": "Schwab", "given": "Josiah" }, "orcid": "0000-0002-4870-8855" }, { "id": "Andreoni-Igor", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew" } }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "id": "Soumagnac-Maayane-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" } ] }, "title": "A highly magnetized and rapidly rotating white dwarf as small as the Moon", "ispublished": "pub", "full_text_status": "public", "keywords": "Astrophysical magnetic fields; Compact astrophysical objects; Stellar evolution", "note": "\u00a9 2021 Nature Publishing Group. \n\nReceived 27 October 2020; Accepted 05 May 2021; Published 30 June 2021. \n\nThe authors thank S.-C. Leung and S. Phinney for discussions, and N. Reindl and M. Kilic for comments. I.C. is a Sherman Fairchild Fellow at Caltech and thanks the Burke Institute at Caltech for supporting her research. J.F. acknowledges support through an Innovator Grant from the Rose Hills Foundation, and the Sloan Foundation through grant FG-2018-10515. K.B.B. thanks NASA and the Heising Simons Foundation for supporting his research. J.S. is supported by the A. F. Morrison Fellowship in Lick Observatory and by the US National Science Foundation (NSF) through grant ACI-1663688. This work is based on observations obtained with the Samuel Oschin 48-inch telescope and the Palomar Observatory 60-inch telescope as part of the ZTF project. ZTF is supported by the NSF under grant no. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by Caltech Optical Observatories, IPAC and the University of Washington. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by 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, the 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, NASA under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, NSF grant no. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This work was supported by the Natural Sciences and Engineering Research Council of Canada. \n\nData availability: Upon request, I.C. will provide the reduced photometric lightcurves and spectroscopic data, and available ZTF data for the object. The spectroscopic data and photometric lightcurves are also available in the GitHub repository https://github.com/ilac/ZTF-J1901-1458. ZTF data are accessible in the ZTF database. The astrometric and photometric data are already in the public domain, and they are readily accessible in the Gaia and Pan-STARSS catalogues and in the Swift database. \n\nCode availability: We used the pyphot package (https://mfouesneau.github.io/docs/pyphot/) and the corner.py package. The LRIS spectra were reduced using the Lpipe pipeline. Upon request, I.C. will provide the code used to analyse the spectroscopic and photometric data. \n\nAuthor Contributions: I.C. reduced the ultraviolet data, conducted the spectral and photometric analysis, identified the magnetic field and is the primary author of the manuscript. K.B.B. performed the period search on ZTF data and reduced the optical data. I.C. and J.H. conducted the mass\u2013radius analysis. I.C., K.B.B., J.F., J.H., S.R.K., T.A.P., H.B.R. and J.S. contributed to the physical interpretation of the object. J.S. constructed preliminary MESA models for the object. I.A., A.D., D.A.D., A.A.M., F.J.M., R.S. and M.T.S. contributed to the implementation of ZTF. G.H. is a co-PI of the ZTF Mid-Scale Innovations Program (MSIP). M.J.G. is the project scientist, E.C.B. is the survey scientist, T.A.P. is the co-PI and S.R.K. is the PI of ZTF. \n\nThe authors declare no competing interests. \n\nPeer review information: Nature thanks the anonymous reviewers for their contribution to the peer review of this work.\n\nCaiazzo, I., Burdge, K.B., Fuller, J. et al. Publisher Correction: A highly magnetized and rapidly rotating white dwarf as small as the Moon. Nature (2021). https://doi.org/10.1038/s41586-021-03799-3\n\nSubmitted - v1_stamped.pdf
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Supplemental Material - 41586_2021_3615_Fig7_ESM.webp
Supplemental Material - 41586_2021_3615_Fig8_ESM.webp
Supplemental Material - 41586_2021_3615_Fig9_ESM.webp
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", "abstract": "White dwarfs represent the last stage of evolution of stars with mass less than about eight times that of the Sun and, like other stars, are often found in binaries. If the orbital period of the binary is short enough, energy losses from gravitational-wave radiation can shrink the orbit until the two white dwarfs come into contact and merge. Depending on the component masses, the merger can lead to a supernova of type Ia or result in a massive white dwarf. In the latter case, the white dwarf remnant is expected to be highly magnetized because of the strong magnetic dynamo that should arise during the merger, and be rapidly spinning from the conservation of the orbital angular momentum. Here we report observations of a white dwarf, ZTF J190132.9+145808.7, that exhibits these properties, but to an extreme: a rotation period of 6.94 minutes, a magnetic field ranging between 600 megagauss and 900 megagauss over its surface, and a stellar radius of 2140+160\u22122302140\u2212230+160 kilometres, only slightly larger than the radius of the Moon. Such a small radius implies that the star's mass is close to the maximum white dwarf mass, or Chandrasekhar mass. ZTF J190132.9+145808.7 is likely to be cooling through the Urca processes (neutrino emission from electron capture on sodium) because of the high densities reached in its core.", "date": "2021-07-01", "date_type": "published", "publication": "Nature", "volume": "595", "number": "7865", "publisher": "Nature Publishing Group", "pagerange": "39-42", "id_number": "CaltechAUTHORS:20210406-112053159", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210406-112053159", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "Rose Hills Foundation" }, { "agency": "Alfred P. Sloan Foundation", "grant_number": "FG-2018-10515" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "Heising-Simons Foundation" }, { "agency": "Lick Observatory" }, { "agency": "NSF", "grant_number": "ACI-1663688" }, { "agency": "ZTF partner institutions" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Gaia Multilateral Agreement" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/s41586-021-03615-y", "primary_object": { "basename": "41586_2021_3615_Fig5_ESM.webp", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Fig5_ESM.webp" }, "related_objects": [ { "basename": "41586_2021_3615_Fig6_ESM.webp", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Fig6_ESM.webp" }, { "basename": "41586_2021_3615_Fig7_ESM.webp", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Fig7_ESM.webp" }, { "basename": "41586_2021_3615_Fig8_ESM.webp", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Fig8_ESM.webp" }, { "basename": "41586_2021_3615_Fig9_ESM.webp", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Fig9_ESM.webp" }, { "basename": "41586_2021_3615_Tab1_ESM.jpg", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Tab1_ESM.jpg" }, { "basename": "41586_2021_3615_Tab2_ESM.jpg", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/41586_2021_3615_Tab2_ESM.jpg" }, { "basename": "v1_stamped.pdf", "url": "https://authors.library.caltech.edu/records/eg5pz-meb32/files/v1_stamped.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Caiazzo, Ilaria; Burdge, Kevin B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0k4f2-j9t41", "eprint_id": 109400, "eprint_status": "archive", "datestamp": "2023-08-20 03:17:44", "lastmod": "2023-10-23 17:55:06", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "name": { "family": "Lunnan", "given": "Ragnhild" }, "orcid": "0000-0001-9454-4639" }, { "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Schulze", "given": "Steve" }, "orcid": "0000-0001-6797-1889" }, { "id": "Das-Kaustav-K", "name": { "family": "Das", "given": "Kaustav K." } }, { "name": { "family": "Dobie", "given": "Dougal" }, "orcid": "0000-0003-0699-7019" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott" }, "orcid": "0000-0001-5855-5939" }, { "id": "Anand-Shreya", "name": { "family": "Anand", "given": "Shreya" }, "orcid": "0000-0003-3768-7515" }, { "id": "Andreoni-Igor", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "Bruch", "given": "Rachel J." }, "orcid": "0000-0001-8208-2473" }, { "id": "Burdge-Kevin-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "name": { "family": "Castro-Tirado", "given": "Alberto J." } }, { "id": "Dahiwale-Aishwarya-S", "name": { "family": "Dahiwale", "given": "Aishwarya" } }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew J." } }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Karambelkar-Viraj-R", "name": { "family": "Karambelkar", "given": "Viraj" }, "orcid": "0000-0003-2758-159X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "name": { "family": "Kool", "given": "Erik C." }, "orcid": "0000-0002-7252-3877" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "name": { "family": "Medford", "given": "Michael S." }, "orcid": "0000-0002-7226-0659" }, { "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "name": { "family": "Nordin", "given": "Jakob" }, "orcid": "0000-0001-8342-6274" }, { "name": { "family": "Ofek", "given": "Eran" }, "orcid": "0000-0002-6786-8774" }, { "name": { "family": "Petitpas", "given": "Glen" } }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Sharma-Yashvi", "name": { "family": "Sharma", "given": "Yashvi" }, "orcid": "0000-0003-4531-1745" }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "name": { "family": "Stewart", "given": "Adam J." } }, { "name": { "family": "Taggart", "given": "Kirsty" }, "orcid": "0000-0002-5748-4558" }, { "name": { "family": "Tartaglia", "given": "Leonardo" }, "orcid": "0000-0003-3433-1492" }, { "id": "Tzanidakis-Anastasios", "name": { "family": "Tzanidakis", "given": "Anastasios" }, "orcid": "0000-0003-0484-3331" }, { "name": { "family": "Winters", "given": "Jan Martin" } } ] }, "title": "The Photometric and Spectroscopic Evolution of Rapidly Evolving Extragalactic Transients in ZTF", "ispublished": "unpub", "full_text_status": "public", "note": "A.Y.Q.H. would like to thank Schuyler van Dyk for a thorough reading of the manuscript; Eliot Quataert, Dan Kasen, and Peter Nugent for useful discussions; and Miika Pursiainen for generously sharing the data for the DES objects. A.G.Y.'s research is supported by the EU via ERC grant No. 725161, the ISF GW excellence center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as The Benoziyo Endowment Fund for the Advancement of Science, the Deloro Institute for Advanced Research in Space and Optics, The Veronika A. Rabl Physics Discretionary Fund, Minerva, Yeda-Sela and the Schwartz/Reisman Collaborative Science Program; A.G.Y. is the recipient of the Helen and Martin Kimmel Award for Innovative Investigation. R.L. acknowledges support from a Marie Sk\u0142odowska-Curie Individual Fellowship within the Horizon 2020 European Union (EU) Framework Programme for Research and Innovation (H2020-MSCA-IF-2017-794467). \n\nD.K. is supported by NSF grant AST-1816492. E.C.K. acknowledges support from the G.R.E.A.T research environment funded by Vetenskapsr\u00e5det, the Swedish Research Council, under project number 2016-06012, and support from The Wenner-Gren Foundations. A.A.M. is funded by the Large Synoptic Survey Telescope Corporation (LSSTC), the Brinson Foundation, and the Moore Foundation in support of the LSSTC Data Science Fellowship Program; he also receives support as a CIERA Fellow by the CIERA Postdoctoral Fellowship Program (Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University). E.O.O. acknowledges support from the Israeli Science Foundation, The Israeli Ministry of Science, The Bi-National Science foundation, and Minerva. A.J.C.T. acknowledges Y.-D. Hu and A. F. Azamat for their assistance regarding the GTC observation. L.T. acknowledges support from MIUR (PRIN 2017 grant 20179ZF5KS). \n\nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). The GROWTH Marshal was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. \n\nSED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundaci\u00f3n Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. \n\nSome 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This work is based on observations carried out under project number S19BC with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The Australian SKA Pathfinder is part of the Australia Telescope National Facility which is managed by CSIRO. Operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. ASKAP uses the resources of the Pawsey Supercomputing Centre. Establishment of ASKAP, the Murchison Radioastronomy Observatory and the Pawsey Supercomputing Centre are initiatives of the Australian Government, with support from the Government of Western Australia and the Science and Industry Endowment Fund. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE170100004. \n\nThis research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018). The ztfquery code was funded by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement n\u00b0759194 - USNAC, PI: Rigault). \n\nThe Legacy Surveys consist of three individual and complementary projects: the Dark Energy Camera Legacy Survey (DECaLS; Proposal ID #2014B-0404; PIs: David Schlegel and Arjun Dey), the Beijing-Arizona Sky Survey (BASS; NOAO Prop. ID #2015A-0801; PIs: Zhou Xu and Xiaohui Fan), and the Mayall z-band Legacy Survey (MzLS; Prop. ID #2016A-0453; PI: Arjun Dey). DECaLS, BASS and MzLS together include data obtained, respectively, at the Blanco telescope, Cerro Tololo Inter-American Observatory, NSF's NOIRLab; the Bok telescope, Steward Observatory, University of Arizona; and the Mayall telescope, Kitt Peak National Observatory, NOIRLab. The Legacy Surveys project is honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham Nation. \n\nThis project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. The Legacy Survey team makes use of data products from the Near-Earth Object Wide-Field Infrared Survey Explorer (NEOWISE), which is a project of the Jet Propulsion Laboratory/California Institute of Technology. NEOWISE is funded by the National Aeronautics and Space Administration. The Legacy Surveys imaging of the DESI footprint is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under Contract No. DE-AC02-05CH1123, by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; and by the U.S. National Science Foundation, Division of Astronomical Sciences under Contract No. AST-0950945 to NOAO.\n\nFacilities: Hale, Swift, EVLA, VLA, Liverpool:2m, PO:1.2m, PO:1.5m, NOT, GTC, Sloan, AAVSO, ASKAP, Keck:1, IRAM:NOEMA, SMA, MMT, TNG, ASKAP, GALEX, PS1, CTIO:2MASS, FLWO:2MASS, WISE, NEOWISE, Blanco \n\nSoftware: CASA (McMullin et al. 2007), astropy (Astropy Collaboration et al. 2013, 2018), matplotlib (Hunter 2007), scipy (Virtanen et al. 2020), ztfquery (Rigault 2018), extinction, penquins\n\nSubmitted - 2105.08811.pdf
", "abstract": "We present 42 rapidly evolving (time spent above half-maximum brightness t_(1/2) \u227e 12d) extragalactic transients from Phase I of the Zwicky Transient Facility (ZTF), of which 22 have spectroscopic classifications. This is one of the largest systematically selected samples of day-timescale transients, and the first with spectroscopic classifications. Most can be classified as core-collapse supernovae (SNe), and we identify several predominant subtypes: (1) subluminous Type IIb or Type Ib SNe; (2) luminous Type Ibn or hybrid IIn/Ibn SNe; and (3) radio-loud, short-duration luminous events similar to AT2018cow. We conclude that rates quoted in the literature for rapidly evolving extragalactic transients are dominated by the subluminous events (mostly Type IIb SNe). From our spectroscopic classifications and radio, X-ray, and millimeter-band upper limits, we are motivated to consider the AT2018cow-like objects a distinct class, and use ZTF's systematic classification experiments to calculate that their rate does not exceed 0.1% of the local core-collapse SN rate, in agreement with previous work. By contrast, most other events are simply the extreme of a continuum of established SN types extending to ordinary timescales. The light curves of our objects are very similar to those of unclassified events in the literature, illustrating how spectroscopically classified samples of low-redshift objects in shallow surveys like ZTF can be used to photometrically classify larger numbers of events at higher redshift.", "date": "2021-06-07", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20210604-142559558", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210604-142559558", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Israel Science Foundation" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Benoziyo Endowment Fund for the Advancement of Science" }, { "agency": "Deloro Institute for Advanced Research in Space and Optics" }, { "agency": "Veronika A. Rabl Physics Discretionary Fund" }, { "agency": "MINERVA (Israel)" }, { "agency": "Yeda-Sela" }, { "agency": "Schwartz/Reisman Collaborative Science Program" }, { "agency": "Helen and Martin Kimmel Award" }, { "agency": "Marie Curie Fellowship", "grant_number": "794467" }, { "agency": "NSF", "grant_number": "AST-1816492" }, { "agency": "Swedish Research Council", "grant_number": "2016-06012" }, { "agency": "Wenner-Gren Foundations" }, { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Brinson Foundation" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)" }, { "agency": "Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)", "grant_number": "20179ZF5KS" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Australian Research Council", "grant_number": "CE170100004" }, { "agency": "European Research Council (ERC)", "grant_number": "759194" }, { "agency": "Dark Energy Survey (DES) collaboration" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "AST-0950945" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.48550/arXiv.2105.08811", "primary_object": { "basename": "2105.08811.pdf", "url": "https://authors.library.caltech.edu/records/0k4f2-j9t41/files/2105.08811.pdf" }, "resource_type": "monograph", "pub_year": "2021", "author_list": "Ho, Anna Y. Q.; Perley, Daniel A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/eetsq-a3251", "eprint_id": 108842, "eprint_status": "archive", "datestamp": "2023-08-22 09:43:21", "lastmod": "2023-10-23 17:22:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "Bryce T." }, "orcid": "0000-0002-4950-6323" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kelley-Michael-S-P", "name": { "family": "Kelley", "given": "Michael S. P." }, "orcid": "0000-0002-6702-7676" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "Michael W." }, "orcid": "0000-0002-8262-2924" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Soumagnac-Maayane-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "van-der-Walt-St\u00e9fan-J", "name": { "family": "van der Walt", "given": "St\u00e9fan J." }, "orcid": "0000-0001-9276-1891" } ] }, "title": "Tails: Chasing Comets with the Zwicky Transient Facility and Deep Learning", "ispublished": "pub", "full_text_status": "public", "keywords": "Astroinformatics; Astronomy data analysis; Convolutional neural networks; Comets", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 January 11; revised 2021 February 23; accepted 2021 February 25; published 2021 April 8. \n\nD.A. Duev would like to thank Ivan Duev for assistance with data labeling. D.A. Duev acknowledges support from Google Cloud and from the Heising-Simons Foundation under grant No. 12540303. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThis research has made use of data and/or services provided by the International Astronomical Union's Minor Planet Center. \n\nThe authors would like to express gratitude to the anonymous referee. \n\nFacilities: PO:1.2 m - , ZTF - . \n\nSoftware: astropy (Astropy Collaboration et al. 2018), Fritz (https://github.com/fritz-marshal/fritz), Kowalski (Duev et al. 2019), matplotlib (Hunter 2007), numpy (Harris et al. 2020), pandas (Pandas Development Team 2020), pypride (Duev et al. 2016), SEP (Barbary 2016), sbpy (Mommert et al. 2019), TensorFlow (Abadi et al. 2016), ZChecker (Kelley et al. 2019).\n\nPublished - Duev_2021_AJ_161_218.pdf
Accepted Version - 2102.13352.pdf
", "abstract": "We present Tails, an open-source deep-learning framework for the identification and localization of comets in the image data of the Zwicky Transient Facility (ZTF), a robotic optical time-domain survey currently in operation at the Palomar Observatory in California, USA. Tails employs a custom EfficientDet-based architecture and is capable of finding comets in single images in near real time, rather than requiring multiple epochs as with traditional methods. The system achieves state-of-the-art performance with 99% recall, a 0.01% false-positive rate, and a 1\u20132 pixel rms error in the predicted position. We report the initial results of the Tails efficiency evaluation in a production setting on the data of the ZTF Twilight survey, including the first AI-assisted discovery of a comet (C/2020 T2) and the recovery of a comet (P/2016 J3 = P/2021 A3).", "date": "2021-05", "date_type": "published", "publication": "Astronomical Journal", "volume": "161", "number": "5", "publisher": "American Astronomical Society", "pagerange": "Art. No. 218", "id_number": "CaltechAUTHORS:20210423-164903652", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210423-164903652", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Google Cloud" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-3881/abea7b", "primary_object": { "basename": "2102.13352.pdf", "url": "https://authors.library.caltech.edu/records/eetsq-a3251/files/2102.13352.pdf" }, "related_objects": [ { "basename": "Duev_2021_AJ_161_218.pdf", "url": "https://authors.library.caltech.edu/records/eetsq-a3251/files/Duev_2021_AJ_161_218.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Duev, Dmitry A.; Bolin, Bryce T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fce15-fnz52", "eprint_id": 109340, "eprint_status": "archive", "datestamp": "2023-08-20 03:01:49", "lastmod": "2023-10-23 17:51:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sutter-Jessica-S", "name": { "family": "Sutter", "given": "Jessica" }, "orcid": "0000-0002-9183-8102" }, { "id": "Dale-Daniel-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Sandstrom-Karin-M", "name": { "family": "Sandstrom", "given": "Karin" }, "orcid": "0000-0002-4378-8534" }, { "id": "Smith-John-David-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Bolatto-Alberto-D", "name": { "family": "Bolatto", "given": "Alberto" }, "orcid": "0000-0002-5480-5686" }, { "id": "Boquien-M\u00e9d\u00e9ric", "name": { "family": "Boquien", "given": "M\u00e9d\u00e9ric" }, "orcid": "0000-0003-0946-6176" }, { "id": "Calzetti-Daniela", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Croxall-Kevin-V", "name": { "family": "Croxall", "given": "Kevin V." }, "orcid": "0000-0002-5258-7224" }, { "id": "De-Looze-Ilse", "name": { "family": "De\u00a0Looze", "given": "Ilse" } }, { "id": "Galametz-Maud", "name": { "family": "Galametz", "given": "Maud" }, "orcid": "0000-0002-0283-8689" }, { "id": "Groves-Brent-A", "name": { "family": "Groves", "given": "Brent A." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Herrera-Camus-Rodrigo", "name": { "family": "Herrera-Camus", "given": "Rodrigo" }, "orcid": "0000-0002-2775-0595" }, { "id": "Hunt-Leslie-K", "name": { "family": "Hunt", "given": "Leslie K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Kennicutt-Robert-C-Jr", "name": { "family": "Kennicutt", "given": "Robert C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Pelligrini-Eric-W", "name": { "family": "Pelligrini", "given": "Eric W." } }, { "id": "Wilson-Christine-D", "name": { "family": "Wilson", "given": "Christine" }, "orcid": "0000-0001-5817-0991" }, { "id": "Wolfire-Mark-G", "name": { "family": "Wolfire", "given": "Mark G." }, "orcid": "0000-0003-0030-9510" } ] }, "title": "The case for thermalization as a contributor to the [C\u2009II] deficit", "ispublished": "pub", "full_text_status": "public", "keywords": "(ISM:) HII Regions \u2013 (ISM:) photodissociation regions \u2013 galaxies: ISM", "note": "\u00a9 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2021 February 16. Received 2021 February 1; in original form 2020 December 9. Published: 20 February 2021. \n\nThis work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, Grant #80NSSC18K1107, as the Wyoming NASA Space Grant Consortium, NASA Grant #NNX15AI08H. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. IRAF, the Image Reduction and Analysis Facility, has been developed by the National Optical Astronomy Observatories and the Space Telescope Science Institute. \n\nData Availability: All data are available through IRSA through the KINGFISH database at https://irsa.ipac.caltech.edu/data/Herschel/KINGFISH/ with the exception of the SPIRE spectroscopy, which is available upon request.\n\nPublished - stab490.pdf
Accepted Version - 2102.08865.pdf
", "abstract": "The [C\u2009II] deficit, which describes the observed decrease in the ratio of [C\u2009II] 158 \u03bcm emission to continuum infrared emission in galaxies with high star formation surface densities, places a significant challenge to the interpretation of [C\u2009II] detections from across the observable universe. In an attempt to further decode the cause of the [C\u2009II] deficit, the [C\u2009II] and dust continuum emission from 18 Local Volume galaxies has been split based on conditions within the interstellar medium where it originated. This is completed using the Key Insights in Nearby Galaxies: a Far-Infrared Survey with Herschel (KINGFISH) and Beyond the Peak (BtP) surveys and the wide-range of wavelength information, from UV to far-infrared emission lines, available for a selection of star-forming regions within these samples. By comparing these subdivided [C\u2009II] emissions to isolated infrared emission and other properties, we find that the thermalization (collisional de-excitation) of the [C\u2009II] line in H\u2009II regions plays a significant role in the deficit observed in our sample.", "date": "2021-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "503", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "911-919", "id_number": "CaltechAUTHORS:20210602-100900704", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210602-100900704", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "80NSSC18K1107" }, { "agency": "Wyoming NASA Space Grant Consortium" }, { "agency": "NASA", "grant_number": "NNX15AI08H" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stab490", "primary_object": { "basename": "2102.08865.pdf", "url": "https://authors.library.caltech.edu/records/fce15-fnz52/files/2102.08865.pdf" }, "related_objects": [ { "basename": "stab490.pdf", "url": "https://authors.library.caltech.edu/records/fce15-fnz52/files/stab490.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Sutter, Jessica; Dale, Daniel A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zxezj-0ma96", "eprint_id": 106895, "eprint_status": "archive", "datestamp": "2023-08-22 09:02:01", "lastmod": "2023-10-23 15:09:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "Bryce T." }, "orcid": "0000-0002-4950-6323" }, { "name": { "family": "Fernandez", "given": "Yanga R." }, "orcid": "0000-0003-1156-9721" }, { "name": { "family": "Lisse", "given": "Carey M." }, "orcid": "0000-0002-9548-1526" }, { "name": { "family": "Holt", "given": "Timothy R." }, "orcid": "0000-0003-0437-3296" }, { "name": { "family": "Lin", "given": "Zhong-Yi" }, "orcid": "0000-0003-3827-8991" }, { "name": { "family": "Purdum", "given": "Josiah N." }, "orcid": "0000-0003-1227-3738" }, { "name": { "family": "Deshmukh", "given": "Kunal P." }, "orcid": "0000-0001-5253-3480" }, { "name": { "family": "Bauer", "given": "James M." }, "orcid": "0000-0001-9542-0953" }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "Bodewits", "given": "Dennis" }, "orcid": "0000-0002-2668-7248" }, { "id": "Burdge-Kevin-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Carey-Sean-J", "name": { "family": "Carey", "given": "Sean J." }, "orcid": "0000-0002-0221-6871" }, { "name": { "family": "Copperwheat", "given": "Chris M." }, "orcid": "0000-0001-7983-8698" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "name": { "family": "Horner", "given": "Jonathan" }, "orcid": "0000-0002-1160-7970" }, { "id": "van-Roestel-Jan", "name": { "family": "van Roestel", "given": "Jan" }, "orcid": "0000-0002-2626-2872" }, { "name": { "family": "Bhalerao", "given": "Varun" }, "orcid": "0000-0002-6112-7609" }, { "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "name": { "family": "Chen", "given": "Christine" }, "orcid": "0000-0002-8382-0447" }, { "name": { "family": "Hsu", "given": "Chen-Yen" } }, { "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Burruss-R-S", "name": { "family": "Burruss", "given": "Rick" } }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "Michael" }, "orcid": "0000-0002-8262-2924" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Delacroix-Alexandre", "name": { "family": "Delacroix", "given": "Alexandre" } }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew" } }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew" }, "orcid": "0000-0002-3168-0139" }, { "id": "Hale-David-D-S", "name": { "family": "Hale", "given": "David" } }, { "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Mr\u00f3z-Przemek", "name": { "family": "Mr\u00f3z", "given": "Przemyslaw J." }, "orcid": "0000-0001-7016-1692" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Rodriguez-Hector", "name": { "family": "Rodriguez", "given": "Hector" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger M." }, "orcid": "0000-0001-7062-9726" }, { "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Walters-Richard", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "Jeffry" } } ] }, "title": "Initial Characterization of Active Transitioning Centaur, P/2019 LD\u2082 (ATLAS), Using Hubble, Spitzer, ZTF, Keck, Apache Point Observatory, and GROWTH Visible and Infrared Imaging and Spectroscopy", "ispublished": "pub", "full_text_status": "public", "keywords": "Celestial mechanics; Centaurs; Short period comets", "note": "\u00a9 2021 The American Astronomical Society. \n\nReceived 2020 November 6; revised 2020 December 21; accepted 2021 January 5; published 2021 February 11. \n\nThe authors wish to thank the two anonymous reviewers for their help in revising this manuscript, which greatly improved its text. \n\nThis work is based on observations with the NASA/ESA Hubble Space Telescope obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Support for program GO 16077 was provided through a grant from the STScI under NASA contract NAS5-26555. \n\nThis work is based on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. \n\nThis work is based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThe Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under PIRE Grant No. 1545949. \n\nSome 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\nB.T.B., G.H., and F.J.M. acknowledge support from NASA with grant No. 80NSSC19K0780. \n\nC.F. gratefully acknowledges the support of his research by the Heising-Simons Foundation (2018-0907). \n\nM.W.C. acknowledges support from the National Science Foundation with grant No. PHY-2010970. \n\nThis publication has made use of data collected at Lulin Observatory, partly supported by MoST grant 108-2112-M-008-001. \n\nC.C.N. gratefully acknowledges the funding from MOST grant 104-2923-M-008-004-MY5. \n\nThe authors would like to acknowledge the helpful discussion of P/2019 LD2 with L. Woodney and Q.-Z. Ye. \n\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nFacilities: Hubble Space Telescope - , Spitzer Space Telescope - , Keck I Telescope - , P48 Oschin Schmidt telescope/Zwicky Transient Facility - , Apache Point Astrophysical Research Consortium 3.5 m telescope - , Liverpool Telescope - , Lulin Optical Telescope - , Mount Laguna Observatory 40 inch Telescope. - \n\nSoftware: Small Body Python, ZChecker, LPipe, REBOUND.\n\nPublished - Bolin_2021_AJ_161_116.pdf
Submitted - 2011.03782.pdf
", "abstract": "We present visible and mid-infrared imagery and photometry of temporary Jovian co-orbital comet P/2019 LD\u2082 taken with Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3), Spitzer Space Telescope/Infrared Array Camera (Spitzer/IRAC), and the GROWTH telescope network, visible spectroscopy from Keck/Low-Resolution Imaging Spectrometer (LRIS), and archival Zwicky Transient Facility observations taken between 2019 April and 2020 August. Our observations indicate that the nucleus of LD\u2082 has a radius between 0.2 and 1.8 km assuming a 0.08 albedo and a coma dominated by ~100 \u03bcm-scale dust ejected at ~1 m s\u207b\u00b9 speeds with a ~1' jet pointing in the southwest direction. LD\u2082 experienced a total dust mass loss of ~10\u2078 kg at a loss rate of ~6 kg s\u207b\u00b9 with Af\u03c1/cross section varying between ~85 cm/125 km\u00b2 and ~200 cm/310 km\u00b2 from 2019 April 9 to 2019 November 8. If the increase in Af\u03c1/cross section remained constant, it implies LD\u2082's activity began ~2018 November when within 4.8 au of the Sun, implying the onset of H\u2082O sublimation. We measure CO/CO\u2082 gas production of \u227e10\u00b2\u2077 mol s\u207b\u00b9/\u227e10\u00b2\u2076 mol s\u207b\u00b9 from our 4.5 \u03bcm Spitzer observations; g\u2013r = 0.59 \u00b1 0.03, r\u2013i = 0.18 \u00b1 0.05, and i\u2013z = 0.01 \u00b1 0.07 from GROWTH observations; and H\u2082O gas production of \u227e80 kg s\u207b\u00b9 scaling from our estimated C\u2082 production of Q_(C\u2082) \u227e7.5\u00d710\u00b2\u2074 mol s\u207b\u00b9 from Keck/LRIS spectroscopy. We determine that the long-term orbit of LD\u2082 is similar to Jupiter-family comets having close encounters with Jupiter within ~0.5 Hill radius in the last ~3 y and within 0.8 Hill radius in ~9 y. Additionally, 78.8% of our orbital clones are ejected from the solar system within 1 \u00d7 10\u2076 yr, having a dynamical half-life of 3.4 \u00d7 10\u2075 yr.", "date": "2021-03", "date_type": "published", "publication": "Astronomical Journal", "volume": "161", "number": "3", "publisher": "American Astronomical Society", "pagerange": "Art. No. 116", "id_number": "CaltechAUTHORS:20201203-151011869", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201203-151011869", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "80NSSC19K0780" }, { "agency": "Heising-Simons Foundation", "grant_number": "2018-0907" }, { "agency": "NSF", "grant_number": "PHY-2010970" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "108-2112-M-008-001" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2923-M-008-004-MY5" }, { "agency": "Gaia Multilateral Agreement" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" } ] }, "doi": "10.3847/1538-3881/abd94b", "primary_object": { "basename": "2011.03782.pdf", "url": "https://authors.library.caltech.edu/records/zxezj-0ma96/files/2011.03782.pdf" }, "related_objects": [ { "basename": "Bolin_2021_AJ_161_116.pdf", "url": "https://authors.library.caltech.edu/records/zxezj-0ma96/files/Bolin_2021_AJ_161_116.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Bolin, Bryce T.; Fernandez, Yanga R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/c1w2h-47513", "eprint_id": 108986, "eprint_status": "archive", "datestamp": "2023-08-20 02:06:20", "lastmod": "2023-10-20 23:06:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Seas-Antonios", "name": { "family": "Seas", "given": "Antonios" } } ] }, "title": "Special Section Guest Editorial: The Origins Space Telescope", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nPublished: 26 March 2021.\n\nPublished - 011001_1.pdf
", "abstract": "The guest editors summarize the Special Section on the Origins Space Telescope.", "date": "2021-03", "date_type": "published", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "volume": "7", "number": "1", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "pagerange": "Art. No. 011001", "id_number": "CaltechAUTHORS:20210506-100456974", "issn": "2329-4124", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210506-100456974", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1117/1.JATIS.7.1.011001", "primary_object": { "basename": "011001_1.pdf", "url": "https://authors.library.caltech.edu/records/c1w2h-47513/files/011001_1.pdf" }, "resource_type": "article", "pub_year": "2021", "author_list": "Helou, George and Seas, Antonios" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a86ag-2x934", "eprint_id": 107209, "eprint_status": "archive", "datestamp": "2023-08-22 08:04:15", "lastmod": "2023-10-23 15:39:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-Eric-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Hensley-Brandon-S", "name": { "family": "Hensley", "given": "B. S." }, "orcid": "0000-0001-7449-4638" }, { "id": "Linden-Sean-T", "name": { "family": "Linden", "given": "S. T." }, "orcid": "0000-0002-1000-6081" }, { "id": "Draine-Bruce-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Dong-Dillon-Z", "name": { "family": "Dong", "given": "D." }, "orcid": "0000-0001-9584-2531" }, { "id": "Momjian-Emmanuel", "name": { "family": "Momjian", "given": "E." }, "orcid": "0000-0003-3168-5922" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Evans-Aaron-S", "name": { "family": "Evans", "given": "A. S." }, "orcid": "0000-0003-2638-1334" } ] }, "title": "Where's the Dust?: The Deepening Anomaly of Microwave Emission in NGC 4725 B", "ispublished": "pub", "full_text_status": "public", "keywords": "Radio continuum emission; Interstellar emissions; Dust continuum emission; H II regions; Star-forming regions; Star formation; Galaxies; Disk galaxies", "note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 October 12; revised 2020 November 3; accepted 2020 November 5; published 2020 December 17. \n\nWe would like to thank the anonymous referee for comments that helped to improve the content and presentation of this Letter. E. J. M. thanks J. J. Condon for useful discussions that helped improve the paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.01826.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. \n\nSoftware: APLpy (Robitaille & Bressert 2012; Robitaille 2019), CASA (v4.6.0, v4.7.0, v5.3.0, v5.4.0, v5.6.1 McMullin et al. 2007), corner (Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), Matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011).\n\nPublished - Murphy_2020_ApJL_905_L23.pdf
Accepted Version - 2011.03060.pdf
", "abstract": "We present new Atacama Large Millimeter Array (ALMA) observations toward NGC 4725 B, a discrete, compact, optically faint region within the star-forming disk of the nearby galaxy NGC 4725 that exhibits strong anomalous microwave emission (AME). These new ALMA data include continuum observations centered at 92, 133, 203, and 221 GHz accompanied by spectral observations of the \u00b9\u00b2CO ( J = 2 \u2192 1) line. NGC 4725 B is detected in the continuum at all frequencies, although the detection at 203 GHz is marginal. While molecular gas is not detected at the exact location of NGC 4725 B, there is molecular gas in the immediate vicinity (i.e., \u227e100 pc) along with associated diffuse 8 \u03bcm emission. When combined with existing Very Large Array continuum data at 1.5, 3, 5.5, 9, 14, 22, 33, and 44 GHz, the spectrum is best fit by a combination of AME, synchrotron, and free\u2013free emission that is free\u2013free absorbed below ~6 GHz. Given the strength of the AME, there is surprisingly no indication of millimeter dust emission associated with NGC 4725 B on \u227e6\" spatial scales at the sensitivity of the ALMA interferometric data. Based on the properties of the nearest molecular gas complex and the inferred star formation rate, NGC 4725 B is consistent with being an extremely young (~3\u20135 Myr) massive (\u227e10\u2075 M_\u2299) cluster that is undergoing active cluster feedback. However, the lack of millimeter thermal dust emission is difficult to reconcile with a spinning dust origin of the 30 GHz emission. On the other hand, modeling NGC 4725 B as a new class of background radio galaxy is also unsatisfactory.", "date": "2020-12-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "905", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L23", "id_number": "CaltechAUTHORS:20201218-153311222", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201218-153311222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/2041-8213/abc7c8", "primary_object": { "basename": "2011.03060.pdf", "url": "https://authors.library.caltech.edu/records/a86ag-2x934/files/2011.03060.pdf" }, "related_objects": [ { "basename": "Murphy_2020_ApJL_905_L23.pdf", "url": "https://authors.library.caltech.edu/records/a86ag-2x934/files/Murphy_2020_ApJL_905_L23.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Murphy, E. J.; Hensley, B. S.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pss8c-29z50", "eprint_id": 107383, "eprint_status": "archive", "datestamp": "2023-08-20 00:58:49", "lastmod": "2024-01-15 21:19:57", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teplitz-Harry-I", "name": { "family": "Teplitz", "given": "Harry I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Benjamin" }, "orcid": "0000-0001-7648-4142" }, { "id": "Aussel-Herv\u00e9", "name": { "family": "Aussel", "given": "Herv\u00e9" }, "orcid": "0000-0002-1371-5705" }, { "id": "Dabin-Christophe", "name": { "family": "Dabin", "given": "Christophe" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Holliman-Mark-S", "name": { "family": "Holliman", "given": "Mark" } }, { "id": "Zacchei-Andrea", "name": { "family": "Zacchei", "given": "Andrea" } } ] }, "title": "Euclid's US Science Data Center: lessons learned from building a small part of a big system", "ispublished": "unpub", "full_text_status": "public", "keywords": "Euclid, distributed data processing, lessons learned, US Science Data Center", "note": "\u00a9 2020 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe Euclid Consortium acknowledges the European Space Agency and the support of a number of agencies and institutes that have supported the development of Euclid. A detailed complete list is available on the Euclid web site (http://www.euclid-ec.org). In particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the Centre National d'Etudes Spatiales, the Deutsches Zentrum fur Luft- and Raumfahrt, the Danish Space Research Institute, the Funda\u00e7\u00e3ao para a Cienca e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the Netherlandse Onderzoekschool Voor Astronomie, the Norvegian Space Center, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency.\n\nPublished - 114491P.pdf
", "abstract": "Euclid is an ESA M-class mission to study the geometry and nature of the dark universe, slated for launch in mid-2022. NASA is participating in the mission through the contribution of the near-infrared detectors and associated electronics, the nomination of scientists for membership in the Euclid Consortium, and by establishing the Euclid NASA Science Center at IPAC (ENSCI) to support the US community. As part of ENSCI's work, we will participate in the Euclid Science Ground Segment (SGS) and build and operate the US Science Data Center (SDC-US), which will be a node in the distributed data processing system for the mission. SDC-US is one of 10 data centers, and will contribute about 5% of the computing and data storage for the distributed system. We discuss lessons learned in developing a node in a distributed system. For example, there is a significant advantage to SDC-US development in sharing of knowledge, problem solving, and resource burden with other parts of the system. On the other hand, fitting into a system that is distributed geographically and relies on diverse computing environments results in added complexity in constructing SDC-US.", "date": "2020-12-13", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 114491P", "id_number": "CaltechAUTHORS:20210108-141852722", "isbn": "9781510636859", "book_title": "Observatory Operations: Strategies, Processes, and Systems VIII", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210108-141852722", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Academy of Finland" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Belgian Federal Science Policy Office (BELSPO)" }, { "agency": "Canadian Euclid Consortium" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Danish Space Research Institute" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "NASA" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Norwegian Space Agency" }, { "agency": "Romanian Space Agency" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Adler-David-S", "name": { "family": "Adler", "given": "David S." } }, { "id": "Seaman-Robert-L", "name": { "family": "Seaman", "given": "Robert L." } }, { "id": "Benn-Chris-R", "name": { "family": "Benn", "given": "Chris R." } } ] }, "corp_creators": { "items": [ "Euclid Consortium" ] }, "doi": "10.1117/12.2560108", "primary_object": { "basename": "114491P.pdf", "url": "https://authors.library.caltech.edu/records/pss8c-29z50/files/114491P.pdf" }, "resource_type": "book_section", "pub_year": "2020", "author_list": "Teplitz, Harry I.; Rusholme, Benjamin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/v8wcx-9w673", "eprint_id": 105433, "eprint_status": "archive", "datestamp": "2023-08-22 07:59:11", "lastmod": "2023-10-20 21:59:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burdge-Kevin-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Fuller-J", "name": { "family": "Fuller", "given": "Jim" }, "orcid": "0000-0002-4544-0750" }, { "id": "Kaplan-David-L", "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Marsh-Thomas-R", "name": { "family": "Marsh", "given": "Thomas R." }, "orcid": "0000-0002-2498-7589" }, { "id": "Tremblay-Pier-Emmanuel", "name": { "family": "Tremblay", "given": "Pier-Emmanuel" }, "orcid": "0000-0001-9873-0121" }, { "id": "Zhuang-Zhuyun", "name": { "family": "Zhuang", "given": "Zhuyun" }, "orcid": "0000-0002-1945-2299" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Caiazzo-Ilaria", "name": { "family": "Caiazzo", "given": "Ilaria" }, "orcid": "0000-0002-4770-5388" }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "Michael W." }, "orcid": "0000-0002-8262-2924" }, { "id": "Dhillon-Vik-S", "name": { "family": "Dhillon", "given": "Vik S." }, "orcid": "0000-0003-4236-9642" }, { "id": "Gaensicke-Boris", "name": { "family": "Gaensicke", "given": "Boris" }, "orcid": "0000-0002-2761-3005" }, { "id": "Rodr\u00edguez-Gil-Pablo", "name": { "family": "Rodr\u00edguez-Gil", "given": "Pablo" }, "orcid": "0000-0002-4717-5102" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Hermes-J-J", "name": { "family": "Hermes", "given": "J. J." }, "orcid": "0000-0001-5941-2286" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Littlefair-Stuart-P", "name": { "family": "Littlefair", "given": "S. P." }, "orcid": "0000-0001-7221-855X" }, { "id": "Mr\u00f3z-Przemek", "name": { "family": "Mr\u00f3z", "given": "Przemek" }, "orcid": "0000-0001-7016-1692" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. S." }, "orcid": "0000-0002-9656-4032" }, { "id": "van-Roestel-Jan", "name": { "family": "van Roestel", "given": "Jan" }, "orcid": "0000-0002-2626-2872" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard G." }, "orcid": "0000-0002-5884-7867" }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew J." } }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Hale-David-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Feeney-Michael-E", "name": { "family": "Feeney", "given": "Michael" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kaye-Stephen", "name": { "family": "Kaye", "given": "Stephen" } }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "id": "Soumagnac-Maayane-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "A Systematic Search of Zwicky Transient Facility Data for Ultracompact Binary LISA-detectable Gravitational-wave Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "Compact binary stars; Close binary stars; Interacting binary stars; Eclipsing binary stars; Ellipsoidal variable stars; Gravitational wave sources; White dwarf stars", "note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 September 4; revised 2020 October 13; accepted 2020 October 15; published 2020 December 9. \n\nK.B.B. thanks the National Aeronautics and Space Administration and the Heising-Simons Foundation for supporting his research. \n\nM.W.C. acknowledges support from the National Science Foundation with grant No. PHY-2010970. \n\nP.R.-G. acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU), and the European Regional Development Fund (FEDER) under grant AYA2017\u201383383\u2013P. \n\nV.S.D., ULTRACAM, and HiPERCAM are supported by STFC. \n\nThe research leading to these results has received funding from the European Research Council under the European Union's Horizon 2020 research and innovation program numbers 677706 (WD3D) and 340040 (HiPERCAM). \n\nThis work is based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThis work is based on observations made with the Gran Telescopio Canarias (GTC) installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias, in the island of La Palma. \n\nThis work is based on observations made at the European Southern Observatory New Technology Telescope (NTT), La Silla. \n\nThe KPED team thanks the National Science Foundation and the National Optical Astronomical Observatory for making the Kitt Peak 2.1 m telescope available. The KPED team thanks the National Science Foundation, the National Optical Astronomical Observatory, and the Murty family for support in the building and operation of KPED. In addition, they thank the CHIMERA project for use of the Electron Multiplying CCD (EMCCD). \n\nSome 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nThis article is based on observations made in the Observatorios de Canarias del IAC with the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Observatorio del Roque de los Muchachos. \n\nThis research benefited from interactions at the ZTF Theory Network Meeting that were funded by the Gordon and Betty Moore Foundation through grant GBMF5076 and support from the National Science Foundation through PHY-1748958. \n\nFacilities: PO:1.2 m (ZTF) - , KPNO:2.1 m (KPED) - , NTT (ULTRACAM) - , Hale (CHIMERA - , DBSP) - , GTC (HiPERCAM) - , Keck:I (LRIS). -\n\nPublished - Burdge_2020_ApJ_905_32.pdf
Submitted - 2009.02567.pdf
", "abstract": "Using photometry collected with the Zwicky Transient Facility, we are conducting an ongoing survey for binary systems with short orbital periods (P_b < 1 hr) with the goal of identifying new gravitational-wave sources detectable by the upcoming Laser Interferometer Space Antenna (LISA). We present a sample of 15 binary systems discovered thus far, with orbital periods ranging from 6.91 to 56.35 minutes. Of the 15 systems, seven are eclipsing systems that do not show signs of significant mass transfer. Additionally, we have discovered two AM Canum Venaticorum systems and six systems exhibiting primarily ellipsoidal variations in their lightcurves. We present follow-up spectroscopy and high-speed photometry confirming the nature of these systems, estimates of their LISA signal-to-noise ratios, and a discussion of their physical characteristics.", "date": "2020-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "905", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 32", "id_number": "CaltechAUTHORS:20200916-113006965", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-113006965", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Heising-Simons Foundation" }, { "agency": "NSF", "grant_number": "PHY-2010970" }, { "agency": "Ministerio de Ciencia, Innovaci\u00f3n y Universidades (MICIU)", "grant_number": "AYA2017-83383-P" }, { "agency": "Fondo Europeo de Desarrollo Regional (FEDER)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "European Research Council (ERC)", "grant_number": "677706" }, { "agency": "European Research Council (ERC)", "grant_number": "340040" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "Murty family" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NSF", "grant_number": "PHY-1748958" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/abc261", "primary_object": { "basename": "Burdge_2020_ApJ_905_32.pdf", "url": "https://authors.library.caltech.edu/records/v8wcx-9w673/files/Burdge_2020_ApJ_905_32.pdf" }, "related_objects": [ { "basename": "2009.02567.pdf", "url": "https://authors.library.caltech.edu/records/v8wcx-9w673/files/2009.02567.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Burdge, Kevin B.; Prince, Thomas A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0z0sc-hap43", "eprint_id": 103706, "eprint_status": "archive", "datestamp": "2023-08-22 07:59:03", "lastmod": "2023-10-20 16:37:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Tzanidakis-Anastasios", "name": { "family": "Tzanidakis", "given": "Anastasios" }, "orcid": "0000-0003-0484-3331" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "U. Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott" }, "orcid": "0000-0001-5855-5939" }, { "name": { "family": "Aloisi", "given": "Robert" }, "orcid": "0000-0003-2822-616X" }, { "id": "Andreoni-Igor", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Bagdasaryan-Ashot", "name": { "family": "Bagdasaryan", "given": "Ashot" } }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Cannella-Christopher-B", "name": { "family": "Cannella", "given": "Christopher" }, "orcid": "0000-0003-2667-7290" }, { "id": "Cook-David-O", "name": { "family": "Cook", "given": "David O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Delacroix-Alexandre", "name": { "family": "Delacroix", "given": "Alexandre" } }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew" } }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry" }, "orcid": "0000-0001-5060-8733" }, { "id": "Dugas-Alison-M", "name": { "family": "Dugas", "given": "Alison" } }, { "name": { "family": "Frederick", "given": "Sara" }, "orcid": "0000-0001-9676-730X" }, { "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Goldstein-Daniel-A", "name": { "family": "Goldstein", "given": "Daniel" }, "orcid": "0000-0003-3461-8661" }, { "name": { "family": "Golkhou", "given": "V. Zach" }, "orcid": "0000-0001-8205-2506" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Hale-David-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Hankins-Matthew-J", "name": { "family": "Hankins", "given": "Matthew" }, "orcid": "0000-0001-9315-8437" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "name": { "family": "Irani", "given": "Ido" }, "orcid": "0000-0002-7996-8780" }, { "name": { "family": "Jencson", "given": "Jacob E." }, "orcid": "0000-0001-5754-4007" }, { "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Kaye-Stephen", "name": { "family": "Kaye", "given": "Stephen" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "name": { "family": "Leadbeater", "given": "Robin" } }, { "id": "Lunnan-Ragnhild", "name": { "family": "Lunnan", "given": "Ragnhild" }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Neill-James-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "name": { "family": "Polin", "given": "Abigail" }, "orcid": "0000-0002-1633-6495" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "name": { "family": "Quataert", "given": "Eliot" }, "orcid": "0000-0001-9185-5044" }, { "id": "Reiley-Daniel-J", "name": { "family": "Reiley", "given": "Dan" } }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed L." }, "orcid": "0000-0002-0387-370X" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Sharma-Yashvi", "name": { "family": "Sharma", "given": "Yashvi" } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Tartaglia", "given": "Leonardo" }, "orcid": "0000-0003-3433-1492" }, { "id": "Walters-Richard", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" } ] }, "title": "The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses", "ispublished": "pub", "full_text_status": "public", "keywords": "Supernovae; Compact objects; White dwarf stars", "note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 April 19; revised 2020 August 7; accepted 2020 August 25; published 2020 December 11. \n\nWe thank the anonymous referee for a careful reading of the manuscript that helped significantly improve its content. We thank H. Perets, K. Shen, E.S. Phinney, J. Fuller, D. Kasen, B. Margalit, and S. Schulze for valuable discussions during this work. We thank M. Coughlin, S. Anand, A. Sagues Carracedo, L. Rauch, and U. Feindt for several discussions on the use of simsurvey. \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under Partnerships for International Research and Education (PIRE) grant no. 1545949. GROWTH is a collaborative project among Caltech (USA), University of Maryland College Park (USA), University of Wisconsin Milwaukee (USA), Texas Tech University (USA), San Diego State University (USA), University of Washington (USA), Los Alamos National Laboratory (USA), Tokyo Institute of Technology (Japan), National Central University (Taiwan), Indian Institute of Astrophysics (India), Indian Institute of Technology Bombay (India), Weizmann Institute of Science (Israel), The Oskar Klein Centre at Stockholm University (Sweden), Humboldt University (Germany), Liverpool John Moores University (UK), and University of Sydney (Australia). This research benefited from interactions at several ZTF Theory Network meetings, funded by the Gordon and Betty Moore Foundation through grant GBMF5076. M.M.K. acknowledges generous support from the David and Lucille Packard Foundation. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the ZTF project. ZTF is supported by the National Science Foundation under grant no. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Centre at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. SEDM is based upon work supported by the National Science Foundation under grant no. 1106171. The ZTF forced-photometry service was funded under Heising-Simons Foundation grant 12540303 (PI: Graham). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Based on observations made with NOT (operated by the Nordic Optical Telescope Scientific Association at Observatorio del Roque de los Muchachos, La Palma, Spain, of Instituto de Astrofisica de Canarias). \n\nA.G.Y.'s research is supported by the European Union via European Research Council grant no. 725161, the ISF GW Excellence Center, an IMOS space infrastructure grant, and BSF/Transformative and GIF grants, as well as The Benoziyo Endowment Fund for the Advancement of Science, the Deloro Institute for Advanced Research in Space and Optics, The Veronika A. Rabl Physics Discretionary Fund, Paul and Tina Gardner, Yeda-Sela, and the WIS\u2013CIT joint research grant. A.G.Y. is a recipient of the Helen and Martin Kimmel Award for Innovative Investigation. A.Y.Q.H. is supported by a National Science Foundation Graduate Research Fellowship under grant no. DGE-1144469 and by the GROWTH project funded by the National Science Foundation under PIRE grant no. 1545949. R.L. is supported by a Marie Sk\u0142odowska-Curie Individual Fellowship within the Horizon 2020 EU Framework Programme for Research and Innovation (H2020-MSCA-IF-2017-794467). Foscgui is a graphic user interface aimed at extracting SN spectroscopy and photometry obtained with FOSC-like instruments. It was developed by E. Cappellaro. A package description can be found at http://sngroup.oapd.inaf.it/foscgui.html. \n\nFacilities: PO:1.2 m (ZTF) - , PO:1.5 m (SEDM) - , Hale (DBSP - , WaSP) - , NOT: ALFOSC - , THO: ALPY200 - , Keck:I (LRIS). - \n\nSoftware: astropy (Astropy Collaboration et al. 2013), matplotlib (Hunter 2007), scipy (Virtanen et al. 2020), pandas (McKinney 2010), SExtractor (Bertin & Arnouts 1996), scamp (Bertin 2006), SWarp (Bertin et al. 2002), PSFEx (Bertin 2011), pysedm (Rigault et al. 2019), pyraf-dbsp (Bellm & Sesar 2016), lpipe (Perley 2019), simsurvey (Feindt et al. 2019).\n\nPublished - De_2020_ApJ_905_58.pdf
Submitted - 2004.09029.pdf
", "abstract": "Using the Zwicky Transient Facility alert stream, we are conducting a large spectroscopic campaign to construct a complete, volume-limited sample of transients brighter than 20 mag, and coincident within 100\" of galaxies in the Census of the Local Universe catalog. We describe the experiment design and spectroscopic completeness from the first 16 months of operations, which have classified 754 supernovae. We present results from a systematic search for calcium-rich gap transients in the sample of 22 low-luminosity (peak absolute magnitude M > \u221217), hydrogen-poor events found in the experiment. We report the detection of eight new events, and constrain their volumetric rate to \u2273 15% \u00b1 5% of the SN Ia rate. Combining this sample with 10 previously known events, we find a likely continuum of spectroscopic properties ranging from events with SN Ia\u2013like features (Ca-Ia objects) to those with SN Ib/c\u2013like features (Ca-Ib/c objects) at peak light. Within the Ca-Ib/c events, we find two populations distinguished by their red (g \u2212 r \u2248 1.5 mag) or green (g - r \u2248 0.5 mag) colors at the r-band peak, wherein redder events show strong line blanketing features and slower light curves (similar to Ca-Ia objects), weaker He lines, and lower [Ca ii]/[O i] in the nebular phase. We find that all together the spectroscopic continuum, volumetric rates, and striking old environments are consistent with the explosive burning of He shells on low-mass white dwarfs. We suggest that Ca-Ia and red Ca-Ib/c objects arise from the double detonation of He shells, while green Ca-Ib/c objects are consistent with low-efficiency burning scenarios like detonations in low-density shells or deflagrations.", "date": "2020-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "905", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 58", "id_number": "CaltechAUTHORS:20200604-151423784", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151423784", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "W. M. Keck Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Israel Science Foundation" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Benoziyo Endowment Fund for the Advancement of Science" }, { "agency": "Deloro Institute for Advanced Research in Space and Optics" }, { "agency": "Veronika A. Rabl Physics Discretionary Fund" }, { "agency": "Paul and Tina Gardner" }, { "agency": "Yeda-Sela" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Helen and Martin Kimmel Award" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "Marie Curie Fellowship", "grant_number": "794467" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/abb45c", "primary_object": { "basename": "2004.09029.pdf", "url": "https://authors.library.caltech.edu/records/0z0sc-hap43/files/2004.09029.pdf" }, "related_objects": [ { "basename": "De_2020_ApJ_905_58.pdf", "url": "https://authors.library.caltech.edu/records/0z0sc-hap43/files/De_2020_ApJ_905_58.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "De, Kishalay; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2a1cd-71a55", "eprint_id": 106615, "eprint_status": "archive", "datestamp": "2023-08-20 00:08:05", "lastmod": "2023-10-20 23:37:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "name": { "family": "Andersen", "given": "K. J." } }, { "name": { "family": "Ashdown", "given": "M." } }, { "name": { "family": "Baccigalupi", "given": "C." }, "orcid": "0000-0002-8211-1630" }, { "name": { "family": "Ballardini", "given": "M." } }, { "name": { "family": "Banday", "given": "A. J." } }, { "name": { "family": "Barreiro", "given": "R. B." }, "orcid": "0000-0002-6139-4272" }, { "name": { "family": "Bartolo", "given": "N." } }, { "name": { "family": "Basak", "given": "S." } }, { "name": { "family": "Benabed", "given": "K." } }, { "name": { "family": "Bernard", "given": "J.-P." } }, { "name": { "family": "Bersanelli", "given": "M." } }, { "name": { "family": "Bielewicz", "given": "P." } }, { "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "name": { "family": "Borrill", "given": "J." } }, { "name": { "family": "Burigana", "given": "C." }, "orcid": "0000-0002-3005-5796" }, { "name": { "family": "Butler", "given": "R. C." } }, { "name": { "family": "Calabrese", "given": "E." } }, { "name": { "family": "Casaponsa", "given": "B." } }, { "name": { "family": "Chiang", "given": "H. C." } }, { "name": { "family": "Colombo", "given": "L. P. L." } }, { "name": { "family": "Combet", "given": "C." } }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "name": { "family": "Cuttaia", "given": "F." } }, { "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "name": { "family": "De Rosa", "given": "A." }, "orcid": "0000-0001-5668-6863" }, { "name": { "family": "de Zotti", "given": "G." }, "orcid": "0000-0003-2868-2595" }, { "name": { "family": "Delabrouille", "given": "J." } }, { "name": { "family": "Di Valentino", "given": "E." } }, { "name": { "family": "Diego", "given": "J. M." }, "orcid": "0000-0001-9065-3926" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "name": { "family": "Douspis", "given": "M." } }, { "name": { "family": "Dupac", "given": "X." } }, { "name": { "family": "Eriksen", "given": "H. K." }, "orcid": "0000-0003-2332-5281" }, { "name": { "family": "Fernandez-Cobos", "given": "R." }, "orcid": "0000-0001-6185-7903" }, { "name": { "family": "Finelli", "given": "F." }, "orcid": "0000-0002-6694-3269" }, { "name": { "family": "Frailis", "given": "M." } }, { "name": { "family": "Fraisse", "given": "A. A." } }, { "name": { "family": "Franceschi", "given": "E." }, "orcid": "0000-0002-0585-6591" }, { "name": { "family": "Frolov", "given": "A." } }, { "name": { "family": "Galeotta", "given": "S." }, "orcid": "0000-0002-3748-5115" }, { "name": { "family": "Galli", "given": "S." } }, { "name": { "family": "Ganga", "given": "K." } }, { "name": { "family": "Gerbino", "given": "M." } }, { "id": "Ghosh-Tuhin", "name": { "family": "Ghosh", "given": "T." } }, { "name": { "family": "Gonz\u00e1lez-Nuevo", "given": "J." } }, { "id": "G\u00f3rski-Krzysztof-M", "name": { "family": "G\u00f3rski", "given": "K. M." }, "orcid": "0000-0003-2933-8630" }, { "name": { "family": "Gruppuso", "given": "A." } }, { "name": { "family": "Gudmundsson", "given": "J. E." } }, { "name": { "family": "Handley", "given": "W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Herranz", "given": "D." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hivon", "given": "E." }, "orcid": "0000-0003-1880-2733" }, { "name": { "family": "Huang", "given": "Z." }, "orcid": "0000-0003-0592-028X" }, { "name": { "family": "Jaffe", "given": "A. H." } }, { "name": { "family": "Jones", "given": "W. C." } }, { "name": { "family": "Keih\u00e4nen", "given": "E." }, "orcid": "0000-0003-1804-7715" }, { "name": { "family": "Keskitalo", "given": "R." } }, { "name": { "family": "Kiiveri", "given": "K." } }, { "name": { "family": "Kim", "given": "J." } }, { "name": { "family": "Kisner", "given": "T. S." } }, { "name": { "family": "Krachmalnicoff", "given": "N." } }, { "name": { "family": "Kunz", "given": "M." }, "orcid": "0000-0003-1676-6126" }, { "name": { "family": "Kurki-Suonio", "given": "H." }, "orcid": "0000-0002-4618-3063" }, { "name": { "family": "Lasenby", "given": "A." } }, { "name": { "family": "Lattanzi", "given": "M." } }, { "id": "Lawrence-Charles-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "name": { "family": "Le Jeune", "given": "M." } }, { "name": { "family": "Levrier", "given": "F." } }, { "name": { "family": "Liguori", "given": "M." } }, { "name": { "family": "Lilje", "given": "P. B." } }, { "name": { "family": "Lilley", "given": "M." } }, { "name": { "family": "Lindholm", "given": "V." } }, { "name": { "family": "L\u00f3pez-Caniego", "given": "M." } }, { "name": { "family": "Lubin", "given": "P. M." } }, { "name": { "family": "Mac\u00edas-P\u00e9rez", "given": "J. F." } }, { "name": { "family": "Maino", "given": "D." }, "orcid": "0000-0002-4761-1242" }, { "name": { "family": "Mandolesi", "given": "N." } }, { "name": { "family": "Marcos-Caballero", "given": "A." } }, { "name": { "family": "Maris", "given": "M." } }, { "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "name": { "family": "Mart\u00ednez-Gonz\u00e1lez", "given": "E." } }, { "name": { "family": "Matarrese", "given": "S." } }, { "name": { "family": "Mauri", "given": "N." } }, { "name": { "family": "McEwen", "given": "J. D." }, "orcid": "0000-0002-5852-8890" }, { "name": { "family": "Meinhold", "given": "P. R." } }, { "name": { "family": "Mennella", "given": "A." } }, { "name": { "family": "Migliaccio", "given": "M." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "name": { "family": "Molinari", "given": "D." } }, { "name": { "family": "Montier", "given": "L." } }, { "name": { "family": "Morgante", "given": "G." } }, { "name": { "family": "Moss", "given": "A." } }, { "name": { "family": "Natoli", "given": "P." } }, { "name": { "family": "Paoletti", "given": "D." } }, { "name": { "family": "Partridge", "given": "B." } }, { "name": { "family": "Patanchon", "given": "G." } }, { "id": "Pearson-D", "name": { "family": "Pearson", "given": "D." } }, { "id": "Pearson-Timothy-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "name": { "family": "Perrotta", "given": "F." } }, { "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "name": { "family": "Polenta", "given": "G." }, "orcid": "0000-0003-4067-9196" }, { "name": { "family": "Rachen", "given": "J. P." } }, { "name": { "family": "Reinecke", "given": "M." } }, { "name": { "family": "Remazeilles", "given": "M." } }, { "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "name": { "family": "Rosset", "given": "C." } }, { "id": "Roudier-Gael-M", "name": { "family": "Roudier", "given": "G." }, "orcid": "0000-0002-7402-7797" }, { "name": { "family": "Rubino-Martin", "given": "J. A." }, "orcid": "0000-0001-5289-3021" }, { "name": { "family": "Ruiz-Granados", "given": "B." } }, { "name": { "family": "Salvati", "given": "L." } }, { "name": { "family": "Savelainen", "given": "M." } }, { "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "name": { "family": "Sirignano", "given": "C." } }, { "name": { "family": "Sirri", "given": "G." } }, { "name": { "family": "Spencer", "given": "L. D." } }, { "name": { "family": "Suur-Uski", "given": "A.-S." } }, { "name": { "family": "Svalheim", "given": "T. L." } }, { "name": { "family": "Tauber", "given": "J. A." } }, { "name": { "family": "Tavagnacco", "given": "D." } }, { "name": { "family": "Tenti", "given": "M." }, "orcid": "0000-0002-4254-5901" }, { "name": { "family": "Terenzi", "given": "L." } }, { "name": { "family": "Thommesen", "given": "H." } }, { "name": { "family": "Toffolatti", "given": "L." } }, { "name": { "family": "Tomasi", "given": "M." } }, { "name": { "family": "Tristram", "given": "M." } }, { "name": { "family": "Trombetti", "given": "T." } }, { "name": { "family": "Valiviita", "given": "J." }, "orcid": "0000-0001-6225-3693" }, { "name": { "family": "Van Tent", "given": "B." } }, { "name": { "family": "Vielva", "given": "P." } }, { "name": { "family": "Villa", "given": "F." } }, { "name": { "family": "Vittorio", "given": "N." } }, { "name": { "family": "Wandelt", "given": "B. D." } }, { "name": { "family": "Wehus", "given": "I. K." }, "orcid": "0000-0003-3821-7275" }, { "name": { "family": "Zacchei", "given": "A." }, "orcid": "0000-0003-0396-1192" }, { "name": { "family": "Zonca", "given": "A." } } ] }, "title": "Planck intermediate results. LVII. Joint Planck LFI and HFI data processing", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 cosmological parameters \u2013 Galaxy: general \u2013 methods: data analysis", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 2 April 2020; Accepted 1 July 2020; Published online 11 November 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This work has received funding from the European Union's Horizon 2020 research and innovation programme under grant numbers 776282, 772253 and 819478. This research would not have been possible without the resources of the National Energy Research Scientific Computing Center (NERSC), a US Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231.\n\nPublished - aa38073-20.pdf
Accepted Version - 2007.04997.pdf
", "abstract": "We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck analysis efforts, and combines some of the most powerful features of the separate LFI and HFI analysis pipelines. For example, following the LFI 2018 processing procedure, NPIPE uses foreground polarization priors during the calibration stage in order to break scanning-induced degeneracies. Similarly, NPIPE employs the HFI 2018 time-domain processing methodology to correct for bandpass mismatch at all frequencies. In addition, NPIPE introduces several improvements, including, but not limited to: inclusion of the 8% of data collected during repointing manoeuvres; smoothing of the LFI reference load data streams; in-flight estimation of detector polarization parameters; and construction of maximally independent detector-set split maps. For component-separation purposes, important improvements include: maps that retain the CMB Solar dipole, allowing for high-precision relative calibration in higher-level analyses; well-defined single-detector maps, allowing for robust CO extraction; and HFI temperature maps between 217 and 857 GHz that are binned into 0\u2032.9 pixels (N_(side) = 4096), ensuring that the full angular information in the data is represented in the maps even at the highest Planck resolutions. The net effect of these improvements is lower levels of noise and systematics in both frequency and component maps at essentially all angular scales, as well as notably improved internal consistency between the various frequency channels. Based on the NPIPE maps, we present the first estimate of the Solar dipole determined through component separation across all nine Planck frequencies. The amplitude is (3366.6 \u00b1 2.7) \u03bcK, consistent with, albeit slightly higher than, earlier estimates. From the large-scale polarization data, we derive an updated estimate of the optical depth of reionization of \u03c4\u2004=\u20040.051 \u00b1 0.006, which appears robust with respect to data and sky cuts. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations.", "date": "2020-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "643", "publisher": "EDP Sciences", "pagerange": "Art. No. A42", "id_number": "CaltechAUTHORS:20201111-122556506", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201111-122556506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "776282" }, { "agency": "European Research Council (ERC)", "grant_number": "772253" }, { "agency": "European Research Council (ERC)", "grant_number": "819478" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/202038073", "primary_object": { "basename": "2007.04997.pdf", "url": "https://authors.library.caltech.edu/records/2a1cd-71a55/files/2007.04997.pdf" }, "related_objects": [ { "basename": "aa38073-20.pdf", "url": "https://authors.library.caltech.edu/records/2a1cd-71a55/files/aa38073-20.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Akrami, Y.; Andersen, K. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qaf81-a9v18", "eprint_id": 105427, "eprint_status": "archive", "datestamp": "2023-08-19 23:19:01", "lastmod": "2023-10-20 21:59:22", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "W.-H." }, "orcid": "0000-0002-3140-5014" }, { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "B." }, "orcid": "0000-0002-4950-6323" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "name": { "family": "Ye", "given": "Q.-Z." }, "orcid": "0000-0002-4838-7676" }, { "id": "Kramer-Emily-A", "name": { "family": "Kramer", "given": "E. A." }, "orcid": "0000-0003-0457-2519" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Ahumada-Tom\u00e1s", "name": { "family": "Ahumada", "given": "T." }, "orcid": "0000-0002-2184-6430" }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "M. W." }, "orcid": "0000-0002-8262-2924" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "M. J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Walters-Richard-S", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "name": { "family": "Deshmukh", "given": "K. P." } }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "name": { "family": "Lin", "given": "Z.-Y." } }, { "id": "Milburn-Jennifer-W", "name": { "family": "Milburn", "given": "J. W." } }, { "name": { "family": "Purdum", "given": "J. N." } }, { "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "name": { "family": "Bodewits", "given": "D." }, "orcid": "0000-0002-2668-7248" }, { "name": { "family": "Chang", "given": "C.-K." } }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "C.-C." }, "orcid": "0000-0001-8771-7554" }, { "name": { "family": "Tan", "given": "H." } }, { "name": { "family": "Zhai", "given": "C." }, "orcid": "0000-0002-0291-4522" }, { "name": { "family": "van Dokkum", "given": "P." }, "orcid": "0000-0002-8282-9888" }, { "name": { "family": "Granvik", "given": "M." }, "orcid": "0000-0002-5624-1888" }, { "name": { "family": "Harikane", "given": "Y." }, "orcid": "0000-0002-6047-430X" }, { "name": { "family": "Mowla", "given": "L. A." } }, { "id": "Burdge-Kevin-B", "name": { "family": "Burdge", "given": "K. B." }, "orcid": "0000-0002-7226-836X" }, { "name": { "family": "Bellm", "given": "E. C." }, "orcid": "0000-0001-8018-5348" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "K." }, "orcid": "0000-0002-8989-0542" }, { "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "name": { "family": "Copperwheat", "given": "C. M." }, "orcid": "0000-0001-7983-8698" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "R." }, "orcid": "0000-0002-5884-7867" }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "D. A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Hale-David-D-S", "name": { "family": "Hale", "given": "D." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Mr\u00f3z-Przemek", "name": { "family": "Mr\u00f3z", "given": "P. J." }, "orcid": "0000-0001-7016-1692" }, { "id": "Neill-James-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "R." }, "orcid": "0000-0002-0387-370X" }, { "id": "Rodriguez-Hector", "name": { "family": "Rodriguez", "given": "H." } }, { "id": "Serabyn-Eugene", "name": { "family": "Serabyn", "given": "E." } }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "R. M." }, "orcid": "0000-0001-7062-9726" }, { "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Soumagnac", "given": "M. T." }, "orcid": "0000-0001-6753-1488" }, { "name": { "family": "Southworth", "given": "J." }, "orcid": "0000-0002-3807-3198" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "A kilometer-scale asteroid inside Venus's orbit", "ispublished": "unpub", "full_text_status": "public", "note": "Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nSED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171 \n\nThe KPED team thanks the National Science Foundation and the National Optical Astronomical Observatory for making the Kitt Peak 2.1-m telescope available. We thank the observatory staff at Kitt Peak for their efforts to assist Robo-AO KP operations. The KPED team thanks the National Science Foundation, the National Optical Astronomical Observatory, the Caltech Space Innovation Council and the Murty family for support in the building and operation of\nKPED. In addition, they thank the CHIMERA project for use of the Electron Multiplying CCD (EMCCD). \n\nThe authors would like to thank Alessandro Morbidelli for useful discussion in the interpretation of the first inner-Venus asteroid discovery as well as providing the synthetic asteroid population used to model our survey efficiencies. \n\nM. W. Coughlin acknowledges support from the National Science Foundation with grant number PHY-2010970. \n\nC.F. gratefully acknowledges the support of his research by the Heising-Simons Foundation (#2018-0907). \n\nSome 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\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nAuthors Contributions. W.-H.I. helped initiate, design and secure P48 time for the ZTF Twilight. B.T.B. discovered 2020 AV\u2082 in the ZTF data and realized it had an orbit interior to Venus', led the study, wrote the manuscript, reviewed and scanned all candidate asteroid detections for the duration of this study, helped design and secure time for the Twilight survey and for follow-up, prepared and executed follow-up observations, reduced the photometric and spectroscopic data, did the astrometry, orbit determination, helped generate the synthetic NEA population, calculated the survey completeness and estimates of the inner-Venus asteroid population. F.J.M. served as the Science Data System Lead of the ZTF collaboration, wrote and maintained software for extraction of moving objects in ZTF data, calculated the survey completeness, maintained the ZTF data system, helped secure P48 time for the ZTF Twilight survey, helped design and initiate the Twilight survey. Q.Y. contributed code used to schedule the ZTF survey and contributed improvements to the moving object identification pipeline, and helped initiate and design the Twilight survey. E.K. monitored the NEA discovery performance of the ZTF survey. G.H. helped with the interpretation of the completeness calculation, helped prepare the manuscript, served as the Primary Investigator of the team observing NEAs with ZTF and as the Data Archive Director of the ZTF collaboration, helped design the cadence, secure P48 time for the ZTF Twilight survey and is one of its initiators. E.K. monitored the NEA discovery performance of the ZTF survey. G.H. served as the Primary Investigator of the team observing NEAs with ZTF and as the Data Archive Director of the ZTF collaboration, helped design the cadence, secure P48 time for the ZTF Twilight survey and is one of its initiators. E.K. monitored the NEA discovery performance of the ZTF survey. G.H. served as the Primary Investigator of the team observing NEAs with ZTF and as the Data Archive Director of the ZTF collaboration, helped design the cadence, secure P48 time for the ZTF Twilight survey and is one of its initiators. T.A. and M.C. performed follow-up observations of 2020 AV\u2082 with KPED and contributed to the reduction of photometry. M.G. served as the Project Scientist of ZTF, secured time with Keck I and took spectroscopic observations of 2020 AV\u2082 with Keck I/LRIS and reduced spectral data. R.W. performed follow-up observations of 2020 AV\u2082 with SEDM. K.P.D. contributed to planning follow-up observations of 2020 AV\u2082. C.F. contributed to the planning of spectroscopy observations of 2020 AV\u2082 with Keck and spectroscopic data reduction. Z.-Y.L. contributed to the interpretation of the 2020 AV\u2082 spectroscopy data. J.W.M. contributed to follow-up observations of 2020 AV\u2082. J.P. and R.Q. contributed to the reduction of photometry and follow-up observations of 2020 AV\u2082. C.-K.C., C.-C.N. and H.T. contributed to securing time with the P48 for ZTF Solar System observations. C.Z., C.M.C and J.S. were members of the team that conducts follow-up observations of ZTF Solar System discoveries. P.D. and L.A.M. helped secure time for follow-up observations of 2020 AV\u2082. M.G. helped generate the synthetic NEA population. K.B.B. and K.D. contributed to the reduction of Keck/LRIS spectroscopy data of 2020 AV\u2082. E.C.B. served as the Survey Scientist of the ZTF collaboration and scheduled the observations taken with the P48 during the ZTF Twilight survey. S.B.C. contributed to the planning of P48 time used in the Twilight survey. D.A.D, A.M. and P.J.M. wrote and maintained software and machine learning algorithms for the ZTF data pipeline and identification of sources in ZTF data. A.M. served as the Machine Learning Lead for the ZTF collaboration. R.D. served as the Project Manager of the ZTF collaboration and contributed to the design and construction of the ZTF camera. D.H. contributed to the design and construction of the ZTF camera. M.K. served as the Primary Investigator of the Global Relay of Observatories Watching Transients Happen (GROWTH) team for follow-up of ZTF discoveries. S.R.K. served as the Principal Investigator of the ZTF collaboration and survey. T.K. and M.T.S. contributed to the ZTF calibration pipeline. J.D.N. contributed to SEDM operations and observations of 2020 AV\u2082. R.R. contributed to maintaining ZTF operations. H.R. contributed to SEDM operations. E.S. contributed to KPED operations and observations of 2020 AV\u2082. R.M.S. served as the Lead Camera Engineer for the ZTF survey and lead the design and construction of the ZTF camera. J.S. contributed to SEDM operations and observations of 2020 AV\u2082. L.Y. contributed to planning and securing of telescope time for follow-up observations of 2020 AV\u2082.\n\nSubmitted - 2009.04125.pdf
", "abstract": "Near-Earth asteroid population models predict the existence of asteroids located inside the orbit of Venus. However, despite searches up to the end of 2019, none have been found. Here we report the discovery by the Zwicky Transient Facility of the first known asteroid located inside of Venus' orbit, 2020 AV\u2082, possessing an aphelion distance of 0.65 au and \u223c2 km in size. While it is possible that 2020 AV\u2082 is the largest of its kind, we find that its discovery is surprising in the context of population models where the expected count is close to zero. If this discovery is not a statistical fluke, then 2020 AV\u2082 may come from a yet undiscovered source population of asteroids interior to Venus, and currently favored asteroid population models may need to be adjusted.", "date": "2020-09-16", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200916-112945883", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112945883", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "Caltech Space Innovation Council" }, { "agency": "Murty family" }, { "agency": "NSF", "grant_number": "PHY-2010970" }, { "agency": "Heising-Simons Foundation", "grant_number": "2018-0907" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Gaia Multilateral Agreement" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "primary_object": { "basename": "2009.04125.pdf", "url": "https://authors.library.caltech.edu/records/qaf81-a9v18/files/2009.04125.pdf" }, "resource_type": "monograph", "pub_year": "2020", "author_list": "Ip, W.-H.; Bolin, B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xqcv3-79f72", "eprint_id": 105268, "eprint_status": "archive", "datestamp": "2023-08-19 23:02:00", "lastmod": "2023-10-20 21:45:21", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga Ram" }, "orcid": "0000-0001-7583-0621" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Brammer-G", "name": { "family": "Brammer", "given": "Gabriel" }, "orcid": "0000-0003-2680-005X" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Flynn-D", "name": { "family": "Flynn", "given": "Dave" } }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "Steven" }, "orcid": "0000-0001-5668-3507" }, { "id": "Ferguson-H-C", "name": { "family": "Ferguson", "given": "Henry C." }, "orcid": "0000-0001-7113-2738" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl" }, "orcid": "0000-0003-4072-169X" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "Anton" }, "orcid": "0000-0002-6610-2048" }, { "id": "Lee-BoMee", "name": { "family": "Lee", "given": "BoMee" } }, { "id": "Malhotra-Sangeeta", "name": { "family": "Malhotra", "given": "Sangeeta" }, "orcid": "0000-0002-9226-5350" }, { "id": "Miyatake-H", "name": { "family": "Miyatake", "given": "Hironao" } }, { "id": "Melchior-P", "name": { "family": "Melchior", "given": "Peter" }, "orcid": "0000-0002-8873-5065" }, { "id": "Momcheva-I-G", "name": { "family": "Momcheva", "given": "Ivelina" } }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "Jeffrey" }, "orcid": "0000-0001-8684-2222" }, { "id": "Masiero-J-R", "name": { "family": "Masiero", "given": "Joseph" }, "orcid": "0000-0003-2638-720X" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "Roberta" }, "orcid": "0000-0002-5158-243X" }, { "id": "Prakash-Abhishek", "name": { "family": "Prakash", "given": "Abhishek" }, "orcid": "0000-0003-4451-4444" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "Benjamin" }, "orcid": "0000-0001-7648-4142" }, { "id": "Stickley-N-R", "name": { "family": "Stickley", "given": "Nathaniel" } }, { "id": "Smith-A-M", "name": { "family": "Smith", "given": "Arfon" } }, { "id": "Wood-Vasey-W-M", "name": { "family": "Wood-Vasey", "given": "Michael" } }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry I." }, "orcid": "0000-0002-7064-5424" } ] }, "title": "Joint Survey Processing of Euclid, Rubin and Roman: Final Report", "ispublished": "unpub", "full_text_status": "public", "note": "Final Report from March 2019 submitted to NASA, NSF, DOE, 41 pages. This is the extended version of the Astro2020 white papers. \n\nWe are very grateful to Daniela Calzetti, George Djorgovski and Bahram Mobasher for their critical review and suggestions which resulted in a significant improvement of this report.\n\nSubmitted - 2008.10663.pdf
", "abstract": "The Euclid, Rubin/LSST and Roman (WFIRST) projects will undertake flagship optical/near-infrared surveys in the next decade. By mapping thousands of square degrees of sky and covering the electromagnetic spectrum between 0.3 and\n2 microns with sub-arcsec resolution, these projects will detect several tens\nof billions of sources, enable a wide range of astrophysical investigations by\nthe astronomical community and provide unprecedented constraints on the nature\nof dark energy and dark matter. The ultimate cosmological, astrophysical and\ntime-domain science yield from these missions will require joint survey\nprocessing (JSP) functionality at the pixel level that is outside the scope of\nthe individual survey projects. The JSP effort scoped here serves two\nhigh-level objectives: 1) provide precise concordance multi-wavelength images\nand catalogs over the entire sky area where these surveys overlap, which\naccounts for source confusion and mismatched isophotes, and 2) provide a\nscience platform to analyze concordance images and catalogs to enable a wide\nrange of astrophysical science goals to be formulated and addressed by the\nresearch community. For the cost of about 200WY, JSP will allow the U.S. (and\ninternational) astronomical community to manipulate the flagship data sets and\nundertake innovative science investigations ranging from solar system object\ncharacterization, exoplanet detections, nearby galaxy rotation rates and dark\nmatter properties, to epoch of reionization studies. It will also allow for the\nultimate constraints on cosmological parameters and the nature of dark energy,\nwith far smaller uncertainties and a better handle on systematics than by any one survey alone.", "date": "2020-09-08", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200908-091428952", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200908-091428952", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.2008.10663", "primary_object": { "basename": "2008.10663.pdf", "url": "https://authors.library.caltech.edu/records/xqcv3-79f72/files/2008.10663.pdf" }, "resource_type": "monograph", "pub_year": "2020", "author_list": "Chary, Ranga Ram; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3tybt-bep85", "eprint_id": 103710, "eprint_status": "archive", "datestamp": "2023-08-22 06:20:13", "lastmod": "2023-10-20 16:38:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "id": "Schulze-S", "name": { "family": "Schulze", "given": "Steve" }, "orcid": "0000-0001-6797-1889" }, { "id": "Li-Zhihui", "name": { "family": "Li", "given": "Zhihui" }, "orcid": "0000-0001-5113-7558" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Fruchter-A-S", "name": { "family": "Fruchter", "given": "Andrew" }, "orcid": "0000-0002-6652-9279" }, { "id": "Rubin-David", "name": { "family": "Rubin", "given": "David" }, "orcid": "0000-0001-5402-4647" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Fuller-J", "name": { "family": "Fuller", "given": "Jim" }, "orcid": "0000-0002-4544-0750" }, { "id": "Piro-A-L", "name": { "family": "Piro", "given": "Anthony L." }, "orcid": "0000-0001-6806-0673" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Burruss-R-S", "name": { "family": "Burruss", "given": "Rick" } }, { "id": "Duev-D-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Feeney-M-E", "name": { "family": "Feeney", "given": "Michael" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Golkhou-V-Z", "name": { "family": "Golkhou", "given": "V. Zach" }, "orcid": "0000-0001-8205-2506" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "id": "Soumagnac-M-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "Jeffry" } } ] }, "title": "SN2019dge: a Helium-rich Ultra-Stripped Envelope Supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "Supernovae; Core-collapse supernovae; Neutron stars; Surveys", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 May 27; revised 2020 July 23; accepted 2020 July 27; published 2020 August 31. \n\nWe thank Takashi Moriya, Thomas Tauris, David Khatami, Dan Kasen, Sterl Phinney, and Wenbin Lu for valuable discussions during this work. We thank Lin Yan for sharing spectra of SN1993J and Gaia16apd. Y.Y. thanks the instructors and organizers of the GROWTH summer school for teaching techniques in time-domain data analysis. This study made use of the open supernova catalog (Guillochon et al. 2017). \n\nC.F. gratefully acknowledges support of his research by the Heising-Simons Foundation (#2018-0907). \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under PIRE grant No. 1545949. \n\nThis work is based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nSoftware: astropy (Astropy Collaboration et al. 2013), corner (Foreman-Mackey 2016), CIGALE (Boquien et al. 2019), emcee (Foreman-Mackey et al. 2013), LAMBDAR (Wright et al. 2016), Lpipe (Perley 2019), matplotlib (Hunter 2007), pandas (McKinney 2010), pyneb (Luridiana et al. 2015), pyraf-dbsp (Bellm & Sesar 2016), scipy (Virtanen et al. 2020), simsurvey (Feindt et al. 2019), sncosmo (Barbary et al. 2016), ztfquery (Rigault 2018).\n\nPublished - Yao_2020_ApJ_900_46.pdf
Submitted - 2005.12922.pdf
", "abstract": "We present observations of ZTF18abfcmjw (SN2019dge), a helium-rich supernova with a fast-evolving light curve indicating an extremely low ejecta mass (\u22480.33 M_\u2299) and low kinetic energy (\u22481.3 \u00d7 10\u2075\u2070 erg). Early-time (<4 days after explosion) photometry reveals evidence of shock cooling from an extended helium-rich envelope of ~0.1 M_\u2299 located ~1.2 \u00d7 10\u00b9\u00b3 cm from the progenitor. Early-time He II line emission and subsequent spectra show signatures of interaction with helium-rich circumstellar material, which extends from \u2273 5 \u00d7 10\u00b9\u00b3 cm to 2 \u00d7 10\u00b9\u2076 cm. We interpret SN2019dge as a helium-rich supernova from an ultra-stripped progenitor, which originates from a close binary system consisting of a mass-losing helium star and a low-mass main-sequence star or a compact object (i.e., a white dwarf, a neutron star, or a black hole). We infer that the local volumetric birth rate of 19dge-like ultra-stripped SNe is in the range of 1400\u20138200 Gpc\u207b\u00b3 yr\u207b\u00b9 (i.e., 2%\u201312% of core-collapse supernova rate). This can be compared to the observed coalescence rate of compact neutron star binaries that are not formed by dynamical capture.", "date": "2020-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "900", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 46", "id_number": "CaltechAUTHORS:20200604-151437761", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151437761", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Heising-Simons Foundation", "grant_number": "2018-0907" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/abaa3d", "primary_object": { "basename": "2005.12922.pdf", "url": "https://authors.library.caltech.edu/records/3tybt-bep85/files/2005.12922.pdf" }, "related_objects": [ { "basename": "Yao_2020_ApJ_900_46.pdf", "url": "https://authors.library.caltech.edu/records/3tybt-bep85/files/Yao_2020_ApJ_900_46.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Yao, Yuhan; De, Kishalay; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/erkpg-pt466", "eprint_id": 96756, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:11", "lastmod": "2023-10-20 21:29:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "G\u00f3rski-K-M", "name": { "family": "G\u00f3rski", "given": "K. M." } }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "G." } }, { "id": "Wehus-I-K", "name": { "family": "Wehus", "given": "I. K." } } ] }, "title": "Planck 2018 results. I. Overview and the cosmological legacy of Planck", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmology: theory \u2013 cosmic background radiation \u2013 surveys", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 16 July 2018; Accepted 27 September 2019; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states (in particular the lead countries France and Italy), with contributions from NASA (USA), and telescope reflectors provided by a collaboration between ESA and a scientific consortium led and funded by Denmark. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.cosmos.esa.int/web/planck/ planck-collaboration. In addition, we thank Sol\u00e8ne Chabanier and Nathalie Palanque-Delabrouille for computing the Ly\u2006\u03b1 forest constraints we have used in Fig. 19 and Inigo Zubeldia for preparing Fig. 32.\n\nPublished - aa33880-18.pdf
Submitted - 1807.06205.pdf
", "abstract": "The European Space Agency's Planck satellite, which was dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013, producing deep, high-resolution, all-sky maps in nine frequency bands from 30 to 857 GHz. This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard cosmological model and some of the tightest limits available on deviations from that model. The 6-parameter \u039bCDM model continues to provide an excellent fit to the cosmic microwave background data at high and low redshift, describing the cosmological information in over a billion map pixels with just six parameters. With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the six parameters to better than 1% (simultaneously), with the best-determined parameter (\u03b8*) now known to 0.03%. We describe the multi-component sky as seen by Planck, the success of the \u039bCDM model, and the connection to lower-redshift probes of structure formation. We also give a comprehensive summary of the major changes introduced in this 2018 release. The Planck data, alone and in combination with other probes, provide stringent constraints on our models of the early Universe and the large-scale structure within which all astrophysical objects form and evolve. We discuss some lessons learned from the Planck mission, and highlight areas ripe for further experimental advances.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "number": "Art. No. A1", "publisher": "EDP Sciences", "id_number": "CaltechAUTHORS:20190626-154014679", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-154014679", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministry of Science, Innovation and Universities (MICINN)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833880", "primary_object": { "basename": "1807.06205.pdf", "url": "https://authors.library.caltech.edu/records/erkpg-pt466/files/1807.06205.pdf" }, "related_objects": [ { "basename": "aa33880-18.pdf", "url": "https://authors.library.caltech.edu/records/erkpg-pt466/files/aa33880-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Akrami, Y.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/q2p3d-94m22", "eprint_id": 96787, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:29", "lastmod": "2023-10-20 21:31:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "G\u00f3rski-K-M", "name": { "family": "G\u00f3rski", "given": "K. M." } }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "G." } } ] }, "title": "Planck 2018 results. IV. Diffuse component separation", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 cosmology: observations \u2013 cosmic background radiation \u2013 diffuse radiation \u2013 Galaxy: general", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 16 July 2018; Accepted 13 January 2019; Published online 11 September 2020.\n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This work has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement numbers 687312, 776282 and 772253.\n\nPublished - aa33881-18.pdf
Submitted - 1807.06208.pdf
", "abstract": "We present full-sky maps of the cosmic microwave background (CMB) and polarized synchrotron and thermal dust emission, derived from the third set of Planck frequency maps. These products have significantly lower contamination from instrumental systematic effects than previous versions. The methodologies used to derive these maps follow closely those described in earlier papers, adopting four methods (Commander, NILC, SEVEM, and SMICA) to extract the CMB component, as well as three methods (Commander, GNILC, and SMICA) to extract astrophysical components. Our revised CMB temperature maps agree with corresponding products in the Planck 2015 delivery, whereas the polarization maps exhibit significantly lower large-scale power, reflecting the improved data processing described in companion papers; however, the noise properties of the resulting data products are complicated, and the best available end-to-end simulations exhibit relative biases with respect to the data at the few percent level. Using these maps, we are for the first time able to fit the spectral index of thermal dust independently over 3\u00b0 regions. We derive a conservative estimate of the mean spectral index of polarized thermal dust emission of \u03b2_d\u2004=\u20041.55\u2006 \u00b1 \u20060.05, where the uncertainty marginalizes both over all known systematic uncertainties and different estimation techniques. For polarized synchrotron emission, we find a mean spectral index of \u03b2_s\u2004=\u2004\u22123.1\u2006 \u00b1 \u20060.1, consistent with previously reported measurements. We note that the current data processing does not allow for construction of unbiased single-bolometer maps, and this limits our ability to extract CO emission and correlated components. The foreground results for intensity derived in this paper therefore do not supersede corresponding Planck 2015 products. For polarization the new results supersede the corresponding 2015 products in all respects.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A4", "id_number": "CaltechAUTHORS:20190627-110918453", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190627-110918453", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Red Espa\u00f1ola de Supercomputaci\u00f3n (RES)" }, { "agency": "Ministry of Employment and the Economy (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "687312" }, { "agency": "European Research Council (ERC)", "grant_number": "776282" }, { "agency": "European Research Council (ERC)", "grant_number": "772253" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833881", "primary_object": { "basename": "1807.06208.pdf", "url": "https://authors.library.caltech.edu/records/q2p3d-94m22/files/1807.06208.pdf" }, "related_objects": [ { "basename": "aa33881-18.pdf", "url": "https://authors.library.caltech.edu/records/q2p3d-94m22/files/aa33881-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Akrami, Y.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6kw2r-1q771", "eprint_id": 96767, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:19", "lastmod": "2023-10-20 21:30:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Ghosh-Tuhin", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-Ranga-Ram", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "G\u00f3rski-Krzysztof-M", "name": { "family": "G\u00f3rski", "given": "K. M." }, "orcid": "0000-0003-2933-8630" }, { "id": "Lawrence-Charles-R", "name": { "family": "Lawrence", "given": "C. R." }, "orcid": "0000-0002-5983-6481" }, { "id": "Roudier-Gael-M", "name": { "family": "Roudier", "given": "G." }, "orcid": "0000-0002-7402-7797" } ] }, "title": "Planck 2018 results. XII. Galactic astrophysics using polarized dust emission", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 magnetic fields \u2013 turbulence \u2013 dust, extinction \u2013 local insterstellar matter \u2013 submillimeter: ISM", "note": "\u00a9 2020 Planck Collaboration. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived 16 July 2018; Accepted 28 February 2019; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nThe Planck Collaboration acknowledges the support of ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The research leading to these results has received funding from the European Research Council under the European Union's Horizon 2020 Research & Innovation Framework Programme/ERC grant agreement ERC-2016-ADG-742719. This research has received funding from the Agence Nationale de la Recherche (ANR-17-CE31-0022). We thank Pekka Teerikorpi and Andrei Berdyugin for kindly providing stellar polarization data and providing insights on stellar polarization references, Gina Panopoulou for discussions of the zero point calibration of the polarization angle, and Ralf Siebenmorgen and Nikolai Voshchinnikov for statistical discussions. We gratefully acknowledge the help of Rosine Lallement regarding the handling of the Gaia data.\n\nPublished - aa33885-18.pdf
Submitted - 1807.06212.pdf
", "abstract": "Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle \u03c8, and dispersion function of polarization angles S. The joint distribution (one-point statistics) of p and N_H confirms that the mean and maximum polarization fractions decrease with increasing N_H. The uncertainty on the maximum observed polarization fraction, p_(max) = 22.0_(\u22121.4)^(+3.5)% at 353 GHz and 80\u2032 resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and S found earlier is seen to be present at high latitudes. This follows the S\u2004\u221d\u2004p\u207b\u00b9 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, \u03c8, and S for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map S \u00d7 p, looking for residual trends. While the polarization fraction p decreases by a factor of 3\u22124 between N_H\u2004=\u200410\u00b2\u2070 cm\u207b\u00b2 and N_H\u2004=\u20042 \u00d7 1022\u2006cm\u207b\u00b2, out of the Galactic plane, this product S \u00d7 p only decreases by about 25%. Because S is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with N_H is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of S \u00d7 p with the dust temperature T_d, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion S tend, on the contrary, to have colder dust than lines of sight with low p and high S. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, R_(P/p) and R_(S/V), which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, p_V/E(B \u2212 V), of 13% at high Galactic latitude, compatible with the polarization fraction p\u2004\u2248\u200420% observed at 353 GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A12", "id_number": "CaltechAUTHORS:20190627-085435272", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190627-085435272", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)", "grant_number": "742719" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "Gaia Multilateral Agreement" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-17-CE31-0022" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833885", "primary_object": { "basename": "1807.06212.pdf", "url": "https://authors.library.caltech.edu/records/6kw2r-1q771/files/1807.06212.pdf" }, "related_objects": [ { "basename": "aa33885-18.pdf", "url": "https://authors.library.caltech.edu/records/6kw2r-1q771/files/aa33885-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Aghanim, N.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5h3j9-apc36", "eprint_id": 105068, "eprint_status": "archive", "datestamp": "2023-08-22 08:03:33", "lastmod": "2023-10-20 21:19:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Anand-Shreya", "name": { "family": "Anand", "given": "Shreya" }, "orcid": "0000-0003-3768-7515" }, { "name": { "family": "Ahumada", "given": "Tom\u00e1s" }, "orcid": "0000-0002-2184-6430" }, { "name": { "family": "Stein", "given": "Robert" }, "orcid": "0000-0003-2434-0387" }, { "name": { "family": "Sagu\u00e9s Carracedo", "given": "Ana" } }, { "id": "Andreoni-Igor", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "Michael W." }, "orcid": "0000-0002-8262-2924" }, { "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "name": { "family": "Kool", "given": "Erik C." }, "orcid": "0000-0002-7252-3877" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "name": { "family": "Kumar", "given": "Harsh" } }, { "name": { "family": "Almualla", "given": "Mouza" }, "orcid": "0000-0002-4694-7123" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" }, { "name": { "family": "Bulla", "given": "Mattia" }, "orcid": "0000-0002-8255-5127" }, { "name": { "family": "Dobie", "given": "Dougal" }, "orcid": "0000-0003-0699-7019" }, { "name": { "family": "Reusch", "given": "Simeon" } }, { "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "name": { "family": "Cenko", "given": "S. 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Zach" }, "orcid": "0000-0001-8205-2506" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Graham-Melissa-Lynn", "name": { "family": "Graham", "given": "Melissa L." }, "orcid": "0000-0002-9154-3136" }, { "id": "Hankins-Matthew-J", "name": { "family": "Hankins", "given": "Matthew J." }, "orcid": "0000-0001-9315-8437" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Hu", "given": "Youdong" }, "orcid": "0000-0002-7400-4608" }, { "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Jaodand-Amruta-D", "name": { "family": "Jaodand", "given": "Amruta" }, "orcid": "0000-0002-3850-6651" }, { "id": "Karambelkar-Viraj-R", "name": { "family": "Karambelkar", "given": "Viraj" }, "orcid": "0000-0003-2758-159X" }, { "name": { "family": "Kong", "given": "Albert K. H." }, "orcid": "0000-0002-5105-344X" }, { "name": { "family": "Kowalski", "given": "Marek" } }, { "name": { "family": "Khandagale", "given": "Maitreya" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "name": { "family": "Kumar", "given": "Brajesh" } }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "name": { "family": "Li", "given": "K. L." }, "orcid": "0000-0001-8229-2024" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "name": { "family": "Mogotsi", "given": "Moses" } }, { "name": { "family": "Mohite", "given": "Siddharth" } }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "Kunal" }, "orcid": "0000-0002-2557-5180" }, { "id": "Mr\u00f3z-Przemek", "name": { "family": "Mr\u00f3z", "given": "Przemek" }, "orcid": "0000-0001-7016-1692" }, { "name": { "family": "Newman", "given": "Jeffrey A." }, "orcid": "0000-0001-8684-2222" }, { "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "name": { "family": "Oates", "given": "Samantha R." }, "orcid": "0000-0001-9309-7873" }, { "name": { "family": "Patil", "given": "Atharva Sunil" } }, { "name": { "family": "Pandey", "given": "Shashi B." } }, { "name": { "family": "Pavana", "given": "M." } }, { "name": { "family": "Pian", "given": "Elena" }, "orcid": "0000-0001-8646-4858" }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "name": { "family": "Sanchez-Ram\u0131rez", "given": "Ruben" }, "orcid": "0000-0002-7158-5099" }, { "id": "Sharma-Yashvi", "name": { "family": "Sharma", "given": "Yashvi" }, "orcid": "0000-0003-4531-1745" }, { "name": { "family": "Singh", "given": "Avinash" } }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "name": { "family": "Taggart", "given": "Kirsty" }, "orcid": "0000-0002-5748-4558" }, { "name": { "family": "Tan", "given": "Hanjie" } }, { "id": "Tzanidakis-Anastasios", "name": { "family": "Tzanidakis", "given": "Anastasios" }, "orcid": "0000-0003-0484-3331" }, { "name": { "family": "Troja", "given": "Eleonora" }, "orcid": "0000-0002-1869-7817" }, { "name": { "family": "Valeev", "given": "Azamat F." }, "orcid": "0000-0003-3513-3527" }, { "id": "Walters-Richard", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "name": { "family": "Waratkar", "given": "Gaurav" }, "orcid": "0000-0003-3630-9440" }, { "name": { "family": "Webb", "given": "Sara" }, "orcid": "0000-0003-2601-1472" }, { "name": { "family": "Yu", "given": "Po-Chieh" }, "orcid": "0000-0001-8894-0854" }, { "name": { "family": "Zhang", "given": "Bin-Bin" } }, { "name": { "family": "Zhou", "given": "Rongpu" }, "orcid": "0000-0001-5381-4372" }, { "id": "Zolkower-Jeffry", "name": { "family": "Zolkower", "given": "Jeffry" } } ] }, "title": "Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3", "ispublished": "pub", "full_text_status": "public", "keywords": "Neutron stars; Black holes; Gravitational waves; Nucleosynthesis; R-process; Compact objects; Spectroscopy; Sky surveys; Photometry", "note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2020 June 19; revised 2020 October 19; accepted 2020 October 19; published 2020 December 22. \n\nThis work was supported by the Global Relay of Observatories Watching Transients Happen (GROWTH) project, funded by the National Science Foundation under PIRE grant No. 1545949. GROWTH is a collaborative project among the California Institute of Technology (USA), University of Maryland College Park (USA), University of Wisconsin Milwaukee (USA), Texas Tech University (USA), San Diego State University (USA), University of Washington (USA), Los Alamos National Laboratory (USA), Tokyo Institute of Technology (Japan), National Central University (Taiwan), Indian Institute of Astrophysics (India), Indian Institute of Technology Bombay (India), Weizmann Institute of Science (Israel), The Oskar Klein Centre at Stockholm University (Sweden), Humboldt University (Germany), Liverpool John Moores University (UK), and University of Sydney (Australia). Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. The ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. The ZTF forced photometry service was funded under Heising-Simons Foundation grant No. 12540303 (PI: Graham). The SED Machine is based upon work supported by the National Science Foundation under grant No. 1106171. \n\nThe GROWTH-India telescope is a 70 cm telescope with a 0.7\u00b0 field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA). The GROWTH-India project is supported by SERB and administered by IUSSTF under grant No. IUSSTF/PIRE Program/GROWTH/2015-16. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France (doi: 10.26093/cds/vizier). The original description of the VizieR service was published in A&AS 143, 23. These results made use of the Lowell Discovery Telescope (LDT) at Lowell Observatory. Lowell is a private, nonprofit institution dedicated to astrophysical research and public appreciation of astronomy and operates the LDT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The Large Monolithic Imager was built by Lowell Observatory using funds provided by the National Science Foundation (AST-1005313). The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale and a grant from the Mt. Cuba Astronomical Foundation. The KPED team thanks the National Science Foundation and the National Optical Astronomical Observatory for making the Kitt Peak 2.1 m telescope available. We thank the observatory staff at Kitt Peak for their efforts to assist Robo-AO KP operations. The KPED team thanks the National Science Foundation, the National Optical Astronomical Observatory, the Caltech Space Innovation Council, and the Murty family for support in the building and operation of KPED. In addition, they thank the CHIMERA project for use of the Electron Multiplying CCD (EMCCD). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Some spectroscopic observations were obtained with the Southern African Large Telescope (SALT). The Photometric Redshifts for the Legacy Surveys (PRLS) catalog used in this paper was produced thanks to funding from the U.S. Department of Energy Office of Science, Office of High Energy Physics, via grant DE-SC0007914. This publication has made use of data collected at Lulin Observatory, partly supported by MoST grant 108-2112-M-008-001. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias on the island of La Palma. \n\nM.M.K. acknowledges generous support from the David and Lucille Packard Foundation. M.W.C. acknowledges support from the National Science Foundation with grant No. PHY-2010970. A.G. and J.S. acknowledge support from the Knut and Alice Wallenberg Foundation and GREAT research environment grant 2016-06012, funded by the Swedish Research Council. Some of the work by D.A.P. was performed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. D.A.P. was partially supported by a grant from the Simons Foundation. H.K. thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. This work has been supported by the Spanish Science Ministry Centro de Excelencia Severo Ochoa Program under grant SEV-2017-0709. A.J.C.T. acknowledges support from the Junta de Andaluc\u00eda (Project P07-TIC-03094) and Spanish Ministry Projects AYA2012-39727-C03-01, AYA2015-71718R, and PID2019-109974RB-I00. V.A.F. was supported by grant RFBR 19-02-00432. I.A. acknowledges support by a Ram\u00f3n y Cajal grant (RYC-2013-14511) of the Ministerio de Ciencia, Innovaci\u00f3n, y Universidades (MICIU) of Spain. He also acknowledges financial support from MCIU through grant AYA2016-80889-P. A.A.M. is funded by the Large Synoptic Survey Telescope Corporation, the Brinson Foundation, and the Moore Foundation in support of the LSSTC Data Science Fellowship Program; he also receives support as a CIERA Fellow by the CIERA Postdoctoral Fellowship Program (Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University). A.C. acknowledges support from the National Science Foundation with grant No. 1907975. W.-H.I., A.K., K.-L.L., C.-C.N., A.P., H.T., and P.-C.Y. acknowledge support from Ministry of Science and Technology (MoST) Taiwan grants 104-2923-M-008-004-MY5, 107-2119-M-008-012, 108-2628-M-007-005-RSP, and 108-2112-M-007-025-MY3. D.D. is supported by an Australian Government Research Training Program Scholarship. S.A. is supported by the GROWTH project, funded by the National Science Foundation under PIRE grant No. 1545949. A.S.C. is supported by GREAT research environment grant 2016-06012, funded by the Swedish Research Council. E.C.K. acknowledges support from the G.R.E.A.T. research environment and the Wenner-Gren Foundations. A.J.C.T. is thankful for fruitful discussions with J. Cepa, E. Fern\u00e1ndez-Garc\u00eda, J. A. Font, S. Jeong, A. Mart\u00edn-Carrillo, A. M. Sintes, and S. Sokolov. D.A.H.B. acknowledges research support from the National Research Foundation of South Africa. S.B.P. and V.B. acknowledge BRICS grant No. \"DST/IMRCD/BRICS/PilotCall1/ProFCheap/2017(G)\" for part of the present work. J.S.B. was partially supported by a Gordon and Betty Moore Foundation Data-Driven Discovery grant and a grant from the National Science Foundation, \"Conceptualization of a Scalable Cyberinfrastructure Center for Multimessenger Astrophysics.\"\n\nPublished - Kasliwal_2020_ApJ_905_145.pdf
Submitted - 2006.11306.pdf
", "abstract": "We present a systematic search for optical counterparts to 13 gravitational wave (GW) triggers involving at least one neutron star during LIGO/Virgo's third observing run (O3). We searched binary neutron star (BNS) and neutron star black hole (NSBH) merger localizations with the Zwicky Transient Facility (ZTF) and undertook follow-up with the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration. The GW triggers had a median localization area of 4480 deg\u00b2, a median distance of 267 Mpc, and false-alarm rates ranging from 1.5 to 10\u207b\u00b2\u2075 yr\u207b\u00b9. The ZTF coverage in the g and r bands had a median enclosed probability of 39%, median depth of 20.8 mag, and median time lag between merger and the start of observations of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UltraViolet/Optical/InfraRed (UVOIR) photometric points, 64 OIR spectra, and three radio images using 17 different telescopes. We find no promising kilonovae (radioactivity-powered counterparts), and we show how to convert the upper limits to constrain the underlying kilonova luminosity function. Initially, we assume that all GW triggers are bona fide astrophysical events regardless of false-alarm rate and that kilonovae accompanying BNS and NSBH mergers are drawn from a common population; later, we relax these assumptions. Assuming that all kilonovae are at least as luminous as the discovery magnitude of GW170817 (\u221216.1 mag), we calculate that our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than \u221216.6 mag (the extrapolated peak magnitude of GW170817) and fade at a rate of 1 mag day\u207b\u00b9 (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations based on the online classifications, the joint probability of zero detections, assuming all kilonovae are brighter than \u221216.6 mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, no more than <57% (<89%) of putative kilonovae could be brighter than \u221216.6 mag assuming flat evolution (fading by 1 mag day\u207b\u00b9) at the 90% confidence level. If we further take into account the online terrestrial probability for each GW trigger, we find that no more than <68% of putative kilonovae could be brighter than \u221216.6 mag. Comparing to model grids, we find that some kilonovae must have M_(ej) < 0.03 M_\u2299, X_(lan) > 10\u207b\u2074, or \u03c6 > 30\u00b0 to be consistent with our limits. We look forward to searches in the fourth GW observing run; even 17 neutron star mergers with only 50% coverage to a depth of \u221216 mag would constrain the maximum fraction of bright kilonovae to <25%.", "date": "2020-08-24", "date_type": "published", "publication": "Astrophysical Journal", "volume": "905", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 145", "id_number": "CaltechAUTHORS:20200824-085517593", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200824-085517593", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Indo-US Science and Technology Forum" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Science and Engineering Research Board (SERB)", "grant_number": "GROWTH/2015-16" }, { "agency": "NSF", "grant_number": "AST-1005313" }, { "agency": "John and Ginger Giovale" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Mt. Cuba Astronomical Foundation" }, { "agency": "National Optical Astronomical Observatory" }, { "agency": "Murty family" }, { "agency": "Caltech Space Innovation Council" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0007914" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "108-2112-M-008-001" }, { "agency": "NSF", "grant_number": "PHY-2010970" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council", "grant_number": "2016-06012" }, { "agency": "NSF", "grant_number": "PHY-1607611" }, { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "NSF", "grant_number": "OAC-1829740" }, { "agency": "Brinson Foundation" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Severo Ochoa", "grant_number": "SEV-2017-0709" }, { "agency": "Junta de Andaluc\u00eda", "grant_number": "P07-TIC-03094" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2012-39727-C03-01" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2015-71718R" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "PID2019-109974RB-I00" }, { "agency": "Russian Foundation for Basic Research", "grant_number": "RFBR 19-02-00432" }, { "agency": "Ram\u00f3n y Cajal Programme", "grant_number": "RYC-2013-14511" }, { "agency": "Ministerio de Ciencia, Innovaci\u00f3n y Universidades (MICIU)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "AYA2016-80889-P" }, { "agency": "Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)" }, { "agency": "Northwestern University" }, { "agency": "NSF", "grant_number": "AST-1907975" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2923-M-008-004-MY5" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "107-2119-M-008-012" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "108-2628-M-007-005-RSP" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "108-2112-M-007-025-MY3" }, { "agency": "Australian Government" }, { "agency": "G.R.E.A.T. Research Environment" }, { "agency": "Wenner-Gren Foundations" }, { "agency": "National Research Foundation (South Africa)" }, { "agency": "BRICS", "grant_number": "DST/IMRCD/BRICS/PilotCall1/ProFCheap/2017(G)" }, { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/abc335", "primary_object": { "basename": "2006.11306.pdf", "url": "https://authors.library.caltech.edu/records/5h3j9-apc36/files/2006.11306.pdf" }, "related_objects": [ { "basename": "Kasliwal_2020_ApJ_905_145.pdf", "url": "https://authors.library.caltech.edu/records/5h3j9-apc36/files/Kasliwal_2020_ApJ_905_145.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Kasliwal, Mansi M.; Anand, Shreya; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/wb9j6-ztd93", "eprint_id": 104570, "eprint_status": "archive", "datestamp": "2023-08-22 05:41:19", "lastmod": "2023-10-20 20:37:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brunker-S-W", "name": { "family": "Brunker", "given": "Samantha W." }, "orcid": "0000-0001-6776-2550" }, { "id": "Salzer-J-J", "name": { "family": "Salzer", "given": "John J." }, "orcid": "0000-0001-8483-603X" }, { "id": "Janowiecki-S", "name": { "family": "Janowiecki", "given": "Steven" }, "orcid": "0000-0001-9165-8905" }, { "id": "Finn-R-A", "name": { "family": "Finn", "given": "Rose A." }, "orcid": "0000-0001-8518-4862" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Properties of the KISS Green Pea Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "Emission line galaxies; Galaxy abundances; Star formation; Starburst galaxies; Galaxy evolution", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 June 8; accepted 2020 June 18; published 2020 July 24. \n\nWe acknowledge financial support from the National Science Foundation for the KISS project, as well as for the subsequent follow-up spectroscopy campaign (NSF-AST-9553020, NSF-AST-0071114, and NSF-AST-0307766). We are grateful to the Indiana University College of Arts and Sciences for their continued support of the WIYN Observatory. We thank the staff of the WIYN Observatory for their excellent support during both our WHIRC NIR imaging observations and our Hydra spectroscopic runs. This work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. 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. Funding for the SDSS 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 website 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\nFacilities: WIYN (Hydra and WHIRC) - , Spitzer - , WISE. -\n\nPublished - Brunker_2020_ApJ_898_68.pdf
Accepted Version - 2006.14663.pdf
", "abstract": "Green peas (GPs) are a class of extreme star-forming galaxies (SFGs) at intermediate redshifts, originally discovered via color selection using multifilter, wide-field survey imaging data. They are commonly thought of as being analogs of high-redshift Ly\u03b1-emitting galaxies. The defining characteristic of GP galaxies is a high-excitation nebular spectrum with very large equivalent width lines, leading to the recognition that GP-like galaxies can also be identified in samples of emission-line galaxies. Here we compare the properties a sample of [O iii]-selected SFGs (z = 0.29\u20130.41) from the KPNO International Spectroscopic Survey (KISS) with the color-selected GPs. We find that the KISS [O iii]-selected galaxies overlap with the parameter space defined by the color-selected GPs; the two samples appear to be drawn from the same population of objects. We compare the KISS GPs with the full H\u03b1-selected KISS SFG sample (z < 0.1) and find that they are extreme systems. Many appear to be young systems at their observed look-back times (3\u20134 Gyr), with more than 90% of their rest-frame B-band luminosity coming from the starburst population. We compute the volume density of the KISS red (KISSR) GPs at z = 0.29\u20130.41 and find that they are extremely rare objects. We do not see galaxies as extreme as the KISSR GPs in the local universe, although we recognize several lower-luminosity systems at z < 0.1.", "date": "2020-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "898", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 68", "id_number": "CaltechAUTHORS:20200724-123517794", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200724-123517794", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9553020" }, { "agency": "NSF", "grant_number": "AST-0071114" }, { "agency": "NSF", "grant_number": "AST-0307766" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/ab9ec0", "primary_object": { "basename": "2006.14663.pdf", "url": "https://authors.library.caltech.edu/records/wb9j6-ztd93/files/2006.14663.pdf" }, "related_objects": [ { "basename": "Brunker_2020_ApJ_898_68.pdf", "url": "https://authors.library.caltech.edu/records/wb9j6-ztd93/files/Brunker_2020_ApJ_898_68.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Brunker, Samantha W.; Salzer, John J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1akcy-zcg63", "eprint_id": 104019, "eprint_status": "archive", "datestamp": "2023-08-19 21:59:37", "lastmod": "2023-10-20 19:00:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Graham-M-J", "name": { "family": "Graham", "given": "M. J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Ford-K-E-S", "name": { "family": "Ford", "given": "K. E. S." } }, { "id": "McKernan-B", "name": { "family": "McKernan", "given": "B." }, "orcid": "0000-0002-9726-0508" }, { "id": "Ross-N-P", "name": { "family": "Ross", "given": "N. P." }, "orcid": "0000-0003-1830-6473" }, { "id": "Stern-D", "name": { "family": "Stern", "given": "D." }, "orcid": "0000-0003-2686-9241" }, { "id": "Burdge-K-B", "name": { "family": "Burdge", "given": "K." }, "orcid": "0000-0002-7226-836X" }, { "id": "Coughlin-M-W", "name": { "family": "Coughlin", "given": "M." }, "orcid": "0000-0002-8262-2924" }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "A. J." } }, { "id": "Duev-D-A", "name": { "family": "Duev", "given": "D." }, "orcid": "0000-0001-5060-8733" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A. A." }, "orcid": "0000-0003-2242-0244" }, { "id": "van-Velzen-S", "name": { "family": "van Velzen", "given": "S." }, "orcid": "0000-0002-3859-8074" }, { "id": "Belecki-J", "name": { "family": "Belecki", "given": "J." } }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E. C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Burruss-R-S", "name": { "family": "Burruss", "given": "R." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cunningham-V", "name": { "family": "Cunningham", "given": "V." }, "orcid": "0000-0003-2292-0441" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T." }, "orcid": "0000-0002-8850-3627" }, { "id": "Reiley-D-J", "name": { "family": "Reiley", "given": "D." } }, { "id": "Rodriguez-Hector", "name": { "family": "Rodriguez", "given": "H." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "R. M." } }, { "id": "Soumagnac-M-T", "name": { "family": "Soumagnac", "given": "M. T." }, "orcid": "0000-0001-6753-1488" } ] }, "title": "Candidate Electromagnetic Counterpart to the Binary Black Hole Merger Gravitational-Wave Event S190521g", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2020 American Physical Society. \n\n(Received 19 March 2020; accepted 5 June 2020; published 25 June 2020) \n\nWe thank the referees for useful, timely comments that have improved this manuscript. M.\u2009J.\u2009G. is supported by NSF Grants No. AST-1518308 and AST-1815034, and NASA Grant No. 16-ADAP16-0232. K.\u2009E.\u2009S.\u2009F. and B.\u2009M. are supported by NSF Grant No. AST-1831415 and Simons Foundation Grant No. 533845. K.\u2009E.\u2009S.\u2009F. and B.\u2009M. acknowledge extremely useful conversations with Mordecai-Mark MacLow and Pierre Marchand. The work of D.\u2009S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.\u2009M.\u2009M.\u2009K. acknowledges the GROWTH project funded by the National Science Foundation under Grant No. 1545949. M.\u2009C. is supported by NSF Grant No. PHY-2010970. Based on observations obtained with the Samuel Oschin 48-inch telescope and the 60-inch telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Z.\u2009T.\u2009F. is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by Caltech Optical Observatories, IPAC, and University of Washington. The ZTF forced-photometry service was funded under the Heising\u2013Simons Foundation Grant No. 12540303 (PI: Graham). N.\u2009P.\u2009R. acknowledges support from the STFC and the Ernest Rutherford Fellowship scheme.\n\nPublished - PhysRevLett.124.251102.pdf
Accepted Version - 2006.14122.pdf
", "abstract": "We report the first plausible optical electromagnetic counterpart to a (candidate) binary black hole merger. Detected by the Zwicky Transient Facility, the electromagnetic flare is consistent with expectations for a kicked binary black hole merger in the accretion disk of an active galactic nucleus [B. McKernan, K.\u2009E.\u2009S. Ford, I. Bartos et al., Astrophys. J. Lett. 884, L50 (2019)] and is unlikely [< O (0.01%))] due to intrinsic variability of this source. The lack of color evolution implies that it is not a supernova and instead is strongly suggestive of a constant temperature shock. Other false-positive events, such as microlensing or a tidal disruption event, are ruled out or constrained to be < O(0.1%). If the flare is associated with S190521g, we find plausible values of total mass M_(BBH) \u223c 100 M_\u2299, kick velocity v_k \u223c 200 km s\u207b\u00b9 at \u03b8 \u223c 60\u00b0 in a disk with aspect ratio H/a \u223c 0.01 (i.e., disk height H at radius a) and gas density \u03c1 \u223c 10\u207b\u00b9\u2070 g cm\u207b\u00b3. The merger could have occurred at a disk migration trap (a \u223c 700r_g; r_g \u2261 GM_(SMBH)/c\u00b2, where M_(SMBH) is the mass of the active galactic nucleus supermassive black hole). The combination of parameters implies a significant spin for at least one of the black holes in S190521g. The timing of our spectroscopy prevents useful constraints on broad-line asymmetry due to an off-center flare. We predict a repeat flare in this source due to a reencountering with the disk in \u223c1.6 yr(M_SMBH)/10\u2078 M_\u2299)(a/10\u00b3r_g)^(3/2).", "date": "2020-06-26", "date_type": "published", "publication": "Physical Review Letters", "volume": "124", "number": "25", "publisher": "American Physical Society", "pagerange": "Art. No. 251102", "id_number": "CaltechAUTHORS:20200624-144534783", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200624-144534783", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1518308" }, { "agency": "NSF", "grant_number": "AST-1815034" }, { "agency": "NASA", "grant_number": "16-ADAP16-0232" }, { "agency": "NSF", "grant_number": "AST-1831415" }, { "agency": "Simons Foundation", "grant_number": "533845" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "PHY-2010970" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "LIGO" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1103/PhysRevLett.124.251102", "primary_object": { "basename": "2006.14122.pdf", "url": "https://authors.library.caltech.edu/records/1akcy-zcg63/files/2006.14122.pdf" }, "related_objects": [ { "basename": "PhysRevLett.124.251102.pdf", "url": "https://authors.library.caltech.edu/records/1akcy-zcg63/files/PhysRevLett.124.251102.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Graham, M. J.; Ford, K. E. S.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7qd8s-h2x86", "eprint_id": 103702, "eprint_status": "archive", "datestamp": "2023-08-19 19:57:35", "lastmod": "2024-01-15 04:31:26", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "name": { "family": "Arenberg", "given": "Jon" } }, { "name": { "family": "Ballantyne", "given": "David" }, "orcid": "0000-0001-8128-6976" }, { "name": { "family": "Bautz", "given": "Mark" } }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles" }, "orcid": "0000-0002-5627-5471" }, { "id": "Booth-J", "name": { "family": "Booth", "given": "Jeffrey" } }, { "name": { "family": "Buckley", "given": "James" } }, { "name": { "family": "Burns", "given": "Jack O." } }, { "name": { "family": "Camp", "given": "Jordan" } }, { "name": { "family": "Conti", "given": "Alberto" } }, { "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "name": { "family": "Danchi", "given": "William" } }, { "name": { "family": "Delabrouille", "given": "Jacques" } }, { "name": { "family": "De Zotti", "given": "Gianfranco" }, "orcid": "0000-0003-2868-2595" }, { "name": { "family": "Flauger", "given": "Raphael" } }, { "name": { "family": "Glenn", "given": "Jason" }, "orcid": "0000-0001-7527-2017" }, { "name": { "family": "Grindlay", "given": "Jonathan" }, "orcid": "0000-0002-1323-5314" }, { "name": { "family": "Hanany", "given": "Shaul" } }, { "name": { "family": "Hartmann", "given": "Dieter" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Herranz", "given": "Diego" } }, { "name": { "family": "Hubmayr", "given": "Johannes" } }, { "name": { "family": "Johnson", "given": "Bradley R." } }, { "name": { "family": "Jones", "given": "William" } }, { "name": { "family": "Kasdin", "given": "N. Jeremy" } }, { "name": { "family": "Kouvoliotou", "given": "Chryssa" } }, { "name": { "family": "Kunze", "given": "Kerstin E." } }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "Charles" } }, { "id": "Lazio-T-J-W", "name": { "family": "Lazio", "given": "Joseph" }, "orcid": "0000-0002-3873-5497" }, { "name": { "family": "Lipscy", "given": "Sarah" } }, { "name": { "family": "Lillie", "given": "Charles F." } }, { "name": { "family": "Maccarone", "given": "Tom" } }, { "id": "Madsen-K-K", "name": { "family": "Madsen", "given": "Kristin C." }, "orcid": "0000-0003-1252-4891" }, { "name": { "family": "Mushotzky", "given": "Richard" }, "orcid": "0000-0002-7962-5446" }, { "name": { "family": "Olinto", "given": "Angela" } }, { "name": { "family": "Plavchan", "given": "Peter" }, "orcid": "0000-0002-8864-1667" }, { "name": { "family": "Pogosian", "given": "Levon" } }, { "name": { "family": "Ptak", "given": "Andrew" }, "orcid": "0000-0001-5655-1440" }, { "name": { "family": "Ray", "given": "Paul" }, "orcid": "0000-0002-5297-5278" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "Graca M." }, "orcid": "0000-0002-4150-8076" }, { "name": { "family": "Scowen", "given": "Paul" } }, { "name": { "family": "Seager", "given": "Sara" }, "orcid": "0000-0002-6892-6948" }, { "id": "Tinto-M", "name": { "family": "Tinto", "given": "Massimo" }, "orcid": "0000-0002-8107-5148" }, { "name": { "family": "Tomsick", "given": "John" }, "orcid": "0000-0001-5506-9855" }, { "name": { "family": "Tucker", "given": "Gregory S." }, "orcid": "0000-0002-6954-6947" }, { "name": { "family": "Ulmer", "given": "Mel" } }, { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "name": { "family": "Wollack", "given": "Edward J." }, "orcid": "0000-0002-7567-4451" } ] }, "title": "The Case for Probe-class NASA Astrophysics Missions", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 2002.12739.pdf
", "abstract": "Astrophysics spans an enormous range of questions on scales from individual planets to the entire cosmos. To address the richness of 21st century astrophysics requires a corresponding richness of telescopes spanning all bands and all messengers. Much scientific benefit comes from having the multi-wavelength capability available at the same time. Most of these bands,or measurement sensitivities, require space-based missions. Historically, NASA has addressed this need for breadth with a small number of flagship-class missions and a larger number of Explorer missions. While the Explorer program continues to flourish, there is a large gap between Explorers and strategic missions. A fortunate combination of new astrophysics technologies with new, high capacity, low dollar-per-kg to orbit launchers, and new satellite buses allow for cheaper missions with capabilities approaching strategic mission levels. NASA has recognized these developments by calling for Probe-class mission ideas for mission studies, spanning most of the electromagnetic spectrum from GeV gamma-rays to the far infrared, and the new messengers of neutrinos and ultra-high energy cosmic rays. The key insight from the Probes exercise is that order-of-magnitude advances in science performance metrics are possible across the board for initial total cost estimates in the range 500M-1B dollars.", "date": "2020-06-08", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200604-151409625", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151409625", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.48550/arXiv.2002.12739", "primary_object": { "basename": "2002.12739.pdf", "url": "https://authors.library.caltech.edu/records/7qd8s-h2x86/files/2002.12739.pdf" }, "resource_type": "monograph", "pub_year": "2020", "author_list": "Elvis, Martin; Arenberg, Jon; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/c1bm9-7b434", "eprint_id": 103703, "eprint_status": "archive", "datestamp": "2023-08-20 01:55:27", "lastmod": "2023-10-20 16:37:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stein-Robert", "name": { "family": "Stein", "given": "Robert" }, "orcid": "0000-0003-2434-0387" }, { "name": { "family": "van Velzen", "given": "Sjoert" }, "orcid": "0000-0002-3859-8074" }, { "name": { "family": "Kowalski", "given": "Marek" }, "orcid": "0000-0001-8594-8666" }, { "name": { "family": "Franckowiak", "given": "Anna" }, "orcid": "0000-0002-5605-2219" }, { "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "name": { "family": "Miller-Jones", "given": "James C. A." }, "orcid": "0000-0003-3124-2814" }, { "name": { "family": "Frederick", "given": "Sara" }, "orcid": "0000-0001-9676-730X" }, { "name": { "family": "Sfaradi", "given": "Itai" }, "orcid": "0000-0003-0466-3779" }, { "name": { "family": "Bietenholz", "given": "Michael F." } }, { "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "name": { "family": "Fender", "given": "Rob" }, "orcid": "0000-0002-5654-2744" }, { "name": { "family": "Garrappa", "given": "Simone" }, "orcid": "0000-0003-2403-4582" }, { "name": { "family": "Ahumada", "given": "Tom\u00e1s" }, "orcid": "0000-0002-2184-6430" }, { "id": "Andreoni-Igor", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Belicki-Justin", "name": { "family": "Belicki", "given": "Justin" } }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "B\u00f6ttcher", "given": "Markus" } }, { "name": { "family": "Brinnel", "given": "Valery" } }, { "id": "Burruss-Rick-S", "name": { "family": "Burruss", "given": "Rick" } }, { "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "name": { "family": "Coughlin", "given": "Michael W." }, "orcid": "0000-0002-8262-2924" }, { "name": { "family": "Cunningham", "given": "Virginia" }, "orcid": "0000-0003-2292-0441" }, { "id": "Drake-Andrew-J", "name": { "family": "Drake", "given": "Andrew" } }, { "name": { "family": "Farrar", "given": "Glennys R." } }, { "id": "Feeney-Michael-E", "name": { "family": "Feeney", "given": "Michael" } }, { "name": { "family": "Foley", "given": "Ryan J." }, "orcid": "0000-0002-2445-5275" }, { "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "name": { "family": "Golkhou", "given": "V. Zach" }, "orcid": "0000-0001-8205-2506" }, { "name": { "family": "Goobar", "given": "Ariel" }, "orcid": "0000-0002-4163-4996" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "name": { "family": "Hammerstein", "given": "Erica" }, "orcid": "0000-0002-5698-8703" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Hung", "given": "Tiara" }, "orcid": "0000-0002-9878-7889" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "name": { "family": "Kilpatrick", "given": "Charles D." }, "orcid": "0000-0002-5740-7747" }, { "name": { "family": "Kong", "given": "Albert K. H." }, "orcid": "0000-0002-5105-344X" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "name": { "family": "Necker", "given": "Jannis" }, "orcid": "0000-0003-0280-7484" }, { "name": { "family": "Nordin", "given": "Jakob" }, "orcid": "0000-0001-8342-6274" }, { "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "name": { "family": "Rigault", "given": "Mickael" }, "orcid": "0000-0002-8121-2560" }, { "name": { "family": "Reusch", "given": "Simeon" }, "orcid": "0000-0002-7788-628X" }, { "id": "Rodriguez-Hector", "name": { "family": "Rodriguez", "given": "Hector" } }, { "name": { "family": "Rojas-Bravo", "given": "C\u00e9sar" }, "orcid": "0000-0002-7559-315X" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Stern-Daniel", "name": { "family": "Stern", "given": "Daniel" }, "orcid": "0000-0003-2686-9241" }, { "name": { "family": "Taggart", "given": "Kirsty" }, "orcid": "0000-0002-5748-4558" }, { "name": { "family": "van Santen", "given": "Jakob" } }, { "name": { "family": "Ward", "given": "Charlotte" }, "orcid": "0000-0002-4557-6682" }, { "name": { "family": "Woudt", "given": "Patrick A." }, "orcid": "0000-0002-6896-1655" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" } ] }, "title": "A tidal disruption event coincident with a high-energy neutrino", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 Nature Publishing Group. \n\nReceived 21 July 2020; Accepted 16 December 2020; Published 22 February 2021. \n\nWe thank C. Lunardini, A. MacFadyen, B. Metzger, A. Mummery, A. Pizzuto, N. Stone, A. Taylor and W. Winter for discussions. We also thank the IceCube Collaboration for publishing high-energy neutrino alerts. We thank S. Digel, K. Fang, D. Horan, M. Kerr, V. Paliya and J. Racusin for feedback provided during a Fermi collaboration review. R.S. is grateful to NYU for facilitating a visit to develop this work. M.K. is grateful for the hospitality received from Columbia University and NYU during a sabbatical visit. This work was supported by the Initiative and Networking Fund of the Helmholtz Association through the Young Investigator Group programme (A.F.). S.v.V. is supported by the James Arthur Postdoctoral Fellowship. This research was partially supported by the Australian Government through the Australian Research Council's Discovery Projects funding scheme (project DP200102471). The work of M.B. is supported through the South African Research Chair Initiative of the National Research Foundation and the Department of Science and Innovation of South Africa, under SARChI Chair grant no. 64789. Any opinion, finding and conclusion or recommendation expressed in this material is that of the authors and the NRF does not accept any liability in this regard. A.H. acknowledges support by the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation. The UCSC transient team is supported in part by NSF grant AST-1518052, NASA/Swift grant 80NSSC19K1386, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation and a fellowship from the David and Lucile Packard Foundation to R.J.F. V.Z.G. is a Moore\u2013Sloan, WRF Innovation in Data Science and DIRAC Fellow. A.G.-Y.'s research is supported by the EU via ERC grant no. 725161, the ISF GW Excellence Center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as the Benoziyo Endowment Fund for the Advancement of Science, the Andr\u00e9 Deloro Institute for Advanced Research in Space and Optics, the Veronika A. Rabl Physics Discretionary Fund, Paul and Tina Gardner, Yeda-Sela and the WIS-CIT joint research grant; A.G.-Y. is the recipient of the Helen and Martin Kimmel Award for Innovative Investigation. M.R. has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 759194-USNAC). The work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The work of S.R. was supported by the Helmholtz Weizmann Research School on Multimessenger Astronomy, funded through the Initiative and Networking Fund of the Helmholtz Association, DESY, the Weizmann Institute, the Humboldt University of Berlin and the University of Potsdam. This work is based on observations obtained with the Samuel Oschin telescope 48-inch and the 60-inch telescope at the Palomar Observatory as part of the ZTF project. ZTF is supported by the National Science Foundation under grant no. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC and UW. SED Machine is based upon work supported by the National Science Foundation under grant no. 1106171. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The MeerKAT telescope is operated by the South African Radio Astronomy Observatory, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation. The work was supported by the GROWTH project funded by the National Science Foundation Partnership in International Research and Education program under grant no. 1545949. GROWTH is a collaborative project between the California Institute of Technology (United States), Pomona College (United States), San Diego State University (United States), Los Alamos National Laboratory (United States), University of Maryland College Park (United States), University of Wisconsin at Milwaukee (United States), Tokyo Institute of Technology (Japan), National Central University (Taiwan), Indian Institute of Astrophysics (India), Inter-University Center for Astronomy and Astrophysics (India), Weizmann Institute of Science (Israel), The Oskar Klein Centre at Stockholm University (Sweden) and Humboldt University (Germany). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias with financial support from the UK Science and Technology Facilities Council. Research at Lick Observatory is partially supported by a gift from Google. The Fermi-LAT Collaboration acknowledges support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK and JAXA (Japan) and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also acknowledged. This work was performed in part under DOE contract DE-AC02-76SF00515. IceCube Neutrino Observatory is a facility of the National Science Foundation operated at the US Amundsen\u2013Scott South Pole Station under the US Antarctic Program. \n\nData availability: The data that support the plots within this paper and other findings of this study are available from https://github.com/robertdstein/at2019dsg, and at https://doi.org/10.5281/zenodo.4308124.\n\nCode availability: Python scripts used to perform significant calculations, and to reproduce all figures, are available from https://github.com/robertdstein/at2019dsg, and at https://doi.org/10.5281/zenodo.4308124. \n\nAuthor Contributions: R.S. first identified AT2019dsg as a candidate neutrino source, performed the neutrino analysis and was the primary author of the manuscript. M.K., R.S. and S.v.V. developed the multizone model. G.R.F., M.K. and R.S. performed the neutrino modelling. A.F., J. Necker, R.S. and S.R. scheduled and analysed ZTF ToO observations. J.C.A.M.-J. and S.v.V. contributed the VLA observations. A.H., R.J.F. and I.S. contributed the AMI-LA observations. M.F.B., M.B., R.J.F., J.C.A.M.-J. and P.W. contributed the MeerKAT observations. S. Gezari and S.v.V. requested and reduced the Swift-UVOT data. D.A.P. and K.T. contributed the Liverpool Telescope observations. S.B.C., S.F. and S. Gezari performed X-ray observations and data analysis. S. Garrappa analysed Fermi gamma-ray data. S.R. and S.v.V. analysed the ZTF data. J.B., E.C.B., R.B., S.B.C., V.C., M.F., V.Z.G., A.G., M.J.G, G.H., M.M.K., T.K., R.R.L., A.A.M, F.J.M., H.R., B.R., D.L.S. and M.T.S contributed to the implementation of ZTF. T.A., I.A., M.W.C., M.M.K. and L.P.S. enabled ZTF ToO observations. A.D., R.J.F., M.J.G., S. Gezari, E.H., T.H., M.M.K., C.D.K., M.R., C.R.-B., D.S, C.W. and Y.Y. contributed to spectroscopic observations and data reduction. R.S. developed the ToO analysis pipeline. V.B., J. Nordin and J.v.S. developed AMPEL, and contributed to the ToO analysis infrastructure. A.G.-Y., A.K.H.K. and J.S. contributed to the manuscript and discussions. All authors reviewed the contents of the manuscript. \n\nThe authors declare no competing interests. \n\nPeer review information: Nature Astronomy thanks Kimitake Hayasaki and the other, anonymous, reviewer(s) for their contribution to the peer review of this work.\n\nSubmitted - 2005.05340.pdf
Supplemental Material - 41550_2020_1295_Fig10_ESM.webp
Supplemental Material - 41550_2020_1295_Fig11_ESM.webp
Supplemental Material - 41550_2020_1295_Fig4_ESM.webp
Supplemental Material - 41550_2020_1295_Fig5_ESM.webp
Supplemental Material - 41550_2020_1295_Fig6_ESM.webp
Supplemental Material - 41550_2020_1295_Fig7_ESM.webp
Supplemental Material - 41550_2020_1295_Fig8_ESM.webp
Supplemental Material - 41550_2020_1295_Fig9_ESM.webp
Supplemental Material - 41550_2020_1295_MOESM1_ESM.pdf
", "abstract": "Cosmic neutrinos provide a unique window into the otherwise hidden mechanism of particle acceleration in astrophysical objects. The IceCube Collaboration recently reported the likely association of one high-energy neutrino with a flare from the relativistic jet of an active galaxy pointed towards the Earth. However a combined analysis of many similar active galaxies revealed no excess from the broader population, leaving the vast majority of the cosmic neutrino flux unexplained. Here we present the likely association of a radio-emitting tidal disruption event, AT2019dsg, with a second high-energy neutrino. AT2019dsg was identified as part of our systematic search for optical counterparts to high-energy neutrinos with the Zwicky Transient Facility. The probability of finding any coincident radio-emitting tidal disruption event by chance is 0.5%, while the probability of finding one as bright in bolometric energy flux as AT2019dsg is 0.2%. Our electromagnetic observations can be explained through a multizone model, with radio analysis revealing a central engine, embedded in a UV photosphere, that powers an extended synchrotron-emitting outflow. This provides an ideal site for petaelectronvolt neutrino production. Assuming that the association is genuine, our observations suggest that tidal disruption events with mildly relativistic outflows contribute to the cosmic neutrino flux.", "date": "2020-06-05", "date_type": "published", "publication": "Nature Astronomy", "publisher": "Nature Publishing Group", "id_number": "CaltechAUTHORS:20200604-151413064", "issn": "2397-3366", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151413064", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF)" }, { "agency": "New York University (NYU)" }, { "agency": "Australian Research Council", "grant_number": "DP200102471" }, { "agency": "National Research Foundation (South Africa)", "grant_number": "64789" }, { "agency": "Department of Science and Innovation (South Africa)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation" }, { "agency": "NSF", "grant_number": "AST-1518052" }, { "agency": "NASA", "grant_number": "80NSSC19K1386" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Washington Research Foundation" }, { "agency": "DIRAC Institute" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Israel Ministry of Science" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Benoziyo Endowment Fund" }, { "agency": "Deloro Institute for Advanced Research in Space and Optics" }, { "agency": "Veronika A. Rabl Physics Discretionary Fund" }, { "agency": "Paul and Tina Gardner" }, { "agency": "Yeda-Sela" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Helen and Martin Kimmel Award" }, { "agency": "European Research Council (ERC)", "grant_number": "759194" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Helmholtz Weizmann Research School on Multimessenger Astronomy" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Humboldt University" }, { "agency": "University of Potsdam" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Google" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Institut de recherche sur les lois fondamentales de l'Univers (Irfu)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "KEK (Japan)" }, { "agency": "Japan Aerospace Exploration Agency (JAXA)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "National Space Board (Sweden)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "Heising-Simons Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/s41550-020-01295-8", "primary_object": { "basename": "2005.05340.pdf", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/2005.05340.pdf" }, "related_objects": [ { "basename": "41550_2020_1295_Fig11_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig11_ESM.webp" }, { "basename": "41550_2020_1295_Fig5_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig5_ESM.webp" }, { "basename": "41550_2020_1295_Fig9_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig9_ESM.webp" }, { "basename": "41550_2020_1295_MOESM1_ESM.pdf", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_MOESM1_ESM.pdf" }, { "basename": "41550_2020_1295_Fig10_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig10_ESM.webp" }, { "basename": "41550_2020_1295_Fig4_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig4_ESM.webp" }, { "basename": "41550_2020_1295_Fig6_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig6_ESM.webp" }, { "basename": "41550_2020_1295_Fig7_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig7_ESM.webp" }, { "basename": "41550_2020_1295_Fig8_ESM.webp", "url": "https://authors.library.caltech.edu/records/c1bm9-7b434/files/41550_2020_1295_Fig8_ESM.webp" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Stein, Robert; van Velzen, Sjoert; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dcp0r-yy108", "eprint_id": 97616, "eprint_status": "archive", "datestamp": "2023-08-19 21:33:35", "lastmod": "2023-10-18 16:08:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zhai-Chengxing", "name": { "family": "Zhai", "given": "Chengxing" }, "orcid": "0000-0002-0291-4522" }, { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Shao-Michael", "name": { "family": "Shao", "given": "Michael" } }, { "id": "Trahan-R", "name": { "family": "Trahan", "given": "Russell" } }, { "id": "Saini-N-S", "name": { "family": "Saini", "given": "Navtej S." } }, { "id": "Shen-Janice", "name": { "family": "Shen", "given": "Janice" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Rosnet-P", "name": { "family": "Rosnet", "given": "Philippe" } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" } ] }, "title": "Synthetic Tracking Using ZTF Deep Drilling Data Sets", "ispublished": "pub", "full_text_status": "public", "keywords": "astronomical object indentification \u2013 astronomy data analysis \u2013 astronomy data reduction \u2013 detection \u2013 GPU computing", "note": "\u00a9 2020 The Astronomical Society of the Pacific. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2020 January 13; accepted 2020 March 23; published 2020 April 21. \n\nWe thank the anonymous reviewer of this paper for many constructive comments that helped us improve the manuscript. These results are based on observations obtained with the Samuel Oschin 48 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The work described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright 2019. Government sponsorship acknowledged.\n\nPublished - Zhai_2020_PASP_132_064502.pdf
Submitted - 1907.11299.pdf
", "abstract": "The Zwicky Transit Facility (ZTF) is a powerful time domain survey telescope with a large field of view of 47 deg\u00b2. We apply the synthetic tracking technique to integrate a ZTF's deep drilling data set, which consists of 133 nominal 30 s exposure frames spanning about 1.5 hr, to search for slowly moving asteroids down to approximately 23rd magnitude. We found 1168 objects from searching 40 of the 64 CCD-quadrant subfields, each of which covers a field size of about 0.73 deg\u00b2. While most of the objects are in the core region of the asteroid belt, there are asteroids belonging to families of Trojan, Hilda, Hungaria, Phocaea, and near-Earth-asteroids. Such an approach is effective and productive for discovering new asteroids. Here we report the data processing and results as well as discuss a potential deep drilling operation mode using this approach for survey facilities.", "date": "2020-06", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "132", "number": "1012", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 064502", "id_number": "CaltechAUTHORS:20190802-105703823", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190802-105703823", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Caltech" }, { "agency": "Infrared Processing and Analysis Center (IPAC)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Stockholm University" }, { "agency": "University of Maryland" }, { "agency": "University of Washington" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Humboldt University" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "TANGO Consortium" }, { "agency": "University of Wisconsin-Milwaukee" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "Gaia Multilateral Agreement" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/ab828b", "primary_object": { "basename": "1907.11299.pdf", "url": "https://authors.library.caltech.edu/records/dcp0r-yy108/files/1907.11299.pdf" }, "related_objects": [ { "basename": "Zhai_2020_PASP_132_064502.pdf", "url": "https://authors.library.caltech.edu/records/dcp0r-yy108/files/Zhai_2020_PASP_132_064502.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Zhai, Chengxing; Ye, Quanzhi; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/k73kj-b3s87", "eprint_id": 101783, "eprint_status": "archive", "datestamp": "2023-08-22 05:06:49", "lastmod": "2023-10-19 23:10:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Dong-Dillon-Z-J", "name": { "family": "Dong", "given": "Dillon Z. J." } }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Chandra-P", "name": { "family": "Chandra", "given": "Poonam" }, "orcid": "0000-0002-0844-6563" }, { "id": "Andreoni-I", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Burdge-K-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Coughlin-M-W", "name": { "family": "Coughlin", "given": "Michael" }, "orcid": "0000-0002-8262-2924" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Feeney-M-E", "name": { "family": "Feeney", "given": "Michael" } }, { "id": "Fredericks-D-D", "name": { "family": "Fredericks", "given": "Dmitry D." }, "orcid": "0000-0002-1153-6340" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Golkhou-V-Z", "name": { "family": "Golkhou", "given": "V. Zach" }, "orcid": "0000-0001-8205-2506" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Hale-D-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Porter-M", "name": { "family": "Porter", "given": "Michael" } }, { "id": "Ridnaia-A", "name": { "family": "Ridnaia", "given": "Anna" } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soumagnac-M-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Svinkin-D-S", "name": { "family": "Svinkin", "given": "Dmitry S." }, "orcid": "0000-0002-2208-2196" } ] }, "title": "The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at z = 0.27", "ispublished": "pub", "full_text_status": "public", "keywords": "Radio transient sources; High energy astrophysics; Supernovae; Core-collapse supernovae; Jets; Sky surveys", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 March 2; revised 2020 April 19; accepted 2020 April 20; published 2020 May 26. \n\nA.Y.Q.H thanks the NRAO staff for their help with data calibration and imaging, particularly Steve Myers, Aaron Lawson, Drew Medlin, and Emmanuel Momjian. She is grateful for their support and hospitality during her visit to Socorro. She also thanks Gregg Hallinan and Brad Cenko for their advice on reducing the radio and X-ray data, respectively, Jochen Greiner and Iair Arcavi for their assistance in obtaining the afterglow-subtracted light curve of SN 2011kl, Miika Pursiainen for sharing light curves of DES fast luminous transients, Griffin Hosseinzadeh for useful discussions about iPTF15ul, Jesper Sollerman and Steve Schulze for carefully reading the manuscript, and Tony Piro and Ben Margalit for other productive conversations. This work made use of the IPN master burst list (ssl.berkeley.edu/ipn3/masterli.html) maintained by Kevin Hurley. We thank Raffaella Margutti for pointing out a typo in an earlier version of this paper, and the anonymous referee for detailed comments that greatly improved the flow and clarity of the paper. \n\nA.Y.Q.H. acknowledges the support of a National Science Foundation Graduate Research Fellowship under grant No. DGE-1144469, the GROWTH project funded by the National Science Foundation under PIRE grant No. 1545949, and the Heising-Simons Foundation. P.C. acknowledges support from the Department of Science and Technology via SwarnaJayanti Fellowship awards (DST/SJF/PSA-01/2014-15). A.H. is grateful for the support by grants from the Israel Science Foundation, the US-Israel Binational Science Foundation, and the I-CORE Program of the Planning and Budgeting Committee and the Israel Science Foundation. This research was funded in part by a grant from the Heising-Simons Foundation and a grant from the Gordon and Betty Moore Foundation through grant GBMF5076, and benefited from interactions with Daniel Kasen and David Khatami, also funded by that grant. A.A.M. is funded by the Large Synoptic Survey Telescope Corporation, the Brinson Foundation, and the Moore Foundation in support of the LSSTC Data Science Fellowship Program; he also receives support as a CIERA Fellow by the CIERA Postdoctoral Fellowship Program (Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University). \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. 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 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: Keck:I (LRIS) - , Hale (DBSP) - , EVLA - , GMRT. - \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018), IPython (P\u00e9rez & Granger 2007), matplotlib (Hunter 2007), numpy (Oliphant 2006), scipy (Virtanen et al. 2019), extinction (Barbary 2016), LPipe (Perley 2019), PYRAF-DBSP (Bellm & Sesar 2016), IDLAstro.\n\nPublished - Ho_2020_ApJ_895_49.pdf
Submitted - 2003.01222.pdf
", "abstract": "We present ZTF18abvkwla (the \"Koala\"), a fast blue optical transient discovered in the Zwicky Transient Facility (ZTF) One-Day Cadence (1DC) Survey. ZTF18abvkwla has a number of features in common with the groundbreaking transient AT 2018cow: blue colors at peak (g \u2013 r \u2248 \u22120.5 mag), a short rise time from half-max of under two days, a decay time to half-max of only three days, a high optical luminosity (M_(g,peak) \u2248 \u221220.6 mag), a hot (\u227340,000 K) featureless spectrum at peak light, and a luminous radio counterpart. At late times (\u0394t > 80 days), the radio luminosity of ZTF18abvkwla (\u03bd_(L\u03bd) \u2273 10\u2074\u2070 erg\u207b\u00b9 at 10 GHz, observer-frame) is most similar to that of long-duration gamma-ray bursts (GRBs). The host galaxy is a dwarf starburst galaxy (M \u2248 5\u00d710\u2078 M\u2299, SFR \u2248 7 M\u2299 yr\u207b\u00b9) that is moderately metal-enriched (log[O/H] \u2248 8.5), similar to the hosts of GRBs and superluminous supernovae. As in AT2018cow, the radio and optical emission in ZTF18abvkwla likely arise from two separate components: the radio from fast-moving ejecta (\u0393\u03b2c > 0.38c) and the optical from shock-interaction with confined dense material (<0.07 M\u2299 in \u223c10\u00b9\u2075 cm). Compiling transients in the literature with t_(rise) < 5 days and M_(peak) < \u221220 mag, we find that a significant number are engine-powered, and suggest that the high peak optical luminosity is directly related to the presence of this engine. From 18 months of the 1DC survey, we find that transients in this rise-luminosity phase space are at least two to three orders of magnitude less common than CC SNe. Finally, we discuss strategies for identifying such events with future facilities like the Large Synoptic Survey Telescope, as well as prospects for detecting accompanying X-ray and radio emission.", "date": "2020-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "895", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 49", "id_number": "CaltechAUTHORS:20200309-115301856", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200309-115301856", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Heising-Simons Foundation" }, { "agency": "Department of Science and Technology (India)", "grant_number": "DST/SJF/PSA-01/2014-15" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Brinson Foundation" }, { "agency": "Northwestern University" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Caltech" }, { "agency": "Infrared Processing and Analysis Center (IPAC)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Stockholm University" }, { "agency": "University of Maryland" }, { "agency": "University of Washington" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Humboldt University" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "TANGO Consortium" }, { "agency": "University of Wisconsin-Milwaukee" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/ab8bcf", "primary_object": { "basename": "Ho_2020_ApJ_895_49.pdf", "url": "https://authors.library.caltech.edu/records/k73kj-b3s87/files/Ho_2020_ApJ_895_49.pdf" }, "related_objects": [ { "basename": "2003.01222.pdf", "url": "https://authors.library.caltech.edu/records/k73kj-b3s87/files/2003.01222.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Ho, Anna Y. Q.; Perley, Daniel A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/03s09-e9y28", "eprint_id": 99964, "eprint_status": "archive", "datestamp": "2023-08-22 05:06:40", "lastmod": "2023-10-18 18:57:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Sharma-Y", "name": { "family": "Sharma", "given": "Y." } }, { "id": "Dugas-A-M", "name": { "family": "Dugas", "given": "A." } }, { "name": { "family": "Perley", "given": "D. A." } }, { "name": { "family": "Taggart", "given": "K." } }, { "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "name": { "family": "Graham", "given": "M. L." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "name": { "family": "Nordin", "given": "J." } }, { "name": { "family": "Rigault", "given": "M." } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Andreoni-I", "name": { "family": "Andreoni", "given": "I." }, "orcid": "0000-0002-8977-1498" }, { "id": "Bagdasaryan-A", "name": { "family": "Bagdasaryan", "given": "A." } }, { "id": "Belicki-J", "name": { "family": "Belicki", "given": "J." } }, { "name": { "family": "Cannella", "given": "C." } }, { "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "K." }, "orcid": "0000-0002-8989-0542" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "R." } }, { "name": { "family": "Frederick", "given": "S." } }, { "name": { "family": "Golkhou", "given": "V. Z." } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "M. J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "A. Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Riddle-R-L", "name": { "family": "Riddle", "given": "R." }, "orcid": "0000-0002-0387-370X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "name": { "family": "Schulze", "given": "S." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "R. M." } }, { "id": "van-Velzen-S", "name": { "family": "van Velzen", "given": "S." }, "orcid": "0000-0002-3859-8074" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Yao-Y", "name": { "family": "Yao", "given": "Y." } }, { "id": "Zhuang-Z", "name": { "family": "Zhuang", "given": "Z." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "The Zwicky Transient Facility Bright Transient Survey I: Spectroscopic Classification and the Redshift Completeness of Local Galaxy Catalogs", "ispublished": "pub", "full_text_status": "public", "keywords": "Supernovae; Galaxies; Redshift surveys; Surveys", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 October 28; revised 2020 March 16; accepted 2020 March 23; published 2020 May 21. \n\nWe thank the anonymous referee for providing comments that improved this manuscript. \n\nOccasional observers on the UW APO ZTF follow-up team include Brigitta Sipocz, James Davenport, Daniela Huppenkothen, Dino Bekte\u0161evi\u0107 Gwendolyn Eadie, and Bryce T. Bolin. \n\nWe thank students Shaney Sze and Ho Ko for assisting with candidate vetting during the summer of 2018.\n\nThis work is based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under PIRE grant No. 1545949. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). The Oskar Klein Centre is funded by the Swedish Research Council. \n\nC.F. gratefully acknowledges support of his research by the Heising-Simons Foundation (#2018-0907). \n\nA.A.M. is funded by the Large Synoptic Survey Telescope Corporation, the Brinson Foundation, and the Moore Foundation in support of the LSSTC Data Science Fellowship Program; he also receives support as a CIERA Fellow by the CIERA Postdoctoral Fellowship Program (Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University). \n\nM.L.G. acknowledges support from the DiRAC Institute in the Department of Astronomy at the University of Washington. The DiRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. \n\nM.R. has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 759194\u2014USNAC). \n\nS.V. is supported by the James Arthur Postdoctoral Fellowship. \n\nA.Y.Q.H. is supported by a National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. \n\nA.G. and J.S. acknowledge support from the K&A Wallenberg foundation and the Swedish National Science foundation, VR. \n\nPartially based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Some of the data presented here were obtained with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. \n\nSome of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThis paper is partly based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundaci\u00f3n Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Partially based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. Partially based on observations from the LCOGT network. Partially based on public observations collected at the WHT, operated on the island of La Palma by the Isaac Newton Group. \n\nThe Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. \n\nThe SED Machine is based upon work supported by the National Science Foundation under grant No. 1106171. \n\nSoftware: SNID (Blondin & Tonry 2007), astropy (Astropy Collaboration et al. 2013), scipy (Virtanen et al. 2020), matplotlib (Hunter 2007), pandas (McKinney 2010), emcee (Foreman-Mackey et al. 2013), corner (Foreman-Mackey 2016), MultinomCI (Signorell et al. 2019), PYSEDM (Rigault et al. 2019), IRAF (Tody 1986), PyRAF (Science Software Branch at STScI 2012), pyraf-dbsp (Bellm & Sesar 2016), LPipe (Perley 2019), pyDIS (Davenport et al. 2016).\n\nPublished - Fremling_2020_ApJ_895_32.pdf
Submitted - 1910.12973.pdf
", "abstract": "The Zwicky Transient Facility (ZTF) is performing a three-day cadence survey of the visible northern sky (~3\u03c0) with newly found transient candidates announced via public alerts. The ZTF Bright Transient Survey (BTS) is a large spectroscopic campaign to complement the photometric survey. BTS endeavors to spectroscopically classify all extragalactic transients with m_(peak) \u2264 18.5 mag in either the g_(ZTF) or r_(ZTF) filters, and publicly announce said classifications. BTS discoveries are predominantly supernovae (SNe), making this the largest flux-limited SN survey to date. Here we present a catalog of 761 SNe, classified during the first nine months of ZTF (2018 April 1\u20132018 December 31). We report BTS SN redshifts from SN template matching and spectroscopic host-galaxy redshifts when available. We analyze the redshift completeness of local galaxy catalogs, the redshift completeness fraction (RCF; the ratio of SN host galaxies with known spectroscopic redshift prior to SN discovery to the total number of SN hosts). Of the 512 host galaxies with SNe Ia, 227 had previously known spectroscopic redshifts, yielding an RCF estimate of 44% \u00b1 4%. The RCF decreases with increasing distance and decreasing galaxy luminosity (for z < 0.05, or ~200 Mpc, RCF \u2248 0.6). Prospects for dramatically increasing the RCF are limited to new multifiber spectroscopic instruments or wide-field narrowband surveys. Existing galaxy redshift catalogs are only ~50% complete at r \u2248 16.9 mag. Pushing this limit several magnitudes deeper will pay huge dividends when searching for electromagnetic counterparts to gravitational wave events or sources of ultra-high-energy cosmic rays or neutrinos.", "date": "2020-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "895", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 32", "id_number": "CaltechAUTHORS:20191120-152035670", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191120-152035670", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Caltech" }, { "agency": "Infrared Processing and Analysis Center (IPAC)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Stockholm University" }, { "agency": "University of Maryland" }, { "agency": "University of Washington" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Humboldt University" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "TANGO Consortium" }, { "agency": "University of Wisconsin-Milwaukee" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Heising-Simons Foundation", "grant_number": "12540303" }, { "agency": "Swedish Research Council" }, { "agency": "Heising-Simons Foundation", "grant_number": "2018-0907" }, { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Brinson Foundation" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)" }, { "agency": "Northwestern University" }, { "agency": "European Research Council (ERC)", "grant_number": "759194" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish National Science Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/ab8943", "primary_object": { "basename": "Fremling_2020_ApJ_895_32.pdf", "url": "https://authors.library.caltech.edu/records/03s09-e9y28/files/Fremling_2020_ApJ_895_32.pdf" }, "related_objects": [ { "basename": "1910.12973.pdf", "url": "https://authors.library.caltech.edu/records/03s09-e9y28/files/1910.12973.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Fremling, C.; Miller, A. A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qt1ea-5w414", "eprint_id": 101097, "eprint_status": "archive", "datestamp": "2023-08-22 03:56:49", "lastmod": "2023-10-23 16:14:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample", "ispublished": "pub", "full_text_status": "public", "keywords": "Astrophysical dust processes; Polycyclic aromatic hydrocarbons; Interstellar medium; Infrared galaxies", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 September 16; revised 2019 December 4; accepted 2019 December 5; published 2020 February. \n\nWe thank the referee for helpful comments. We are grateful to R.H. Lupton for availability of the SM graphics program. L.K.H. thanks Princeton University for kind hospitality during a very pleasant and productive visit and acknowledges funding from the INAF PRIN-SKA 2017 program 1.05.01.88.04. This research was supported in part by JPL grants 1329088 and 1373687, and by NSF grants AST-0406883, AST-1008570, and AST-1408723. K.S. was supported in part by NSF grant AST-1615728 and NASA ADP grant NNX17AF39G. \n\nFacilities: Spitzer Space Telescope - , Herschel Space Observatory - , Karl G. Jansky Very Large Array - , IRAM 30 m telescope - , Westerbork Synthesis Radio Telescope - , Nobeyama Radio Observatory. - \n\nSoftware: CASA (McMullin et al. 2007); SINGS Fifth Data Delivery Pipeline; Local Volume Legacy Project Pipeline; HIPE v11.1.0 (Ott 2010); Scanamorphos v24.0 (Roussel 2013); R (R Core Team 2014); SM.\n\nPublished - Aniano_2020_ApJ_889_150.pdf
Accepted Version - 1912.04914.pdf
Erratum - Aniano_2020_ApJ_897_184.pdf
", "abstract": "Interstellar dust and starlight are modeled for the galaxies of the project \"Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel.\" The galaxies were observed by the Infrared Array Camera and the Multiband Imaging Photometer for Spitzer on Spitzer Space Telescope, and the Photodetector Array Camera and Spectrometer and the Spectral and Photometric Imaging Receiver on Herschel Space Observatory. With data from 3.6 to 500 \u03bcm, dust models are strongly constrained. Using a physical dust model, for each pixel in each galaxy we estimate (1) dust surface density, (2) dust mass fraction in polycyclic aromatic hydrocarbons (PAHs), (3) distribution of starlight intensities heating the dust, (4) total infrared (IR) luminosity emitted by the dust, and (5) IR luminosity originating in subregions with high starlight intensity. The dust models successfully reproduce the observed global and resolved spectral energy distributions. With the angular resolution of Herschel, we obtain well-resolved maps (available online) for the dust properties. As in previous studies, we find the PAH fraction q_(PAH) to be an increasing function of metallicity, with a threshold oxygen abundance Z/Z\u2299 \u2248 0.1, but we find the data to be fitted best with q_(PAH) increasing linearly with log(O/H) above a threshold value of 0.15(O/H)\u2299. We obtain total dust masses for each galaxy by summing the dust mass over the individual map pixels; these \"resolved\" dust masses are consistent with the masses inferred from a model fit to the global photometry. The global dust-to-gas ratios obtained from this study are found to correlate with galaxy metallicities. Systems with Z/Z\u2299 \u2273 0.5 have most of their refractory elements locked up in dust, whereas in systems with Z/Z\u2299 \u227e 0.3 most of these elements tend to remain in the gas phase. Within galaxies, we find that q_(PAH) is suppressed in regions with unusually warm dust with vL_v(70 \u03bcm) \u2273 0.4L_(dust). With knowledge of one long-wavelength flux density ratio (e.g., f\u2081\u2086\u2080/f\u2085\u2080\u2080), the minimum starlight intensity heating the dust (U_(min)) can be estimated to within ~50%, despite a variation in U_(min) of more than two orders of magnitude. For the adopted dust model, dust masses can be estimated to within ~0.2 dex accuracy using the f\u2081\u2086\u2080/f\u2085\u2080\u2080 flux ratio and the integrated dust luminosity, and to ~0.07 dex accuracy using the 500 \u03bcm luminosity vL_v(500 \u00b5m) alone. There are additional systematic errors arising from the choice of dust model, but these are hard to estimate. These calibrated prescriptions for estimating starlight heating intensity and dust mass may be useful for studies of high-redshift galaxies.", "date": "2020-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "889", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 150", "id_number": "CaltechAUTHORS:20200204-074914004", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-074914004", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-SKA 2017" }, { "agency": "JPL", "grant_number": "1329088" }, { "agency": "JPL", "grant_number": "1373687" }, { "agency": "NSF", "grant_number": "AST-0406883" }, { "agency": "NSF", "grant_number": "AST-1008570" }, { "agency": "NSF", "grant_number": "AST-1408723" }, { "agency": "NSF", "grant_number": "AST-1615728" }, { "agency": "NASA", "grant_number": "NNX17AF39G" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/ab5fdb", "primary_object": { "basename": "Aniano_2020_ApJ_889_150.pdf", "url": "https://authors.library.caltech.edu/records/qt1ea-5w414/files/Aniano_2020_ApJ_889_150.pdf" }, "related_objects": [ { "basename": "Aniano_2020_ApJ_897_184.pdf", "url": "https://authors.library.caltech.edu/records/qt1ea-5w414/files/Aniano_2020_ApJ_897_184.pdf" }, { "basename": "1912.04914.pdf", "url": "https://authors.library.caltech.edu/records/qt1ea-5w414/files/1912.04914.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Aniano, G.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/j2eg0-01z04", "eprint_id": 100903, "eprint_status": "archive", "datestamp": "2023-08-22 03:48:38", "lastmod": "2023-10-19 22:14:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Farnocchia-D", "name": { "family": "Farnocchia", "given": "Davide" }, "orcid": "0000-0003-0774-884X" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Reiley-D-J", "name": { "family": "Reiley", "given": "Daniel J." } }, { "id": "Soumagnac-M-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" } ] }, "title": "A Twilight Search for Atiras, Vatiras, and Co-orbital Asteroids: Preliminary Results", "ispublished": "pub", "full_text_status": "public", "keywords": "Atira group; Near-Earth objects; Earth trojans; Sky surveys", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2019 October 6; revised 2019 December 11; accepted 2019 December 12; published 2020 January 23. \n\nWe thank the anonymous referee for comments. Q.-Z.Y. acknowledges support by the Global Relay of Observatories Watching Transients Happen (GROWTH) project funded by the National Science Foundation Partnership in International Research and Education (PIRE) program under grant No. 1545949. We also thank Dave Tholen for discussion in the early phase of ZTF-TS and Bryce Bolin for comments. The work of W.-H.I. was supported in part by grant No. 107-2119-M-008-012 of MOST, Taiwan, and grant No. 119/2017/A3 of FCDT of Macau, MSAR. D.F. conducted this research at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by Caltech Optical Observatories, Infrared Processing and Analysis Center, and the University of Washington. \n\nFacility: PO:1.2m. - \n\nSoftware: astcheck, Matplotlib (Hunter 2007), NEOPOP (Granvik et al. 2018), sbpy (Mommert et al. 2018).\n\nPublished - Ye_2020_AJ_159_70.pdf
Accepted Version - 1912.06109.pdf
", "abstract": "Near-Earth objects (NEOs) that orbit the Sun on or within Earth's orbit are tricky to detect for Earth-based observers due to their proximity to the Sun in the sky. These small bodies hold clues to the dynamical history of the inner solar system as well as the physical evolution of planetesimals in extreme environments. Populations in this region include the Atira and Vatira asteroids, as well as Venus and Earth co-orbital asteroids. Here we present a twilight search for these small bodies, conducted using the 1.2 m Oschin Schmidt and the Zwicky Transient Facility (ZTF) camera at Palomar Observatory. The ZTF twilight survey operates at solar elongations down to 35\u00b0 with a limiting magnitude of r = 19.5. During a total of 40 evening sessions and 62 morning sessions conducted between 2018 November 15 and 2019 June 23, we detected six Atiras, including two new discoveries, 2019 AQ\u2083 and 2019 LF\u2086, but no Vatiras or Earth/Venus co-orbital asteroids. NEO population models show that these new discoveries are likely only the tip of the iceberg, with the bulk of the population yet to be found. The population models also suggest that we have only detected 5%\u20137% of the H < 20 Atira population over the seven month survey. Co-orbital asteroids are smaller in diameter and require deeper surveys. A systematic and efficient survey of the near-Sun region will require deeper searches and/or facilities that can operate at small solar elongations.", "date": "2020-02", "date_type": "published", "publication": "Astronomical Journal", "volume": "159", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 70", "id_number": "CaltechAUTHORS:20200124-134730965", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200124-134730965", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "107-2119-M-008-012" }, { "agency": "Macao Science and Technology Development Fund (FDCT)", "grant_number": "119/2017/A3" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1440341" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-3881/ab629c", "primary_object": { "basename": "1912.06109.pdf", "url": "https://authors.library.caltech.edu/records/j2eg0-01z04/files/1912.06109.pdf" }, "related_objects": [ { "basename": "Ye_2020_AJ_159_70.pdf", "url": "https://authors.library.caltech.edu/records/j2eg0-01z04/files/Ye_2020_AJ_159_70.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Ye, Quanzhi; Masci, Frank J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bcv1w-4we73", "eprint_id": 100325, "eprint_status": "archive", "datestamp": "2023-08-19 14:56:03", "lastmod": "2024-01-14 22:04:28", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "Philip N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "Fran\u00e7ois" } }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "Matt" }, "orcid": "0000-0001-5261-7094" }, { "id": "Braine-Jonathan", "name": { "family": "Braine", "given": "Jonathan" } }, { "id": "Bromm-V", "name": { "family": "Bromm", "given": "Volker" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "Michelle" }, "orcid": "0000-0002-9871-6490" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "D\u00edaz-Santos-T", "name": { "family": "D\u00edaz-Santos", "given": "Tanio" }, "orcid": "0000-0003-0699-6083" }, { "id": "Egami-Eiichi", "name": { "family": "Egami", "given": "Eiichi" } }, { "id": "Emonts-B", "name": { "family": "Emonts", "given": "Bjorn" } }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "Pierre" }, "orcid": "0000-0002-2421-1350" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Lanz-L", "name": { "family": "Lanz", "given": "Lauranne" }, "orcid": "0000-0002-3249-8224" }, { "id": "Madden-S", "name": { "family": "Madden", "given": "Susanne" } }, { "id": "Medling-A-M", "name": { "family": "Medling", "given": "Anne" }, "orcid": "0000-0001-7421-2944" }, { "id": "O'Sullivan-E", "name": { "family": "O'Sullivan", "given": "Ewan" } }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick" }, "orcid": "0000-0002-3471-981X" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "Alexandra" }, "orcid": "0000-0001-8592-2706" }, { "id": "Pineau-des-For\u00eats-G", "name": { "family": "Pineau des For\u00eats", "given": "Guillaume" } }, { "id": "Shull-J-M", "name": { "family": "Shull", "given": "J. Michael" } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David" }, "orcid": "0000-0003-1545-5078" }, { "id": "Togi-A", "name": { "family": "Togi", "given": "Aditya" }, "orcid": "0000-0001-5042-3421" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. Kevin" }, "orcid": "0000-0002-1588-6700" } ] }, "title": "Warm H\u2082 as a probe of massive accretion and feedback through shocks and turbulence across cosmic time", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted as a science White Paper to the Astronomy and Astrophysics Astro 2020 Decadal Survey call issued by the National Academies of Sciences, Engineering and Medicine (March 11 2019).\n\nSubmitted - 1903.06653.pdf
", "abstract": "Galaxy formation depends on a complex interplay between gravitational collapse, gas accretion, merging, and feedback processes. Yet, after many decades of investigation, these concepts are poorly understood. This paper presents the argument that warm H\u2082 can be used as a tool to unlock some of these mysteries. Turbulence, shocks and outflows, driven by star formation, AGN activity or inflows, may prevent the rapid buildup of star formation in galaxies. Central to our understanding of how gas is converted into stars is the process by which gas can dissipate its mechanical energy through turbulence and shocks in order to cool. H\u2082 lines provide direct quantitative measurements of kinetic energy dissipation in molecular gas in galaxies throughout the Universe. Based on the detection of very powerful H\u2082 lines from z = 2 galaxies and proto-clusters at the detection limits of Spitzer, we are confident that future far-IR and UV H\u2082 observations will provide a wealth of new information and insight into galaxy evolution to high-z. Finally, at the very earliest epoch of star and galaxy formation, warm H\u2082 may also provide a unique glimpse of molecular gas collapse at 7 < z < 12 in massive dark matter (DM) halos on their way to forming the very first galaxies. Such measurements are beyond the reach of existing and planned observatories.", "date": "2019-12-17", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20191217-095259394", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191217-095259394", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.1903.06653", "primary_object": { "basename": "1903.06653.pdf", "url": "https://authors.library.caltech.edu/records/bcv1w-4we73/files/1903.06653.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Appleton, Philip N.; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/45n07-53r39", "eprint_id": 99900, "eprint_status": "archive", "datestamp": "2023-08-22 03:02:09", "lastmod": "2023-10-18 18:54:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kelley-Michael-S-P", "name": { "family": "Kelley", "given": "Michael S. P." }, "orcid": "0000-0002-6702-7676" }, { "id": "Bodewits-Dennis", "name": { "family": "Bodewits", "given": "Dennis" }, "orcid": "0000-0002-2668-7248" }, { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Farnham-Tony-L", "name": { "family": "Farnham", "given": "Tony L." }, "orcid": "0000-0002-4767-9861" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soumagnac-Maayane-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Zolkower-Jeffry-N", "name": { "family": "Zolkower", "given": "Jeffry" } } ] }, "title": "Comet 240P/NEAT Is Stirring", "ispublished": "pub", "full_text_status": "public", "keywords": "Cometary studies; Light curves", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 July 16; revised 2019 October 22; accepted 2019 November 4; published 2019 November 18. \n\nWe thank all amateur astronomers contributing to the discovery of cometary outbursts. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch at the Palomar Observatory as part of the Zwicky Transient Facility project. Z.T.F. is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nFacilities: PO:1.2 m (NEAT - , PTF - , ZTF). - \n\nSoftware: Astropy (Astropy Collaboration et al. 2018), SEP (Barbary 2016), ZChecker (Kelley et al. 2019), Calviacat (Kelley & Lister 2019).\n\nPublished - Kelley_2019_ApJL_886_L16.pdf
Accepted Version - 1911.02383.pdf
", "abstract": "Comets are primitive objects that formed in the protoplanetary disk, and have been largely preserved over the history of the solar system. However, they are not pristine, and surfaces of cometary nuclei do evolve. In order to understand the extent of their primitive nature, we must define the mechanisms that affect their surfaces and comae. We examine the lightcurve of comet 240P/NEAT over three consecutive orbits, and investigate three events of significant brightening (\u0394m ~ \u22122 mag). Unlike typical cometary outbursts, each of the three events are long-lived, with enhanced activity for at least 3\u20136 months. The third event, observed by the Zwicky Transient Facility, occurred in at least two stages. The anomalous behavior appears to have started after the comet was perturbed by Jupiter in 2007, reducing its perihelion distance from 2.53 to 2.12 au. We suggest that the brightening events are temporary transitions to a higher baseline activity level, brought on by the increased insolation, which has warmed previously insulated sub-surface layers. The new activity is isolated to one or two locations on the nucleus, indicating that the surface or immediate sub-surface is heterogeneous. Further study of this phenomenon may provide insight into cometary outbursts, the structure of the near-surface nucleus, and cometary nucleus mantling.", "date": "2019-11-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "886", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L16", "id_number": "CaltechAUTHORS:20191118-120700599", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191118-120700599", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Caltech" }, { "agency": "Infrared Processing and Analysis Center (IPAC)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Stockholm University" }, { "agency": "University of Maryland" }, { "agency": "University of Washington" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Humboldt University" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "TANGO Consortium" }, { "agency": "University of Wisconsin-Milwaukee" }, { "agency": "Lawrence Berkeley National Laboratory" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/2041-8213/ab53e0", "primary_object": { "basename": "1911.02383.pdf", "url": "https://authors.library.caltech.edu/records/45n07-53r39/files/1911.02383.pdf" }, "related_objects": [ { "basename": "Kelley_2019_ApJL_886_L16.pdf", "url": "https://authors.library.caltech.edu/records/45n07-53r39/files/Kelley_2019_ApJL_886_L16.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Kelley, Michael S. P.; Bodewits, Dennis; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/05e4p-d0928", "eprint_id": 96484, "eprint_status": "archive", "datestamp": "2023-08-19 18:47:13", "lastmod": "2023-10-20 21:13:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob E." }, "orcid": "0000-0001-5754-4007" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Bond-H-E", "name": { "family": "Bond", "given": "Howard E." }, "orcid": "0000-0003-1377-7145" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "Joel" }, "orcid": "0000-0001-5975-290X" }, { "id": "Karambelkar-V", "name": { "family": "Karambelkar", "given": "Viraj" } }, { "id": "Lau-R-M", "name": { "family": "Lau", "given": "Ryan M." } }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Ryder-S-D", "name": { "family": "Ryder", "given": "Stuart D." }, "orcid": "0000-0003-4501-8100" }, { "id": "Cody-A-M", "name": { "family": "Cody", "given": "Ann Marie" }, "orcid": "0000-0002-3656-6706" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Bally-J", "name": { "family": "Bally", "given": "John" }, "orcid": "0000-0001-8135-6612" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "Nadejda" }, "orcid": "0000-0003-0901-1606" }, { "id": "Castell\u00f3n-S", "name": { "family": "Castell\u00f3n", "given": "Sergio" } }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Gehrz-R-D", "name": { "family": "Gehrz", "given": "Robert D." }, "orcid": "0000-0003-1319-4089" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kilpatrick-C-D", "name": { "family": "Kilpatrick", "given": "Charles D." }, "orcid": "0000-0002-5740-7747" }, { "id": "Milne-P-A", "name": { "family": "Milne", "given": "Peter A." }, "orcid": "0000-0002-0370-157X" }, { "id": "Morrell-N", "name": { "family": "Morrell", "given": "Nidia" }, "orcid": "0000-0003-2535-3091" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Phillips-M-M", "name": { "family": "Phillips", "given": "M. M." }, "orcid": "0000-0003-2734-0796" }, { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Williams-R-E", "name": { "family": "Williams", "given": "Robert E." } } ] }, "title": "The SPIRITS sample of Luminous Infrared Transients: Uncovering Hidden Supernovae and Dusty Stellar Outbursts in Nearby Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction \u2013 infrared: general \u2013 stars: massive \u2013 supernovae: general \u2013 supernovae: individual\n(SPIRITS 14buu, SPIRITS 15c, SPIRITS 15ud, SPIRITS 16ix, SPIRITS 16tn, SPIRITS 17lb)", "note": "\u00a9 2019 The American Astronomical Society.\n\nReceived 2019 February 27; revised 2019 September 29; accepted 2019 September 30; published 2019 November 18.\n\nThis paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.\n\nWe thank the anonymous referee for their thorough read of the paper and helpful comments. We thank C. Contreras and the staff of Las Campanas Observatory for help with conducting observations and data reduction. We thank E. Hsiao for helpful commentary and advice in the analysis and discussion of the spectra. We thank K. Mooley, D. Dong, M. Anderson, M. Eastwood, and A. Horesh for helpful advice and assistance with VLA data reduction. We thank S. Mattila and T. Reynolds for valuable discussions in revising this work.\n\nThis material is based on work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144469. H.E.B. acknowledges that support for HST program Nos. GO-13935, GO-14258, and AR-15005 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. R.D.G. was supported by NASA and the United States Air Force. This work is part of the research program VENI, with project No. 016.192.277, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO).\n\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is based in part on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute and from the Mikulski Archive for Space Telescopes at STScI, which are operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We acknowledge the use of public data from the Swift data archive.\n\nSome 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPart of the optical and near-infrared photometric data included in this paper were obtained by the Carnegie Supernova Project through the support of NSF grant AST-1008343.\n\nBased on observations obtained at the Gemini Observatory acquired through the Gemini Observatory Archive and processed using the Gemini IRAF package, 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), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea).\n\nUKIRT is owned by the University of Hawaii (UH) and operated by the UH Institute for Astronomy; operations are enabled through the cooperation of the East Asian Observatory. When the data reported here were acquired, UKIRT was supported by NASA and operated under an agreement among the University of Hawaii, the University of Arizona, and Lockheed Martin Advanced Technology Center; operations were enabled through the cooperation of the East Asian Observatory.\n\nSome of the data used in this paper were acquired with the RATIR instrument, funded by the University of California and NASA Goddard Space Flight Center, and the 1.5 m Harold L. Johnson telescope at the Observatorio Astron\u00f3mico Nacional on the Sierra de San Pedro M\u00e1rtir, operated and maintained by the Observatorio Astron\u00f3mico Nacional and the Instituto de Astronom\u00eda of the Universidad Nacional Aut\u00f3noma de M\u00e9xico. We acknowledge the contribution of Leonid Georgiev and Neil Gehrels to the development of RATIR.\n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nThe Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. This paper includes archived data obtained through the Australia Telescope Online Archive (http://atoa.atnf.csiro.au).\n\nThe Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory. The UK Schmidt Telescope was operated by the Royal Observatory Edinburgh, with funding from the UK Science and Engineering Research Council (later the UK Particle Physics and Astronomy Research Council), until 1988 June, and thereafter by the Anglo-Australian Observatory. The blue plates of the southern Sky Atlas and its Equatorial Extension (together known as the SERC-J), as well as the Equatorial Red (ER) and the Second Epoch [red] Survey (SES), were all taken with the UK Schmidt. Supplemental funding for sky-survey work at the STScI is provided by the European Southern Observatory.\n\nFunding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.\n\nThis 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.\n\nFacilities: Spitzer (IRAC) - , HST (WFPC2 - , WFC3) - , Swift (UVOT) - , PO:1.5 m (CCD) - , PO:1.2 m - , Swope (CCD) - , Du Pont (RetroCam) - , Magellan:Baade (FourStar - , FIRE) - , Keck:I (LRIS - , MOSFIRE) - , Keck:II (DEIMOS - , NIRES) - , Hale (WIRC) - , Gemini:Gillett (GNIRS) - , Gemini:South (FLAMINGOS-2) - , UKIRT (WFCAM) - , OANSPM:HJT (RATIR) - , EVLA - , ATCA - , AMI - .\n\nSoftware: DOLPHOT (Dolphin 2000, 2016), DAOPHOT/ALLSTAR package (Stetson 1987), IRAF (Tody 1986, 1993), Gemini IRAF package (http://www.gemini.edu/sciops/data-and-results/processing-software), LPipe (Perley 2019, http://www.astro.caltech.edu/~dperley/programs/lpipe.html), MOSFIRE Data Reduction Pipeline (https://keck-datareductionpipelines.github.io/MosfireDRP/), Spextool (Cushing et al. 2004), CASA (McMullin et al. 2007).\n\nPublished - Jencson_2019_ApJ_886_40.pdf
Submitted - 1901.00871.pdf
", "abstract": "We present a systematic study of the most luminous (M IR [Vega magnitudes] brighter than \u221214) infrared (IR) transients discovered by the SPitzer InfraRed Intensive Transients Survey (SPIRITS) between 2014 and 2018 in nearby galaxies (D < 35 Mpc). The sample consists of nine events that span peak IR luminosities of M_([4.5],peak) between \u221214 and \u221218.2, show IR colors between 0.2 < ([3.6]\u2013[4.5]) < 3.0, and fade on timescales between 55 days < t_(fade) < 480 days. The two reddest events (A V > 12) show multiple, luminous IR outbursts over several years and have directly detected, massive progenitors in archival imaging. With analyses of extensive, multiwavelength follow-up, we suggest the following possible classifications: five obscured core-collapse supernovae (CCSNe), two erupting massive stars, one luminous red nova, and one intermediate-luminosity red transient. We define a control sample of all optically discovered transients recovered in SPIRITS galaxies and satisfying the same selection criteria. The control sample consists of eight CCSNe and one Type Iax SN. We find that 7 of the 13 CCSNe in the SPIRITS sample have lower bounds on their extinction of 2 < A V < 8. We estimate a nominal fraction of CCSNe in nearby galaxies that are missed by optical surveys as high as 38.5^(+26.0)_(-21.9)% (90% confidence). This study suggests that a significant fraction of CCSNe may be heavily obscured by dust and therefore undercounted in the census of nearby CCSNe from optical searches.", "date": "2019-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "886", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 40", "id_number": "CaltechAUTHORS:20190617-152842446", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190617-152842446", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NASA", "grant_number": "GO-13935" }, { "agency": "NASA", "grant_number": "GO-14258" }, { "agency": "NASA", "grant_number": "AR-15005" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "U.S. Air Force" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "016.192.277" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "Gemini Partnership" }, { "agency": "NSF", "grant_number": "AST-1008343" }, { "agency": "NASA", "grant_number": "NAG W-2166" }, { "agency": "National Geographic Society" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Samuel Oschin Foundation" }, { "agency": "Eastman Kodak Corporation" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab4a01", "primary_object": { "basename": "1901.00871.pdf", "url": "https://authors.library.caltech.edu/records/05e4p-d0928/files/1901.00871.pdf" }, "related_objects": [ { "basename": "Jencson_2019_ApJ_886_40.pdf", "url": "https://authors.library.caltech.edu/records/05e4p-d0928/files/Jencson_2019_ApJ_886_40.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Jencson, Jacob E.; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/maqaa-b9a15", "eprint_id": 100307, "eprint_status": "archive", "datestamp": "2023-08-22 03:02:24", "lastmod": "2023-10-18 19:50:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sutter-J", "name": { "family": "Sutter", "given": "Jessica" }, "orcid": "0000-0002-9183-8102" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "Kevin V." }, "orcid": "0000-0002-5258-7224" }, { "id": "Pelligrini-E-W", "name": { "family": "Pelligrini", "given": "Eric W." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "Philip N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "Pedro" } }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "Alberto D." }, "orcid": "0000-0002-5480-5686" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Crocker-A-F", "name": { "family": "Crocker", "given": "Alison" }, "orcid": "0000-0001-8513-4945" }, { "id": "De-Looze-I", "name": { "family": "De Looze", "given": "Ilse" } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce" }, "orcid": "0000-0002-0846-936X" }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "Maud" }, "orcid": "0000-0002-0283-8689" }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "Brent A." }, "orcid": "0000-0002-9768-0246" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Herrera-Camus-R", "name": { "family": "Herrera-Camus", "given": "Rodrigo" }, "orcid": "0000-0002-2775-0595" }, { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "Leslie K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H\u00e9l\u00e8ne" } }, { "id": "Wolfire-M-G", "name": { "family": "Wolfire", "given": "Mark G." }, "orcid": "0000-0003-0030-9510" } ] }, "title": "Using [C II] 158 \u03bcm Emission from Isolated ISM Phases as a Star Formation Rate Indicator", "ispublished": "pub", "full_text_status": "public", "keywords": "Galactic and extragalactic astronomy; Far infrared astronomy; Interstellar medium; Photodissociation regions; Star forming regions", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 March 15; revised 2019 October 1; accepted 2019 October 10; published 2019 November 20. \n\nWe would like to thank George Privon and Tanio D\u00edaz-Santos for enlightening discussions and contributions. D.A.D. would like to thank IPAC/Caltech for hosting him during the beginning stages of this research. This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, Grant #80NSSC18K1107, as the Wyoming NASA Space Grant Consortium, NASA Grant #NNX15AI08H. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. IRAF, the Image Reduction and Analysis Facility, has been developed by the National Optical Astronomy Observatories and the Space Telescope Science Institute.\n\nPublished - Sutter_2019_ApJ_886_60.pdf
Submitted - 1910.05416.pdf
", "abstract": "The brightest observed emission line in many star-forming galaxies is the [C II] 158 \u03bcm line, making it detectable up to z ~ 7. In order to better understand and quantify the [C II] emission as a tracer of star formation, the theoretical ratio between the [N II] 205 \u03bcm emission and the [C II] 158 \u03bcm emission has been employed to empirically determine the fraction of [C II] emission that originates from the ionized and neutral phases of the interstellar medium (ISM). Sub-kiloparsec measurements of the [C II] 158 \u03bcm and [N II] 205 \u03bcm lines in nearby galaxies have recently become available as part of the Key Insights in Nearby Galaxies: a Far Infrared Survey with Herschel (KINGFISH) and Beyond the Peak programs. With the information from these two far-infrared lines along with the multi-wavelength suite of KINGFISH data, a calibration of the [C II] emission line as a star formation rate (SFR) indicator and a better understanding of the [C II] deficit are pursued. [C II] emission is also compared to polycyclic aromatic hydrocarbon (PAH) emission in these regions to compare photoelectric heating from PAH molecules to cooling by [C II] in the neutral and ionized phases of the ISM. We find that the [C II] emission originating in the neutral phase of the ISM does not exhibit a deficit with respect to the infrared luminosity and is therefore preferred over the [C II] emission originating in the ionized phase of the ISM as an SFR indicator for the normal star-forming galaxies included in this sample.", "date": "2019-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "886", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 60", "id_number": "CaltechAUTHORS:20191216-140847928", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191216-140847928", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "80NSSC18K1107" }, { "agency": "NASA", "grant_number": "NNX15AI08H" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/ab4da5", "primary_object": { "basename": "1910.05416.pdf", "url": "https://authors.library.caltech.edu/records/maqaa-b9a15/files/1910.05416.pdf" }, "related_objects": [ { "basename": "Sutter_2019_ApJ_886_60.pdf", "url": "https://authors.library.caltech.edu/records/maqaa-b9a15/files/Sutter_2019_ApJ_886_60.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Sutter, Jessica; Dale, Daniel A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/t5mct-16v77", "eprint_id": 99004, "eprint_status": "archive", "datestamp": "2023-08-19 17:44:48", "lastmod": "2023-10-18 17:47:13", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mennesson-B", "name": { "family": "Mennesson", "given": "Bertrand" }, "orcid": "0000-0003-4205-4800" }, { "id": "Akeson-R-L", "name": { "family": "Akeson", "given": "R." }, "orcid": "0000-0001-9674-1564" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Berriman-G-B", "name": { "family": "Berriman", "given": "B." }, "orcid": "0000-0001-8388-534X" }, { "id": "Calchi-Novati-S", "name": { "family": "Calchi Novati", "given": "S." }, "orcid": "0000-0002-7669-1069" }, { "id": "Gelino-C-R", "name": { "family": "Gelino", "given": "C." } }, { "id": "Gelino-D-M", "name": { "family": "Gelino", "given": "D." }, "orcid": "0000-0003-1274-2784" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "S." }, "orcid": "0000-0003-1250-8314" }, { "id": "Lowrance-P-J", "name": { "family": "Lowrance", "given": "P." }, "orcid": "0000-0001-8014-0270" }, { "id": "Meshkat-T", "name": { "family": "Meshkat", "given": "T." }, "orcid": "0000-0001-6126-2467" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Ramirez-S-V", "name": { "family": "Ramirez", "given": "S." } }, { "id": "Ygouf-M", "name": { "family": "Ygouf", "given": "M." }, "orcid": "0000-0001-7591-2731" } ] }, "title": "The Potential of Exozodiacal Disks Observations with the WFIRST Coronagraph Instrument", "ispublished": "unpub", "full_text_status": "public", "note": "Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nSubmitted - 1909.02161.pdf
", "abstract": "The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) will be the first high-performance stellar coronagraph using active wavefront control for deep starlight suppression in space, providing unprecedented levels of contrast, spatial resolution, and sensitivity for astronomical observations in the optical. One science case enabled by the CGI will be taking images and(R~50)spectra of faint interplanetary dust structures present in the habitable zone of nearby sunlike stars (~10 pc) and within the snow-line of more distant ones(~20pc), down to dust density levels commensurate with that of the solar system zodiacal cloud. Reaching contrast levels below~10-7 for the first time, CGI will cross an important threshold in debris disks physics, accessing disks with low enough optical depths that their structure is dominated by transport phenomena than collisions. Hence, CGI results will be crucial for determining how exozodiacal dust grains are produced and transported in low-density disks around mature stars. Additionally, CGI will be able to measure the brightness level and constrain the degree of asymmetry of exozodiacal clouds around individual nearby sunlike stars in the optical, at the ~10x solar zodiacal emission level. This information will be extremely valuable for optimizing the observational strategy of possible future exo-Earth direct imaging missions, especially those planning to operate at optical wavelengths, such as Habitable Exoplanet Observatory (HabEx) and the Large Ultraviolet/Optical/Infrared Surveyor (LUVOIR).", "date": "2019-10-02", "date_type": "published", "id_number": "CaltechAUTHORS:20191002-085537714", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191002-085537714", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.1909.02161", "primary_object": { "basename": "1909.02161.pdf", "url": "https://authors.library.caltech.edu/records/t5mct-16v77/files/1909.02161.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Mennesson, Bertrand; Akeson, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pvkrq-baa86", "eprint_id": 98979, "eprint_status": "archive", "datestamp": "2023-08-22 02:39:35", "lastmod": "2023-10-18 17:46:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Prakash-A", "name": { "family": "Prakash", "given": "Abhishek" }, "orcid": "0000-0003-4451-4444" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga Ram" }, "orcid": "0000-0001-7583-0621" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Lee-Bomee", "name": { "family": "Lee", "given": "Bomee" }, "orcid": "0000-0003-1954-5046" } ] }, "title": "A Flaring AGN in a ULIRG Candidate in Stripe 82", "ispublished": "pub", "full_text_status": "public", "keywords": "Active galactic nuclei; AGN host galaxies; Black holes; Light curves; Surveys", "note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2019 February 28; revised 2019 August 11; accepted 2019 August 12; published 2019 September 30. \n\nThis work was supported by Joint Survey Processing (JSP) at IPAC/Caltech, which is aimed at combined analysis of Euclid, LSST, and WFIRST. Funding for JSP has been provided by NASA grant 80NM0018F0803. \n\nThis publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. \n\nThis research has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by JPL/Caltech, under contract with NASA. Ned Wright's Cosmology Calculator was also used in preparing this paper. \n\nWe thank the Spitzer Science Center Director and observation support team for an award of Director's Discretionary Time for this project. \n\nFunding 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 acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. \n\nSDSS 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, the Korean Participation Group, 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\u00f3rio 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\nThe Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the PanSTARRS 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\nThe Catalina Real-time Transient 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. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182.\n\nPublished - Prakash_2019_ApJ_883_154.pdf
Accepted Version - 1908.04280.pdf
", "abstract": "We report the discovery of a mid-infrared variable AGN that is hosted by an ultraluminous infrared galaxy (ULIRG) in the Sloan Stripe 82 field. WISE J030654.88+010833.6 is a red, extended galaxy, which we estimate to be at a photometric redshift of 0.28 \u2264 z \u2264 0.31, based on its optical and near-infrared spectral energy distribution (SED). The factor of two variability over 8 yr seen in the Wide-field Infrared Survey Explorer (WISE) 3.4 and 4.6 \u03bcm wavelength channels is not clearly correlated with optical variability in archival data. Based on our estimation of the physical parameters of the host galaxy, J030654.88+010833.6 is possibly a composite AGN/starburst ULIRG in a phase where high star formation ~70 M_\u2299 yr^(\u22121) is occurring. Our estimate of the black hole mass to stellar mass ratio also appears to be consistent with that of broad line AGN in the local universe. The long-term variability of J030654.88+010833.6 as seen in the WISE W1 and W2 light curves is likely due to variations in the accretion rate, with the energy being reprocessed by dust in the vicinity of the AGN.", "date": "2019-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "883", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 154", "id_number": "CaltechAUTHORS:20191001-101354875", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191001-101354875", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "80NM0018F0803" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" }, { "agency": "University of Utah" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" }, { "agency": "Eotvos Lorand University (ELTE)" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/ab3b0b", "primary_object": { "basename": "1908.04280.pdf", "url": "https://authors.library.caltech.edu/records/pvkrq-baa86/files/1908.04280.pdf" }, "related_objects": [ { "basename": "Prakash_2019_ApJ_883_154.pdf", "url": "https://authors.library.caltech.edu/records/pvkrq-baa86/files/Prakash_2019_ApJ_883_154.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Prakash, Abhishek; Chary, Ranga Ram; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bswdb-bnn85", "eprint_id": 98840, "eprint_status": "archive", "datestamp": "2023-08-19 17:30:35", "lastmod": "2024-01-14 21:57:49", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "name": { "family": "Dickinson", "given": "Mark" } }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne" } }, { "name": { "family": "Robberto", "given": "Massimo" } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "name": { "family": "Ballardini", "given": "Mario" } }, { "name": { "family": "Barkhouser", "given": "Robert" } }, { "name": { "family": "Bartlett", "given": "James" } }, { "name": { "family": "Behroozi", "given": "Peter" } }, { "name": { "family": "Benjamin", "given": "Robert A." } }, { "name": { "family": "Brinchmann", "given": "Jarle" } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga-Ram" }, "orcid": "0000-0001-7583-0621" }, { "name": { "family": "Chuang", "given": "Chia-Hsun" } }, { "name": { "family": "Cimatti", "given": "Andrea" } }, { "name": { "family": "Conroy", "given": "Charlie" } }, { "name": { "family": "Content", "given": "Robert" } }, { "name": { "family": "Daddi", "given": "Emanuele" } }, { "name": { "family": "Donahue", "given": "Megan" } }, { "name": { "family": "Dore", "given": "Olivier" } }, { "name": { "family": "Eisenhardt", "given": "Peter" } }, { "name": { "family": "Ferguson", "given": "Henry C." } }, { "id": "Faisst-A-L", "name": { "family": "Faisst", "given": "Andreas" }, "orcid": "0000-0002-9382-9832" }, { "name": { "family": "Fraser", "given": "Wesley C." } }, { "name": { "family": "Glazebrook", "given": "Karl" } }, { "name": { "family": "Gorjian", "given": "Varoujan" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "name": { "family": "Hirata", "given": "Christopher M." } }, { "name": { "family": "Hudson", "given": "Michael" } }, { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "name": { "family": "Malhotra", "given": "Sangeeta" } }, { "name": { "family": "Mei", "given": "Simona" } }, { "name": { "family": "Moscardini", "given": "Lauro" } }, { "name": { "family": "Newman", "given": "Jeffrey A." } }, { "name": { "family": "Ninkov", "given": "Zoran" } }, { "name": { "family": "Orsi", "given": "Alvaro" } }, { "name": { "family": "Ressler", "given": "Michael" } }, { "name": { "family": "Rhoads", "given": "James" } }, { "name": { "family": "Rhodes", "given": "Jason" } }, { "name": { "family": "Ryan", "given": "Russell" } }, { "name": { "family": "Samushia", "given": "Lado" } }, { "name": { "family": "Scarlata", "given": "Claudia" } }, { "name": { "family": "Scolnic", "given": "Daniel" } }, { "name": { "family": "Seiffert", "given": "Michael" } }, { "name": { "family": "Shapley", "given": "Alice" } }, { "name": { "family": "Smee", "given": "Stephen" } }, { "name": { "family": "Valentino", "given": "Francesco" } }, { "name": { "family": "Vorobiev", "given": "Dmitry" } }, { "name": { "family": "Wechsler", "given": "Risa H." } } ] }, "title": "ATLAS Probe: Breakthrough Science of Galaxy Evolution, Cosmology, Milky Way, and the Solar System", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1909.00070.pdf
", "abstract": "ATLAS (Astrophysics Telescope for Large Area Spectroscopy) is a concept for a NASA probe-class space mission. It is the spectroscopic follow-up mission to WFIRST, boosting its scientific return by obtaining deep NIR & MIR slit spectroscopy for most of the galaxies imaged by the WFIRST High Latitude Survey at z>0.5. ATLAS will measure accurate and precise redshifts for ~200M galaxies out to z=7 and beyond, and deliver spectra that enable a wide range of diagnostic studies of the physical properties of galaxies over most of cosmic history. ATLAS and WFIRST together will produce a definitive 3D map of the Universe over 2000 sq deg. ATLAS Science Goals are: (1) Discover how galaxies have evolved in the cosmic web of dark matter from cosmic dawn through the peak era of galaxy assembly. (2) Discover the nature of cosmic acceleration. (3) Probe the Milky Way's dust-enshrouded regions, reaching the far side of our Galaxy. (4) Discover the bulk compositional building blocks of planetesimals formed in the outer Solar System. These flow down to the ATLAS Scientific Objectives: (1A) Trace the relation between galaxies and dark matter with less than 10% shot noise on relevant scales at 1", "date": "2019-09-25", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20190925-085020406", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190925-085020406", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.1909.00070", "primary_object": { "basename": "1909.00070.pdf", "url": "https://authors.library.caltech.edu/records/bswdb-bnn85/files/1909.00070.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Wang, Yun; Dickinson, Mark; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/eggz6-sja14", "eprint_id": 98632, "eprint_status": "archive", "datestamp": "2023-08-19 17:48:39", "lastmod": "2024-01-14 21:57:08", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Leisawitz-D-T", "name": { "family": "Leisawitz", "given": "D." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Carey-S-J", "name": { "family": "Carey", "given": "S." }, "orcid": "0000-0002-0221-6871" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "The Origins Space Telescope", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2019 Society of Photo-Optical Instrumentation Engineers.\n\nPublished - 111150Q.pdf
", "abstract": "The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the universe today? How do habitable planets form? How common are life-bearing worlds? To answer these alluring questions, Origins will operate at mid- and far-infrared wavelengths and offer powerful spectroscopic instruments and sensitivity three orders of magnitude better than that of Herschel, the largest telescope flown in space to date. After a 3 \u00bd year study, the Origins Science and Technology Definition Team will recommend to the Decadal Survey a concept for Origins with a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. A mid-infrared instrument (MISC-T) will measure the spectra of transiting exoplanets in the 2.8 \u2013 20 \u03bcm wavelength range and offer unprecedented sensitivity, enabling definitive biosignature detections. The Far-IR Imager Polarimeter (FIP) will be able to survey thousands of square degrees with broadband imaging at 50 and 250 \u03bcm. The Origins Survey Spectrometer (OSS) will cover wavelengths from 25 \u2013 588 \u03bcm, make wide-area and deep spectroscopic surveys with spectral resolving power R ~ 300, and pointed observations at R ~ 40,000 and 300,000 with selectable instrument modes. Origins was designed to minimize complexity. The telescope has a Spitzer-like architecture and requires very few deployments after launch. The cryo-thermal system design leverages JWST technology and experience. A combination of current-state-of-the-art cryocoolers and next-generation detector technology will enable Origins' natural backgroundlimited sensitivity.", "date": "2019-09-09", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 111150Q", "id_number": "CaltechAUTHORS:20190913-085723191", "isbn": "9781510629233", "book_title": "UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts IX", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190913-085723191", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "contributors": { "items": [ { "id": "Barto-A-A", "name": { "family": "Barto", "given": "Allison A." } }, { "id": "Breckinridge-J-B", "name": { "family": "Breckinridge", "given": "James B." } }, { "id": "Stahl-H-P", "name": { "family": "Stahl", "given": "H. Philip" } } ] }, "doi": "10.1117/12.2530514", "primary_object": { "basename": "111150Q.pdf", "url": "https://authors.library.caltech.edu/records/eggz6-sja14/files/111150Q.pdf" }, "resource_type": "book_section", "pub_year": "2019", "author_list": "Leisawitz, D.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x4q6x-9kr65", "eprint_id": 98481, "eprint_status": "archive", "datestamp": "2023-08-19 17:44:44", "lastmod": "2023-10-18 17:24:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kelley-Michael-S-P", "name": { "family": "Kelley", "given": "Michael S. P." }, "orcid": "0000-0002-6702-7676" }, { "id": "Bodewits-Dennis", "name": { "family": "Bodewits", "given": "Dennis" }, "orcid": "0000-0002-2668-7248" }, { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Ahumada-Tom\u00e1s", "name": { "family": "Ahumada", "given": "Tom\u00e1s" }, "orcid": "0000-0002-2184-6430" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Cromer-John-L", "name": { "family": "Cromer", "given": "John" } }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" } ] }, "title": "Outbursts at Comets 46P/Wirtanen, 64P/Swift-Gehrels, and 78P/Gehrels 2 in 2018", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 August 28. Accepted 2019 August 30. Published 2019 September 5. \n\nBased on observations obtained with the Samuel Oschin 48-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW.\n\nPublished - Outbursts_at_Comets_46P_Wirtanen,_64P_Swift-Gehrels,_and_78P_Gehrels_2_in_2018_-_IOPscience.html
", "abstract": "Cometary outbursts are brief increases in the mass-loss rates of comets (Hughes 1990). Most observed outbursts have \u0394m \u2273 1\u2009mag, but smaller outbursts do occur, such as those observed by the Deep Impact and Rosetta spacecraft at comets 9P/Tempel 1 and 67P/Churyumov-Gerasimenko (A'Hearn et al. 2005; Vincent et al. 2016). The outbursts are smaller than the Deep Impact excavation, suggesting strengths near \u22120.2 to \u22121\u2009mag (A'Hearn et al. 2005; Meech et al. 2005; Feldman et al. 2007). \n\nWide-field, time-domain surveys are well-suited to the discovery of cometary outbursts (Graham et al. 2019). We describe initial results from our outburst search using the Zwicky Transient Facility archive (ZTF; Bellm et al. 2019), based on observations of three comets: 46P/Wirtanen, 64P/Swift-Gehrels, and 78P/Gehrels 2. The data are calibrated to the Pan-STARRS 1 photometric system (Masci et al. 2019), and color corrected assuming a reddened solar spectrum (g\u2212r = 0.52\u2009mag, r\u2212i = 0.15\u2009mag). We measured photometry in 7'' radius apertures, then fit and removed a linear trend from each lightcurve: 46P, \u22120.053\u2009mag day^(\u22121) (rms 0.02\u2009mag); 64P, \u22120.053\u2009mag day^(\u22121) (rms 0.04\u2009mag); 78P, \u22120.039\u2009mag day^(\u22121) (rms 0.04\u2009mag).", "date": "2019-09-05", "date_type": "published", "publication": "Research Notes of the AAS", "volume": "3", "number": "9", "publisher": "American Astronomical Society", "pagerange": "Art No. 126", "id_number": "CaltechAUTHORS:20190906-100700610", "issn": "2515-5172", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190906-100700610", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" } ] }, "local_group": { "items": [ { "id": "Zwicky-Transient-Facility" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/2515-5172/ab3fb4", "primary_object": { "basename": "Outbursts_at_Comets_46P_Wirtanen,_64P_Swift-Gehrels,_and_78P_Gehrels_2_in_2018_-_IOPscience.html", "url": "https://authors.library.caltech.edu/records/x4q6x-9kr65/files/Outbursts_at_Comets_46P_Wirtanen,_64P_Swift-Gehrels,_and_78P_Gehrels_2_in_2018_-_IOPscience.html" }, "resource_type": "article", "pub_year": "2019", "author_list": "Kelley, Michael S. P.; Bodewits, Dennis; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qs3jc-2v076", "eprint_id": 96510, "eprint_status": "archive", "datestamp": "2023-08-19 17:11:46", "lastmod": "2023-10-20 21:15:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob E." }, "orcid": "0000-0001-5754-4007" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Bond-H-E", "name": { "family": "Bond", "given": "Howard E." }, "orcid": "0000-0003-1377-7145" }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Bally-J", "name": { "family": "Bally", "given": "John" }, "orcid": "0000-0001-8135-6612" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "Nadja" }, "orcid": "0000-0003-0901-1606" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Yao-Yuhan", "name": { "family": "Yao", "given": "Yuhan" }, "orcid": "0000-0001-6747-8509" }, { "id": "Fruchter-A", "name": { "family": "Fruchter", "given": "A." } }, { "id": "Rubin-D", "name": { "family": "Rubin", "given": "David" } }, { "id": "Barbarino-C", "name": { "family": "Barbarino", "given": "Cristina" }, "orcid": "0000-0002-3821-6144" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Hicks-E-K-S", "name": { "family": "Hicks", "given": "Erin K. S." } }, { "id": "Malkan-M-A", "name": { "family": "Malkan", "given": "Matthew" }, "orcid": "0000-0001-6919-1237" }, { "id": "Andreoni-I", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Buchheim-R", "name": { "family": "Buchheim", "given": "Robert" } }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" } }, { "id": "Feeney-M", "name": { "family": "Feeney", "given": "Michael" } }, { "id": "Frederick-S", "name": { "family": "Frederick", "given": "Sara" }, "orcid": "0000-0001-9676-730X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Gehrz-R-D", "name": { "family": "Gehrz", "given": "R. D." }, "orcid": "0000-0003-1319-4089" }, { "id": "Giomi-M", "name": { "family": "Giomi", "given": "Matteo" } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Green-W", "name": { "family": "Green", "given": "Wayne" } }, { "id": "Hale-D", "name": { "family": "Hale", "given": "David" } }, { "id": "Hankins-M-J", "name": { "family": "Hankins", "given": "Matthew J." }, "orcid": "0000-0001-9315-8437" }, { "id": "Hanson-M", "name": { "family": "Hanson", "given": "Mark" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "id": "Hung-T", "name": { "family": "Hung", "given": "T." } }, { "id": "Juri\u0107-M", "name": { "family": "Juri\u0107", "given": "Mario" }, "orcid": "0000-0003-1996-9252" }, { "id": "Kendurkar-M-R", "name": { "family": "Kendurkar", "given": "Malhar R." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Lau-Ryan-M", "name": { "family": "Lau", "given": "Ryan M." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Quin-K", "name": { "family": "Quin", "given": "Kevin" } }, { "id": "Riddle-R-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Sims-F", "name": { "family": "Sims", "given": "Forrest" } }, { "id": "Smith-N", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger M." } }, { "id": "Soumagnac-M-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Tachibana-Yutaro", "name": { "family": "Tachibana", "given": "Yutaro" }, "orcid": "0000-0001-6584-6945" }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Watson-S", "name": { "family": "Watson", "given": "Stanley" } }, { "id": "Williams-R-E", "name": { "family": "Williams", "given": "Robert E." } } ] }, "title": "Discovery of an Intermediate-luminosity Red Transient in M51 and Its Likely Dust-obscured, Infrared-variable Progenitor", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter \u2013 galaxies: individual (M51) \u2013 stars: evolution \u2013 stars: variables: general \u2013 stars:\nwinds, outflows \u2013 supernovae: individual (M51 OT2019-1)", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 April 12; revised 2019 June 3; accepted 2019 June 5; published 2019 July 26. \n\nWe thank J. Prieto and E. Ofek for valuable discussions in revising this work. We also thank the anonymous referee for their helpful comments, which improved the manuscript. \n\nThis material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144469. H.E.B. acknowledges support from program numbers GO-14258 and AR-15005, provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work is part of the research programme VENI, with project number 016.192.277, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO). A.G.-Y. is supported by the EU via ERC grant No. 725161, the ISF, the BSF Transformative program and by a Kimmel award. R.D.G. was supported by NASA and the United States Air Force. Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. This work was supported by the GROWTH project funded by the National Science Foundation under grant No. 1545949. SED Machine is based upon work supported by the National Science Foundation under grant No. 1106171. The work presented here is based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. We thank the Apache Point Observatory Observing Specialists for their assistance during the observations. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. Based on observations obtained at the Gemini Observatory acquired through the Gemini Observatory Archive and processed using the Gemini IRAF package, 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), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. 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. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Some of these observations are associated with program #15675. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. 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\nFacilities: PO:1.2 m (ZTF) - , PO:1.5 m (SEDM) - , Hale (DBSP - , WIRC - , TripleSpec) - , NOT (ALFOSC) - , Gemini:Gillett (GMOS) - , Keck:I (LRIS) - , Keck:II (NIRC2) - , ARC (NICFPS - , ARCTIC) - , Spitzer (IRAC) - , HST (ACS - , WFC3) - , WISE. - \n\nSoftware: AstroDrizzle (Hack et al. 2012, http://drizzlepac.stsci.edu), DOLPHOT (Dolphin 2000, 2016), IRAF (Tody 1986, 1993), Gemini IRAF package (http://www.gemini.edu/sciops/data-and-results/processing-software), PyRAF (http://www.stsci.edu/institute/software_hardware/pyraf), pyraf-dbsp (Bellm & Sesar 2016, https://github.com/ebellm/pyraf-dbsp), LPipe (Perley 2019, http://www.astro.caltech.edu/~dperley/programs/lpipe.html).\n\nPublished - Jencson_2019_ApJL_880_L20.pdf
Submitted - 1904.07857.pdf
", "abstract": "We present the discovery of an optical transient (OT) in Messier 51, designated M51 OT2019-1 (also ZTF 19aadyppr, AT 2019abn, ATLAS19bzl), by the Zwicky Transient Facility (ZTF). The OT rose over 15 days to an observed luminosity of M_r = \u221213 (\u03bdL \u03bd = 9 \u00d7 10^6 L_\u2299), in the luminosity gap between novae and typical supernovae (SNe). Spectra during the outburst show a red continuum, Balmer emission with a velocity width of \u2248400 km s^(\u22121), Ca II and [Ca II] emission, and absorption features characteristic of an F-type supergiant. The spectra and multiband light curves are similar to the so-called \"SN impostors\" and intermediate-luminosity red transients (ILRTs). We directly identify the likely progenitor in archival Spitzer Space Telescope imaging with a 4.5 \u03bcm luminosity of M_([4.5]) \u2248 \u221212.2 mag and a [3.6]\u2013[4.5] color redder than 0.74 mag, similar to those of the prototype ILRTs SN 2008S and NGC 300 OT2008-1. Intensive monitoring of M51 with Spitzer further reveals evidence for variability of the progenitor candidate at [4.5] in the years before the OT. The progenitor is not detected in pre-outburst Hubble Space Telescope optical and near-IR images. The optical colors during outburst combined with spectroscopic temperature constraints imply a higher reddening of E(B \u2212 V) \u2248 0.7 mag and higher intrinsic luminosity of M_r \u2248 \u221214.9 mag (\u03bdL_\u03bd = 5.3 \u00d7 10^7 L\u2299) near peak than seen in previous ILRT candidates. Moreover, the extinction estimate is higher on the rise than on the plateau, suggestive of an extended phase of circumstellar dust destruction. These results, enabled by the early discovery of M51 OT2019-1 and extensive pre-outburst archival coverage, offer new clues about the debated origins of ILRTs and may challenge the hypothesis that they arise from the electron-capture induced collapse of extreme asymptotic giant branch stars.", "date": "2019-08-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "880", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L20", "id_number": "CaltechAUTHORS:20190619-074207862", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-074207862", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NASA", "grant_number": "GO-14258" }, { "agency": "NASA", "grant_number": "AR-15005" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "016.192.277" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Kimmel Award" }, { "agency": "U.S. Air Force" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "Gemini Partnership" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/2041-8213/ab2c05", "primary_object": { "basename": "Jencson_2019_ApJL_880_L20.pdf", "url": "https://authors.library.caltech.edu/records/qs3jc-2v076/files/Jencson_2019_ApJL_880_L20.pdf" }, "related_objects": [ { "basename": "1904.07857.pdf", "url": "https://authors.library.caltech.edu/records/qs3jc-2v076/files/1904.07857.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Jencson, Jacob E.; Adams, Scott M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jxq4g-9zq68", "eprint_id": 95495, "eprint_status": "archive", "datestamp": "2023-08-19 16:50:39", "lastmod": "2023-10-20 20:17:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burdge-K-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Coughlin-M-W", "name": { "family": "Coughlin", "given": "Michael W." }, "orcid": "0000-0002-8262-2924" }, { "id": "Fuller-J", "name": { "family": "Fuller", "given": "Jim" }, "orcid": "0000-0002-4544-0750" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kaplan-D-L", "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "van-Roestel-J", "name": { "family": "van Roestel", "given": "Jan" }, "orcid": "0000-0002-2626-2872" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." } }, { "id": "Duev-D-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Feeney-M-E", "name": { "family": "Feeney", "given": "Michael" } }, { "id": "Giomi-M", "name": { "family": "Giomi", "given": "Matteo" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kaye-S", "name": { "family": "Kaye", "given": "Stephen" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Riddle-R-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soumagnac-M-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger M." } }, { "id": "Szkody-P", "name": { "family": "Szkody", "given": "Paula" } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" } ] }, "title": "General relativistic orbital decay in a seven-minute-orbital-period eclipsing binary system", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2019 Springer Nature Publishing AG\n\nReceived 21 February 2019. Accepted 23 May 2019. Published 24 July 2019. \n\nK.B.B. thanks the National Aeronautics and Space Administration and the Heising Simons Foundation for supporting his research. This work was based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant number AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington (UW), Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and the Lawrence Berkeley National Laboratories. Operations are conducted by Caltech Optical Observatories, IPAC, and the University of Washington. The KPED team thanks the National Science Foundation and the National Optical Astronomical Observatory for making the Kitt Peak 2.1-m telescope available. The KPED team thanks the National Science Foundation, the National Optical Astronomical Observatory and the Murty family for support in the building and operation of KPED. In addition, they thank the CHIMERA project for use of the Electron Multiplying CCD (EMCCD). 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. We wish to recognize and acknowledge the very important 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 benefited from interactions at the ZTF Theory Network Meeting that were funded by the Gordon and Betty Moore Foundation through grant GBMF5076 and support from the National Science Foundation through PHY-1748958. We thank J. Hoffman, the creator of cuvarbase. We thank T. Marsh, S. Phinney and V. Korol for discussions. We thank G. Hallinan and C. Fremling for helping to observe the object. \n\nAuthor Contributions: K.B.B. discovered the object, conducted the lightcurve analysis and eclipse time analysis, and was the primary author of the manuscript. K.B.B. and M.W.C. conducted the spectroscopic analysis. K.B.B., M.W.C. and T.A.P. conducted the combined mass\u2013radius analysis. K.B.B. and M.W.C. reduced the optical data. K.B.B., M.W.C. and D.L.K. reduced and analysed the X-ray observations. J.F. conducted the theoretical analysis, including that on tides, and developed the MESA evolutionary models. K.B.B., M.W.C., T.K., S.R.K., J.v.R. and T.A.P. all contributed to collecting data on the object. K.B.B., M.W.C., J.F., T.K., E.C.B., L.B., M.J.G., D.L.K., J.v.R., S.R.K. and T.A.P. contributed to the physical interpretation of the object. T.K., E.C.B., R.G.D., M.F., M.G., S.K., R.R.L., A.A.M., F.J.M., R.R., D.L.S., M.T.S., R.M.S., P.S. and R.W. contributed to the implementation of ZTF; M.J.G. is the project scientist, T.A.P. and G.H. are co-PIs, and S.R.K. is the PI of ZTF. R.G.D., D.A.D., M.F. and R.R. contributed to the implementation of KPED; M.W.C. is project scientist, and S.R.K. is PI of KPED. T.A.P. is K.B.B.'s PhD advisor. \n\nData availability: Upon request, K.B.B. will provide reduced photometric and spectroscopic data, and available ZTF data for the object. We have included the eclipse time data used to construct the orbital decay diagram in Fig. 2a, and Extended Data Figs. 2 and 3. The X-ray observations are already in the public domain, and their observation IDs have been supplied in the text. The proprietary period for the spectroscopic data will expire at the start of 2020, at which point this data will also be public and readily accessible. \n\nCode availability: Upon request, K.B.B. will provide the code (primarily in Python) used to analyse the observations and data such as the posterior distributions used to produce the figures in the text (MATLAB was used to generate most of the figures). \n\nThe authors declare no competing interests.\n\nAccepted Version - 1907.11291.pdf
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Supplemental Material - 41586_2019_1403_Fig6_ESM.jpg
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Supplemental Material - 41586_2019_1403_Fig8_ESM.jpg
Supplemental Material - 41586_2019_1403_Fig9_ESM.jpg
Supplemental Material - 41586_2019_1403_MOESM1_ESM.csv
Supplemental Material - 41586_2019_1403_Tab1_ESM.jpg
", "abstract": "General relativity predicts that short-orbital-period binaries emit considerable amounts of gravitational radiation. The upcoming Laser Interferometer Space Antenna (LISA) is expected to detect tens of thousands of such systems but few have been identified4, of which only one5 is eclipsing\u2014the double-white-dwarf binary SDSS J065133.338+284423.37, which has an orbital period of 12.75 minutes. Here we report the discovery of an eclipsing double-white-dwarf binary system, ZTF J153932.16+502738.8, with an orbital period of 6.91 minutes. This system has an orbit so compact that the entire binary could fit within the diameter of the planet Saturn. The system exhibits a deep eclipse, and a double-lined spectroscopic nature. We see rapid orbital decay, consistent with that expected from general relativity. ZTF J153932.16+502738.8 is a strong source of gravitational radiation close to the peak of LISA's sensitivity, and we expect it to be detected within the first week of LISA observations, once LISA launches in approximately 2034.", "date": "2019-07-24", "date_type": "published", "publication": "Nature", "volume": "571", "number": "7767", "publisher": "Nature Publishing Group", "pagerange": "528-531", "id_number": "CaltechAUTHORS:20190514-142944629", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190514-142944629", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Heising-Simons Foundation" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF Partner Institutions" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NSF", "grant_number": "PHY-1748958" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/s41586-019-1403-0", "primary_object": { "basename": "41586_2019_1403_Fig6_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Fig6_ESM.jpg" }, "related_objects": [ { "basename": "41586_2019_1403_Fig7_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Fig7_ESM.jpg" }, { "basename": "41586_2019_1403_Fig8_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Fig8_ESM.jpg" }, { "basename": "41586_2019_1403_MOESM1_ESM.csv", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_MOESM1_ESM.csv" }, { "basename": "1907.11291.pdf", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/1907.11291.pdf" }, { "basename": "41586_2019_1403_Fig5_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Fig5_ESM.jpg" }, { "basename": "41586_2019_1403_Fig9_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Fig9_ESM.jpg" }, { "basename": "41586_2019_1403_Tab1_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Tab1_ESM.jpg" }, { "basename": "41586_2019_1403_Fig10_ESM.jpg", "url": "https://authors.library.caltech.edu/records/jxq4g-9zq68/files/41586_2019_1403_Fig10_ESM.jpg" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Burdge, Kevin B.; Coughlin, Michael W.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gyqzp-yyg45", "eprint_id": 96733, "eprint_status": "archive", "datestamp": "2023-08-19 16:30:21", "lastmod": "2023-10-20 21:28:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick M." }, "orcid": "0000-0002-3471-981X" }, { "id": "Lanz-L", "name": { "family": "Lanz", "given": "Lauranne" }, "orcid": "0000-0002-3249-8224" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "Philip N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Mazzarella-J-M", "name": { "family": "Mazzarella", "given": "Joseph" }, "orcid": "0000-0002-8204-8619" } ] }, "title": "A Catalog of the Most Optically Luminous Galaxies at z < 0.3: Super Spirals, Super Lenticulars, Super Post-Mergers, and Giant Ellipticals", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD \u2013 galaxies: spiral", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 June 28; revised 2019 April 4; accepted 2019 April 8; published 2019 July 15. \n\nWe thank Katey Alatalo for insightful discussions regarding the properties of post-merger and post-starburst galaxies. This work was made possible by the NASA/IPAC Extragalactic Database and the NASA/IPAC Infrared Science Archive, which are both operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank Ben Chan, Marion Schmitz, and the rest of the NED team for useful discussions and their support of this work. This publication makes use of data from the Galaxy Evolution Explorer and the Hubble Space Telescope, retrieved from the Mikulski Archive for Space Telescopes (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 provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. 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 acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration. 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 publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.\n\nPublished - Ogle_2019_ApJS_243_14.pdf
Submitted - 1904.02806.pdf
", "abstract": "We present a catalog of the 1525 most optically luminous galaxies from the Sloan Digital Sky Survey with r-band luminosity L_r > 8L* and redshift z < 0.3, including 84 super spirals, 15 super lenticulars, 14 super post-merger galaxies, and 1400 giant ellipticals. With mass in stars of 10^(11.3)\u201310^(12) M\u2299, super spirals and lenticulars are the most massive disk galaxies currently known. The specific star formation rates of super spirals place them on or below the star-forming main sequence. They must have formed stars at a high rate throughout their history in order to grow their massive, gigantic stellar disks and maintain their blue u \u2212 r integrated colors. Their disks are red on the inside and blue on the outside, consistent with inside-out growth. They tend to have small bulge-to-total (B/T) r-band luminosity ratios, characteristic of disk building via minor mergers and cold accretion. A large percentage of super disk galaxies (41%) have double nuclei, double disks, or other signatures of ongoing mergers. Most (72%) are found in moderate- to low-density environments, while the rest are found at the outskirts of clusters. It is likely that super spirals survive in these environments because they continue to accrete cold gas and experience only minor mergers at late times, by virtue of their enormous masses and angular momenta. We suggest that super post-mergers are the product of super spiral major mergers and may be the precursors of some giant elliptical galaxies found in low-density environments. We present two new gravitational lens candidates in an appendix.", "date": "2019-07", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "243", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 14", "id_number": "CaltechAUTHORS:20190626-102331374", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-102331374", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA", "grant_number": "NNX09AF08G" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4365/ab21c3", "primary_object": { "basename": "1904.02806.pdf", "url": "https://authors.library.caltech.edu/records/gyqzp-yyg45/files/1904.02806.pdf" }, "related_objects": [ { "basename": "Ogle_2019_ApJS_243_14.pdf", "url": "https://authors.library.caltech.edu/records/gyqzp-yyg45/files/Ogle_2019_ApJS_243_14.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Ogle, Patrick M.; Lanz, Lauranne; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qr7vb-95k31", "eprint_id": 92892, "eprint_status": "archive", "datestamp": "2023-08-19 16:26:39", "lastmod": "2023-10-20 16:36:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "S. M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Barbarino-Cristina", "name": { "family": "Barbarino", "given": "Cristina" }, "orcid": "0000-0002-3821-6144" }, { "id": "Blagorodnova-Nadejda", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Bodewits-Dennis", "name": { "family": "Bodewits", "given": "Dennis" }, "orcid": "0000-0002-2668-7248" }, { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "Bryce" }, "orcid": "0000-0002-4950-6323" }, { "id": "Brady-Patrick-R", "name": { "family": "Brady", "given": "Patrick R." }, "orcid": "0000-0002-4611-9387" }, { "id": "Cenko-S-Bradley", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "M. 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T." }, "orcid": "0000-0001-7120-7234" }, { "id": "Walters-Richard-S", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Ward-Charlotte-A", "name": { "family": "Ward", "given": "Charlotte A." }, "orcid": "0000-0002-4557-6682" }, { "id": "Zhang-Chaoran", "name": { "family": "Zhang", "given": "Chaoran" }, "orcid": "0000-0001-8288-5823" }, { "id": "Zolkower-Jeffry-N", "name": { "family": "Zolkower", "given": "Jeffry" } } ] }, "title": "The Zwicky Transient Facility: Science Objectives", "ispublished": "pub", "full_text_status": "public", "keywords": "(stars:) supernovae: general \u2013 surveys \u2013 (galaxies:) quasars: general", "note": "\u00a9 2019 Astronomical Society of the Pacific. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2018 September 6; accepted 2019 January 21; published 2019 May 22. \n\nBased on observations obtained with the Samuel Oschin 48-inch Telescope and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project, a scientific collaboration among the California Institute of Technology, the Oskar Klein Centre, the Weizmann Institute of Science, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron, the University of Wisconsin-Milwaukee, and the TANGO Program of the University System of Taiwan. Further support is provided by the U.S. National Science Foundation under grant No. AST-1440341. \n\nJ. Sollerman acknowledges support from the Knut and Alice Wallenberg Foundation. \n\nE. Ofek is grateful for support by a grant from the Israeli Ministry of Science, ISF, Minerva, BSF, BSF transformative program, and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant No. 1829/12). \n\nA. Gal-Yam is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program and by a Kimmel award. \n\nS. Gezari is supported in part by NSF CAREER grant 1454816 and NSF AAG grant 1616566. \n\nC.-K. Chang, W.-H. Ip, C.-D. Lee, Z.-Y. Lin, C.-C. Ngeow, and P.-C. Yu thank the funding from Ministry of Science and Technology (Taiwan) under grant 104-2923-M-008-004-MY5, 104-2112-M-008-014-MY3, 105-2112-M-008-002-MY3, 106-2811-M-008-081, and 106-2112-M-008-007. \n\nM. Bulla and A. Goobar acknowledge support from the Swedish Research Council (Vetenskapsr\u00e5det) and the Swedish National Space Board. \n\nE. Bellm, B. Bolin, A. Connolly, V. Z. Golkhou, D. Huppenkothen, Z. Ivezi\u0107 L. Jones, M. Juric, and M. Patterson acknowledge support from the University of Washington College of Arts and Sciences, Department of Astronomy, and the DIRAC Institute. University of Washington's DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. M. Juric and A. Connolly acknowledge the support of the Washington Research Foundation Data Science Term Chair fund, and the UW Provost's Initiative in Data-Intensive Discovery. \n\nE. Bellm, A. Connolly, Z. Ivezi\u0107 L. Jones, M. Juric, and M. Patterson acknowledge support from the Large Synoptic Survey Telescope, which is supported in part by the National Science Foundation through Cooperative Agreement 1258333 managed by the Association of Universities for Research in Astronomy (AURA), and the Department of Energy under contract No. DE-AC02-76SF00515 with the SLAC National Accelerator Laboratory. Additional LSST funding comes from private donations, grants to universities, and in-kind support from LSSTC Institutional Members. \n\nB.T. Bolin acknowledges funding for the Asteroid Institute program provided by B612 Foundation, W.K. Bowes Jr. Foundation, P. Rawls Family Fund, and two anonymous donors in addition to general support from the B612 Founding Circle. \n\nM.T. Soumagnac acknowledges support by a grant from IMOS/ISA, the Ilan Ramon fellowship from the Israel Ministry of Science and Technology and the Benoziyo center for Astrophysics at the Weizmann Institute of Science. \n\nA. A. Miller is funded by the Large Synoptic Survey Telescope Corporation in support of the Data Science Fellowship Program. \n\nJ. Bauer, T. Farnham, and M. Kelley gratefully acknowledge the NASA/University of Maryland/MPC Augmentation through the NASA Planetary Data System Cooperative Agreement NNX16AB16A. \n\nM. M. Kasliwal and Q.-Z. Ye acknowledge support by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation PIRE (Partnership in International Research and Education) program under Grant No 1545949. \n\nA. A. Mahabal acknowledges support from the following grants: NSF AST-1749235, NSF-1640818, and NASA 16-ADAP16-0232. \n\nM. W. Coughlin is supported by the David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology. \n\nS. Ghosh acknowledges the NSF award PHY-1607585. \n\nM. Rigault acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 759194\u2014USNAC). \n\nFacilities: PO:1.2 m - , PO:1.5m -.\n\nPublished - Graham_2019_PASP_131_078001.pdf
Submitted - 1902.01945.pdf
", "abstract": "The Zwicky Transient Facility (ZTF), a public\u2013private enterprise, is a new time-domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg^2 field of view and an 8 second readout time. It is well positioned in the development of time-domain astronomy, offering operations at 10% of the scale and style of the Large Synoptic Survey Telescope (LSST) with a single 1-m class survey telescope. The public surveys will cover the observable northern sky every three nights in g and r filters and the visible Galactic plane every night in g and r. Alerts generated by these surveys are sent in real time to brokers. A consortium of universities that provided funding (\"partnership\") are undertaking several boutique surveys. The combination of these surveys producing one million alerts per night allows for exploration of transient and variable astrophysical phenomena brighter than r ~ 20.5 on timescales of minutes to years. We describe the primary science objectives driving ZTF, including the physics of supernovae and relativistic explosions, multi-messenger astrophysics, supernova cosmology, active galactic nuclei, and tidal disruption events, stellar variability, and solar system objects.", "date": "2019-07", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "131", "number": "1001", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 078001", "id_number": "CaltechAUTHORS:20190213-135514906", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190213-135514906", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "MINERVA (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Kimmel Award" }, { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "NSF", "grant_number": "AST-1616566" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2923-M-008-004-MY5" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2112-M-008-014-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "105-2112-M-008-002-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "106-2811-M-008-081" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "106-2112-M-008-007" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "University of Washington" }, { "agency": "DIRAC Institute" }, { "agency": "Charles and Lisa Simonyi Fund for Arts and Sciences" }, { "agency": "Washington Research Foundation" }, { "agency": "Large Synoptic Survey Telescope" }, { "agency": "NSF", "grant_number": "AST-1258333" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "B612 Foundation" }, { "agency": "W. K. Bowes Jr. Foundation" }, { "agency": "P. Rawls Family Fund" }, { "agency": "IMOS/ISA" }, { "agency": "Weizmann Institute of Science" }, { "agency": "NASA", "grant_number": "NNX16AB16A" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "AST-1749235" }, { "agency": "NSF", "grant_number": "OAC-1640818" }, { "agency": "NASA", "grant_number": "16-ADAP16-0232" }, { "agency": "David and Ellen Lee Postdoctoral Scholarship" }, { "agency": "NSF", "grant_number": "PHY-1607585" }, { "agency": "European Research Council (ERC)", "grant_number": "759194" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/ab006c", "primary_object": { "basename": "1902.01945.pdf", "url": "https://authors.library.caltech.edu/records/qr7vb-95k31/files/1902.01945.pdf" }, "related_objects": [ { "basename": "Graham_2019_PASP_131_078001.pdf", "url": "https://authors.library.caltech.edu/records/qr7vb-95k31/files/Graham_2019_PASP_131_078001.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Graham, Matthew J.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/z24gp-a1228", "eprint_id": 95128, "eprint_status": "archive", "datestamp": "2023-08-19 16:27:51", "lastmod": "2023-10-20 18:35:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing Wen" }, "orcid": "0000-0001-7737-6784" }, { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "Bryce" }, "orcid": "0000-0002-4950-6323" }, { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Kaplan-David-L", "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Kramer-Emily-A", "name": { "family": "Kramer", "given": "Emily" }, "orcid": "0000-0003-0457-2519" }, { "id": "Mahabal-Ashish-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Nielsen-Avery-J", "name": { "family": "Nielsen", "given": "Avery J." } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Tan-Hanjie", "name": { "family": "Tan", "given": "Hanjie" } }, { "id": "Yeh-Ting-Shuo", "name": { "family": "Yeh", "given": "Ting-Shuo" } }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Giomi-Matteo", "name": { "family": "Giomi", "given": "Matteo" } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Ward-Charlotte-A", "name": { "family": "Ward", "given": "Charlotte" }, "orcid": "0000-0002-4557-6682" } ] }, "title": "Towards Efficient Detection of Small Near-Earth Asteroids Using the Zwicky Transient Facility (ZTF)", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys - minor planets, asteroids: general", "note": "\u00a9 2019 The Astronomical Society of the Pacific. \n\nReceived 2019 February 20; accepted 2019 April 19; published 2019 May 23. \n\nWe thank the anonymous referee for helpful comments. We extend our thanks to many professional and amateur astronomers around the world for their valuable and timely follow-up observations which are critical for FMO discoveries. We thank Bill Gray in particular for his find_orb and sat_id software, which has been very useful to our work. We also thank Eric Christensen, Davide Farnocchia and Gareth Williams for beneficial discussions. \n\nQ.-Z. Ye acknowledges support by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation PIRE (Partnership in International Research and Education) program under Grant No 1545949. Q.-Z. Ye is grateful for the Spacewatch FMO Project which sparked his interest in asteroids. \n\nC.-C. Ngeow thanks the funding from Ministry of Science and Technology (Taiwan) under grant 104-2923-M-008-004-MY5. \n\nBased on observations obtained with the Samuel Oschin Telescope 48-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. \n\nThis research has made use of data and/or services provided by the International Astronomical Union's Minor Planet Center. The National Geographic Society - Palomar Observatory Sky Atlas (POSS-I) image of 107P/(4015) Wilson-Harrington presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. POSS-I was made by the California Institute of Technology with grants from the National Geographic Society. \n\nFacility: PO:1.2m. - \n\nSoftware: Scikit-learn (Pedregosa et al. 2012).\n\nSubmitted - 1904.09645.pdf
", "abstract": "We describe ZStreak, a semi-real-time pipeline specialized in detecting small, fast-moving, near-Earth asteroids (NEAs), which is currently operating on the data from the newly commissioned Zwicky Transient Facility (ZTF) survey. Based on a prototype originally developed by Waszczak et al. (2017) for the Palomar Transient Factory (PTF), the predecessor of ZTF, ZStreak features an improved machine-learning model that can cope with the 10\u00d7 data rate increment between PTF and ZTF. Since its first discovery on 2018 February 5 (2018 CL), ZTF/ZStreak has discovered 45 confirmed new NEAs over a total of 232 observable nights until 2018 December 31. Most of the discoveries are small NEAs, with diameters less than ~100 m. By analyzing the discovery circumstances, we find that objects having the first to last detection time interval under 2 hr are at risk of being lost. We will further improve real-time follow-up capabilities, and work on suppressing false positives using deep learning.", "date": "2019-07", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "131", "number": "1001", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 078002", "id_number": "CaltechAUTHORS:20190501-093856077", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190501-093856077", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2923-M-008-004-MY5" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "Caltech" }, { "agency": "Infrared Processing and Analysis Center (IPAC)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Stockholm University" }, { "agency": "University of Maryland" }, { "agency": "University of Washington" }, { "agency": "Deutsches Elektronen-Synchrotron" }, { "agency": "Humboldt University" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "TANGO Consortium" }, { "agency": "University of Wisconsin-Milwaukee" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "National Geographic Society" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/ab1b18", "primary_object": { "basename": "1904.09645.pdf", "url": "https://authors.library.caltech.edu/records/z24gp-a1228/files/1904.09645.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Ye, Quanzhi; Masci, Frank J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kt280-ph874", "eprint_id": 96746, "eprint_status": "archive", "datestamp": "2023-08-19 13:53:45", "lastmod": "2023-10-20 21:29:15", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bailey-V-P", "name": { "family": "Bailey", "given": "Vanessa P." }, "orcid": "0000-0002-5407-2806" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Balasubramanian-B", "name": { "family": "Balasubramanian", "given": "Bala" } }, { "id": "Berriman-G-B", "name": { "family": "Berriman", "given": "Bruce" }, "orcid": "0000-0001-8388-534X" }, { "id": "Cady-E", "name": { "family": "Cady", "given": "Eric" }, "orcid": "0000-0002-8789-2931" }, { "id": "Calchi-Novati-S", "name": { "family": "Calchi Novati", "given": "Sebastiano" }, "orcid": "0000-0002-7669-1069" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David" }, "orcid": "0000-0002-5741-3047" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "Brendan" }, "orcid": "0000-0002-4650-8518" }, { "id": "Demers-R", "name": { "family": "Demers", "given": "Richard" } }, { "id": "Effinger-R-T", "name": { "family": "Effinger", "given": "Robert" } }, { "id": "Frerking-M-A", "name": { "family": "Frerking", "given": "Margaret" } }, { "id": "Gelino-D-M", "name": { "family": "Gelino", "given": "Dawn" }, "orcid": "0000-0003-1274-2784" }, { "id": "Harding-L-K", "name": { "family": "Harding", "given": "Leon" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kern-B-D", "name": { "family": "Kern", "given": "Brian" } }, { "id": "Krist-John-E", "name": { "family": "Krist", "given": "John" } }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "Seppo" }, "orcid": "0000-0003-1250-8314" }, { "id": "Lindensmith-C-A", "name": { "family": "Lindensmith", "given": "Chris" } }, { "id": "Lowrance-P-J", "name": { "family": "Lowrance", "given": "Patrick" }, "orcid": "0000-0001-8014-0270" }, { "id": "Prada-C-M", "name": { "family": "Prada", "given": "Camilo Mejia" } }, { "id": "Mennesson-B", "name": { "family": "Mennesson", "given": "Bertrand" }, "orcid": "0000-0003-4205-4800" }, { "id": "Meshkat-T", "name": { "family": "Meshkat", "given": "Tiffany" }, "orcid": "0000-0001-6126-2467" }, { "id": "Moody-D-C", "name": { "family": "Moody", "given": "Dwight" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Moustakas-L-A", "name": { "family": "Moustakas", "given": "Leonidas" }, "orcid": "0000-0003-3030-2360" }, { "id": "Noecker-C", "name": { "family": "Noecker", "given": "Charley" }, "orcid": "0000-0003-1417-2383" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "Roberta" }, "orcid": "0000-0002-5158-243X" }, { "id": "Poberezhskiy-I", "name": { "family": "Poberezhskiy", "given": "Ilya" } }, { "id": "Ram\u00edrez-S-V", "name": { "family": "Ram\u00edrez", "given": "Solange" } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Riggs-A-J-E", "name": { "family": "Riggs", "given": "A. J. E." }, "orcid": "0000-0002-0863-6228" }, { "id": "Seo-Byoung-Joon", "name": { "family": "Seo", "given": "Byoung-Joon" } }, { "id": "Shaklan-S-B", "name": { "family": "Shaklan", "given": "Stuart" } }, { "id": "Shi-Fang", "name": { "family": "Shi", "given": "Fang" } }, { "id": "Stapelfeldt-K-R", "name": { "family": "Stapelfeldt", "given": "Karl" }, "orcid": "0000-0002-2805-7338" }, { "id": "Tang-Hong", "name": { "family": "Tang", "given": "Hong" } }, { "id": "Trauger-J-T", "name": { "family": "Trauger", "given": "John" } }, { "id": "Ygouf-M", "name": { "family": "Ygouf", "given": "Marie" }, "orcid": "0000-0001-7591-2731" }, { "id": "Zhao-Feng", "name": { "family": "Zhao", "given": "Feng" } }, { "id": "Zhou-Hanying", "name": { "family": "Zhou", "given": "Hanying" } } ] }, "title": "Key Technologies for the Wide Field Infrared Survey Telescope Coronagraph Instrument", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2018 California Institute of Technology. Government sponsorship acknowledged. The work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The decision to implement the WFIRST mission will not be finalized until NASA's completion of the National Environmental Policy Act (NEPA) process. This document is being made available for information purposes only. \n\nThis whitepaper was submitted to the Exoplanet Science Strategy call in March 2018 and is presented here without modification. An updated version of Fig. 2 and associated detailed description can be found in ref (21).\n\nSubmitted - 1901.04050.pdf
", "abstract": "The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) is a high-contrast imager and integral field spectrograph that will enable the study of exoplanets and circumstellar disks at visible wavelengths. Ground-based high-contrast instrumentation has fundamentally limited performance at small working angles, even under optimistic assumptions for 30m-class telescopes. There is a strong scientific driver for better performance, particularly at visible wavelengths. Future flagship mission concepts aim to image Earth analogues with visible light flux ratios of more than 10^10. CGI is a critical intermediate step toward that goal, with a predicted 10^8-9 flux ratio capability in the visible. CGI achieves this through improvements over current ground and space systems in several areas: (i) Hardware: space-qualified (TRL9) deformable mirrors, detectors, and coronagraphs, (ii) Algorithms: wavefront sensing and control; post-processing of integral field spectrograph, polarimetric, and extended object data, and (iii) Validation of telescope and instrument models at high accuracy and precision. This white paper, submitted to the 2018 NAS Exoplanet Science Strategy call, describes the status of key CGI technologies and presents ways in which performance is likely to evolve as the CGI design matures.", "date": "2019-06-27", "date_type": "published", "id_number": "CaltechAUTHORS:20190626-141746696", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-141746696", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.1901.04050", "primary_object": { "basename": "1901.04050.pdf", "url": "https://authors.library.caltech.edu/records/kt280-ph874/files/1901.04050.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Bailey, Vanessa P.; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5f4rf-p8x96", "eprint_id": 96745, "eprint_status": "archive", "datestamp": "2023-08-19 14:53:32", "lastmod": "2024-01-14 21:48:54", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "id": "Bartlett-James", "name": { "family": "Bartlett", "given": "James" } }, { "id": "Behroozi-P-S", "name": { "family": "Behroozi", "given": "Peter" } }, { "id": "Brinchmann-J", "name": { "family": "Brinchmann", "given": "Jarle" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga" }, "orcid": "0000-0001-7583-0621" }, { "id": "Cimatti-A", "name": { "family": "Cimatti", "given": "Andrea" } }, { "id": "Coil-A-L", "name": { "family": "Coil", "given": "Alison" } }, { "id": "Conroy-C", "name": { "family": "Conroy", "given": "Charlie" }, "orcid": "0000-0002-1590-8551" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "Emanuele" }, "orcid": "0000-0002-3331-9590" }, { "id": "Donahue-Megan", "name": { "family": "Donahue", "given": "Megan" }, "orcid": "0000-0002-2808-0853" }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "Peter" } }, { "id": "Ferguson-H-C", "name": { "family": "Ferguson", "given": "Henry C." }, "orcid": "0000-0001-7113-2738" }, { "id": "Furlanetto-S-R", "name": { "family": "Furlanetto", "given": "Steve" }, "orcid": "0000-0002-0658-1243" }, { "id": "Glazebrook-K", "name": { "family": "Glazebrook", "given": "Karl" } }, { "id": "Gonzalez-A-H", "name": { "family": "Gonzalez", "given": "Anthony" }, "orcid": "0000-0002-0933-8601" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan" }, "orcid": "0000-0001-9187-3605" }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice" }, "orcid": "0000-0002-2278-9407" }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "Sangeeta" }, "orcid": "0000-0002-9226-5350" }, { "id": "Marshall-J-L", "name": { "family": "Marshall", "given": "Jennifer" } }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "Jeffrey A." }, "orcid": "0000-0001-8684-2222" }, { "id": "Orsi-Alvaro", "name": { "family": "Orsi", "given": "Alvaro" } }, { "id": "Rhoads-J-E", "name": { "family": "Rhoads", "given": "James" }, "orcid": "0000-0002-1501-454X" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Shapley-A-E", "name": { "family": "Shapley", "given": "Alice" }, "orcid": "0000-0003-3509-4855" }, { "id": "Wechsler-R-H", "name": { "family": "Wechsler", "given": "Risa H." }, "orcid": "0000-0003-2229-011X" } ] }, "title": "Observing Galaxy Evolution in the Context of Large-Scale Structure", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1903.07409.pdf
", "abstract": "Galaxies form and evolve in the context of their local and large-scale environments. Their baryonic content that we observe with imaging and spectroscopy is intimately connected to the properties of their dark matter halos, and to their location in the \"cosmic web\" of large-scale structure. Very large spectroscopic surveys of the local universe (e.g., SDSS and GAMA) measure galaxy positions (location within large-scale structure), statistical clustering (a direct constraint on dark matter halo masses), and spectral features (measuring physical conditions of the gas and stars within the galaxies, as well as internal velocities). Deep surveys with the James Webb Space Telescope (JWST) will revolutionize spectroscopic measurements of redshifts and spectral properties for galaxies out to the epoch of reionization, but with numerical statistics and over cosmic volumes that are too small to map large-scale structure and to constrain halo properties via clustering. Here, we consider advances in understanding galaxy evolution that would be enabled by very large spectroscopic surveys at high redshifts: very large numbers of galaxies (outstanding statistics) over large co-moving volumes (large-scale structure on all scales) over broad redshift ranges (evolution over most of cosmic history). The required observational facility can be established as part of the probe portfolio by NASA within the next decade.", "date": "2019-06-27", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20190626-140614418", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-140614418", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.1903.07409", "primary_object": { "basename": "1903.07409.pdf", "url": "https://authors.library.caltech.edu/records/5f4rf-p8x96/files/1903.07409.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Dickinson, Mark; Wang, Yun; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/hy9b9-m1q58", "eprint_id": 96734, "eprint_status": "archive", "datestamp": "2023-08-19 14:55:54", "lastmod": "2024-01-14 21:48:52", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "Philip N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "Francois" } }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "Charles M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Braine-J", "name": { "family": "Braine", "given": "Jonathan" } }, { "id": "Bromm-V", "name": { "family": "Bromm", "given": "Volker" } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "Michelle" }, "orcid": "0000-0002-9871-6490" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "D\u00edaz-Santos-T", "name": { "family": "D\u00edaz-Santos", "given": "Tanio" }, "orcid": "0000-0003-0699-6083" }, { "id": "Egami-Eiichi", "name": { "family": "Egami", "given": "Eiichi" } }, { "id": "Emonts-B", "name": { "family": "Emonts", "given": "Bjorn" } }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "Pierre" }, "orcid": "0000-0002-2421-1350" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Lanz-L", "name": { "family": "Lanz", "given": "Lauranne" }, "orcid": "0000-0002-3249-8224" }, { "id": "Madden-S", "name": { "family": "Madden", "given": "Susanne" } }, { "id": "Medling-A-M", "name": { "family": "Medling", "given": "Anne" }, "orcid": "0000-0001-7421-2944" }, { "id": "O'Sullivan-E", "name": { "family": "O'Sullivan", "given": "Ewan" } }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick" }, "orcid": "0000-0002-3471-981X" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "Alexandra" }, "orcid": "0000-0001-8592-2706" }, { "id": "Pineau-des-For\u00eats-G", "name": { "family": "Pineau des For\u00eats", "given": "Guillaume" } }, { "id": "Shull-J-M", "name": { "family": "Shull", "given": "J. Michael" } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David" }, "orcid": "0000-0003-1545-5078" }, { "id": "Togi-A", "name": { "family": "Togi", "given": "Aditya" }, "orcid": "0000-0001-5042-3421" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. Kevin" }, "orcid": "0000-0002-1588-6700" } ] }, "title": "Warm H_2 as a probe of massive accretion and feedback through shocks and turbulence across cosmic time", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1903.06653.pdf
", "abstract": "Galaxy formation depends on a complex interplay between gravitational collapse, gas accretion, merging, and feedback processes. Yet, after many decades of investigation, these concepts are poorly understood. This paper presents the argument that warm H_2 can be used as a tool to unlock some of these mysteries. Turbulence, shocks and outflows, driven by star formation, AGN activity or inflows, may prevent the rapid buildup of star formation in galaxies. Central to our understanding of how gas is converted into stars is the process by which gas can dissipate its mechanical energy through turbulence and shocks in order to cool. H_2 lines provide direct quantitative measurements of kinetic energy dissipation in molecular gas in galaxies throughout the Universe. Based on the detection of very powerful H_2 lines from z = 2 galaxies and proto-clusters at the detection limits of Spitzer, we are confident that future far-IR and UV H_2 observations will provide a wealth of new information and insight into galaxy evolution to high-z. Finally, at the very earliest epoch of star and galaxy formation, warm H_2 may also provide a unique glimpse of molecular gas collapse at 7 < z < 12 in massive dark matter (DM) halos on their way to forming the very first galaxies. Such measurements are beyond the reach of existing and planned observatories.", "date": "2019-06-26", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20190626-104726557", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-104726557", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.48550/arXiv.1903.06653", "primary_object": { "basename": "1903.06653.pdf", "url": "https://authors.library.caltech.edu/records/hy9b9-m1q58/files/1903.06653.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Appleton, Philip N.; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/961vq-qqt80", "eprint_id": 96701, "eprint_status": "archive", "datestamp": "2023-08-22 01:52:43", "lastmod": "2023-10-20 21:26:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Joshi-B-A", "name": { "family": "Joshi", "given": "Bhavin A." }, "orcid": "0000-0002-7593-8584" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "Philip N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Blanc-G-A", "name": { "family": "Blanc", "given": "Guillermo A." } }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "Pierre" }, "orcid": "0000-0002-2421-1350" }, { "id": "Rich-J-A", "name": { "family": "Rich", "given": "Jeffrey" }, "orcid": "0000-0002-5807-5078" }, { "id": "Struck-C-J", "name": { "family": "Struck", "given": "Curtis" }, "orcid": "0000-0002-6490-2156" }, { "id": "Freeland-E-E", "name": { "family": "Freeland", "given": "Emily E." } }, { "id": "Peterson-B-W", "name": { "family": "Peterson", "given": "Bradley W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Alatalo-K", "name": { "family": "Alatalo", "given": "Katherine" }, "orcid": "0000-0002-4261-2326" } ] }, "title": "Evidence for Shock-heated Gas in the Taffy Galaxies and Bridge from Optical Emission-line IFU Spectroscopy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (UGC 12914&5); galaxies: interactions; galaxies: ISM; galaxies: kinematics and dynamics", "note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2018 December 18; revised 2019 April 28; accepted 2019 May 11; published 2019 June 25. \n\nB.A.J. would like to thank the Visiting Graduate Fellowship Program at IPAC/Caltech for six months of support toward work performed for this paper. B.A.J. is also grateful to Drs. Rogier Windhorst and Rolf Jansen for helpful discussions on work done in this paper. The authors thank the anonymous referee for their helpful review and suggestions. This research has made use of NASA's Astrophysics Data System. This research has made use of the Python programming language along with the Numpy, Scipy, and Matplotlib packages. This research has also made use of Astropy, a community-developed core Python package for Astronomy (The Astropy Collaboration 2018).\n\nPublished - Joshi_2019_ApJ_878_161.pdf
Accepted Version - 1812.07743
", "abstract": "We present optical integral field unit observations of the Taffy system (UGC 12914/15), named for the radio emission that stretches between the two galaxies. Given that these gas-rich galaxies are believed to have recently collided head-on, the pair exhibits a surprisingly normal total (sub-LIRG) IR luminosity (L_(FIR) ~ 4.5 \u00d7 10^(10) L_\u2299). Previous observations have demonstrated that a large quantity of molecular and neutral gas has been drawn out of the galaxies into a massive multiphase bridge. We present, for the first time, spatially resolved spectroscopy of the ionized gas in the system. The results show that the ionized gas is highly disturbed kinematically, with gas spread in two main filaments between the two galaxies. The line profiles exhibit widespread double components in both the bridge and parts of the disks of the galaxies. We investigate the spatial distribution of the excitation properties of the ionized gas using emission-line diagnostic diagrams and conclude that a large quantity (up to 40%) of the emission from the entire system is consistent with gas heated in ~200 km s^(\u22121) shocks. While the shocked gas is mainly associated with the bridge, there is a significant amount of shocked gas associated with both galaxies. Confirming other multiwavelength indicators, the results suggest that the effects of shocks and turbulence can continue to be felt in a high-speed galaxy collision long after the collision has occurred. The persistence of shocks in the Taffy system may explain the relatively low current star formation rates in the system as a whole.", "date": "2019-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "878", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 161", "id_number": "CaltechAUTHORS:20190625-125512734", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190625-125512734", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Infrared Processing and Analysis Center (IPAC)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/ab2124", "primary_object": { "basename": "1812.07743", "url": "https://authors.library.caltech.edu/records/961vq-qqt80/files/1812.07743" }, "related_objects": [ { "basename": "Joshi_2019_ApJ_878_161.pdf", "url": "https://authors.library.caltech.edu/records/961vq-qqt80/files/Joshi_2019_ApJ_878_161.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Joshi, Bhavin A.; Appleton, Philip N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/g3z1z-ptz92", "eprint_id": 96511, "eprint_status": "archive", "datestamp": "2023-08-19 14:57:49", "lastmod": "2024-01-14 21:48:10", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott" }, "orcid": "0000-0001-5855-5939" }, { "id": "Andreoni-I", "name": { "family": "Andreoni", "given": "Igor" }, "orcid": "0000-0002-8977-1498" }, { "id": "Ashley-M-C-B", "name": { "family": "Ashley", "given": "Michael" } }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "Nadia" }, "orcid": "0000-0003-0901-1606" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Frostig-D", "name": { "family": "Frostig", "given": "Danielle" } }, { "id": "F\u0171r\u00e9sz-G", "name": { "family": "F\u0171r\u00e9sz", "given": "G\u00e1bor" } }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob" }, "orcid": "0000-0001-5754-4007" }, { "id": "Hankins-M-J", "name": { "family": "Hankins", "given": "Matthew" }, "orcid": "0000-0001-9315-8437" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Lau-Ryan-M", "name": { "family": "Lau", "given": "Ryan M." } }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran" }, "orcid": "0000-0002-6786-8774" }, { "id": "Simcoe-R-A", "name": { "family": "Simcoe", "given": "Rob" }, "orcid": "0000-0003-3769-9559" }, { "id": "Sokoloski-J-L", "name": { "family": "Sokoloski", "given": "Jennifer" } }, { "id": "Soon-Jamie", "name": { "family": "Soon", "given": "Jamie" } }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Travouillon-T-D", "name": { "family": "Travouillon", "given": "Tony" } } ] }, "title": "The Dynamic Infrared Sky", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1903.08128.pdf
", "abstract": "Opening up the dynamic infrared sky for systematic time-domain exploration would yield many scientific advances. Multi-messenger pursuits such as localizing gravitational waves from neutron star mergers and quantifying the nucleosynthetic yields require the infrared. Another multi-messenger endeavor that needs infrared surveyors is the study of the much-awaited supernova in our own Milky Way. Understanding shocks in novae, true rates of supernovae and stellar mergers are some other examples of stellar evolution and high energy physics wherein the answers are buried in the infrared. We discuss some of the challenges in the infrared and pathfinders to overcome them. We conclude with recommendations on both infrared discovery engines and infrared follow-up machines that would enable this field to flourish in the next decade.", "date": "2019-06-19", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20190619-075911840", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-075911840", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.1903.08128", "primary_object": { "basename": "1903.08128.pdf", "url": "https://authors.library.caltech.edu/records/g3z1z-ptz92/files/1903.08128.pdf" }, "resource_type": "monograph", "pub_year": "2019", "author_list": "Kasliwal, Mansi M.; Adams, Scott; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1yh6m-1ja98", "eprint_id": 92109, "eprint_status": "archive", "datestamp": "2023-08-19 15:21:19", "lastmod": "2023-10-19 23:58:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga" }, "orcid": "0000-0001-7583-0621" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } } ] }, "title": "ATLAS Probe: Breakthrough Science of Galaxy Evolution, Cosmology, Milky Way, and the Solar System", "ispublished": "pub", "full_text_status": "public", "keywords": "space mission \u2014 galaxy evolution \u2014 cosmology", "note": "\u00a9 2019 Astronomical Society of Australia. \n\nPublished online: 08 April 2019. \n\nWe are grateful to Lee Armus, Dominic Benford, Peter Capak, Jeff Kruk, Ian Smail, John Stauffer, Mike Werner, and Rien Weygaert for invaluable discussions. We acknowledge Falk Baumgarten for help with the computation of the EZmocks, Charles Shapiro for providing information on the detectors, and Alex Merson for advice on cosmic web visualization options. Andrea Cimatti acknowledges the grants ASI n.I/023/12/0 \"Attivit\u00e0 relative alla fase B2/C per la missione Euclid\" and PRIN MIUR 2015 \"Cosmology and Fundamental Physics: illuminating the Dark Universe with Euclid\". Wesley Fraser acknowledges funding from Science and Technology Facilities Council grant ST/P0003094/1. Christopher Hirata is supported by the US Department of Energy, NASA, the National Science Foundation, and the Simons Foundation. Jeffrey Newman acknowledges support from DOE grant DOE DE-SC0007914. Zoran Ninkov acknowledges NASA's Strategic Astrophysics Technology (SAT) Program (grant number NNX14AI62G) in support of the development of DMD technology for use in space. James Bartlett, Olivier Dor\u00e9, Peter Eisenhardt, Michael Ressler, and Jason Rhodes are supported by JPL, which is run by Caltech under a contract from NASA.\n\nAccepted Version - 1802.01539.pdf
", "abstract": "Astrophysics Telescope for Large Area Spectroscopy Probe is a concept for a National Aeronautics and Space Administration probe-class space mission that will achieve ground-breaking science in the fields of galaxy evolution, cosmology, Milky Way, and the Solar System. It is the follow-up space mission to Wide Field Infrared Survey Telescope (WFIRST), boosting its scientific return by obtaining deep 1\u20134 \u03bcm slit spectroscopy for \u223c70% of all galaxies imaged by the \u223c2 000 deg^2 WFIRST High Latitude Survey at z > 0.5. Astrophysics Telescope for Large Area Spectroscopy will measure accurate and precise redshifts for \u223c200 M galaxies out to z < 7, and deliver spectra that enable a wide range of diagnostic studies of the physical properties of galaxies over most of cosmic history. Astrophysics Telescope for Large Area Spectroscopy Probe and WFIRST together will produce a 3D map of the Universe over 2 000 deg^2, the definitive data sets for studying galaxy evolution, probing dark matter, dark energy and modifications of General Relativity, and quantifying the 3D structure and stellar content of the Milky Way. Astrophysics Telescope for Large Area Spectroscopy Probe science spans four broad categories: (1) Revolutionising galaxy evolution studies by tracing the relation between galaxies and dark matter from galaxy groups to cosmic voids and filaments, from the epoch of reionisation through the peak era of galaxy assembly; (2) Opening a new window into the dark Universe by weighing the dark matter filaments using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of General Relativity using galaxy clustering; (3) Probing the Milky Way's dust-enshrouded regions, reaching the far side of our Galaxy; and (4) Exploring the formation history of the outer Solar System by characterising Kuiper Belt Objects. Astrophysics Telescope for Large Area Spectroscopy Probe is a 1.5 m telescope with a field of view of 0.4 deg^2, and uses digital micro-mirror devices as slit selectors. It has a spectroscopic resolution of R = 1 000, and a wavelength range of 1\u20134 \u03bcm. The lack of slit spectroscopy from space over a wide field of view is the obvious gap in current and planned future space missions; Astrophysics Telescope for Large Area Spectroscopy fills this big gap with an unprecedented spectroscopic capability based on digital micro-mirror devices (with an estimated spectroscopic multiplex factor greater than 5 000). Astrophysics Telescope for Large Area Spectroscopy is designed to fit within the National Aeronautics and Space Administration probe-class space mission cost envelope; it has a single instrument, a telescope aperture that allows for a lighter launch vehicle, and mature technology (we have identified a path for digital micro-mirror devices to reach Technology Readiness Level 6 within 2 yr). Astrophysics Telescope for Large Area Spectroscopy Probe will lead to transformative science over the entire range of astrophysics: from galaxy evolution to the dark Universe, from Solar System objects to the dusty regions of the Milky Way.", "date": "2019-04-08", "date_type": "published", "publication": "Publications of the Astronomical Society of Australia", "volume": "36", "publisher": "CSIRO Publishing", "pagerange": "Art. No. e015", "id_number": "CaltechAUTHORS:20190107-102223398", "issn": "1323-3580", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190107-102223398", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/12/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN MIUR 2015" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P0003094/1" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0007914" }, { "agency": "NASA", "grant_number": "NNX14AI62G" }, { "agency": "NSF" }, { "agency": "Simons Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1017/pasa.2019.5", "primary_object": { "basename": "1802.01539.pdf", "url": "https://authors.library.caltech.edu/records/1yh6m-1ja98/files/1802.01539.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Wang, Yun; Kirkpatrick, J. Davy; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/k5v2n-n5r58", "eprint_id": 94288, "eprint_status": "archive", "datestamp": "2023-08-22 01:18:06", "lastmod": "2023-10-20 17:50:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quanzhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Kelley-Michael-S-P", "name": { "family": "Kelley", "given": "Michael S. P." }, "orcid": "0000-0002-6702-7676" }, { "id": "Bodewits-Dennis", "name": { "family": "Bodewits", "given": "Dennis" }, "orcid": "0000-0002-2668-7248" }, { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "Bryce" }, "orcid": "0000-0002-4950-6323" }, { "id": "Jones-Lynne", "name": { "family": "Jones", "given": "Lynne" }, "orcid": "0000-0001-5916-0031" }, { "id": "Lin-Zhong-Yi", "name": { "family": "Lin", "given": "Zhong-Yi" }, "orcid": "0000-0003-3827-8991" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Groom-Steven-L", "name": { "family": "Groom", "given": "Steven" }, "orcid": "0000-0001-5668-3507" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Soumagnac-Maayane-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" } ] }, "title": "Multiple Outbursts of Asteroid (6478) Gault", "ispublished": "pub", "full_text_status": "public", "keywords": "comets: individual ((6478 Gault); minor planets, asteroids: individual ((6478 Gault)", "note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2019 February 20; revised 2019 March 6; accepted 2019 March 8; published 2019 March 29. \n\nWe thank the referee for a prompt and helpful review, as well as Charles Bell and Man-To Hui for proofreading and comments. Q.-Z. Ye is supported by the GROWTH project funded by the National Science Foundation under grant No. 1545949. Bryce Bolin and Lynne Jones acknowledge support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. Funding for the Asteroid Institute program is provided by B612 Foundation, W.K. Bowes Jr. Foundation, P. Rawls Family Fund, and two anonymous donors in addition to general support from the B612 Founding Circle (https://b612foundation.org/member_group/founding-circle/). \n\nThis work is based on observations obtained with the Samuel Oschin Telescope 48 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Major funding has been provided by the U.S. National Science Foundation under grant No. AST-1440341 and by the ZTF partner institutions: the California Institute of Technology, the Oskar Klein Centre, the Weizmann Institute of Science, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron, the University of Wisconsin-Milwaukee, and the TANGO Program of the University System of Taiwan. \n\nThis work made use of sbpy (http://sbpy.org), a community-driven Python package for small-body planetary astronomy supported by NASA PDART Grant 80NSSC18K0987. \n\nFacility: PO:1.2 m. - \n\nSoftware: Astropy (Astropy Collaboration et al. 2018), Jupyter Notebooks (Kluyver et al. 2016), Matplotlib (Hunter 2007), MERCURY6 (Chambers & Migliorini 1997), sbpy (NASA-Planetary-Science/sbpy), ZChecker (mkelley/zchecker). \n\nNote added: During the proofreading stage of this Letter, we learned of an independent paper by Kleyna et al. (2019) describing the original ATLAS detection of the event, as well as the Hubble Space Telescope and ground-based observations from a follow-up campaign. They independently reaches conclusions similar to those presented in this Letter.\n\nPublished - Ye_2019_ApJL_874_L16.pdf
Accepted Version - 1903.05320.pdf
", "abstract": "Main-belt asteroid (6478) Gault unexpectedly sprouted two tails in late 2018 and early 2019, identifying it as a new active asteroid. Here we present observations obtained by the 1.2 m Zwicky Transient Facility survey telescope that provide detailed time-series coverage of the onset and evolution of Gault's activity. Gault exhibited two brightening events, with the first one starting on 2018 October 18 \u00b1 5 days and a second one starting on 2018 December 24 \u00b1 1 days. The amounts of mass released are 2 \u00d7 10^7 kg and 1 \u00d7 10^6 kg, respectively. Based on photometric measurements, each event persisted for about a month. Gault's color has not changed appreciably over time, with a pre-outburst color of g_(PS1) \u2212 r_(PS1) = 0.50 \u00b1 0.04 and g_(PS1) \u2212 r_(PS1) = 0.46 \u00b1 0.04 during the two outbursts. Simulations of dust dynamics shows that the ejecta consists of dust grains of up to 10 \u03bcm in size that are ejected at low velocities below 1 m s^(-1) regardless of particle sizes. This is consistent with non-sublimation-driven ejection events. The size distribution of the dust exhibits a broken power law, with particles at 10\u201320 \u03bcm following a power law of \u22122.5 to \u22123.0, while larger particles follow a steeper slope of \u22124.0. The derived properties can be explained by either rotational excitation of the nucleus or a merger of a near-contact binary, with the latter scenario to be statistically more likely.", "date": "2019-04-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "874", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L16", "id_number": "CaltechAUTHORS:20190329-083647975", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190329-083647975", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "DIRAC Institute" }, { "agency": "Charles and Lisa Simonyi Fund for Arts and Sciences" }, { "agency": "Washington Research Foundation" }, { "agency": "B612 Foundation" }, { "agency": "William K. Bowes, Jr. Foundation" }, { "agency": "P. Rawls Family Fund" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NASA", "grant_number": "80NSSC18K0987" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/2041-8213/ab0f3c", "primary_object": { "basename": "Ye_2019_ApJL_874_L16.pdf", "url": "https://authors.library.caltech.edu/records/k5v2n-n5r58/files/Ye_2019_ApJL_874_L16.pdf" }, "related_objects": [ { "basename": "1903.05320.pdf", "url": "https://authors.library.caltech.edu/records/k5v2n-n5r58/files/1903.05320.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Ye, Quanzhi; Kelley, Michael S. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1yfh3-zj930", "eprint_id": 93785, "eprint_status": "archive", "datestamp": "2023-08-19 14:48:53", "lastmod": "2023-10-20 17:25:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Krafton-K", "name": { "family": "Krafton", "given": "Kelsie" } }, { "id": "Lau-Ryan-M", "name": { "family": "Lau", "given": "Ryan" } }, { "id": "Rho-Jeonghee", "name": { "family": "Rho", "given": "Jeonghee" }, "orcid": "0000-0003-3643-839X" }, { "id": "Leonard-D-C", "name": { "family": "Leonard", "given": "Douglas C." } }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob" }, "orcid": "0000-0001-5754-4007" }, { "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735" }, { "id": "Millar-Blanchaer-M-A", "name": { "family": "Millar-Blanchaer", "given": "Maxwell" }, "orcid": "0000-0001-6205-9233" }, { "id": "Nilsson-R", "name": { "family": "Nilsson", "given": "Ricky" }, "orcid": "0000-0002-5408-4954" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Gehrz-R-D", "name": { "family": "Gehrz", "given": "Robert D." }, "orcid": "0000-0003-1319-4089" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Serabyn-E", "name": { "family": "Serabyn", "given": "Eugene" } }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "Ori D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Clayton-G", "name": { "family": "Clayton", "given": "Geoffrey" }, "orcid": "0000-0002-0141-7436" } ] }, "title": "Supernova 2017eaw: Molecule and Dust Formation from Infrared Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter \u2013 supernovae: individual (SN2017eaw)", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 January 28; revised 2019 February 16; accepted 2019 February 18; published 2019 March 13. \n\nWe thank Jim Fuller and Luc Dessart for helpful discussions and input on the paper draft. We also thank the anonymous referee for reviewing the article. 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 Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some of the data presented herein were obtained at Palomar Observatory, which is operated by a collaboration between California Institute of Technology, Jet Propulsion Laboratory, Yale University, and National Astronomical Observatories of China. 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 an award issued by JPL/Caltech. 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. R.D.G. was supported by NASA and the United States Air Force. \n\nFacilities: Hale (WIRC, TripleSpec) - , Spitzer - Spitzer Space Telescope satellite, Keck (MOSFIRE, NIRES) - . \n\nSoftware: astropy (Astropy Collaboration et al. 2013; Price-Whelan et al. 2018), spextool (Cushing et al. 2004), xtellcor (Vacca et al. 2003), MOSFIRE data reduction pipeline (McLean et al. 2012), MOCASSIN (v.2.02.72 Ercolano et al. 2003, 2005, 2008), Matplotlib (Hunter 2007).\n\nPublished - Tinyanont_2019_ApJ_873_127.pdf
Submitted - 1901.01940.pdf
", "abstract": "We present infrared (IR) photometry and spectroscopy of the Type II-P SN 2017eaw and its progenitor in the nearby galaxy NGC 6946. Progenitor observations in the Ks band in four epochs from 1 yr to 1 day before the explosion reveal no significant variability in the progenitor star greater than 6% that lasts longer than 200 days. SN 2017eaw is a typical SN II-P with near-IR and mid-IR photometric evolution similar to those of SNe 2002hh and 2004et, other normal SNe II-P in the same galaxy. Spectroscopic monitoring during the plateau phase reveals a possible high-velocity He I 1.083 \u03bcm absorption line, indicative of a shock interaction with the circumstellar medium. Spectra between 389 and 480 days postexplosion reveal a strong CO first overtone emission at 389 days, with a line profile matching that of SN 1987A from the same epoch, indicating ~10^(\u22123) M\u2299 of CO at 1800 K. From the 389 days epoch until the most recent observation at 566 days, the first overtone feature fades while the 4.5 \u03bcm excess, likely from the CO fundamental band, remains. This behavior indicates that the CO has not been destroyed, but that the gas has cooled enough that the levels responsible for first overtone emissions are no longer populated. Finally, the evolution of Spitzer 3.6 \u03bcm photometry shows evidence for dust formation in SN 2017eaw, with a dust mass of 10^(\u22126) or 10^(\u22124) M\u2299 assuming carbonaceous or silicate grains, respectively.", "date": "2019-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "873", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 127", "id_number": "CaltechAUTHORS:20190313-132337168", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190313-132337168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab0897", "primary_object": { "basename": "Tinyanont_2019_ApJ_873_127.pdf", "url": "https://authors.library.caltech.edu/records/1yfh3-zj930/files/Tinyanont_2019_ApJ_873_127.pdf" }, "related_objects": [ { "basename": "1901.01940.pdf", "url": "https://authors.library.caltech.edu/records/1yfh3-zj930/files/1901.01940.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Tinyanont, Samaporn; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pfh76-zfr89", "eprint_id": 91561, "eprint_status": "archive", "datestamp": "2023-08-19 13:44:53", "lastmod": "2023-10-19 23:11:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "Steven" }, "orcid": "0000-0001-5668-3507" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Jackson-Edward", "name": { "family": "Jackson", "given": "Edward" } }, { "id": "Monkewitz-S-M", "name": { "family": "Monkewitz", "given": "Serge" } }, { "id": "Beck-R", "name": { "family": "Beck", "given": "R." } }, { "id": "Flynn-David", "name": { "family": "Flynn", "given": "David" } }, { "id": "Terek-Scott", "name": { "family": "Terek", "given": "Scott" } }, { "id": "Landry-Walter", "name": { "family": "Landry", "given": "Walter" } }, { "id": "Hacopians-Eugean", "name": { "family": "Hacopians", "given": "Eugean" } }, { "id": "Desai-Vandana-R", "name": { "family": "Desai", "given": "Vandana" }, "orcid": "0000-0002-1340-0543" }, { "id": "Howell-J-H", "name": { "family": "Howell", "given": "Justin" } }, { "id": "Brooke-T-Y", "name": { "family": "Brooke", "given": "Timothy Y." } }, { "id": "Imel-D-A", "name": { "family": "Imel", "given": "D." }, "orcid": "0000-0002-6118-7396" }, { "id": "Wachter-Stefanie", "name": { "family": "Wachter", "given": "Stefanie" } }, { "id": "Ye-Quan-Zhi", "name": { "family": "Ye", "given": "Quan-Zhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cunningham-Virginia", "name": { "family": "Cunningham", "given": "Virginia" }, "orcid": "0000-0003-2292-0441" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "U. D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "B. D." }, "orcid": "0000-0002-7856-3570" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish" }, "orcid": "0000-0003-2242-0244" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Patterson-M-T", "name": { "family": "Patterson", "given": "Maria T." }, "orcid": "0000-0002-4753-3387" }, { "id": "Juri\u0107-Mario", "name": { "family": "Juri\u0107", "given": "Mario" }, "orcid": "0000-0003-1996-9252" }, { "id": "Golkhou-V-Z", "name": { "family": "Golkhou", "given": "V. Zach" }, "orcid": "0000-0001-8205-2506" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." }, "orcid": "0000-0002-5884-7867" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Burdge-K-B", "name": { "family": "Burdge", "given": "Kevin B." }, "orcid": "0000-0002-7226-836X" }, { "id": "Cannella-C-B", "name": { "family": "Cannella", "given": "C." }, "orcid": "0000-0003-2667-7290" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Thomas" } }, { "id": "Van-Sistine-Angela", "name": { "family": "Van Sistine", "given": "Angela" }, "orcid": "0000-0003-4131-173X" }, { "id": "Giomi-Matteo", "name": { "family": "Giomi", "given": "Matteo" } }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Riddle-R-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "The Zwicky Transient Facility: Data Processing, Products, and Archive", "ispublished": "pub", "full_text_status": "public", "keywords": "astronomical databases: miscellaneous \u2013 catalogs \u2013 methods: data analysis \u2013 techniques: image processing \u2013 techniques: photometric", "note": "\u00a9 2018. The Astronomical Society of the Pacific. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2018 July 14; accepted 2018 October 15; published 2018 December 7. \n\nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Major funding has been provided by the U.S National Science Foundation under Grant No. AST-1440341 and by the ZTF partner institutions: the California Institute of Technology, the Oskar Klein Centre, the Weizmann Institute of Science, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron, the University of Wisconsin-Milwaukee, and the TANGO Program of the University System of Taiwan. \n\nPart of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nThe High Performance Wireless Research & Education Network (HPWREN; https://hpwren.ucsd.edu) is a project at the University of California, San Diego and the National Science Foundation (grant numbers 0087344 (in 2000), 0426879 (in 2004), and 0944131 (in 2009)). \n\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia),processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nThis work has also made use of the Pan-STARRS1 (PS1) Surveys (http://pshttp://www.ifa.hawaii.edu/pswww/) and the PS1 public science archive (https://panstarrs.stsci.edu). \n\nFacilities: PO:1.2 m - , PO:1.5m - .\n\nPublished - Masci_2019_PASP_131_018003.pdf
", "abstract": "The Zwicky Transient Facility (ZTF) is a new robotic time-domain survey currently in progress using the Palomar 48-inch Schmidt Telescope. ZTF uses a 47 square degree field with a 600 megapixel camera to scan the entire northern visible sky at rates of ~3760 square degrees/hour to median depths of g ~ 20.8 and r ~ 20.6 mag (AB, 5\u03c3 in 30 sec). We describe the Science Data System that is housed at IPAC, Caltech. This comprises the data-processing pipelines, alert production system, data archive, and user interfaces for accessing and analyzing the products. The real-time pipeline employs a novel image-differencing algorithm, optimized for the detection of point-source transient events. These events are vetted for reliability using a machine-learned classifier and combined with contextual information to generate data-rich alert packets. The packets become available for distribution typically within 13 minutes (95th percentile) of observation. Detected events are also linked to generate candidate moving-object tracks using a novel algorithm. Objects that move fast enough to streak in the individual exposures are also extracted and vetted. We present some preliminary results of the calibration performance delivered by the real-time pipeline. The reconstructed astrometric accuracy per science image with respect to Gaia DR1 is typically 45 to 85 milliarcsec. This is the RMS per-axis on the sky for sources extracted with photometric S/N \u2265 10 and hence corresponds to the typical astrometric uncertainty down to this limit. The derived photometric precision (repeatability) at bright unsaturated fluxes varies between 8 and 25 millimag. The high end of these ranges corresponds to an airmass approaching ~2\u2014the limit of the public survey. Photometric calibration accuracy with respect to Pan-STARRS1 is generally better than 2%. The products support a broad range of scientific applications: fast and young supernovae; rare flux transients; variable stars; eclipsing binaries; variability from active galactic nuclei; counterparts to gravitational wave sources; a more complete census of Type Ia supernovae; and solar-system objects.", "date": "2019-01-01", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "131", "number": "995", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 018003", "id_number": "CaltechAUTHORS:20181207-084047467", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181207-084047467", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "OAC-0087344" }, { "agency": "NSF", "grant_number": "OAC-0426879" }, { "agency": "NSF", "grant_number": "OAC-0944131" }, { "agency": "Gaia Multilateral Agreement" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/aae8ac", "primary_object": { "basename": "Masci_2019_PASP_131_018003.pdf", "url": "https://authors.library.caltech.edu/records/pfh76-zfr89/files/Masci_2019_PASP_131_018003.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Masci, Frank J.; Laher, Russ R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/j3pvq-p2n83", "eprint_id": 92340, "eprint_status": "archive", "datestamp": "2023-08-19 13:39:13", "lastmod": "2023-10-20 00:12:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Comprehensive comparison of models for spectral energy distributions from 0.1 \u03bcm to 1 mm of nearby star-forming galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: fundamental parameters \u2013 galaxies: star formation \u2013 galaxies: ISM \u2013 galaxies: spiral \u2013 infrared: galaxies \u2013 ultraviolet: galaxies", "note": "\u00a9 2019 ESO. Article published by EDP Sciences. \n\nReceived 9 September 2018; Accepted 6 November 2018; Published online 07 January 2019. \n\nWe thank the anonymous referee for a very timely report and constructive comments. We thank Paolo Serra for insights into star-formation rates for early-type galaxies, and Anna Gallazzi for kindly passing us her SDSS sample in digital form for comparison. We are also grateful to Michael Brown for helpful input, and Elisabete da Cunha for her careful comments on the manuscript in advance of publication. SB, GLG, LKH, AR, and LS acknowledge funding by an Italian research grant, PRIN-INAF/2012, and SB, GLG, LKH, LS, and SZ by the INAF PRIN-SKA 2017 program 1.05.01.88.04. MB was supported by the FONDECYT regular project 1170618 and the MINEDUC-UA projects codes ANT 1655 and ANT 1656. IDL gratefully acknowledges the support of the Flemish Fund for Scientific Research (FWO-Vlaanderen). RN acknowledges partial support by FONDECYT grant No. 3140436, and MR support by Spanish MEC Grant AYA-2014-53506-P. 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 - aa34212-18.pdf
Accepted Version - 1809.04088.pdf
", "abstract": "We have fit the far-ultraviolet (FUV) to sub-millimeter (850 \u03bcm) spectral energy distributions (SEDs) of the 61 galaxies from the Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel (KINGFISH). The fitting has been performed using three models: the Code for Investigating GALaxy Evolution (CIGALE), the GRAphite-SILicate approach (GRASIL), and the Multiwavelength Analysis of Galaxy PHYSical properties (MAGPHYS). We have analyzed the results of the three codes in terms of the SED shapes, and by comparing the derived quantities with simple \"recipes\" for stellar mass (M_(star)), star-formation rate (SFR), dust mass (M_(dust)), and monochromatic luminosities. Although the algorithms rely on different assumptions for star-formation history, dust attenuation and dust reprocessing, they all well approximate the observed SEDs and are in generally good agreement for the associated quantities. However, the three codes show very different behavior in the mid-infrared regime: in the 5\u201310 \u03bcm region dominated by PAH emission, and also between 25 and 70 \u03bcm where there are no observational constraints for the KINGFISH sample. We find that different algorithms give discordant SFR estimates for galaxies with low specific SFR, and that the standard recipes for calculating FUV absorption overestimate the extinction compared to the SED-fitting results. Results also suggest that assuming a \"standard\" constant stellar mass-to-light ratio overestimates M_(star) relative to the SED fitting, and we provide new SED-based formulations for estimating M_(star) from WISE W1 (3.4 \u03bcm) luminosities and colors. From a principal component analysis of M_(star), SFR, M_(dust), and O/H, we reproduce previous scaling relations among M_(star), SFR, and O/H, and find that M_(dust) can be predicted to within \u223c0.3 dex using only M_(star) and SFR.", "date": "2019-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "621", "publisher": "EDP Sciences", "pagerange": "Art. No. A51", "id_number": "CaltechAUTHORS:20190117-093606026", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190117-093606026", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2012" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-SKA 2017" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "1.05.01.88.04" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1170618" }, { "agency": "MINEDUC-UA Project", "grant_number": "ANT 1655" }, { "agency": "MINEDUC-UA Project", "grant_number": "ANT 1656" }, { "agency": "Fonds voor Wetenschappelijk Onderzoek (FWO)" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3140436" }, { "agency": "Ministerio de Educaci\u00f3n y Ciencia (MEC)", "grant_number": "AYA-2014-53506-P" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201834212", "primary_object": { "basename": "1809.04088.pdf", "url": "https://authors.library.caltech.edu/records/j3pvq-p2n83/files/1809.04088.pdf" }, "related_objects": [ { "basename": "aa34212-18.pdf", "url": "https://authors.library.caltech.edu/records/j3pvq-p2n83/files/aa34212-18.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Hunt, L. K. and Helou, G." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2v7ke-fqq30", "eprint_id": 91216, "eprint_status": "archive", "datestamp": "2023-08-19 13:35:17", "lastmod": "2023-10-19 22:17:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Patterson-M-T", "name": { "family": "Patterson", "given": "Maria T." }, "orcid": "0000-0002-4753-3387" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "Ben" }, "orcid": "0000-0001-7648-4142" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Juric-M", "name": { "family": "Juric", "given": "Mario" }, "orcid": "0000-0003-1996-9252" }, { "id": "Krughoff-K-S", "name": { "family": "Krughoff", "given": "K. Simon" }, "orcid": "0000-0002-4410-7868" }, { "id": "Golkhou-V-Z", "name": { "family": "Golkhou", "given": "V. Zach" }, "orcid": "0000-0001-8205-2506" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "The Zwicky Transient Facility Alert Distribution System", "ispublished": "pub", "full_text_status": "public", "keywords": "astronomical databases: miscellaneous \u2013 instrumentation: iscellaneous \u2013 surveys", "note": "\u00a9 2018 The Astronomical Society of the Pacific. \n\nReceived 2018 September 14; accepted 2018 October 10; published 2018 November 27. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project, a scientific collaboration among the California Institute of Technology, the Oskar Klein Centre, the Weizmann Institute of Science, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron, the University of Wisconsin-Milwaukee, and the TANGO Program of the University System of Taiwan. Further support is provided by the U.S. National Science Foundation under grant No. AST-1440341. \n\nM. Patterson, E. Bellm., and K. S. Krughoff acknowledge support from the Large Synoptic Survey Telescope program, which is supported in part by the National Science Foundation through Cooperative Agreement 1258333 managed by the Association of Universities for Research in Astronomy (AURA), and the Department of Energy under contract No. DE-AC02-76SF00515 with the SLAC National Accelerator Laboratory. Additional LSST funding comes from private donations, grants to universities, and in-kind support from LSSTC Institutional Members. \n\nM. Patterson, E. Bellm, V. Z. Golkhou, and M. Juric acknowledge support from the University of Washington College of Arts and Sciences, Department of Astronomy, and the DIRAC Institute. University of Washington's DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. \n\nE. Bellm is supported in part by the NSF AAG grant 1812779 and grant #2018-0908 from the Heising-Simons Foundation. \n\nM. Juric acknowledges the support of the Washington Research Foundation Data Science Term Chair fund, and the UW Provost's Initiative in Data-Intensive Discovery.\n\nSubmitted - 1902.02227.pdf
", "abstract": "The Zwicky Transient Facility (ZTF) survey generates real-time alerts for optical transients, variables, and moving objects discovered in its wide-field survey. We describe the ZTF alert stream distribution and processing (filtering) system. The system uses existing open-source technologies developed in industry: Kafka, a real-time streaming platform, and Avro, a binary serialization format. The technologies used in this system provide a number of advantages for the ZTF use case, including (1) built-in replication, scalability, and stream rewind for the distribution mechanism; (2) structured messages with strictly enforced schemas and dynamic typing for fast parsing; and (3) a Python-based stream processing interface that is similar to batch for a familiar and user-friendly plug-in filter system, all in a modular, primarily containerized system. The production deployment has successfully supported streaming up to 1.2 million alerts or roughly 70 GB of data per night, with each alert available to a consumer within about 10 s of alert candidate production. Data transfer rates of about 80,000 alerts/minute have been observed. In this paper, we discuss this alert distribution and processing system, the design motivations for the technology choices for the framework, performance in production, and how this system may be generally suitable for other alert stream use cases, including the upcoming Large Synoptic Survey Telescope.", "date": "2019-01", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "131", "number": "995", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 018001", "id_number": "CaltechAUTHORS:20181127-101530598", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181127-101530598", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "NSF", "grant_number": "AST-1258333" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "University of Washington" }, { "agency": "DIRAC Institute" }, { "agency": "NSF", "grant_number": "AST-1812779" }, { "agency": "Heising-Simons Foundation", "grant_number": "2018-0908" }, { "agency": "Washington Research Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "Zwicky Transient Facility Collaboration" ] }, "doi": "10.1088/1538-3873/aae904", "primary_object": { "basename": "1902.02227.pdf", "url": "https://authors.library.caltech.edu/records/2v7ke-fqq30/files/1902.02227.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Patterson, Maria T.; Bellm, Eric C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/f58y4-9tk79", "eprint_id": 91560, "eprint_status": "archive", "datestamp": "2023-08-19 13:36:42", "lastmod": "2023-10-19 23:11:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Dekany-Richard-G", "name": { "family": "Dekany", "given": "Richard" }, "orcid": "0000-0002-5884-7867" }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger M." }, "orcid": "0000-0001-7062-9726" }, { "id": "Riddle-Reed-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Barbarino-Cristina", "name": { "family": "Barbarino", "given": "C." }, "orcid": "0000-0002-3821-6144" }, { "id": "Barlow-Thomas-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Bauer-James-M", "name": { "family": "Bauer", "given": "James M." }, "orcid": "0000-0001-9542-0953" }, { "id": "Beck-R", "name": { "family": "Beck", "given": "R." } }, { "id": "Belicki-Justin", "name": { "family": "Belicki", "given": "Justin" } }, { "id": "Biswas-Rahul", "name": { "family": "Biswas", "given": "Rahul" }, "orcid": "0000-0002-5741-7195" }, { "id": "Blagorodnova-Nadejda", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Bodewits-Dennis", "name": { "family": "Bodewits", "given": "Dennis" }, "orcid": "0000-0002-2668-7248" }, { "id": "Bolin-Bryce-T", "name": { "family": "Bolin", "given": "Bryce" }, "orcid": "0000-0002-4950-6323" }, { "id": "Brinnel-Valery", "name": { "family": "Brinnel", "given": "V." } }, { "id": "Brooke-Timothy-Y", "name": { "family": "Brooke", "given": "T. Y." } }, { "id": "Bue-Brian-D", "name": { "family": "Bue", "given": "Brian" }, "orcid": "0000-0002-7856-3570" }, { "id": "Bulla-Mattia", "name": { "family": "Bulla", "given": "Mattia" }, "orcid": "0000-0002-8255-5127" }, { "id": "Burruss-Rick-S", "name": { "family": "Burruss", "given": "Rick S." } }, { "id": "Cenko-S-Bradley", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Connolly-Andrew-J", "name": { "family": "Connolly", "given": "Andrew" } }, { "id": "Coughlin-Michael-W", "name": { "family": "Coughlin", "given": "Michael W." }, "orcid": "0000-0002-8262-2924" }, { "id": "Cromer-John-L", "name": { "family": "Cromer", "given": "John" } }, { "id": "Cunningham-Virginia", "name": { "family": "Cunningham", "given": "Virginia" }, "orcid": "0000-0003-2292-0441" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "id": "Delacroix-Alexandre", "name": { "family": "Delacroix", "given": "Alex" } }, { "id": "Desai-Vandana-R", "name": { "family": "Desai", "given": "Vandana" }, "orcid": "0000-0002-1340-0543" }, { "id": "Duev-Dmitry-A", "name": { "family": "Duev", "given": "Dmitry A." }, "orcid": "0000-0001-5060-8733" }, { "id": "Eadie-Gwendolyn", "name": { "family": "Eadie", "given": "Gwendolyn" }, "orcid": "0000-0003-3734-8177" }, { "id": "Farnham-Tony-L", "name": { "family": "Farnham", "given": "Tony L." }, "orcid": "0000-0002-4767-9861" }, { "id": "Feeney-Michael-E", "name": { "family": "Feeney", "given": "Michael" } }, { "id": "Feindt-Ulrich", "name": { "family": "Feindt", "given": "U." }, "orcid": "0000-0002-9435-2167" }, { "id": "Flynn-David", "name": { "family": "Flynn", "given": "David" } }, { "id": "Franckowiak-A", "name": { "family": "Franckowiak", "given": "A." } }, { "id": "Frederick-Sara", "name": { "family": "Frederick", "given": "Sara" }, "orcid": "0000-0001-9676-730X" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Gal-Yam-Avishay", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Gezari-Suvi", "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "id": "Giomi-Matteo", "name": { "family": "Giomi", "given": "Matteo" } }, { "id": "Goldstein-Daniel-A", "name": { "family": "Goldstein", "given": "Daniel A." }, "orcid": "0000-0003-3461-8661" }, { "id": "Golkhou-V-Zach", "name": { "family": "Golkhou", "given": "V. 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L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Singer-Leo-P", "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "id": "Soumagnac-Maayane-T", "name": { "family": "Soumagnac", "given": "Maayane T." }, "orcid": "0000-0001-6753-1488" }, { "id": "Stein-Robert-M", "name": { "family": "Stein", "given": "Robert" } }, { "id": "Surace-Jason-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Szkody-Paula", "name": { "family": "Szkody", "given": "Paula" }, "orcid": "0000-0003-4373-7777" }, { "id": "Taddia-Francesco", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Terek-Scott", "name": { "family": "Terek", "given": "Scott" } }, { "id": "Van-Sistine-Angela", "name": { "family": "Van Sistine", "given": "Angela" }, "orcid": "0000-0003-4131-173X" }, { "id": "van-Velzen-Sjoert", "name": { "family": "van Velzen", "given": "Sjoert" }, "orcid": "0000-0002-3859-8074" }, { "id": "Vestrand-W-Thomas", "name": { "family": "Vestrand", "given": "W. T." }, "orcid": "0000-0001-7120-7234" }, { "id": "Walters-Richard-S", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Ward-Charlotte-A", "name": { "family": "Ward", "given": "Charlotte" }, "orcid": "0000-0002-4557-6682" }, { "id": "Yi-Quan-Zhi", "name": { "family": "Yi", "given": "Quan-Zhi" } }, { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "Po-Chieh" }, "orcid": "0000-0001-8894-0854" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "The Zwicky Transient Facility: System Overview, Performance, and First Results", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: photometers \u2013 telescopes", "note": "\u00a9 2018. The Astronomical Society of the Pacific. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2018 August 21; accepted 2018 October 25; published 2018 December 7. \n\nBased on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. Major funding has been provided by the U.S. National Science Foundation under grant No. AST-1440341 and by the ZTF partner institutions: the California Institute of Technology, the Oskar Klein Centre, the Weizmann Institute of Science, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron, the University of Wisconsin-Milwaukee, and the TANGO Program of the University System of Taiwan. \n\nThis work is partly based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. This work is partly based on observations made with DOLoRes@TNG. \n\nJ. Bauer, T. Farnham, and M. Kelley gratefully acknowledge the NASA/University of Maryland/MPC Augmentation through the NASA Planetary Data System Cooperative Agreement NNX16AB16A. \n\nE. Bellm, B. Bolin, A. Connolly, V. Z. Golkhou, D. Huppenkothen, Z. Ivezi\u0107 L. Jones, M. Juric, and M. Patterson acknowledge support from the University of Washington College of Arts and Sciences, Department of Astronomy, and the DIRAC Institute. University of Washington's DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. M. Juric and A. Connolly acknowledge the support of the Washington Research Foundation Data Science Term Chair fund, and the UW Provost's Initiative in Data-Intensive Discovery. \n\nE. Bellm, A. Connolly, Z. Ivezi\u0107 L. Jones, M. Juric, and M. Patterson acknowledge support from the Large Synoptic Survey Telescope, which is supported in part by the National Science Foundation through Cooperative Agreement 1258333 managed by the Association of Universities for Research in Astronomy (AURA), and the Department of Energy under Contract No. DE-AC02-76SF00515 with the SLAC National Accelerator Laboratory. Additional LSST funding comes from private donations, grants to universities, and in-kind support from LSSTC Institutional Members. \n\nE. Bellm is supported in part by the NSF AAG grant 1812779 and grant #2018-0908 from the Heising-Simons Foundation. \n\nB.T. Bolin acknowledges funding for the Asteroid Institute program provided by B612 Foundation, W.K. Bowes Jr. Foundation, P. Rawls Family Fund and two anonymous donors in addition to general support from the B612 Founding Circle. \n\nM. Bulla acknowledges support from the Swedish Research Council (Vetenskapsr\u00e5det) and the Swedish National Space Board. \n\nC.-K. Chang, W.-H. Ip, C.-D. Lee, Z.-Y. Lin, C.-C. Ngeow and P.-C. Yu thank the funding from Ministry of Science and Technology (Taiwan) under grant 104-2923-M-008-004-MY5, 104-2112-M-008-014-MY3, 105-2112-M-008-002-MY3, 106-2811-M-008-081 and 106-2112-M-008-007. \n\nA. Gal-Yam is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program and by a Kimmel award. \n\nS. Gezari is supported in part by NSF CAREER grant 1454816 and NSF AAG grant 1616566. \n\nD. A. Goldstein acknowledges support from Hubble Fellowship grant HST-HF2-51408.001-A. Support for Program number HST-HF2-51408.001-A is provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. \n\nM. M. Kasliwal and Q.-Z. Ye acknowledge support by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation PIRE (Partnership in International Research and Education) program under grant No. 1545949. \n\nA. A. Mahabal acknowledges support from the following grants: NSF AST-1749235, NSF-1640818 and NASA 16-ADAP16-0232. \n\nA. A. Miller is funded by the Large Synoptic Survey Telescope Corporation in support of the Data Science Fellowship Program. \n\nE. Ofek is grateful for support by a grant from the Israeli Ministry of Science, ISF, Minerva, BSF, BSF transformative program, and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant No. 1829/12). \n\nM. Rigault is supported by the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 759194\u2014USNAC). \n\nJ. Sollerman acknowledges support from the Knut and Alice Wallenberg Foundation. \n\nM. T. Soumagnac acknowledges support by a grant from IMOS/ISA, the Ilan Ramon fellowship from the Israel Ministry of Science and Technology and the Benoziyo center for Astrophysics at the Weizmann Institute of Science. \n\nPart of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nFacilities: PO:1.2m - , PO:1.5m - , ARC - , DCT - , NOT. -\n\nPublished - Bellm_2019_PASP_131_018002.pdf
", "abstract": "The Zwicky Transient Facility (ZTF) is a new optical time-domain survey that uses the Palomar 48 inch Schmidt telescope. A custom-built wide-field camera provides a 47 deg^2 field of view and 8 s readout time, yielding more than an order of magnitude improvement in survey speed relative to its predecessor survey, the Palomar Transient Factory. We describe the design and implementation of the camera and observing system. The ZTF data system at the Infrared Processing and Analysis Center provides near-real-time reduction to identify moving and varying objects. We outline the analysis pipelines, data products, and associated archive. Finally, we present on-sky performance analysis and first scientific results from commissioning and the early survey. ZTF's public alert stream will serve as a useful precursor for that of the Large Synoptic Survey Telescope.", "date": "2019-01", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "131", "number": "995", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 018002", "id_number": "CaltechAUTHORS:20181207-084047368", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181207-084047368", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "NASA", "grant_number": "NNX16AB16A" }, { "agency": "University of Washington" }, { "agency": "DIRAC Institute" }, { "agency": "Charles and Lisa Simonyi Fund for Arts and Sciences" }, { "agency": "Washington Research Foundation" }, { "agency": "NSF", "grant_number": "AST-1258333" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "LSSTC Institutional Members" }, { "agency": "NSF", "grant_number": "AST-1812779" }, { "agency": "Heising-Simons Foundation", "grant_number": "2018-0908" }, { "agency": "B612 Foundation" }, { "agency": "William K. Bowes, Jr. Foundation" }, { "agency": "P. Rawls Family Fund" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2923-M-008-004-MY5" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2112-M-008-014-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "105-2112-M-008-002-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "106-2811-M-008-081" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "106-2112-M-008-007" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Kimmel Award" }, { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "NSF", "grant_number": "AST-1616566" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51408.001-A" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NSF", "grant_number": "AST-1749235" }, { "agency": "NSF", "grant_number": "OAC-1640818" }, { "agency": "NASA", "grant_number": "16-ADAP16-0232" }, { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "MINERVA (Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "European Research Council (ERC)", "grant_number": "759194" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Israel Space Agency" }, { "agency": "Ministry of Science and Technology (Israel)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/aaecbe", "primary_object": { "basename": "Bellm_2019_PASP_131_018002.pdf", "url": "https://authors.library.caltech.edu/records/f58y4-9tk79/files/Bellm_2019_PASP_131_018002.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Bellm, Eric C.; Kulkarni, Shrinivas R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/31ky4-2ma39", "eprint_id": 96766, "eprint_status": "archive", "datestamp": "2023-08-19 13:28:52", "lastmod": "2024-01-14 21:48:56", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "L." }, "orcid": "0000-0001-6381-515X" }, { "id": "Desai-V", "name": { "family": "Desai", "given": "V." }, "orcid": "0000-0002-1340-0543" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H." }, "orcid": "0000-0002-7064-5424" }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "S." }, "orcid": "0000-0001-5668-3507" }, { "id": "Akeson-R-L", "name": { "family": "Akeson", "given": "R." }, "orcid": "0000-0001-9674-1564" }, { "id": "Berriman-G-B", "name": { "family": "Berriman", "given": "G. B." }, "orcid": "0000-0001-8388-534X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Imel-D-A", "name": { "family": "Imel", "given": "D." }, "orcid": "0000-0002-6118-7396" }, { "id": "Mazzarella-J-M", "name": { "family": "Mazzarella", "given": "J. M." }, "orcid": "0000-0002-8204-8619" }, { "id": "Accomazzi-A", "name": { "family": "Accomazzi", "given": "A." } }, { "id": "McGlynn-T-A", "name": { "family": "McGlynn", "given": "T." }, "orcid": "0000-0003-3973-432X" }, { "id": "Smale-A-P", "name": { "family": "Smale", "given": "A." } }, { "id": "White-R", "name": { "family": "White", "given": "R." } } ] }, "title": "NASA's Long-Term Astrophysics Data Archives", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2019 Astronomical Society of the Pacific.\n\nPublished - 521-0036.pdf
Submitted - 1709.09566.pdf
", "abstract": "NASA regards data handling and archiving as an integral part of space missions, and has a strong track record of serving astrophysics data to the public, beginning with the the IRAS satellite in 1983. Archives enable a major science return on the significant investment required to develop a space mission. In fact, the presence and accessibility of an archive can more than double the number of papers resulting from the data. In order for the community to be able to use the data, they have to be able to find the data (ease of access) and interpret the data (ease of use). Funding of archival research (e.g., the ADAP program) is also important not only for making scientific progress, but also for encouraging authors to deliver data products back to the archives to be used in future studies. NASA has also enabled a robust system that can be maintained over the long term, through technical innovation and careful attention to resource allocation. This article provides a brief overview of some of NASA's major astrophysics archive systems, including IRSA, MAST, HEASARC, KOA, NED, the Exoplanet Archive, and ADS.", "date": "2019", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "36-45", "id_number": "CaltechAUTHORS:20190627-085011585", "isbn": "978-1-58381-929-6", "book_title": "Astronomical Data Analysis Software and Systems XXVI", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190627-085011585", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Molinaro-M", "name": { "family": "Molinaro", "given": "Marco" } }, { "id": "Shortridge-K", "name": { "family": "Shortridge", "given": "Keith" } }, { "id": "Pasian-F", "name": { "family": "Pasian", "given": "Fabio" } } ] }, "doi": "10.48550/arXiv.1709.09566", "primary_object": { "basename": "1709.09566.pdf", "url": "https://authors.library.caltech.edu/records/31ky4-2ma39/files/1709.09566.pdf" }, "related_objects": [ { "basename": "521-0036.pdf", "url": "https://authors.library.caltech.edu/records/31ky4-2ma39/files/521-0036.pdf" } ], "resource_type": "book_section", "pub_year": "2019", "author_list": "Rebull, L.; Desai, V.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r5ga3-54w68", "eprint_id": 94793, "eprint_status": "archive", "datestamp": "2023-08-22 00:13:16", "lastmod": "2023-10-20 18:16:22", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "Steve" }, "orcid": "0000-0001-5668-3507" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "Benjamin" }, "orcid": "0000-0001-7648-4142" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Jackson-Edward", "name": { "family": "Jackson", "given": "Ed" } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Flynn-David", "name": { "family": "Flynn", "given": "Dave" } }, { "id": "Landry-Walter", "name": { "family": "Landry", "given": "Walter" } }, { "id": "Terek-Scott", "name": { "family": "Terek", "given": "Scott" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Beck-Ron", "name": { "family": "Beck", "given": "Ron" } }, { "id": "Hasscopians-Eugean", "name": { "family": "Hasscopians", "given": "Eugean" } }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "Umaa" }, "orcid": "0000-0002-2560-3495" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "Brian" }, "orcid": "0000-0002-7856-3570" }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger M." }, "orcid": "0000-0001-7062-9726" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." }, "orcid": "0000-0002-5884-7867" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Patterson-M-T", "name": { "family": "Patterson", "given": "Maria" }, "orcid": "0000-0002-4753-3387" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom" } }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew" }, "orcid": "0000-0002-3168-0139" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "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" } ] }, "title": "Processing Images from the Zwicky Transient Facility", "ispublished": "unpub", "full_text_status": "public", "keywords": "asteroids; stars: variables, binaries, supernovae, cataclysmic variables; galactic: active nuclei; techniques: image processing, photometric; methods: observational, data analysis", "note": "CC BY-NC-ND license. \n\nWe are grateful to Joel Johansson of the Oskar Klein Center at Stockholm University and the Weizmann Institute of Science for permission to use the original creative work shown in Figure 1. ZTF is led by the California Institute of Technology, US and includes IPAC, US; the Joint Space-Science Institute (via the University of Maryland, College Park), US; Oskar Klein Centre of the University of Stockholm, Sweden; University of Washington, US; Weizmann Institute of Science, Israel; DESY and Humboldt University of Berlin, Germany; University of Wisconsin at Milwaukee, US; the University System of Taiwan, Taiwan; and Los Alamos National Laboratory, US; ZTF acknowledges the generous support of the National Science Foundation under AST MSIP Grant No 1440341. The alert distribution service is provided by the DIRAC Institute at the University of Washington. \n\nPart of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nPublished - document.pdf
Submitted - 1708.01584.pdf
", "abstract": "The Zwicky Transient Facility is a new robotic-observing program, in which a newly engineered 600-MP digital camera with a pioneeringly large field of view, 47 square degrees, will be installed into the 48-inch Samuel Oschin Telescope at the Palomar Observatory. The camera will generate ~1 petabyte of raw image data over three years of operations. In parallel related work, new hardware and software systems are being developed to process these data in real time and build a long-term archive for the processed products. The first public release of archived products is planned for early 2019, which will include processed images and\nastronomical-source catalogs of the northern sky in the g and r bands. Source catalogs based on two different methods will be generated for the archive: aperture photometry and\npoint-spread-function fitting.", "date": "2018-10-19", "date_type": "published", "pagerange": "329-336", "id_number": "CaltechAUTHORS:20190418-145841579", "isbn": "9780648399605", "book_title": "Robotic Telescope, Student Research and Education Proceedings", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190418-145841579", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "contributors": { "items": [ { "id": "Fitzgerald-M-P", "name": { "family": "Fitzgerald", "given": "M." } }, { "id": "James-C-R", "name": { "family": "James", "given": "C. R." } }, { "id": "Buxner-S", "name": { "family": "Buxner", "given": "S." } }, { "id": "White-S", "name": { "family": "White", "given": "S." } } ] }, "doi": "10.32374/rtsre.2017.031", "primary_object": { "basename": "document.pdf", "url": "https://authors.library.caltech.edu/records/r5ga3-54w68/files/document.pdf" }, "related_objects": [ { "basename": "1708.01584.pdf", "url": "https://authors.library.caltech.edu/records/r5ga3-54w68/files/1708.01584.pdf" } ], "resource_type": "book_section", "pub_year": "2018", "author_list": "Laher, Russ R.; Masci, Frank J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/edp4c-jkp25", "eprint_id": 89366, "eprint_status": "archive", "datestamp": "2023-08-19 09:41:45", "lastmod": "2023-10-18 22:42:01", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stauffer-John-R", "name": { "family": "Stauffer", "given": "John" }, "orcid": "0000-0003-3595-7382" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Benjamin-Robert-A", "name": { "family": "Benjamin", "given": "Robert A." } }, { "id": "Marengo-Massimo", "name": { "family": "Marengo", "given": "Massimo" }, "orcid": "0000-0001-9910-9230" }, { "id": "Kirkpatrick-J-Davy", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "id": "Capak-Peter", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi" }, "orcid": "0000-0002-5619-4938" }, { "id": "Bauer-James-M", "name": { "family": "Bauer", "given": "James M." } }, { "id": "Minniti-Dante", "name": { "family": "Minniti", "given": "Dante" }, "orcid": "0000-0002-7064-099X" }, { "id": "Bally-John", "name": { "family": "Bally", "given": "John" }, "orcid": "0000-0001-8135-6612" }, { "id": "Lodieu-Nicolas", "name": { "family": "Lodieu", "given": "Nicolas" } }, { "id": "Bowler-Brendan-P", "name": { "family": "Bowler", "given": "Brendan" }, "orcid": "0000-0003-2649-2288" }, { "id": "Zhang-ZengHua", "name": { "family": "Zhang", "given": "ZengHua" } }, { "id": "Carey-Sean-J", "name": { "family": "Carey", "given": "Sean J." }, "orcid": "0000-0002-0221-6871" }, { "id": "Milam-Stefanie-N", "name": { "family": "Milam", "given": "Stefanie" }, "orcid": "0000-0001-7694-4129" }, { "id": "Holler-Bryan-J", "name": { "family": "Holler", "given": "Bryan" } } ] }, "title": "The Science Advantage of a Redder Filter for WFIRST", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1806.00554.pdf
", "abstract": "WFIRST will be capable of providing Hubble-quality imaging performance over several thousand square degrees of the sky. The wide-area, high spatial resolution survey data from WFIRST will be unsurpassed for many decades into the future. With the current baseline design, the WFIRST filter complement will extend from the bluest wavelength allowed by the optical design to a reddest filter (F184W) that has a red cutoff at 2.0 microns. In this white paper, we outline some of the science advantages for adding a K_s filter with a 2.15 micron central wavelength in order to extend the wavelength coverage for WFIRST as far to the red as the possible given the thermal performance of the observatory and the sensitivity of the detectors.", "date": "2018-09-04", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20180904-152042633", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-152042633", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.1806.00554", "primary_object": { "basename": "1806.00554.pdf", "url": "https://authors.library.caltech.edu/records/edp4c-jkp25/files/1806.00554.pdf" }, "resource_type": "monograph", "pub_year": "2018", "author_list": "Stauffer, John; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2d6nt-2j991", "eprint_id": 89371, "eprint_status": "archive", "datestamp": "2023-08-19 08:45:48", "lastmod": "2023-10-18 22:42:13", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "Olivier" }, "orcid": "0000-0001-7432-2932" }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher" }, "orcid": "0000-0002-2951-4932" }, { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "id": "Weinberg-D", "name": { "family": "Weinberg", "given": "David" } }, { "id": "Baronchelli-I", "name": { "family": "Baronchelli", "given": "Ivano" }, "orcid": "0000-0003-0556-2929" }, { "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew" }, "orcid": "0000-0001-5501-6008" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Choi-Ami", "name": { "family": "Choi", "given": "Ami" } }, { "id": "Eifler-T-F", "name": { "family": "Eifler", "given": "Tim" }, "orcid": "0000-0002-1894-3301" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" }, { "id": "Ho-Shirley", "name": { "family": "Ho", "given": "Shirley" } }, { "id": "Izard-A", "name": { "family": "Izard", "given": "Albert" } }, { "id": "Jain-B", "name": { "family": "Jain", "given": "Bhuvnesh" } }, { "id": "Jarvis-M", "name": { "family": "Jarvis", "given": "Mike" } }, { "id": "Kiessling-A", "name": { "family": "Kiessling", "given": "Alina" } }, { "id": "Krause-E", "name": { "family": "Krause", "given": "Elisabeth" } }, { "id": "Massara-E", "name": { "family": "Massara", "given": "Elena" } }, { "id": "Masters-D-C", "name": { "family": "Masters", "given": "Dan" }, "orcid": "0000-0001-5382-6138" }, { "id": "Merson-A-I", "name": { "family": "Merson", "given": "Alex" } }, { "id": "Miyatake-Hironao", "name": { "family": "Miyatake", "given": "Hironao" } }, { "id": "Malagon-A-P", "name": { "family": "Malagon", "given": "Andres Plazas" } }, { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "Rachel" }, "orcid": "0000-0003-2271-1527" }, { "id": "Samushia-L", "name": { "family": "Samushia", "given": "Lado" } }, { "id": "Shapiro-C", "name": { "family": "Shapiro", "given": "Chaz" } }, { "id": "Simet-M", "name": { "family": "Simet", "given": "Melanie" } }, { "id": "Spergel-D-N", "name": { "family": "Spergel", "given": "David" }, "orcid": "0000-0002-5151-0006" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry" }, "orcid": "0000-0002-7064-5424" }, { "id": "Troxel-M", "name": { "family": "Troxel", "given": "Michael" } }, { "id": "Bean-R", "name": { "family": "Bean", "given": "Rachel" } }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "James" } }, { "id": "Heinrich-Chen-He", "name": { "family": "Heinrich", "given": "Chen He" } }, { "id": "Heitmann-K", "name": { "family": "Heitmann", "given": "Katrin" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hudson-M-J", "name": { "family": "Hudson", "given": "Michael" } }, { "id": "Huff-E-M", "name": { "family": "Huff", "given": "Eric" }, "orcid": "0000-0002-9378-3424" }, { "id": "Leauthaud-A", "name": { "family": "Leauthaud", "given": "Alexie" }, "orcid": "0000-0002-3677-3617" }, { "id": "MacCrann-N", "name": { "family": "MacCrann", "given": "Niall" } }, { "id": "Padmanabhan-N", "name": { "family": "Padmanabhan", "given": "Nikhil" } }, { "id": "Pisani-A", "name": { "family": "Pisani", "given": "Alice" } }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Rozo-E", "name": { "family": "Rozo", "given": "Eduardo" } }, { "id": "Seiffert-M", "name": { "family": "Seiffert", "given": "Mike" } }, { "id": "Smith-Kendrick", "name": { "family": "Smith", "given": "Kendrick" } }, { "id": "Takada-Masahiro", "name": { "family": "Takada", "given": "Masahiro" } }, { "id": "von-der-Linden-A", "name": { "family": "von der Linden", "given": "Anja" } }, { "id": "Lupton-R-H", "name": { "family": "Lupton", "given": "Robert" }, "orcid": "0000-0003-1666-0962" }, { "id": "Yoshida-Naoki", "name": { "family": "Yoshida", "given": "Naoki" } }, { "id": "Wu-Hao-Yi", "name": { "family": "Wu", "given": "Hao-Yi" } }, { "id": "Zu-Ying", "name": { "family": "Zu", "given": "Ying" } } ] }, "title": "WFIRST Science Investigation Team \"Cosmology with the High Latitude Survey\" Annual Report 2017", "ispublished": "unpub", "full_text_status": "public", "note": "We warmly thank our colleagues from the WFIRST Project Office and all the Science Investigation Teams for continuous constructive and stimulating interactions. We acknowledge use of the Annual Review of Astronomy and Astrophysics LaTeX template as a basis for our report. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The decision to implement the WFIRST mission will not be finalized until NASA's completion of the National Environmental Policy Act (NEPA) process. This document is being made available for information purposes only.\n\nSubmitted - 1804.03628.pdf
", "abstract": "Cosmic acceleration is the most surprising cosmological discovery in many decades. Testing and distinguishing among possible explanations requires cosmological measurements of extremely high precision probing the full history of cosmic expansion and structure growth and, ideally, compare and contrast matter and relativistic tracers of the gravity potential. This program is one of the defining objectives of the Wide-Field Infrared Survey Telescope (WFIRST), as set forth in the New Worlds, New Horizons report (NWNH) in 2010. The WFIRST mission has the ability to improve these measurements by 1-2 orders of magnitude compared to the current state of the art, while simultaneously extending their redshift grasp, greatly improving control of systematic effects, and taking a unified approach to multiple probes that provide complementary physical information and cross-checks of cosmological results. We describe in this annual report the activities of the Science Investigation Team (SIT) \"Cosmology with the High Latitude Survey (HLS)\" during the year 2017. This team was selected by NASA in December 2015 in order to address the stringent challenges of the WFIRST dark energy (DE) program through the Project's formulation phase. This SIT has elected to jointly address Galaxy Redshift Survey, Weak Lensing and Cluster Growth and thus fully embrace the fact that the imaging and spectroscopic elements of the HLS will be realized as an integrated observing program, and they jointly impose requirements on performance and operations. WFIRST is designed to be able to deliver a definitive result on the origin of cosmic acceleration. It is not optimized for Figure of Merit sensitivity but for control of systematic uncertainties and for having multiple techniques each with multiple cross-checks. Our SIT work focuses on understanding the potential systematics in the WFIRST DE measurements.", "date": "2018-09-04", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20180904-161455265", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-161455265", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.1804.03628", "primary_object": { "basename": "1804.03628.pdf", "url": "https://authors.library.caltech.edu/records/2d6nt-2j991/files/1804.03628.pdf" }, "resource_type": "monograph", "pub_year": "2018", "author_list": "Dor\u00e9, Olivier; Hirata, Christopher; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9ap0e-kpw63", "eprint_id": 99178, "eprint_status": "archive", "datestamp": "2023-08-19 11:10:58", "lastmod": "2024-01-14 21:59:21", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Content-R", "name": { "family": "Content", "given": "Robert" } }, { "id": "Wang-Yun", "name": { "family": "Wang", "given": "Yun" } }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne" } }, { "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "orcid": "0000-0003-4269-260X" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga" }, "orcid": "0000-0001-7583-0621" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "ATLAS probe for the study of galaxy evolution with 300,000,000 galaxy spectra", "ispublished": "unpub", "full_text_status": "public", "keywords": "Space telescope, NIR spectroscopy, Digital Micro-mirror Devices, prism spectroscopy, Multi-Object Spectroscopy", "note": "\u00a9 2018 Society of Photo-Optical Instrumentation Engineers (SPIE).\n\nPublished - 106980I.pdf
", "abstract": "ATLAS (Astrophysics Telescope for Large Area Spectroscopy) Probe is a mission concept for a NASA probe-class space mission with primary science goal the definitive study of galaxy evolution through the capture of 300,000,000 galaxy spectra up to z=7. It is made of a 1.5-m Ritchey-Chretien telescope with a field of view of solid angle 0.4 deg^2. The wavelength range is at least 1 \u03bcm to 4 \u03bcm with a goal of 0.9 \u03bcm to 5 \u03bcm. Average resolution is 600 but with a possible trade-off to get 1000 at the longer wavelengths. The ATLAS Probe instrument is made of 4 identical spectrographs each using a Digital Micro-mirror Device (DMD) as a multi-object mask. It builds on the work done for the ESA SPACE and Phase-A EUCLID projects. Three-mirror fore-optics re-image each sub-field on its DMD which has 2048 x 1080 mirrors 13.6 \u03bcm wide with 2 possible tilts, one sending light to the spectrograph, the other to a light dump. The ATLAS Probe spectrographs use prisms as dispersive elements because of their higher and more uniform transmission, their larger bandwidth, and the ability to control the resolution slope with the choice of glasses. Each spectrograph has 2 cameras. While the collimator is made of 4 mirrors, each camera is made of only one mirror which reduces the total number of optics. All mirrors are aspheric but with a relatively small P-V with respect to their best fit sphere making them easily manufacturable. For imaging, a simple mirror to replace the prism is not an option because the aberrations are globally corrected by the collimator and camera together which gives large aberrations when the mirror is inserted. An achromatic grism is used instead. There are many variations of the design that permit very different packaging of the optics. ATLAS Probe will enable ground-breaking science in all areas of astrophysics. It will (1) revolutionize galaxy evolution studies by tracing the relation between galaxies and dark matter from the local group to cosmic voids and filaments, from the epoch of reionization through the peak era of galaxy assembly; (2) open a new window into the dark universe by mapping the dark matter filaments to unveil the nature of the dark Universe using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of gravity using cosmic large-scale structure; (3) probe the Milky Way's dust-shrouded regions, reaching the far side of our Galaxy; and (4) characterize asteroids and other objects in the outer solar systems.", "date": "2018-08-22", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 106980I", "id_number": "CaltechAUTHORS:20191009-090203213", "isbn": "9781510619494", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191009-090203213", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "contributors": { "items": [ { "id": "Lystrup-M", "name": { "family": "Lystrup", "given": "Makenzie" } }, { "id": "MacEwen-H-A", "name": { "family": "MacEwen", "given": "Howard A." } }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "Giovanni G." } }, { "id": "Batalha-N-M", "name": { "family": "Batalha", "given": "Natalie" } }, { "id": "Siegler-N", "name": { "family": "Siegler", "given": "Nicholas" } }, { "id": "Tong-Edward-C", "name": { "family": "Tong", "given": "Edward C." } } ] }, "doi": "10.1117/12.2313082", "primary_object": { "basename": "106980I.pdf", "url": "https://authors.library.caltech.edu/records/9ap0e-kpw63/files/106980I.pdf" }, "resource_type": "book_section", "pub_year": "2018", "author_list": "Content, Robert; Wang, Yun; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cwbz4-59w53", "eprint_id": 88472, "eprint_status": "archive", "datestamp": "2023-08-21 23:42:08", "lastmod": "2023-10-18 22:05:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Linden-S-T", "name": { "family": "Linden", "given": "S. T." }, "orcid": "0000-0002-1000-6081" }, { "id": "Dong-Dillon", "name": { "family": "Dong", "given": "D." }, "orcid": "0000-0001-9584-2531" }, { "id": "Hensley-B-S", "name": { "family": "Hensley", "given": "B. S." }, "orcid": "0000-0001-7449-4638" }, { "id": "Momjian-E", "name": { "family": "Momjian", "given": "E." }, "orcid": "0000-0003-3168-5922" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Evans-A-S", "name": { "family": "Evans", "given": "A. S." }, "orcid": "0000-0003-2638-1334" } ] }, "title": "A New Detection of Extragalactic Anomalous Microwave Emission in a Compact, Optically Faint Region of NGC 4725", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (NGC 4725); H ii regions; radio continuum: general; stars: formation", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2018 April 20; revised 2018 May 11; accepted 2018 May 15; published 2018 July 18. \n\nWe would like to thank the anonymous referee for very useful comments that helped to improve the content and presentation of this paper. E.J.M. thanks J. J. Condon and B. T. Draine for useful discussions that helped improve the paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This 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.\n\nPublished - Murphy_2018_ApJ_862_20.pdf
Accepted Version - 1805.05965
", "abstract": "We discuss the nature of a discrete, compact radio source (NGC 4725 B) located \u22481.9 kpc from the nucleus in the nearby star-forming galaxy NGC 4725, which we believe to be a new detection of extragalactic anomalous microwave emission (AME). Based on detections at 3, 15, 22, 33, and 44 GHz, NGC 4725 B is a microjansky radio source peaking at \u224833 GHz. While the source is not identified in optical (BVRI) photometry, we detect counterparts in the midinfrared Spitzer/IRAC bands (3.6, 4.5, 5.8, 8.0 \u03bcm) that appear to be associated with dust emission in the central region of NGC 4725. Consequently, we conclude that NGC 4725 B is a new detection of AME and is very similar to a recent detection of AME in an outer-disk star-forming region in NGC 6946. We find that models of electric dipole emission from rapidly rotating ultra-small grains are able to reproduce the radio spectrum for reasonable interstellar medium conditions. Given the lack of an optical counterpart and the shape of the radio spectrum, NGC 4725 B appears consistent with a nascent star-forming region in which young (\u227e 3 Myr) massive stars are still highly enshrouded by their natal cocoons of gas and dust with insufficient supernovae occurring to produce a measurable amount of synchrotron emission.", "date": "2018-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "862", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 20", "id_number": "CaltechAUTHORS:20180801-142726478", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-142726478", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aac5f5", "primary_object": { "basename": "1805.05965", "url": "https://authors.library.caltech.edu/records/cwbz4-59w53/files/1805.05965" }, "related_objects": [ { "basename": "Murphy_2018_ApJ_862_20.pdf", "url": "https://authors.library.caltech.edu/records/cwbz4-59w53/files/Murphy_2018_ApJ_862_20.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Murphy, E. J.; Linden, S. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kqaa8-1r756", "eprint_id": 85481, "eprint_status": "archive", "datestamp": "2023-08-21 22:57:22", "lastmod": "2023-10-18 18:15:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Peterson-B-W", "name": { "family": "Peterson", "given": "B. W." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Bitsakis-T", "name": { "family": "Bitsakis", "given": "T." }, "orcid": "0000-0001-5787-8242" }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "P." }, "orcid": "0000-0002-2421-1350" }, { "id": "Alatalo-K", "name": { "family": "Alatalo", "given": "K." }, "orcid": "0000-0002-4261-2326" }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "F." } }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "M." }, "orcid": "0000-0002-9871-6490" }, { "id": "Duc-P-A", "name": { "family": "Duc", "given": "P.-A." } }, { "id": "Falgarone-E", "name": { "family": "Falgarone", "given": "E." } }, { "id": "Gallagher-S-C", "name": { "family": "Gallagher", "given": "S." } }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Y." }, "orcid": "0000-0003-0007-2197" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Joshi-B", "name": { "family": "Joshi", "given": "B." } }, { "id": "Lisenfeld-U", "name": { "family": "Lisenfeld", "given": "U." }, "orcid": "0000-0002-9471-5423" }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Pineau-des-For\u00eats-G", "name": { "family": "Pineau des For\u00eats", "given": "G." } }, { "id": "van-der-Werf-P-P", "name": { "family": "van der Werf", "given": "P." }, "orcid": "0000-0001-5434-5942" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" } ] }, "title": "Herschel Spectroscopy of the Taffy Galaxies (UGC 12914/12915 = VV 254): Enhanced [C II] Emission in the Collisionally Formed Bridge", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (UGC 12914, UGC 12915); galaxies: interactions; intergalactic medium", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2018 January 4; accepted 2018 January 29; published 2018 March 16. \n\nThis work is based on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. B.W.P. also thanks the UW-BC Foundation for its generous support. U.L. acknowledges support by the research projects AYA2014-53506-P from the Spanish Ministerio de Econom\u00eda y Competitividad, from the European Regional Development Funds (FEDER) and the Junta de Andaluc\u00eda (Spain) grants FQM108. N.L. acknowledges support by National Key R&D Program of China, #2017YFA0402704 and NSFC #11673028. Y.G. acknowledges support by National Key R&D Program of China (2017YFA0402704), the NSFC #11420101002 and the CAS Key Research Program of Frontier Sciences.\n\nPublished - Peterson_2018_ApJ_855_141.pdf
Accepted Version - 1801.10230
", "abstract": "Using the PACS and SPIRE spectrometers on board Herschel, we obtained observations of the Taffy galaxies (UGC 12914/12915) and bridge. The Taffy system is believed to be the result of a face-on collision between two gas-rich galaxies, in which the stellar disks passed through each other, but the gas was dispersed into a massive H i and molecular bridge between them. Emission is detected and mapped in both galaxies and the bridge in the [C ii]157.7 \u03bcm and [O i]63.2 \u03bcm fine-structure lines. Additionally, SPIRE FTS spectroscopy detects the [C i] ^3P_2 \u2192 ^3p_1(809.3 GHz) and [C i] ^3P_1 \u2192 ^3p_0(492.2 GHz) neutral carbon lines, and weakly detects high-J CO transitions in the bridge. These results indicate that the bridge is composed of a warm multi-phase medium consistent with shock and turbulent heating. Despite low star formation rates in the bridge, the [C ii] emission appears to be enhanced, reaching [C ii]/FIR ratios of 3.3% in parts of the bridge. Both the [C ii] and [O i] lines show broad intrinsic multi-component profiles, similar to those seen in previous CO (1\u20130) and H i observations. The [C ii] emission shares similar line profiles with both the double-peaked H i profiles and shares a high-velocity component with single-peaked CO profiles in the bridge, suggesting that the [C ii] emission originates in both the neutral and molecular phases. We show that it is feasible that a combination of turbulently heated H_2 and high column-density H i, resulting from the galaxy collision, is responsible for the enhanced [C ii] emission.", "date": "2018-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "855", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 141", "id_number": "CaltechAUTHORS:20180328-133308085", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180328-133308085", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "UW-Barron County Foundation" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "AYA2014-53506-P" }, { "agency": "Fondo Europeo de Desarrollo Regional (FEDER)" }, { "agency": "Junta de Andaluc\u00eda", "grant_number": "FQM108" }, { "agency": "China National R&D Program", "grant_number": "2017YFA0402704" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11673028" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11420101002" }, { "agency": "Chinese Academy of Sciences" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aaac2c", "primary_object": { "basename": "1801.10230", "url": "https://authors.library.caltech.edu/records/kqaa8-1r756/files/1801.10230" }, "related_objects": [ { "basename": "Peterson_2018_ApJ_855_141.pdf", "url": "https://authors.library.caltech.edu/records/kqaa8-1r756/files/Peterson_2018_ApJ_855_141.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Peterson, B. W.; Appleton, P. N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jnv0t-d6y26", "eprint_id": 84645, "eprint_status": "archive", "datestamp": "2023-08-21 22:44:15", "lastmod": "2023-10-18 16:25:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Gu-Qiusheng", "name": { "family": "Gu", "given": "Qiusheng" }, "orcid": "0000-0002-3890-3729" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Qiu-Keping", "name": { "family": "Qiu", "given": "Keping" }, "orcid": "0000-0002-5093-5088" }, { "id": "Gwyn-S", "name": { "family": "Gwyn", "given": "Stephen" } }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" }, { "id": "Fang-Min", "name": { "family": "Fang", "given": "Min" }, "orcid": "0000-0001-8060-1321" }, { "id": "Chen-Yanmei", "name": { "family": "Chen", "given": "Yanmei" } }, { "id": "Zhou-Luwenjia", "name": { "family": "Zhou", "given": "Luwenjia" } }, { "id": "Wu-Jingwen", "name": { "family": "Wu", "given": "Jingwen" }, "orcid": "0000-0001-7808-3756" }, { "id": "Zheng-Xianzhong", "name": { "family": "Zheng", "given": "Xianzhong" }, "orcid": "0000-0003-3728-9912" }, { "id": "Zhang-Zhi-Yu", "name": { "family": "Zhang", "given": "Zhi-Yu" }, "orcid": "0000-0002-7299-2876" }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Yu" }, "orcid": "0000-0003-0007-2197" }, { "id": "Wang-Junzhi", "name": { "family": "Wang", "given": "Junzhi" } } ] }, "title": "Revisiting the Extended Schmidt Law: The Important Role of Existing Stars in Regulating Star Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst; ISM: atoms; ISM: molecules; stars: formation", "note": "\u00a9 2018 American Astronomical Society.\n\nReceived 2017 August 8. Accepted 2017 December 19. Published 2018 February 1. \n\nWe thank the anonymous referee for the helpful and constructive suggestions that improved the quality of the paper, Eve Ostriker for discussions of their model and Pereira-Santaella for providing their measurements of SFRs and gas mass of IC 4687. The work is supported by the National Key R&D Program of China (No. 2017YFA0402704) and the National Natural Science Foundation of China (NSFC grants 11773013, 11733002, and 11373021) and the Excellent Youth Foundation of the Jiangsu Scientific Committee (BK20150014). K.Q. acknowledges the support from NSFC (11473011 and 11590781). This work is based on observations obtained at the Canada\u2013France\u2013Hawaii Telescope (CFHT), which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. The GALEX is a NASA Small Explorer. The mission was developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00182.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research has made use of the NASA/IPAC Extra-galactic 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 - Shi_2018_ApJ_853_149.pdf
Submitted - 1801.00888.pdf
", "abstract": "We revisit the proposed extended Schmidt law, which posits that the star formation efficiency in galaxies depends on the stellar mass surface density, by investigating spatially resolved star formation rates (SFRs), gas masses, and stellar masses of star formation regions in a vast range of galactic environments, from the outer disks of dwarf galaxies, to spiral disks and to merging galaxies, as well as individual molecular clouds in M33. We find that these regions are distributed in a tight power law as \u03a3 _SFR \u221d (\u03a3_(star)^0.5 \u03a3__gas)^(1.09), which is also valid for the integrated measurements of disk and merging galaxies at high-z. Interestingly, we show that star formation regions in the outer disks of dwarf galaxies with \u03a3_(SFR) down to 10^(\u22125) M_ \u2299 yr^(\u22121) kpc^(\u22122), which are outliers of both the Kennicutt\u2013Schmidt and Silk\u2013Elmegreen laws, also follow the extended Schmidt law. Other outliers in the Kennicutt\u2013Schmidt law, such as extremely metal-poor star formation regions, also show significantly reduced deviation from the extended Schmidt law. These results suggest an important role for existing stars in helping to regulate star formation through the effect of their gravity on the midplane pressure in a wide range of galactic environments.", "date": "2018-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "853", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 149", "id_number": "CaltechAUTHORS:20180202-082630507", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180202-082630507", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "China National R&D Program", "grant_number": "2017YFA0402704" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11773013" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11733002" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11373021" }, { "agency": "Jiangsu Scientific Committee Excellent Youth Foundation", "grant_number": "BK20150014" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11473011" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11590781" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aaa3e6", "primary_object": { "basename": "1801.00888.pdf", "url": "https://authors.library.caltech.edu/records/jnv0t-d6y26/files/1801.00888.pdf" }, "related_objects": [ { "basename": "Shi_2018_ApJ_853_149.pdf", "url": "https://authors.library.caltech.edu/records/jnv0t-d6y26/files/Shi_2018_ApJ_853_149.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Shi, Yong; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zeqjz-dd973", "eprint_id": 81916, "eprint_status": "archive", "datestamp": "2023-08-19 06:58:25", "lastmod": "2023-10-17 21:55:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cook-D-O", "name": { "family": "Cook", "given": "D. O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Lau-Ryan-M", "name": { "family": "Lau", "given": "R. M." } }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "J. E." }, "orcid": "0000-0001-5754-4007" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "S. M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Cannella-C-B", "name": { "family": "Cannella", "given": "C." }, "orcid": "0000-0003-2667-7290" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "K." }, "orcid": "0000-0002-8989-0542" }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "G." }, "orcid": "0000-0002-7083-4049" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "F." }, "orcid": "0000-0003-2992-8024" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "A. Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Madsen-K-K", "name": { "family": "Madsen", "given": "K." }, "orcid": "0000-0003-1252-4891" }, { "id": "Xu-Yong", "name": { "family": "Xu", "given": "Y." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Illuminating Gravitational Waves: A Concordant Picture of Photons from a Neutron Star Merger", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Association for the Advancement of Science.\n\n14 September 2017; accepted 5 October 2017; Published online 16 October 2017.\n\nWe thank Iva Kostadinova for seamlessly coordinating the GROWTH (Global Relay of Observatories Watching Transients Happen) program and Britt Griswold for beautiful graphic arts. We thank Patricia Whitelock for facilitating IRSF observations. We thank Scott Barthelmy for setting up an LVC GCN system that facilitated quick, citable communication between astronomers and maximized the science return. We thank Sterl Phinney, Shri Kulkarni and Lars Bildsten for valuable comments. We thank the staff of Gemini Observatory, in particular the director Laura Ferrarese for rapidly approving our Director's Discretionary Time request, and our program contact scientists Mischa Shirmer, Hwihyun Kim, Karleyne Silva, Morten Andersen, and Ricardo Salinas for supporting and executing observations. We especially grateful to Gemini for postponing scheduled maintenance on the FLAMINGOS-2 instrument in order to obtain as much data as possible on this extraordinary event. This work was supported by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation under PIRE Grant No 1545949. GROWTH is a collaborative project among California Institute of Technology (USA), University of Maryland College Park (USA), University of Wisconsin Milwaukee (USA), Texas Tech University (USA), San Diego State University (USA), Los Alamos National Laboratory (USA), Tokyo Institute of Technology (Japan), National Central University (Taiwan), Indian Institute of Astrophysics (India), Inter-University Center for Astronomy and Astrophysics (India), Weizmann Institute of Science (Israel), The Oskar Klein Centre at Stockholm University (Sweden), Humboldt University (Germany), Liverpool John Moores University (UK). Full facility and funding acknowledgements are provided in the supplementary materials. The photometric data we used are tabulated in table S1. All of our raw observations are available in observatory archives; URLs and project numbers are provided in the supplementary materials. The PLUTO software used for our simulations is available at http://plutocode.ph.unito.it/; our simulation input and output files are provided as data S1 and S2.\n\nGemini observatory data were obtained primarily under programs GS-2017B-DD-1 and GS-2017B-DD-6 (PI L. P. Singer) and is available at https://archive.gemini.edu. CTIO1.3m data obtained under program NOAO 2017B-0160 (PI B. Cobb) is available at http://archive.noao.edu/.\nHubble Space Telescope data obtained under program HST-GO-15436 (PI M. M. Kasliwal) is available at https://archive.stsci.edu/. Keck Observatory data (PI G. Hallinan) is available at\nhttps://koa.ipac.caltech.edu/. VLT data is available at http://archive.eso.org/. The data of GALEX presented in this paper were obtained from the Mikulski Archive for\nSpace Telescopes (MAST). STScI is operated by the Association of Universities for Research\nin Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants\nand contracts. PS1: The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project\nOffice, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy,\nHeidelberg 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\nGlobal 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\nDirectorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). 2MASS: This publication makes use\nof 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\nFoundation. WISE: This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics\nand Space Administration. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of\nTechnology, under contract with the National Aeronautics and Space Administration. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with\nthe National Science Foundation. PYRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. Some observations were obtained at the Gemini\nObservatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT\n(Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil). A.H. acknowledges support by the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation. T.M. acknowledges the support of the Australian Research\nCouncil through grant FT150100099. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through\nproject number CE110001020. The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. D.L.K. is additionally supported by NSF grant AST-1412421. A.A.M. is funded by the Large Synoptic Survey Telescope Corporation in support of the Data Science Fellowship Program. P.C.Y., C.C.N. and W.H.I. thank the support from grant MOST104-2923-M-008-004-MY5 and MOST106-2112-M-008-007. A.C. acknowledges\nsupport from the National Science Foundation CAREER award 1455090, \"CAREER: Radio and gravitational-wave emission from the largest explosions since the Big Bang\". T.P. acknowledges the support of Advanced ERC grant TReX and the Templeton Foundation. B.E.C, thanks SMARTS 1.3-m Queue Manager Bryndis Cruz for prompt scheduling of the SMARTS observations. Basic research in radio astronomy at the Naval Research Laboratory (NRL) is funded by 6.1 Base funding. Construction and installation of VLITE was supported by NRL Sustainment Restoration and Maintenance funding. K.P.M's research is supported by the Oxford Centre for Astrophysical Surveys which is funded through the Hintze Family Charitable Foundation. J.S. and A.G. are grateful for support from the Knut and Alice Wallenberg Foundation. Together with S.R they are also supported by the research environment grant \"Gravitational Radiation and\nElectromagnetic Astrophysical Transients (GREAT)\" funded by the Swedish Research Council (VR) under Dnr 2016-06012. S.R. has also been supported by VR (grant number 2016-\n036573), and by the Swedish National Space Board (107/16). E.O.O. is grateful for the support by grants from the Israel Science Foundation, Minerva, Israeli ministry of Science, the US Israel Binational Science Foundation, and the I-CORE Program of the Planning and Budgeting\nCommittee and The Israel Science Foundation. We thank the staff of the GMRT that made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. A.Y.Q.H. was supported by a National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. J.E.J. acknowledges supported by the National Science Foundation Graduate Research Fellowship under grant\nno. DGE-1144469. S.G. acknowledges support from NSF Award PHY-1607585. G.C.A. and V.B. acknowledge the support of the Science and Engineering Research Board, Department of\nScience and Technology, India and the Indo-US Science and Technology Foundation for the GROWTH-India project. J.B. acknowledges support from the Einstein Fellowship grant PF7-180162. N.K., R.I. and Y.Y. acknowledge the support of Japan Society for the Promotion of Science for the GROWTH project. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics in 3D (ASTRO 3D)\nthrough project number CE170100013. F.R. acknowledges support from the U.S. Department of Energy Early Career Award DE-SC0012160 \"Scalable and Energy-Efficient Methods for Interactive Exploration of Scientific Data.\" E.N. and O.G. acknowledge the support of an ERC starting grant (GRB/SN) and an ISF grant (1277/13). P.E.N. acknowledges support from the DOE through DE-FOA-0001088, \"Analytical Modeling for Extreme-Scale Computing Environments.\"\nThis 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.\n\nSubmitted - 1710.05436.pdf
Supplemental Material - aap9455_Kasliwal_SM.pdf
Supplemental Material - aap9455_Kasliwal_SM_data_S1.zip
Supplemental Material - aap9455_Kasliwal_SM_data_S2.zip
Supplemental Material - aap9455_Kasliwal_SM_interactive_light_curve.zip
Supplemental Material - aap9455_Kasliwal_SM_movie_S1.mp4
", "abstract": "Merging neutron stars offer an exquisite laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) to gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic dataset, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma-rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultra-relativistic jets. Instead, we suggest that breakout of a wide-angle, mildly-relativistic cocoon engulfing the jet elegantly explains the low-luminosity gamma-rays, the high-luminosity ultraviolet-optical-infrared and the delayed radio/x-ray emission. We posit that all merging neutron stars may lead to a wide-angle cocoon breakout; sometimes accompanied by a successful jet and sometimes a choked jet.", "date": "2017-12-22", "date_type": "published", "publication": "Science", "volume": "358", "number": "6370", "publisher": "American Association for the Advancement of Science", "pagerange": "1559-1565", "id_number": "CaltechAUTHORS:20170929-091827113", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170929-091827113", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA", "grant_number": "NNX09AF08G" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "I-Core Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation" }, { "agency": "Australian Research Council", "grant_number": "FT150100099" }, { "agency": "Australian Research Council", "grant_number": "CE110001020" }, { "agency": "Australian Government" }, { "agency": "NSF", "grant_number": "AST-1412421" }, { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2923-M-008-004-MY5" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "106-2112-M-008-007" }, { "agency": "NSF", "grant_number": "AST-1455090" }, { "agency": "European Research Council (ERC)", "grant_number": "TReX" }, { "agency": "John Templeton Foundation" }, { "agency": "Naval Research Laboratory", "grant_number": "6.1 Base funding" }, { "agency": "Hintze Family Charitable Foundation" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council", "grant_number": "Dnr 2016-06012" }, { "agency": "Swedish Research Council", "grant_number": "2016-036573" }, { "agency": "Swedish National Space Board", "grant_number": "107/16" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Israeli Ministry of Science" }, { "agency": "US-Israel Binational Science Foundation" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NSF", "grant_number": "PHY-1607585" }, { "agency": "Science and Engineering Research Board (SERB)" }, { "agency": "Department of Science and Technology (India)" }, { "agency": "Indo-US Science and Technology Foundation" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF7-180162" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "Indian Space Research Organisation" }, { "agency": "Australian Research Council", "grant_number": "CE170100013" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0012160" }, { "agency": "European Research Council (ERC)" }, { "agency": "Israel Science Foundation", "grant_number": "1277/13" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FOA-0001088" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1126/science.aap9455", "primary_object": { "basename": "1710.05436.pdf", "url": "https://authors.library.caltech.edu/records/zeqjz-dd973/files/1710.05436.pdf" }, "related_objects": [ { "basename": "aap9455_Kasliwal_SM.pdf", "url": "https://authors.library.caltech.edu/records/zeqjz-dd973/files/aap9455_Kasliwal_SM.pdf" }, { "basename": "aap9455_Kasliwal_SM_data_S1.zip", "url": "https://authors.library.caltech.edu/records/zeqjz-dd973/files/aap9455_Kasliwal_SM_data_S1.zip" }, { "basename": "aap9455_Kasliwal_SM_data_S2.zip", "url": "https://authors.library.caltech.edu/records/zeqjz-dd973/files/aap9455_Kasliwal_SM_data_S2.zip" }, { "basename": "aap9455_Kasliwal_SM_interactive_light_curve.zip", "url": "https://authors.library.caltech.edu/records/zeqjz-dd973/files/aap9455_Kasliwal_SM_interactive_light_curve.zip" }, { "basename": "aap9455_Kasliwal_SM_movie_S1.mp4", "url": "https://authors.library.caltech.edu/records/zeqjz-dd973/files/aap9455_Kasliwal_SM_movie_S1.mp4" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Kasliwal, M. M.; Cook, D. O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/sd3sx-ggq65", "eprint_id": 83792, "eprint_status": "archive", "datestamp": "2023-08-19 06:20:12", "lastmod": "2023-10-17 23:30:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "Jason" }, "orcid": "0000-0002-4485-8549" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hemmati-S", "name": { "family": "Hemmati", "given": "Shoubaneh" }, "orcid": "0000-0003-2226-5395" } ] }, "title": "Scientific Synergy between LSST and Euclid", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters \u2013 cosmology: dark energy \u2013 galaxies: clusters: general \u2013 gravitational lensing:\nweak \u2013 surveys \u2013 telescopes", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 July 31; revised 2017 October 17; accepted 2017 October 18; published 2017 December 7. \n\nJ.R. and A.K. were supported by JPL, which is run under a contract for NASA by Caltech. J.R., A.K., P.C., R.B., R.L., and R. Mandelbaum were supported in part by NASA ROSES grant 12-EUCLID12-0004. A.N.T. is supported by a UK Space Agency Euclid grant and a Royal Society Wolfson Research Merit Award. Y.M. was supported by the French CNES Space Agency and Institut National des Sciences de l'Univers of CNRS. T.S. acknowledges travel support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project No. 50QE1103. T.K. is supported by a Royal Society University Research Fellowship. V.F.C. is funded by the Italian Space Agency (ASI) through contract Euclid\u2014IC (I/031/10/0) and acknowledges financial contribution from the agreement ASI/INAF/I/023/12/0. R. Massey acknowledges support from UK STFC grant ST/N001494/1. B.N. is supported by a UK Space Agency Euclid grant. This paper benefited from ideas developed in the UK Dark Energy Strategy 2020 Document.(37) We thank Michael Brown, Elisa Chisari, Henk Hoekstra, \u017deljko Ivezi\u0107 Bhuvnesh Jain, Roberto Scaramella, and Peter Schneider for useful feedback on this paper. We thank Katrin Heitmann for useful discussions on high-performance computing. We thank the anonymous referee for useful suggestions on adding quantitative rigor to sections of this paper and useful feedback on the structure of the paper.\n\nPublished - Rhodes_2017_ApJS_233_21.pdf
Submitted - 1710.08489.pdf
", "abstract": "Euclid and the Large Synoptic Survey Telescope (LSST) are poised to dramatically change the astronomy landscape early in the next decade. The combination of high-cadence, deep, wide-field optical photometry from LSST with high-resolution, wide-field optical photometry, and near-infrared photometry and spectroscopy from Euclid will be powerful for addressing a wide range of astrophysical questions. We explore Euclid/LSST synergy, ignoring the political issues associated with data access to focus on the scientific, technical, and financial benefits of coordination. We focus primarily on dark energy cosmology, but also discuss galaxy evolution, transient objects, solar system science, and galaxy cluster studies. We concentrate on synergies that require coordination in cadence or survey overlap, or would benefit from pixel-level co-processing that is beyond the scope of what is currently planned, rather than scientific programs that could be accomplished only at the catalog level without coordination in data processing or survey strategies. We provide two quantitative examples of scientific synergies: the decrease in photo-z errors (benefiting many science cases) when high-resolution Euclid data are used for LSST photo-z determination, and the resulting increase in weak-lensing signal-to-noise ratio from smaller photo-z errors. We briefly discuss other areas of coordination, including high-performance computing resources and calibration data. Finally, we address concerns about the loss of independence and potential cross-checks between the two missions and the potential consequences of not collaborating.", "date": "2017-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "233", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 21", "id_number": "CaltechAUTHORS:20171211-101259862", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171211-101259862", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "12-EUCLID12-0004" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Royal Society" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Bundesministerium f\u00fcr Wirtschaft und Energie (BMWi)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50QE1103" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/031/10/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/023/12/0" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N001494/1" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4365/aa96b0", "primary_object": { "basename": "1710.08489.pdf", "url": "https://authors.library.caltech.edu/records/sd3sx-ggq65/files/1710.08489.pdf" }, "related_objects": [ { "basename": "Rhodes_2017_ApJS_233_21.pdf", "url": "https://authors.library.caltech.edu/records/sd3sx-ggq65/files/Rhodes_2017_ApJS_233_21.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Rhodes, Jason; Capak, Peter; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1jcb4-hae18", "eprint_id": 96875, "eprint_status": "archive", "datestamp": "2023-08-19 05:53:00", "lastmod": "2023-10-20 21:35:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. LII. Planet flux densities", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 planets and satellites: general", "note": "\u00a9 2017 ESO. Article published by EDP Sciences.\n\nReceived 21 December 2016; Accepted 30 March 2017; Published online 27 November 2017.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSUIN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. The authors thank Lyman Page for useful discussion. J.E. Gudmundsson acknowledges support through a grant from the Swedish Research Council (Contract No. 638-2013-8993).\n\nPublished - aa30311-16.pdf
Submitted - 1612.07151.pdf
", "abstract": "Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100\u2013857\u2009GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70\u2009GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of \u03b2_(ring) = 2.30 \u00b1 0.03 over the 30\u20131000\u2009GHz frequency range. Estimates of the polarization amplitude of the planets have also been made in the four bands that have polarization-sensitive detectors (100\u2013353\u2009GHz); this analysis provides a 95% confidence level upper limit on Mars's polarization of 1.8, 1.7, 1.2, and 1.7% at 100, 143, 217, and 353\u2009GHz, respectively. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353\u2009GHz) is 1.004, 1.002, 1.021, and 1.033 for 100, 143, 217, and 353\u2009GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2%. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.", "date": "2017-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "607", "publisher": "EDP Sciences", "pagerange": "Art. No. A122", "id_number": "CaltechAUTHORS:20190702-090414194", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190702-090414194", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201630311", "primary_object": { "basename": "1612.07151.pdf", "url": "https://authors.library.caltech.edu/records/1jcb4-hae18/files/1612.07151.pdf" }, "related_objects": [ { "basename": "aa30311-16.pdf", "url": "https://authors.library.caltech.edu/records/1jcb4-hae18/files/aa30311-16.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Akrami, Y.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jbtqq-f3r28", "eprint_id": 76663, "eprint_status": "archive", "datestamp": "2023-08-19 02:40:22", "lastmod": "2023-10-25 16:11:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob E." }, "orcid": "0000-0001-5754-4007" }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Cook-D-O", "name": { "family": "Cook", "given": "David O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Lau-Ryan-M", "name": { "family": "Lau", "given": "Ryan M." } }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "O'Sullivan-Donal", "name": { "family": "O'Sullivan", "given": "Donal" }, "orcid": "0000-0002-4959-9179" }, { "id": "Perez-Andres", "name": { "family": "Perez", "given": "Andres" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" } ] }, "title": "SPIRITS: Uncovering Unusual Infrared Transients with Spitzer", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: general \u2013 novae, cataclysmic variables \u2013 stars: AGB and post-AGB \u2013 stars: mass-loss \u2013 supernovae: general \u2013 surveys", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 July 18; revised 2017 March 23; accepted 2017 March 23; published 2017 April 19. \n\nWe thank O. Pejcha, E. Lovegrove, S. Woosley, A.L. Piro, E.S. Phinney, S.R. Kulkarni, L. Bildsten, and E. Quataert for valuable discussions. We thank the anonymous referee for constructive suggestions that improved this manuscript. This work is based 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. The SPIRITS team acknowledges generous support from the NASA Spitzer grants for SPIRITS. M.M.K. thanks the National Science Foundation for a PIRE Grant No. 1545949 for the GROWTH project. J.J. acknowledges the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. P.A.W. and S.M. are grateful to the South African National Research Foundation (NRF) for a research grant. R.D.G. and the MLOF group were supported, in part, by the United States Air Force. H.E.B. acknowledges support by NASA through grant GO-13935 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.\n\nPublished - Kasliwal_2017_ApJ_839_88.pdf
Submitted - 1701.01151.pdf
", "abstract": "We present an ongoing, five-year systematic search for extragalactic infrared transients, dubbed SPIRITS\u2014SPitzer InfraRed Intensive Transients Survey. In the first year, using Spitzer/IRAC, we searched 190 nearby galaxies with cadence baselines of one month and six months. We discovered over 1958 variables and 43 transients. Here, we describe the survey design and highlight 14 unusual infrared transients with no optical counterparts to deep limits, which we refer to as SPRITEs (eSPecially Red Intermediate-luminosity Transient Events). SPRITEs are in the infrared luminosity gap between novae and supernovae, with [4.5] absolute magnitudes between \u221211 and \u221214 (Vega-mag) and [3.6]\u2013[4.5] colors between 0.3 mag and 1.6 mag. The photometric evolution of SPRITEs is diverse, ranging from <0.1 mag yr^(\u22121) to >7 mag yr^(\u22121). SPRITEs occur in star-forming galaxies. We present an in-depth study of one of them, SPIRITS 14ajc in Messier 83, which shows shock-excited molecular hydrogen emission. This shock may have been triggered by the dynamic decay of a non-hierarchical system of massive stars that led to either the formation of a binary or a protostellar merger.", "date": "2017-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "839", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 88", "id_number": "CaltechAUTHORS:20170419-090643097", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170419-090643097", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "South African National Research Foundation" }, { "agency": "U.S. Air Force" }, { "agency": "NASA", "grant_number": "GO-13935" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa6978", "primary_object": { "basename": "1701.01151.pdf", "url": "https://authors.library.caltech.edu/records/jbtqq-f3r28/files/1701.01151.pdf" }, "related_objects": [ { "basename": "Kasliwal_2017_ApJ_839_88.pdf", "url": "https://authors.library.caltech.edu/records/jbtqq-f3r28/files/Kasliwal_2017_ApJ_839_88.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Kasliwal, Mansi M.; Masci, Frank; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pcf5t-cvj39", "eprint_id": 60292, "eprint_status": "archive", "datestamp": "2023-08-19 02:13:10", "lastmod": "2023-10-24 16:24:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "S." }, "orcid": "0000-0002-1481-4676" }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "J." }, "orcid": "0000-0001-5754-4007" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "O. D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Kromer-M", "name": { "family": "Kromer", "given": "M." } }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Banerjee-D-P-K", "name": { "family": "Banerjee", "given": "D. P. K." } }, { "id": "Joshi-V", "name": { "family": "Joshi", "given": "V." } }, { "id": "Jerkstrand-A", "name": { "family": "Jerkstrand", "given": "A." } }, { "id": "Kankare-E", "name": { "family": "Kankare", "given": "E." }, "orcid": "0000-0001-8257-3512" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" } ] }, "title": "Spitzer observations of SN 2014J and properties of mid-IR emission in Type Ia Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter, supernovae: general, supernovae: individual: 2005df, 2006X, 2007af, 2007le, 2007sr, 2009ig, 2012cg, 2011fe, 2014J, dust, extinction", "note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 December 20. Received 2016 December 1; in original form 2016 December 1. Published: 07 January 2017. \n\nWe are grateful to Claes Fransson for stimulating discussions. RA and AG acknowledge support from the Swedish Research Council and the Swedish Space Board. MMK acknowledges support from the Hubble Fellowship and Carnegie-Princeton Fellowship. We acknowledge the John von Neumann Institute for Computing for granting computing time on the supercomputer JUQUEEN at the J\u00fclich Supercomputing Centre. Observations are made with the Spitzer telescope, the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias and the Mount Abu 1.2-m Infrared Telescope, India.\n\nPublished - stw3350.pdf
Submitted - 1411.3332v1.pdf
", "abstract": "SN 2014J in M 82 is the closest Type Ia supernova (SN Ia) in decades. The proximity allows for detailed studies of supernova physics and provides insights into the circumstellar and interstellar environment. In this work, we analyse Spitzer mid-infrared (mid-IR) data of SN 2014J in the 3.6 and 4.5\u2009\u03bcm wavelength range, together with several other nearby and well-studied SNe Ia. We compile the first composite mid-IR light-curve templates from our sample of SNe Ia, spanning the range from before peak brightness well into the nebular phase. Our observations indicate that SNe Ia form a very homogeneous class of objects at these wavelengths. Using the low-reddening supernovae for comparison, we constrain possible thermal emission from circumstellar dust around the highly reddened SN 2014J. We also study SNe 2006X and 2007le, where the presence of matter in the circumstellar environment has been suggested. No significant mid-IR excess is detected, allowing us to place upper limits on the amount of pre-existing dust in the circumstellar environment. For SN 2014J, M_(dust) \u2272 10^(\u2212 5)\u2009M\u2299 within r_(dust) \u223c 10^(17) cm, which is insufficient to account for the observed extinction. Similar limits are obtained for SNe 2006X and 2007le.", "date": "2017-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "466", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3442-3449", "id_number": "CaltechAUTHORS:20150917-071005971", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-071005971", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stw3350", "primary_object": { "basename": "1411.3332v1.pdf", "url": "https://authors.library.caltech.edu/records/pcf5t-cvj39/files/1411.3332v1.pdf" }, "related_objects": [ { "basename": "stw3350.pdf", "url": "https://authors.library.caltech.edu/records/pcf5t-cvj39/files/stw3350.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Johansson, J.; Goobar, A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a6b6e-dc685", "eprint_id": 75202, "eprint_status": "archive", "datestamp": "2023-08-19 01:59:29", "lastmod": "2023-10-25 14:50:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob E." }, "orcid": "0000-0001-5754-4007" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "Joel" }, "orcid": "0000-0001-5975-290X" }, { "id": "Contreras-C", "name": { "family": "Contreras", "given": "Carlos" } }, { "id": "Castell\u00f3n-S", "name": { "family": "Castell\u00f3n", "given": "Sergio" } }, { "id": "Bond-H-E", "name": { "family": "Bond", "given": "Howard E." }, "orcid": "0000-0003-1377-7145" }, { "id": "Monson-A-J", "name": { "family": "Monson", "given": "Andrew J." }, "orcid": "0000-0002-0048-2586" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Cody-A-M", "name": { "family": "Cody", "given": "Ann Marie" }, "orcid": "0000-0002-3656-6706" }, { "id": "Andrews-J-E", "name": { "family": "Andrews", "given": "Jennifer E." }, "orcid": "0000-0003-0123-0062" }, { "id": "Bally-J", "name": { "family": "Bally", "given": "John" }, "orcid": "0000-0001-8135-6612" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "Ori D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Gburek-T", "name": { "family": "Gburek", "given": "Timothy" }, "orcid": "0000-0002-7732-9205" }, { "id": "Gehrz-R-D", "name": { "family": "Gehrz", "given": "Robert D." }, "orcid": "0000-0003-1319-4089" }, { "id": "Green-W", "name": { "family": "Green", "given": "Wayne" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "Eric" } }, { "id": "Morrell-N", "name": { "family": "Morrell", "given": "Nidia" }, "orcid": "0000-0003-2535-3091" }, { "id": "Phillips-M-M", "name": { "family": "Phillips", "given": "Mark" }, "orcid": "0000-0003-2734-0796" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Simcoe-R-A", "name": { "family": "Simcoe", "given": "Robert A." }, "orcid": "0000-0003-3769-9559" }, { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Williams-R", "name": { "family": "Williams", "given": "Robert" } } ] }, "title": "SPIRITS 15c and SPIRITS 14buu: Two Obscured Supernovae in the Nearby Star-forming Galaxy IC 2163", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (SPIRITS 15c, SPIRITS 14buu) \u2013 surveys", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 14; revised 2017 February 14; accepted 2017 February 18; published 2017 March 15. \n\nWe thank the anonymous referee for the comments that improved the manuscript. We thank M. Kaufman, B. Elmegreen, and the authors of Elmegreen et al. (2016) and Kaufman et al. (2016) for providing H\u03b1, 24 \u00b5m, and CO measurements at the location of SPIRITS 15c. We also thank P. Groot, R. Lau, and S. Adams for valuable discussions. \n\nThis material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant no. DGE-1144469. H.E.B. acknowledges support for this work provided by NASA through grants GO-13935 and GO-14258 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. R.D.G. was supported in part by the United States Air Force. \n\nThis work makes use of observations from the LCO network. This paper includes data gathered with the 6.5 m Magellan Telescopes located at LCO, Chile. \n\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The work is based, in part, on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. \n\nFunding 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 web site is www.sdss.org. \n\nSDSS-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 - Jencson_2017_ApJ_837_167.pdf
Submitted - 1609.04444.pdf
", "abstract": "SPitzer InfraRed Intensive Transients Survey\u2014SPIRITS\u2014is an ongoing survey of nearby galaxies searching for infrared (IR) transients with Spitzer/IRAC. We present the discovery and follow-up observations of one of our most luminous (M_([4.5]) = \u221217.1 \u00b1 0.4 mag, Vega) and reddest ([3.6] \u2212 [4.5] = 3.0 \u00b1 0.2 mag) transients, SPIRITS 15c. The transient was detected in a dusty spiral arm of IC 2163 (D \u2248 35.5 Mpc). Pre-discovery ground-based imaging revealed an associated, shorter-duration transient in the optical and near-IR (NIR). NIR spectroscopy showed a broad (\u22488400 km s^(\u22121)), double-peaked emission line of He I at 1.083 \u03bcm, indicating an explosive origin. The NIR spectrum of SPIRITS 15c is similar to that of the Type IIb SN 2011dh at a phase of \u2248200 days. Assuming an A_V = 2.2 mag of extinction in SPIRITS 15c provides a good match between their optical light curves. The NIR light curves, however, show some minor discrepancies when compared with SN 2011dh, and the extreme [3.6]\u2013[4.5] color has not been previously observed for any SN IIb. Another luminous (M_(4.5) = \u221216.1 \u00b1 0.4 mag) event, SPIRITS 14buu, was serendipitously discovered in the same galaxy. The source displays an optical plateau lasting \u227380 days, and we suggest a scenario similar to the low-luminosity Type IIP SN 2005cs obscured by A V \u2248 1.5 mag. Other classes of IR-luminous transients can likely be ruled out in both cases. If both events are indeed SNe, this may suggest that \u227318% of nearby core-collapse SNe are missed by currently operating optical surveys.", "date": "2017-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "837", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 167", "id_number": "CaltechAUTHORS:20170317-110327657", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170317-110327657", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NASA", "grant_number": "GO-13935" }, { "agency": "NASA", "grant_number": "GO-14258" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "U.S. Air Force" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa618f", "primary_object": { "basename": "1609.04444.pdf", "url": "https://authors.library.caltech.edu/records/a6b6e-dc685/files/1609.04444.pdf" }, "related_objects": [ { "basename": "Jencson_2017_ApJ_837_167.pdf", "url": "https://authors.library.caltech.edu/records/a6b6e-dc685/files/Jencson_2017_ApJ_837_167.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Jencson, Jacob E.; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x8by3-61435", "eprint_id": 77893, "eprint_status": "archive", "datestamp": "2023-08-22 19:50:36", "lastmod": "2023-10-25 23:32:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Cook-D-O", "name": { "family": "Cook", "given": "D. O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Turner-J-A", "name": { "family": "Turner", "given": "J. A." }, "orcid": "0000-0003-2261-5746" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "A. D." }, "orcid": "0000-0002-5480-5686" }, { "id": "Boquien-M", "name": { "family": "Boquien", "given": "M." }, "orcid": "0000-0003-0946-6176" }, { "id": "Brown-M-J-I", "name": { "family": "Brown", "given": "M. J. I." }, "orcid": "0000-0002-1207-9137" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "De-Looze-I", "name": { "family": "De Looze", "given": "I." } }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "B. A." }, "orcid": "0000-0002-9768-0246" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Herrera-Camus-R", "name": { "family": "Herrera-Camus", "given": "R." }, "orcid": "0000-0002-2775-0595" }, { "id": "Hinz-J-L", "name": { "family": "Hinz", "given": "J. L." } }, { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Rest-A", "name": { "family": "Rest", "given": "A." } }, { "id": "Sandstrom-K-M", "name": { "family": "Sandstrom", "given": "K. M." }, "orcid": "0000-0002-4378-8534" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J.-D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Tabatabaei-F-S", "name": { "family": "Tabatabaei", "given": "F. S." } }, { "id": "Wilson-C-D", "name": { "family": "Wilson", "given": "C. D." }, "orcid": "0000-0001-5817-0991" } ] }, "title": "Updated 34-band Photometry for the SINGS/KINGFISH Samples of Nearby Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: photometry; galaxies: ISM; infrared: ISM; ISM: general", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 December 5. Accepted 2017 February 10. Published 2017 March 7. \n\nWe thank the referee for excellent suggestions that improved this work. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based on observations made with the Spitzer Space Telescope and utilizes the NASA/IPAC Infrared Science Archive, both operated by JPL/Caltech under a contract with NASA. 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. Funding for the Sloan Digital Sky Survey and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U.S. Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the JPL/Caltech, funded by NASA. The Pan-STARRS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating 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 NSF, the University of Maryland, and Eotvos Lorand University and the Los Alamos National Laboratory.\n\nPublished - Dale_2017_ApJ_837_90.pdf
Submitted - 1702.05205.pdf
", "abstract": "We present an update to the ultraviolet-to-radio database of global broadband photometry for the 79 nearby galaxies that comprise the union of the KINGFISH (Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel) and SINGS (Spitzer Infrared Nearby Galaxies Survey) samples. The 34-band data set presented here includes contributions from observational work carried out with a variety of facilities including GALEX, SDSS, Pan-STARRS1, NOAO, 2MASS, Wide-Field Infrared Survey Explorer, Spitzer, Herschel, Planck, JCMT, and the VLA. Improvements of note include recalibrations of previously published SINGS BVR _CI_C and KINGFISH far-infrared/submillimeter photometry. Similar to previous results in the literature, an excess of submillimeter emission above model predictions is seen primarily for low-metallicity dwarf or irregular galaxies. This 33-band photometric data set for the combined KINGFISH+SINGS sample serves as an important multiwavelength reference for the variety of galaxies observed at low redshift. A thorough analysis of the observed spectral energy distributions is carried out in a companion paper.", "date": "2017-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "837", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 90", "id_number": "CaltechAUTHORS:20170601-134218692", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170601-134218692", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/aa6032", "primary_object": { "basename": "1702.05205.pdf", "url": "https://authors.library.caltech.edu/records/x8by3-61435/files/1702.05205.pdf" }, "related_objects": [ { "basename": "Dale_2017_ApJ_837_90.pdf", "url": "https://authors.library.caltech.edu/records/x8by3-61435/files/Dale_2017_ApJ_837_90.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Dale, D. A.; Cook, D. O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/nczs8-85808", "eprint_id": 96874, "eprint_status": "archive", "datestamp": "2023-08-19 01:53:40", "lastmod": "2023-10-20 21:35:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. L. Evidence of spatial variation of the polarized thermal dust spectral energy distribution and implications for CMB B-mode analysis", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 submillimeter: ISM \u2013 dust, extinction", "note": "\u00a9 2017 ESO. Article published by EDP Sciences.\n\nReceived 22 June 2016; Accepted 16 November 2; Published online 28 February 2017.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.\n\nPublished - aa29164-16.pdf
Submitted - 1606.07335.pdf
", "abstract": "The characterization of the Galactic foregrounds has been shown to be the main obstacle in thechallenging quest to detect primordial B-modes in the polarized microwave sky. We make use of the Planck-HFI 2015 data release at high frequencies to place new constraints on the properties of the polarized thermal dust emission at high Galactic latitudes. Here, we specifically study the spatial variability of the dust polarized spectral energy distribution (SED), and its potential impact on the determination of the tensor-to-scalar ratio, r. We use the correlation ratio of the C^(BB)_\u2113 angular power spectra between the 217 and 353\u2009GHz channels as a tracer of these potential variations, computed on different high Galactic latitude regions, ranging from 80% to 20% of the sky. The new insight from Planck data is a departure of the correlation ratio from unity that cannot be attributed to a spurious decorrelation due to the cosmic microwave background, instrumental noise, or instrumental systematics. The effect is marginally detected on each region, but the statistical combination of all the regions gives more than 99% confidence for this variation in polarized dust properties. In addition, we show that the decorrelation increases when there is a decrease in the mean column density of the region of the sky being considered, and we propose a simple power-law empirical model for this dependence, which matches what is seen in the Planck data. We explore the effect that this measured decorrelation has on simulations of the BICEP2-Keck Array/Planck analysis and show that the 2015 constraints from these data still allow a decorrelation between the dust at 150 and 353\u2009GHz that is compatible with our measured value. Finally, using simplified models, we show that either spatial variation of the dust SED or of the dust polarization angle are able to produce decorrelations between 217 and 353\u2009GHz data similar to the values we observe in the data.", "date": "2017-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "599", "publisher": "EDP Sciences", "pagerange": "Art. No. A51", "id_number": "CaltechAUTHORS:20190702-083349509", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190702-083349509", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201629164", "primary_object": { "basename": "1606.07335.pdf", "url": "https://authors.library.caltech.edu/records/nczs8-85808/files/1606.07335.pdf" }, "related_objects": [ { "basename": "aa29164-16.pdf", "url": "https://authors.library.caltech.edu/records/nczs8-85808/files/aa29164-16.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Aghanim, N.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4bfk7-vc046", "eprint_id": 74089, "eprint_status": "archive", "datestamp": "2023-08-19 01:44:15", "lastmod": "2023-10-24 22:05:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "Brian" }, "orcid": "0000-0002-7856-3570" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "Umaa" }, "orcid": "0000-0002-2560-3495" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom" } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas" }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Small Near-Earth Asteroids in the Palomar Transient Factory Survey: a Real-Time Streak-detection System", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets \u2013 asteroids: general", "note": "\u00a9 2017 The Astronomical Society of the Pacific. \n\nReceived 2016 July 13; accepted 2016 September 11; published 2017 February 7. \n\nThis work uses data obtained with the 1.2-m Samuel Oschin Telescope at Palomar Observatory as part of the Palomar Transient Factory project, a scientific collaboration among the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science, and the Intermediate Palomar Transient Factory project, a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the universe. \n\nThe authors thank Robert Jedicke and Quan-Zhi Ye for valuable comments on the paper, as well as the informative comments and suggestions by the referee. \n\nA. Waszczak has been supported in part by the W.M. Keck Institute for Space Studies (KISS) at Caltech and this work was part of his thesis research. The work presented in this paper was in part inspired by a workshop on an Asteroid Retrieval Mission organized and funded by KISS in 2010\u20132012. This work also was also supported by NASA JPL internal research and technology development funds. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nAccepted Version - 1609.08018.pdf
", "abstract": "Near-Earth asteroids (NEAs) in the 1\u2013100 meter size range are estimated to be ~1,000 times more numerous than the ~15,000 currently cataloged NEAs, most of which are in the 0.5\u201310 kilometer size range. Impacts from 10\u2013100 meter size NEAs are not statistically life-threatening, but may cause significant regional damage, while 1\u201310 meter size NEAs with low velocities relative to Earth are compelling targets for space missions. We describe the implementation and initial results of a real-time NEA-discovery system specialized for the detection of small, high angular rate (visually streaked) NEAs in Palomar Transient Factory (PTF) images. PTF is a 1.2-m aperture, 7.3 deg^2 field of view (FOV) optical survey designed primarily for the discovery of extragalactic transients (e.g., supernovae) in 60-second exposures reaching ~20.5 visual magnitude. Our real-time NEA discovery pipeline uses a machine-learned classifier to filter a large number of false-positive streak detections, permitting a human scanner to efficiently and remotely identify real asteroid streaks during the night. Upon recognition of a streaked NEA detection (typically within an hour of the discovery exposure), the scanner triggers follow-up with the same telescope and posts the observations to the Minor Planet Center for worldwide confirmation. We describe our 11 initial confirmed discoveries, all small NEAs that passed 0.3\u201315 lunar distances from Earth. Lastly, we derive useful scaling laws for comparing streaked-NEA-detection capabilities of different surveys as a function of their hardware and survey-pattern characteristics. This work most directly informs estimates of the streak-detection capabilities of the Zwicky Transient Facility (ZTF, planned to succeed PTF in 2017), which will apply PTF's current resolution and sensitivity over a 47-deg^2 FOV.", "date": "2017-03", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "129", "number": "973", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 034402", "id_number": "CaltechAUTHORS:20170206-134306305", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170206-134306305", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "JPL Internal Research and Technology Development Program" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/129/973/034402", "primary_object": { "basename": "1609.08018.pdf", "url": "https://authors.library.caltech.edu/records/4bfk7-vc046/files/1609.08018.pdf" }, "resource_type": "article", "pub_year": "2017", "author_list": "Waszczak, Adam; Prince, Thomas A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ry2tb-7qb18", "eprint_id": 69707, "eprint_status": "archive", "datestamp": "2023-08-19 00:55:40", "lastmod": "2023-10-20 20:30:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "Umaa D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Doran-G-B", "name": { "family": "Doran", "given": "Gary B." } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi" }, "orcid": "0000-0002-5619-4938" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Jackson-E", "name": { "family": "Jackson", "given": "Ed" } }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom" } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "Lisa J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "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" } ] }, "title": "The IPAC Image Subtraction and Discovery Pipeline for the intermediate Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: analytical \u2013 methods: data analysis \u2013 methods: statistical \u2013 techniques: image processing \u2013\ntechniques: photometric", "note": "\u00a9 2016 The Astronomical Society of the Pacific.\n\nReceived 2016 August 5; accepted 2016 September 27; published 2016 December 8.\n\nThis work was funded in part by the iPTF and ZTF projects at the California Institute of Technology. iPTF is a partnership led by the California Institute of Technology and includes the Infrared Processing & Astronomical Center; Los Alamos National Laboratory; University of Wisconsin at Milwaukee; Oskar-Klein Center of the University of Stockholm, Sweden; Weizmann Institute of Sciences, Israel; University System of Taiwan, Taiwan; the Institute for Physics & Mathematics of the universe, Japan; Lawrence Berkeley National Laboratory and the University of California, Berkeley. ZTF is funded by the National Science Foundation under grant no. AST-144034. M.M.K. acknowledges support from the National Science Foundation PIRE GROWTH award. A.A.M. acknowledges support for this work by NASA from a Hubble Fellowship grant: HST-HF-51325.01, awarded by STScI, operated by AURA, Inc., for NASA, under contract NAS 5-26555. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.\n\nThe pipelines use a number of software packages from other institutions and past projects (see Table 1), for which we are indebted. Portions of the analysis presented here made use of the Perl Data Language (PDL) developed by K. Glazebrook, J. Brinchmann, J. Cerney, C. DeForest, D. Hunt, T. Jenness, T. Lukka, R. Schwebel, and C. Soeller and can be obtained from http://pdl.perl.org.\n\nPDL provides a high-level numerical functionality for the Perl scripting language (Glazebrook & Economou 1997).\n\nWe thank the anonymous referee for valuable comments that helped improve the quality of this manuscript.\n\nFacility: PO:1.2m.\n\nSubmitted - 1608.01733v1.pdf
", "abstract": "We describe the near real-time transient-source discovery engine for the intermediate Palomar Transient Factory (iPTF), currently in operations at the Infrared Processing and Analysis Center (IPAC), Caltech. We coin this system the IPAC/iPTF Discovery Engine (or IDE). We review the algorithms used for PSF-matching, image subtraction, detection, photometry, and machine-learned (ML) vetting of extracted transient candidates. We also review the performance of our ML classifier. For a limiting signal-to-noise ratio of 4 in relatively unconfused regions, bogus candidates from processing artifacts and imperfect image subtractions outnumber real transients by \u224310:1. This can be considerably higher for image data with inaccurate astrometric and/or PSF-matching solutions. Despite this occasionally high contamination rate, the ML classifier is able to identify real transients with an efficiency (or completeness) of \u224397% for a maximum tolerable false-positive rate of 1% when classifying raw candidates. All subtraction-image metrics, source features, ML probability-based real-bogus scores, contextual metadata from other surveys, and possible associations with known Solar System objects are stored in a relational database for retrieval by the various science working groups. We review our efforts in mitigating false-positives and our experience in optimizing the overall system in response to the multitude of science projects underway with iPTF.", "date": "2017-01-01", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "129", "number": "971", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 014002", "id_number": "CaltechAUTHORS:20160817-123122578", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160817-123122578", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Intermediate Palomar Transient Facility (iPTF)" }, { "agency": "Zwicky Transient Facility (ZTF), Caltech" }, { "agency": "NSF", "grant_number": "AST-144034" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51325.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/1538-3873/129/971/014002", "primary_object": { "basename": "1608.01733v1.pdf", "url": "https://authors.library.caltech.edu/records/ry2tb-7qb18/files/1608.01733v1.pdf" }, "resource_type": "article", "pub_year": "2017", "author_list": "Masci, Frank J.; Laher, Russ R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0sksv-k0517", "eprint_id": 74264, "eprint_status": "archive", "datestamp": "2023-08-22 19:29:37", "lastmod": "2023-10-24 22:16:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "Kevin" }, "orcid": "0000-0002-5258-7224" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce" }, "orcid": "0000-0002-0846-936X" }, { "id": "De-Looze-I", "name": { "family": "De Looze", "given": "Ilse" } }, { "id": "Sandstrom-K-M", "name": { "family": "Sandstrom", "given": "Karin. M." }, "orcid": "0000-0002-4378-8534" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "Pedro" } }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "Alberto" }, "orcid": "0000-0002-5480-5686" }, { "id": "Boquien-M", "name": { "family": "Boquien", "given": "M\u00e9d\u00e9ric" }, "orcid": "0000-0003-0946-6176" }, { "id": "Brandl-B-R", "name": { "family": "Brandl", "given": "Bernhard" } }, { "id": "Crocker-A-F", "name": { "family": "Crocker", "given": "Alison" }, "orcid": "0000-0001-8513-4945" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "Maud" }, "orcid": "0000-0002-0283-8689" }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "Brent" }, "orcid": "0000-0002-9768-0246" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Herrera-Camus-R", "name": { "family": "Herrera-Camus", "given": "Roberto" }, "orcid": "0000-0002-2775-0595" }, { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "Leslie" }, "orcid": "0000-0001-9162-2371" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert" }, "orcid": "0000-0001-5448-1821" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Wolfire-M-G", "name": { "family": "Wolfire", "given": "Mark" }, "orcid": "0000-0003-0030-9510" } ] }, "title": "The Spatially Resolved [CII] Cooling Line Deficit in Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: ISM; infrared: galaxies; techniques: spectroscopic", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 July 1; revised 2016 November 2; accepted 2016 November 3; published 2016 December 22. \n\nThis work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We thank Steve Hailey-Dunsheath, T. Rawle, and Tanio Diaz-Santos for advanced access to their compiled [C II] data sets. We also thank them, as well as Gordon Stacey, Carl Ferkinhoff, M. Kapala, and R. Decarli, for helpful discussions which improved this work. J.D.S. gratefully acknowledges visiting support from the Alexander von Humboldt Foundation and the Max Planck Institute f\u00fcr Astronomie as well as support from the Research Corporation for Science Advancement through its Cottrell Scholars program.\n\nPublished - Smith_2017_ApJ_834_5.pdf
Accepted Version - 1611.01521.pdf
", "abstract": "We present [C II] 158 \u03bcm measurements from over 15,000 resolved regions within 54 nearby galaxies of the Kingfish program to investigate the so-called [C II] \"line-cooling deficit\" long known to occur in galaxies with different luminosities. The [C II]/TIR ratio ranges from above 1% to below 0.1% in the sample, with a mean value of 0.48 \u00b1 0.21%. We find that the surface density of 24 \u03bcm emission dominates this trend, with [C II]/TIR dropping as \u03bdl_\u03bd (24 \u00b5m) increases. Deviations from this overall decline are correlated with changes in the gas-phase metal abundance, with higher metallicity associated with deeper deficits at a fixed surface brightness. We supplement the local sample with resolved [C II] measurements from nearby luminous infrared galaxies and high-redshift sources from z = 1.8\u20136.4, and find that star formation rate density drives a continuous trend of deepening [C II] deficit across six orders of magnitude in \u03a3_(SFR). The tightness of this correlation suggests that an approximate \u03a3_(SFR) can be estimated directly from global measurements of [C II]/TIR, and a relation is provided to do so. Several low-luminosity active galactic nucleus (AGN) hosts in the sample show additional and significant central suppression of [C II]/TIR, but these deficit enhancements occur not in those AGNs with the highest X-ray luminosities, but instead those with the highest central starlight intensities. Taken together, these results demonstrate that the [C II] line-cooling line deficit in galaxies likely arises from local physical phenomena in interstellar gas.", "date": "2017-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "834", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 5", "id_number": "CaltechAUTHORS:20170213-145705837", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170213-145705837", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Max Planck Institute f\u00fcr Astronomie" }, { "agency": "Cottrell Scholar of Research Corporation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4357/834/1/5", "primary_object": { "basename": "1611.01521.pdf", "url": "https://authors.library.caltech.edu/records/0sksv-k0517/files/1611.01521.pdf" }, "related_objects": [ { "basename": "Smith_2017_ApJ_834_5.pdf", "url": "https://authors.library.caltech.edu/records/0sksv-k0517/files/Smith_2017_ApJ_834_5.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Smith, J. D. T.; Croxall, Kevin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cce7g-0e530", "eprint_id": 73215, "eprint_status": "archive", "datestamp": "2023-08-22 19:24:53", "lastmod": "2023-10-24 15:08:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steer-Ian", "name": { "family": "Steer", "given": "Ian" } }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "Barry F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Mazzarella-J-M", "name": { "family": "Mazzarella", "given": "Joseph M." }, "orcid": "0000-0002-8204-8619" }, { "id": "Schmitz-M", "name": { "family": "Schmitz", "given": "Marion" } }, { "id": "Corwin-Harold-G", "name": { "family": "Corwin", "given": "Harold G." } }, { "id": "Chan-Ben-Hiu-Pan", "name": { "family": "Chan", "given": "Ben H. P." } }, { "id": "Ebert-R", "name": { "family": "Ebert", "given": "Rick" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Baker-Kay", "name": { "family": "Baker", "given": "Kay" } }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "Xi" }, "orcid": "0000-0001-9152-6224" }, { "id": "Frayer-Cren", "name": { "family": "Frayer", "given": "Cren" } }, { "id": "Jacobson-J-D", "name": { "family": "Jacobson", "given": "Jeff" } }, { "id": "Lo-Tak", "name": { "family": "Lo", "given": "Tak" } }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick" }, "orcid": "0000-0002-3471-981X" }, { "id": "Pevunova-O", "name": { "family": "Pevunova", "given": "Olga" } }, { "id": "Terek-S", "name": { "family": "Terek", "given": "Scott" } } ] }, "title": "Redshift-independent Distances in the NASA/IPAC Extragalactic Database: Methodology, Content, and Use of NED-D", "ispublished": "pub", "full_text_status": "public", "keywords": "astronomical databases: miscellaneous; catalogs; distance scale; galaxies: distances and redshifts; galaxies: fundamental parameters", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 March 18; revised 2016 October 3; accepted 2016 October 10; published 2016 December 29. \n\nThe authors are grateful to the many authors who publish redshift-independent extragalactic distance estimates. In particular we would like to thank Edward Baron, Jonathan Bird, Massimiliano Bonamente, Dmitry Bizyaev, John Blakeslee, Jean Brodie, Heather Campbell, Chris Corbally, Igor Drozdovsky, Wendy Freedman, Mohan Ganeshalingam, Gretchen Harris, William Harris, Raoul Haschke, Martha Haynes, Robert Hurt, George Jacoby, Igor Karachentsev, David Lagattuta, Tod Lauer, Mario Livio, Lucas Macri, Daniel Majaess, Dmitry Makarov, Karen Masters, Kristen McQuinn, Fulvio Melia, Jeremy Mould, Robert Quimby, Armin Rest, Adam Riess, Luca Rizzi, Dave Russell, Christoph Saulder, Riccardo Scarpa, Bradley Schaefer, David Schlegel, Daniel Scolnic, Chris Springob, Gilles Theureau, Brent Tully, Alan Whiting, and Henrique Xavier for many helpful comments over the years. This research has made extensive use of the SAO/NASA Astrophysics Data System Bibliographic services. This work has also made extensive use of, and is funded by, 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. Additional generous support to IS from the Carnegie Institution of Canada is also gratefully appreciated.\n\nPublished - Steer_2017_AJ_153_37.pdf
Accepted Version - 1612.09263.pdf
", "abstract": "Estimates of galaxy distances based on indicators that are independent of cosmological redshift are fundamental to astrophysics. Researchers use them to establish the extragalactic distance scale, to underpin estimates of the Hubble constant, and to study peculiar velocities induced by gravitational attractions that perturb the motions of galaxies with respect to the \"Hubble flow\" of universal expansion. In 2006 the NASA/IPAC Extragalactic Database (NED) began making available a comprehensive compilation of redshift-independent extragalactic distance estimates. A decade later, this compendium of distances (NED-D) now contains more than 100,000 individual estimates based on primary and secondary indicators, available for more than 28,000 galaxies, and compiled from over 2000 references in the refereed astronomical literature. This paper describes the methodology, content, and use of NED-D, and addresses challenges to be overcome in compiling such distances. Currently, 75 different distance indicators are in use. We include a figure that facilitates comparison of the indicators with significant numbers of estimates in terms of the minimum, 25th percentile, median, 75th percentile, and maximum distances spanned. Brief descriptions of the indicators, including examples of their use in the database, are given in an appendix.", "date": "2017-01", "date_type": "published", "publication": "Astronomical Journal", "volume": "153", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 37", "id_number": "CaltechAUTHORS:20170104-135122413", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170104-135122413", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Carnegie Institution of Canada" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-3881/153/1/37", "primary_object": { "basename": "1612.09263.pdf", "url": "https://authors.library.caltech.edu/records/cce7g-0e530/files/1612.09263.pdf" }, "related_objects": [ { "basename": "Steer_2017_AJ_153_37.pdf", "url": "https://authors.library.caltech.edu/records/cce7g-0e530/files/Steer_2017_AJ_153_37.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Steer, Ian; Madore, Barry F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qb5z6-qkr53", "eprint_id": 73992, "eprint_status": "archive", "datestamp": "2023-08-19 00:17:21", "lastmod": "2023-10-24 21:59:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results XLVII. Planck constraints on reionization history", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / dark ages, reionization, first stars / polarization", "note": "\u00a9 ESO, 2016. \n\nReceived 11 May 2016. Accepted 23 July 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa28897-16.pdf
Submitted - 1605.03507v3.pdf
", "abstract": "We investigate constraints on cosmic reionization extracted from the Planck cosmic microwave background (CMB) data. We combine the Planck CMB anisotropy data in temperature with the low-multipole polarization data to fit \u039bCDM models with various parameterizations of the reionization history. We obtain a Thomson optical depth \u03c4 = 0.058 \u00b1 0.012 for the commonly adopted instantaneous reionization model. This confirms, with data solely from CMB anisotropies, the low value suggested by combining Planck 2015 results with other data sets, and also reduces the uncertainties. We reconstruct the history of the ionization fraction using either a symmetric or an asymmetric model for the transition between the neutral and ionized phases. To determine better constraints on the duration of the reionization process, we also make use of measurements of the amplitude of the kinetic Sunyaev-Zeldovich (kSZ) effect using additional information from the high-resolution Atacama Cosmology Telescope and South Pole Telescope experiments. The average redshift at which reionization occurs is found to lie between z = 7.8 and 8.8, depending on the model of reionization adopted. Using kSZ constraints and a redshift-symmetric reionization model, we find an upper limit to the width of the reionization period of \u0394z < 2.8. In all cases, we find that the Universe is ionized at less than the 10% level at redshifts above z \u2243 10. This suggests that an early onset of reionization is strongly disfavoured by the Planck data. We show that this result also reduces the tension between CMB-based analyses and constraints from other astrophysical sources.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A108", "id_number": "CaltechAUTHORS:20170202-143503710", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170202-143503710", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Centro Nazionale delle Ricerche (CNR)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Innovation" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "PRACE (EU)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Ministro da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201628897", "primary_object": { "basename": "1605.03507v3.pdf", "url": "https://authors.library.caltech.edu/records/qb5z6-qkr53/files/1605.03507v3.pdf" }, "related_objects": [ { "basename": "aa28897-16.pdf", "url": "https://authors.library.caltech.edu/records/qb5z6-qkr53/files/aa28897-16.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2n1hc-bwh23", "eprint_id": 96867, "eprint_status": "archive", "datestamp": "2023-08-19 00:23:22", "lastmod": "2023-10-20 21:34:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck intermediate results. XL. The Sunyaev-Zeldovich signal from the Virgo cluster", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 galaxies: clusters: individual: Virgo \u2013 galaxies: clusters: intracluster medium \u2013 cosmic background radiation \u2013 large-scale structure of Universe", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 13 November 2015; Accepted 27 September 20; Published online 12 December 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results presented in this work are based on observations obtained with XMM-Newton\u2009 an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.\n\nPublished - aa27743-15.pdf
Submitted - 1511.05156.pdf
", "abstract": "The Virgo cluster is the largest Sunyaev-Zeldovich (SZ) source in the sky, both in terms of angular size and total integrated flux. Planck's wide angular scale and frequency coverage, together with its high sensitivity, enable a detailed study of this big object through the SZ effect. Virgo is well resolved by Planck, showing an elongated structure that correlates well with the morphology observed from X-rays, but extends beyond the observed X-ray signal. We find good agreement between the SZ signal (or Compton parameter, yc) observed by Planck and the expected signal inferred from X-ray observations and simple analytical models. Owing to its proximity to us, the gas beyond the virial radius in Virgo can be studied with unprecedented sensitivity by integrating the SZ signal over tens of square degrees. We study the signal in the outskirts of Virgo and compare it with analytical models and a constrained simulation of the environment of Virgo. Planck data suggest that significant amounts of low-density plasma surround Virgo, out to twice the virial radius. We find the SZ signal in the outskirts of Virgo to be consistent with a simple model that extrapolates the inferred pressure at lower radii, while assuming that the temperature stays in the keV range beyond the virial radius. The observed signal is also consistent with simulations and points to a shallow pressure profile in the outskirts of the cluster. This reservoir of gas at large radii can be linked with the hottest phase of the elusivewarm/hot intergalactic medium. Taking the lack of symmetry of Virgo into account, we find that a prolate model is favoured by the combination of SZ and X-ray data, in agreement with predictions. Finally, based on the combination of the same SZ and X-ray data, we constrain the total amount of gas in Virgo. Under the hypothesis that the abundance of baryons in Virgo is representative of the cosmic average, we also infer a distance for Virgo of approximately 18\u2009Mpc, in good agreement with previous estimates.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A101", "id_number": "CaltechAUTHORS:20190701-135500084", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-135500084", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "ESA Member States" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527743", "primary_object": { "basename": "1511.05156.pdf", "url": "https://authors.library.caltech.edu/records/2n1hc-bwh23/files/1511.05156.pdf" }, "related_objects": [ { "basename": "aa27743-15.pdf", "url": "https://authors.library.caltech.edu/records/2n1hc-bwh23/files/aa27743-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/44q2q-zmy63", "eprint_id": 96870, "eprint_status": "archive", "datestamp": "2023-08-19 00:23:30", "lastmod": "2023-10-20 21:35:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. XLIV. Structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap", "ispublished": "pub", "full_text_status": "public", "keywords": "magnetohydrodynamics (MHD) \u2013 polarization \u2013 methods: data analysis \u2013 dust, extinction \u2013 cosmic background radiation \u2013\nISM: magnetic fields", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 4 April 2016; Accepted 13 July 2016; Published online 12 December 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planckcollaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007\u20132013)/ERC grant agreement No. 267934.\n\nPublished - aa28636-16.pdf
Submitted - 1604.01029.pdf
", "abstract": "Using data from the Planck satellite, we study the statistical properties of interstellar dust polarization at high Galactic latitudes around the south pole (b < \u221260\u00b0). Our aim is to advance the understanding of the magnetized interstellar medium (ISM), and to provide a modelling framework of the polarized dust foreground for use in cosmic microwave background (CMB) component-separation procedures. We examine the Stokes I, Q, and U maps at 353\u2009GHz, and particularly the statistical distribution of the polarization fraction (p) and angle (\u03c8), in order to characterize the ordered and turbulent components of the Galactic magnetic field (GMF) in the solar neighbourhood. The Q and U maps show patterns at large angular scales, which we relate to the mean orientation of the GMF towards Galactic coordinates (l_0,b_0) = (70\u00b0 \u00b1 5\u00b0,24\u00b0 \u00b1 5\u00b0). The histogram of the observed p values shows a wide dispersion up to 25%. The histogram of \u03c8 has a standard deviation of 12\u00b0 about the regular pattern expected from the ordered GMF. We build a phenomenological model that connects the distributions of p and \u03c8 to a statistical description of the turbulent component of the GMF, assuming a uniform effective polarization fraction (p_0) of dust emission. To compute the Stokes parameters, we approximate the integration along the line of sight (LOS) as a sum over a set of N independent polarization layers, in each of which the turbulent component of the GMF is obtained from Gaussian realizations of a power-law power spectrum. We are able to reproduce the observed p and \u03c8 distributions using a p0 value of 26%, a ratio of 0.9 between the strengths of the turbulent and mean components of the GMF, and a small value of N. The mean value of p (inferred from the fit of the large-scale patterns in the Stokes maps) is 12 \u00b1 1%. We relate the polarization layers to the density structure and to the correlation length of the GMF along the LOS. We emphasize the simplicity of our model (involving only a few parameters), which can be easily computed on the celestial sphere to produce simulated maps of dust polarization. Our work is an important step towards a model that can be used to assess the accuracy of component-separation methods in present and future CMB experiments designed to search the B mode CMB polarization from primordial gravity waves.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A105", "id_number": "CaltechAUTHORS:20190701-141615396", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-141615396", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201628636", "primary_object": { "basename": "1604.01029.pdf", "url": "https://authors.library.caltech.edu/records/44q2q-zmy63/files/1604.01029.pdf" }, "related_objects": [ { "basename": "aa28636-16.pdf", "url": "https://authors.library.caltech.edu/records/44q2q-zmy63/files/aa28636-16.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Aghanim, N.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/q9hh2-weh50", "eprint_id": 96871, "eprint_status": "archive", "datestamp": "2023-08-19 00:23:37", "lastmod": "2023-10-20 21:35:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. XLVI. Reduction of large-scale systematic effects in HFI polarization maps and estimation of the reionization optical depth", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 dark ages, reionization, first stars \u2013 cosmic background radiation \u2013 space vehicles: instruments \u2013\ninstrumentation: detectors", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 10 May 2016; Accepted 14 July 2016; Published online 12 December 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa28890-16.pdf
Submitted - 1605.02985.pdf
", "abstract": "This paper describes the identification, modelling, and removal of previously unexplained systematic effects in the polarization data of the Planck High Frequency Instrument (HFI) on large angular scales, including new mapmaking and calibration procedures, new and more complete end-to-end simulations, and a set of robust internal consistency checks on the resulting maps. These maps, at 100, 143, 217, and 353\u2009GHz, are early versions of those that will be released in final form later in 2016. The improvements allow us to determine the cosmic reionization optical depth \u03c4 using, for the first time, the low-multipole EE data from HFI, reducing significantly the central value and uncertainty, and hence the upper limit. Two different likelihood procedures are used to constrain \u03c4 from two estimators of the CMB E- and B-mode angular power spectra at 100 and 143\u2009GHz, after debiasing the spectra from a small remaining systematic contamination. These all give fully consistent results. A further consistency test is performed using cross-correlations derived from the Low Frequency Instrument maps of the Planck 2015 data release and the new HFI data. For this purpose, end-to-end analyses of systematic effects from the two instruments are used to demonstrate the near independence of their dominant systematic error residuals. The tightest result comes from the HFI-based \u03c4 posterior distribution using the maximum likelihood power spectrum estimator from EE data only, giving a value 0.055 \u00b1 0.009. In a companion paper these results are discussed in the context of the best-fit Planck\u039bCDM cosmological model and recent models of reionization.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A107", "id_number": "CaltechAUTHORS:20190702-073429800", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190702-073429800", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201628890", "primary_object": { "basename": "aa28890-16.pdf", "url": "https://authors.library.caltech.edu/records/q9hh2-weh50/files/aa28890-16.pdf" }, "related_objects": [ { "basename": "1605.02985.pdf", "url": "https://authors.library.caltech.edu/records/q9hh2-weh50/files/1605.02985.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Aghanim, N.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/kmchs-91k93", "eprint_id": 96873, "eprint_status": "archive", "datestamp": "2023-08-19 00:23:45", "lastmod": "2023-10-20 21:35:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. XLVIII. Disentangling Galactic dust emission and cosmic infrared background anisotropies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 methods: data analysis \u2013 ISM: general \u2013 dust, extinction \u2013 infrared: diffuse background \u2013\nlarge-scale structure of Universe", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 27 May 2016; Accepted 9 August 2016; Published online 12 December 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. The research leading to these results has received funding from the ERC Grant No. 307209.\n\nPublished - aa29022-16.pdf
Accepted Version - 1605.09387.pdf
", "abstract": "Using the Planck 2015 data release (PR2) temperature maps, we separate Galactic thermal dust emission from cosmic infrared background (CIB) anisotropies. For this purpose, we implement a specifically tailored component-separation method, the so-called generalized needlet internal linear combination (GNILC) method, which uses spatial information (the angular powerspectra) to disentangle the Galactic dust emission and CIB anisotropies. We produce significantly improved all-sky maps of Planck thermal dust emission, with reduced CIB contamination, at 353, 545, and 857 GHz. By reducing the CIB contamination of the thermal dust maps, we provide more accurate estimates of the local dust temperature and dust spectral index over the sky with reduced dispersion, especially at high Galactic latitudes above b = \u00b120\u00b0. We find that the dust temperature is T = (19.4 \u00b1 1.3) K and the dust spectral index is \u03b2 = 1.6 \u00b1 0.1 averaged over the whole sky, while T = (19.4 \u00b1 1.5) K and \u03b2 = 1.6 \u00b1 0.2 on 21% of the sky at high latitudes. Moreover, subtracting the new CIB-removed thermal dust maps from the CMB-removed Planck maps gives access to the CIB anisotropies over 60% of the sky at Galactic latitudes |b| > 20\u00b0. Because they are a significant improvement over previous Planck products, the GNILC maps are recommended for thermal dust science. The new CIB maps can be regarded as indirect tracers of the dark matter and they are recommended for exploring cross-correlations with lensing and large-scale structure optical surveys. The reconstructed GNILC thermal dust and CIB maps are delivered as Planck products.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A109", "id_number": "CaltechAUTHORS:20190702-075533029", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190702-075533029", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)", "grant_number": "307209" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201629022", "primary_object": { "basename": "1605.09387.pdf", "url": "https://authors.library.caltech.edu/records/kmchs-91k93/files/1605.09387.pdf" }, "related_objects": [ { "basename": "aa29022-16.pdf", "url": "https://authors.library.caltech.edu/records/kmchs-91k93/files/aa29022-16.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Aghanim, N.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cfctm-cbk31", "eprint_id": 96850, "eprint_status": "archive", "datestamp": "2023-08-19 00:23:14", "lastmod": "2023-10-20 21:34:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2013 submillimeter: galaxies \u2013 galaxies: high-redshift \u2013 galaxies: clusters: general \u2013 large-scale structure of Universe", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 17 August 2015; Accepted 7 October 2016; Published online 12 December 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa27206-15.pdf
Accepted Version - 1508.04171.pdf
", "abstract": "The Planck mission, thanks to its large frequency range and all-sky coverage, has a unique potential for systematically detecting the brightest, and rarest, submillimetre sources on the sky, including distant objects in the high-redshift Universe traced by their dust emission. A novel method, based on a component-separation procedure using a combination of Planck and IRAS data, has been validated and characterized on numerous simulations, and applied to select the most luminous cold submillimetre sources with spectral energy distributions peaking between 353 and 857\u2009GHz at 5\u2032 resolution. A total of 2151 Planck high-z source candidates (the PHZ) have been detected in the cleanest 26% of the sky, with flux density at 545\u2009GHz above 500\u2009mJy. Embedded in the cosmic infrared background close to the confusion limit, these high-z candidates exhibit colder colours than their surroundings, consistent with redshifts z > 2, assuming a dust temperature of T_(xgal) = 35\u2009K and a spectral index of \u03b2_(xgal) = 1.5. Exhibiting extremely high luminosities, larger than 10^(14)L\u2299, the PHZ objects may be made of multiple galaxies or clumps at high redshift, as suggested by a first statistical analysis based on a comparison with number count models. Furthermore, first follow-up observations obtained from optical to submillimetre wavelengths, which can be found in companion papers, have confirmed that this list consists of two distinct populations. A small fraction (around 3%) of the sources have been identified as strongly gravitationally lensed star-forming galaxies at redshift 2 to 4, while the vast majority of the PHZ sources appear as overdensities of dusty star-forming galaxies, having colours consistent with being at z > 2, and may be considered as proto-cluster candidates. The PHZ provides an original sample, which is complementary to the Planck Sunyaev-Zeldovich Catalogue (PSZ2); by extending the population of virialized massive galaxy clusters detected below z < 1.5 through their SZ signal to a population of sources at z > 1.5, the PHZ may contain the progenitors of today's clusters. Hence the Planck list of high-redshift source candidates opens a new window on the study of the early stages of structure formation, particularly understanding the intensively star-forming phase at high-z.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A100", "id_number": "CaltechAUTHORS:20190701-074006145", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-074006145", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527206", "primary_object": { "basename": "1508.04171.pdf", "url": "https://authors.library.caltech.edu/records/cfctm-cbk31/files/1508.04171.pdf" }, "related_objects": [ { "basename": "aa27206-15.pdf", "url": "https://authors.library.caltech.edu/records/cfctm-cbk31/files/aa27206-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3depd-be733", "eprint_id": 60299, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:06", "lastmod": "2023-10-24 16:24:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Pelkonen-Veli-Matti", "name": { "family": "Pelkonen", "given": "V.-M." }, "orcid": "0000-0002-8898-1047" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. I. Overview of products and scientific results", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 surveys \u2013 space vehicles: instruments \u2013 instrumentation: detectors", "note": "\u00a9 2016 ESO.\n\nReceived 1 August 2015; Accepted 18 January 2016;\nPublished online 20 September 2016.\n\n\nPlanck is a project of the European Space Agency in cooperation with the scientific community, which started in 1993. ESA led the project, developed the satellite, integrated the payload into it, and launched and operated the satellite. Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed and operated the scientific instruments LFI and HFI. The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's US Planck Project, based at JPL and involving scientists at many US institutions, contributes significantly to the efforts of these two Consortia. A third Consortium, led by H.U. Norgaard-Nielsen and supported by the Danish Natural Research Council, contributed to the reflector programme. These three Consortia, together with ESA's Planck Science Office, form the Planck Collaboration. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). We thank Diego Falceta-Gon\u00e7alves for providing the technique for making the line-integral-convolution maps presented in Figs. 23 and 25.\n\nPublished - aa27101-15.pdf
Submitted - 1502.01582v2.pdf
", "abstract": "The European Space Agency's Planck satellite, which is dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013. In February 2015, ESA and the Planck Collaboration released the second set of cosmology products based ondata from the entire Planck mission, including both temperature and polarization, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the main characteristics of the data and the data products in the release, as well as the associated cosmological and astrophysical science results and papers. The data products include maps of the cosmic microwave background (CMB), the thermal Sunyaev-Zeldovich effect, diffuse foregrounds in temperature and polarization, catalogues of compact Galactic and extragalactic sources (including separate catalogues of Sunyaev-Zeldovich clusters and Galactic cold clumps), and extensive simulations of signals and noise used in assessing uncertainties and the performance of the analysis methods. The likelihood code used to assess cosmological models against the Planck data is described, along with a CMB lensing likelihood. Scientific results include cosmological parameters derived from CMB power spectra, gravitational lensing, and cluster counts, as well as constraints on inflation, non-Gaussianity, primordial magnetic fields, dark energy, and modified gravity, and new results on low-frequency Galactic foregrounds.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A1", "id_number": "CaltechAUTHORS:20150917-084452506", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-084452506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National D'\u00e9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Danish Natural Research Council" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Institut for Rumforskning og Rumteknologi (DTU Space)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway (RCN)" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Ministro da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527101", "primary_object": { "basename": "1502.01582v2.pdf", "url": "https://authors.library.caltech.edu/records/3depd-be733/files/1502.01582v2.pdf" }, "related_objects": [ { "basename": "aa27101-15.pdf", "url": "https://authors.library.caltech.edu/records/3depd-be733/files/aa27101-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3pama-rd204", "eprint_id": 60302, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:22", "lastmod": "2023-10-24 16:24:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. X. Diffuse component separation: Foreground maps", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general / cosmology: observations / polarization / cosmic background radiation / diffuse radiation / Galaxy: general", "note": "\u00a9 2016 ESO. \n\nReceived: 26 February 2015; Accepted: 22 February 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration\n\nPublished - aa25967-15.pdf
Submitted - 1502.01588v2.pdf
", "abstract": "Planck has mapped the microwave sky in temperature over nine frequency bands between 30 and 857\u2009GHz and in polarization over seven frequency bands between 30 and 353\u2009GHz in polarization. In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive an internally consistent set of full-sky astrophysical component maps. Component separation dedicated to cosmic microwave background (CMB) reconstruction is described in a companion paper. For the temperature analysis, we combine the Planck observations with the 9-yr Wilkinson Microwave Anisotropy Probe (WMAP) sky maps and the Haslam et al. 408\u2009MHz map, to derive a joint model of CMB, synchrotron, free-free, spinning dust, CO, line emission in the 94 and 100\u2009GHz channels, and thermal dust emission. Full-sky maps are provided for each component, with an angular resolution varying between 7.\u03015 and 1deg. Global parameters (monopoles, dipoles, relative calibration, and bandpass errors) are fitted jointly with the sky model, and best-fit values are tabulated. For polarization, the model includes CMB, synchrotron, and thermal dust emission. These models provide excellent fits to the observed data, with rms temperature residuals smaller than 4\u03bcK over 93% of the sky for all Planck frequencies up to 353\u2009GHz, and fractional errors smaller than 1% in the remaining 7% of the sky. The main limitations of the temperature model at the lower frequencies are internal degeneracies among the spinning dust, free-free, and synchrotron components; additional observations from external low-frequency experiments will be essential to break these degeneracies. The main limitations of the temperature model at the higher frequencies are uncertainties in the 545 and 857\u2009GHz calibration and zero-points. For polarization, the main outstanding issues are instrumental systematics in the 100\u2013353\u2009GHz bands on large angular scales in the form of temperature-to-polarization leakage, uncertainties in the analogue-to-digital conversion, and corrections for the very long time constant of the bolometer detectors, all of which are expected to improve in the near future.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A10", "id_number": "CaltechAUTHORS:20150917-134706855", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-134706855", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525967", "primary_object": { "basename": "1502.01588v2.pdf", "url": "https://authors.library.caltech.edu/records/3pama-rd204/files/1502.01588v2.pdf" }, "related_objects": [ { "basename": "aa25967-15.pdf", "url": "https://authors.library.caltech.edu/records/3pama-rd204/files/aa25967-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gdt8x-q8b76", "eprint_id": 60321, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:12", "lastmod": "2023-10-24 16:25:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "id": "Pearson-Timothy-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmological parameters / cosmology: observations / methods: data analysis / methods: statistical", "note": "\u00a9 2016 ESO. \n\nReceived: 9 July 2015; Accepted: 18 May 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. \n\nWe further acknowledge the use of the CLASS Boltzmann code (Lesgourgues 2011) and the Monte Python package (Audren et al. 2013) in earlier stages of this work. The likelihood code and some of the validation work was built on the library pmclib from the CosmoPMC package (Kilbinger et al. 2011). \n\nThis research used resources of the IN2P3 Computer Center (http://cc.in2p3.fr) as well as of the Planck-HFI DPC infrastructure hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES.\n\nPublished - aa26926-15.pdf
Submitted - 1507.02704v1.pdf
", "abstract": "This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlationfunctions of the cosmic microwave background (CMB) temperature and polarization fluctuations that account for relevant uncertainties, both instrumental and astrophysical in nature. They are based on the same hybrid approach used for the previous release, i.e., a pixel-based likelihood at low multipoles (\u2113< 30) and a Gaussian approximation to the distribution of cross-power spectra at higher multipoles. The main improvements are the use of more and better processed data and of Planck polarization information, along with more detailed models of foregrounds and instrumental uncertainties. The increased redundancy brought by more than doubling the amount of data analysed enables further consistency checks and enhanced immunity to systematic effects. It also improves the constraining power of Planck, in particular with regard to small-scale foreground properties. Progress in the modelling of foreground emission enables the retention of a larger fraction of the sky to determine the properties of the CMB, which also contributes to the enhanced precision of the spectra. Improvements in data processing and instrumental modelling further reduce uncertainties. Extensive tests establish the robustness and accuracy of the likelihood results, from temperature alone, from polarization alone, and from their combination. For temperature, we also perform a full likelihood analysis of realistic end-to-end simulations of the instrumental response to the sky, which were fed into the actual data processing pipeline; this does not reveal biases from residual low-level instrumental systematics. Even with the increase in precision and robustness, the \u039bCDM cosmological model continues to offer a very good fit to the Planck data. The slope of the primordial scalar fluctuations, n_s, is confirmed smaller than unity at more than 5\u03c3 from Planck alone. We further validate the robustness of the likelihood results against specific extensions to the baseline cosmology, which are particularly sensitive to data at high multipoles. For instance, the effective number of neutrino species remains compatible with the canonical value of 3.046. For this first detailed analysis of Planck polarization spectra, we concentrate at high multipoles on the E modes, leaving the analysis of the weaker B modes to future work. At low multipoles we use temperature maps at all Planck frequencies along with a subset of polarization data. These data take advantage of Planck's wide frequency coverage to improve the separation of CMB and foreground emission. Within the baseline \u039bCDM cosmology this requires \u03c4 = 0.078 \u00b1 0.019 for the reionization optical depth, which is significantly lower than estimates without the use of high-frequency data for explicit monitoring of dust emission. At high multipoles we detect residual systematic errors in E polarization, typically at the \u03bcK^2 level; we therefore choose to retain temperature information alone for high multipoles as the recommended baseline, in particular for testing non-minimal models. Nevertheless, the high-multipole polarization spectra from Planck are already good enough to enable a separate high-precision determination of the parameters of the \u039bCDM model, showing consistency with those established independently from temperature information alone.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A11", "id_number": "CaltechAUTHORS:20150918-110504749", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-110504749", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526926", "primary_object": { "basename": "1507.02704v1.pdf", "url": "https://authors.library.caltech.edu/records/gdt8x-q8b76/files/1507.02704v1.pdf" }, "related_objects": [ { "basename": "aa26926-15.pdf", "url": "https://authors.library.caltech.edu/records/gdt8x-q8b76/files/aa26926-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Aghanim, N.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x1rn2-33y63", "eprint_id": 60313, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:30", "lastmod": "2023-10-24 16:25:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIII. Cosmological parameters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations / cosmology: theory / cosmic background radiation / cosmological parameters", "note": "\u00a9 2016 ESO. \n\nReceived: 6 February 2015; Accepted: 4 June 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007\u22122013)/ERC Grant Agreement No. [616170] and from the UK Science and Technology Facilities Council [grant number ST/L000652/1]. Part of this work was undertaken on the STFC DiRAC HPC Facilities at the University of Cambridge, funded by UK BIS National E-infrastructure capital grants, and on the Andromeda cluster of the University of Geneva. A large set of cosmological parameter constraints from different data combinations, and including many separate extensions to the 6-parameter base \u039bCDM model, are available at http://pla.esac.esa.int/pla/#cosmology.\n\nPublished - aa25830-15.pdf
Submitted - 1502.01589v2.pdf
", "abstract": "This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Our results are in very good agreement with the 2013 analysis of the Planck nominal-mission temperature data, but with increased precision. The temperature and polarization power spectra are consistent with the standard spatially-flat 6-parameter \u039bCDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted \"base \u039bCDM\" in this paper). From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H_0 = (67.8 \u00b1 0.9) km s^(-1)Mpc^(-1), a matter density parameter \u03a9_m = 0.308 \u00b1 0.012, and a tilted scalar spectral index with n_s = 0.968 \u00b1 0.006, consistent with the 2013 analysis. Note that in this abstract we quote 68% confidence limits on measured parameters and 95% upper limits on other parameters. We present the first results of polarization measurements with the Low Frequency Instrument at large angular scales. Combined with the Planck temperature and lensing data, these measurements give a reionization optical depth of \u03c4 = 0.066 \u00b1 0.016, corresponding to a reionization redshift of Z_(re) = 8.8^(+1.7)_(-1.4). These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. We find no evidence for any departure from base \u039bCDM in the neutrino sector of the theory; for example, combining Planck observations with other astrophysical data we find N_(eff) = 3.15 \u00b1 0.23 for the effective number of relativistic degrees of freedom, consistent with the value N_(eff) = 3.046 of the Standard Model of particle physics. The sum of neutrino masses is constrained to \u2211 m_\u03bd < 0.23 eV. The spatial curvature of our Universe is found to be very close to zero, with | \u03a9_K | < 0.005. Adding a tensor component as a single-parameter extension to base \u039bCDM we find an upper limit on the tensor-to-scalar ratio of r_(0.002)< 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP B-mode data to our analysis leads to a tighter constraint of r_(0.002) < 0.09 and disfavours inflationarymodels with a V(\u03c6) \u221d \u03c6^2 potential. The addition of Planck polarization data leads to strong constraints on deviations from a purely adiabatic spectrum of fluctuations. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w = \u22121.006 \u00b1 0.045, consistent with the expected value for a cosmological constant. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base \u039bCDM cosmology are in excellent agreement with observations. We also constraints on annihilating dark matter and on possible deviations from the standard recombination history. In neither case do we find no evidence for new physics. The Planck results for base \u039bCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. We show that these tensions cannot easily be resolved with simple modifications of the base \u039bCDM cosmology. Apart from these tensions, the base \u039bCDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A13", "id_number": "CaltechAUTHORS:20150918-070918069", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-070918069", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "616170" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000652/1" }, { "agency": "UK BIS National E-Infrastructure" }, { "agency": "University of Geneva" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525830", "primary_object": { "basename": "1502.01589v2.pdf", "url": "https://authors.library.caltech.edu/records/x1rn2-33y63/files/1502.01589v2.pdf" }, "related_objects": [ { "basename": "aa25830-15.pdf", "url": "https://authors.library.caltech.edu/records/x1rn2-33y63/files/aa25830-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/f8gw3-6cm87", "eprint_id": 60314, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:36", "lastmod": "2023-10-24 16:25:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIV. Dark energy and modified gravity", "ispublished": "pub", "full_text_status": "public", "keywords": "dark energy / cosmic background radiation / cosmology: theory / gravitation", "note": "\u00a9 2016 ESO. \n\nReceived 5 February 2015; Accepted 19 February 2016; Published online 20 September 2016. \n\nIt is a pleasure to thank Luca Amendola, Emilio Bellini, Diego Blas, Sarah Bridle, Noemi Frusciante, Catherine Heymans, Alireza Hojjati, Bin Hu, Thomas Kitching, Niall MacCrann, Marco Raveri, Ignacy Sawicki, Alessandra Silvestri, Fergus Simpson, Christof Wetterich and Gongbo Zhao for interesting discussions on theories, external data sets and numerical codes. Part of the analysis for this paper was run on the Andromeda and Perseus clusters of the University of Geneva and on WestGrid computers in Canada. We deeply thank Andreas Malaspinas for invaluable help with the Andromeda and Perseus Clusters. This research was partly funded by the DFG TransRegio TRR33 grant on \"The Dark Universe\" and by the Swiss NSF. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa25814-15.pdf
Submitted - 1502.01590v1.pdf
", "abstract": "We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG) beyond the standard cosmological constant scenario. We start with cases where the DE only directly affects the background evolution, considering Taylor expansions of the equation of state w(a), as well as principal component analysis and parameterizations related to the potential of a minimally coupled DE scalar field. When estimating the density of DE at early times, we significantly improve present constraints and find that it has to be below ~2% (at 95% confidence) of the critical density, even when forced to play a role for z < 50 only. We then move to general parameterizations of the DE or MG perturbations that encompass both effective field theories and the phenomenology of gravitational potentials in MG models. Lastly, we test a range of specific models, such as k-essence, f(R) theories, and coupled DE. In addition to the latest Planck data, for our main analyses, we use background constraints from baryonic acoustic oscillations, type-Ia supernovae, and local measurements of the Hubble constant. We further show the impact of measurements of the cosmological perturbations, such as redshift-space distortions and weak gravitational lensing. These additional probes are important tools for testing MG models and for breaking degeneracies that are still present in the combination of Planck and background data sets. All results that include only background parameterizations (expansion of the equation of state, early DE, general potentials in minimally-coupled scalar fields or principal component analysis) are in agreement with \u039bCDM. When testing models that also change perturbations (even when the background is fixed to \u039bCDM), some tensions appear in a few scenarios: the maximum one found is ~2\u03c3 for Planck TT+lowP when parameterizing observables related to the gravitational potentials with a chosen time dependence; the tension increases to, at most, 3\u03c3 when external data sets are included. It however disappears when including CMB lensing.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A14", "id_number": "CaltechAUTHORS:20150918-080156740", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-080156740", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TRR33" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525814", "primary_object": { "basename": "1502.01590v1.pdf", "url": "https://authors.library.caltech.edu/records/f8gw3-6cm87/files/1502.01590v1.pdf" }, "related_objects": [ { "basename": "aa25814-15.pdf", "url": "https://authors.library.caltech.edu/records/f8gw3-6cm87/files/aa25814-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/sqgt0-nz529", "eprint_id": 60286, "eprint_status": "archive", "datestamp": "2023-08-20 13:56:58", "lastmod": "2023-10-24 16:23:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIX. Constraints on primordial magnetic fields", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 19 February 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. 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 US Department of Energy under Contract No. DE-AC02-05CH11231. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa25821-15.pdf
Submitted - 1502.01594v1.pdf
", "abstract": "We compute and investigate four types of imprint of a stochastic background of primordial magnetic fields (PMFs) on the cosmic microwave background (CMB) anisotropies: the impact of PMFs on the CMB temperature and polarization spectra, which is related to their contribution to cosmological perturbations; the effect on CMB polarization induced by Faraday rotation; the impact of PMFs on the ionization history; magnetically-induced non-Gaussianities and related non-zero bispectra; and the magnetically-induced breaking of statistical isotropy. We present constraints on the amplitude of PMFs that are derived from different Planck data products, depending on the specific effect that is being analysed. Overall, Planck data constrain the amplitude of PMFs to less than a few nanoGauss, with different bounds that depend on the considered model. In particular, individual limits coming from the analysis of the CMB angular power spectra, using the Planck likelihood, are B_(1 Mpc) < 4.4 nG (where B_(1 Mpc) is the comoving field amplitude at a scale of 1\u2009Mpc) at 95% confidence level, assuming zero helicity. By considering the Planck likelihood, based only on parity-even angular power spectra, we obtain B_(1 Mpc) < 5.6 nG for a maximally helical field. For nearly scale-invariant PMFs we obtain B_(1 Mpc) < 2.0\u2009nG and B_(1 Mpc) < 0.9\u2009nG if the impact of PMFs on the ionization history of the Universe is included in the analysis. From the analysis of magnetically-induced non-Gaussianity, we obtain three different values, corresponding to three applied methods, all below 5\u2009nG. The constraint from the magnetically-induced passive-tensor bispectrum is B_(1 Mpc) < 2.8\u2009nG. A search for preferred directions in the magnetically-induced passive bispectrum yields B_(1 Mpc) < 4.5\u2009nG, whereas the compensated-scalar bispectrum gives B_(1 Mpc) < 3\u2009nG. The analysis of the Faraday rotation of CMB polarization by PMFs uses the Planck power spectra in EE and BB at 70\u2009GHz and gives B_(1 Mpc) < 1380\u2009nG. In our final analysis, we consider the harmonic-space correlations produced by Alfv\u00e9n waves, finding no significant evidence for the presence of these waves. Together, these results comprise a comprehensive set of constraints on possible PMFs with Planck data.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A19", "id_number": "CaltechAUTHORS:20150916-145551601", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-145551601", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525821", "primary_object": { "basename": "1502.01594v1.pdf", "url": "https://authors.library.caltech.edu/records/sqgt0-nz529/files/1502.01594v1.pdf" }, "related_objects": [ { "basename": "aa25821-15.pdf", "url": "https://authors.library.caltech.edu/records/sqgt0-nz529/files/aa25821-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/eyhw3-dfk52", "eprint_id": 60315, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:44", "lastmod": "2023-10-24 16:25:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XVII. Constraints on primordial non-Gaussianity", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmology: observations / cosmology: theory / early Universe / inflation / methods: data analysis", "note": "\u00a9 2016 ESO. \n\nReceived: 6 February 2015; Accepted: 27 January 2016;\nPublished online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. Part of this work was undertaken on the STFC COSMOS@DiRAC HPC Facility at the University of Cambridge, funded by UK BIS NEI grants. We gratefully acknowledge IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for the analysis with the binned bispectrum estimator. 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. We also acknowledge the IAP magique3 computer facilities. Some computations were performed on the GPC cluster at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, and the University of Toronto.\n\nPublished - aa25836-15.pdf
Submitted - 1502.01592v1.pdf
", "abstract": "The Planck full mission cosmic microwave background (CMB) temperature and E-mode polarization maps are analysed to obtain constraints on primordial non-Gaussianity (NG). Using three classes of optimal bispectrum estimators \u2013 separable template-fitting (KSW), binned, and modal \u2013 we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result from temperature alone \u0192^(local)_(NL) = 2.5 \u00b1 5.7, \u0192^(equil)_(NL)= -16 \u00b1 70, , and \u0192^(ortho)_(NL) = -34 \u00b1 32 (68% CL, statistical). Combining temperature and polarization data we obtain \u0192^(local)_(NL) = 0.8 \u00b1 5.0, \u0192^(equil)_(NL)= -4 \u00b1 43, and \u0192^(ortho)_(NL) = -26 \u00b1 21 (68% CL, statistical). The results are based on comprehensive cross-validation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are consistent with estimators based on measuring the Minkowski functionals of the CMB. The effect of time-domain de-glitching systematics on the bispectrum is negligible. In spite of these test outcomes we conservatively label the results including polarization data as preliminary, owing to a known mismatch of the noise model in simulations and the data. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and derive constraints on early universe scenarios that generate primordial NG, including general single-field models of inflation, axion inflation, initial state modifications, models producing parity-violating tensor bispectra, and directionally dependent vector models. We present a wide survey of scale-dependent feature and resonance models, accounting for the \"look elsewhere\" effect in estimating the statistical significance of features. We also look for isocurvature NG, and find no signal, but we obtain constraints that improve significantly with the inclusion of polarization. The primordial trispectrum amplitude in the local model is constrained to be g^(local)_(NL) = (\u22129.0\u00b17.7)\u00d710^4 (68% CL statistical), and we perform an analysis of trispectrum shapes beyond the local case. The global picture that emerges is one of consistency with the premises of the \u039bCDM cosmology, namely that the structure we observe today was sourced by adiabatic, passive, Gaussian, and primordial seed perturbations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A17", "id_number": "CaltechAUTHORS:20150918-082428843", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-082428843", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "UK BIS NEI Grants" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "University of Toronto" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525836", "primary_object": { "basename": "aa25836-15.pdf", "url": "https://authors.library.caltech.edu/records/eyhw3-dfk52/files/aa25836-15.pdf" }, "related_objects": [ { "basename": "1502.01592v1.pdf", "url": "https://authors.library.caltech.edu/records/eyhw3-dfk52/files/1502.01592v1.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/08mjd-84k07", "eprint_id": 96866, "eprint_status": "archive", "datestamp": "2023-08-20 14:07:24", "lastmod": "2023-10-20 21:34:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" } ] }, "title": "Planck 2015 results. XXIII. The thermal Sunyaev-Zeldovich effect-cosmic infrared background correlation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general \u2013 infrared: galaxies \u2013 large-scale structure of Universe \u2013 methods: data analysis", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 22 September 2015; Accepted 23 April 2016; Published online 20 September 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. We also acknowledge the support of the French Agence Nationale de la Recherche under grant ANR-11-BD56-015.\n\nPublished - aa27418-15.pdf
Submitted - 1509.06555.pdf
", "abstract": "We use Planck data to detect the cross-correlation between the thermal Sunyaev-Zeldovich (tSZ) effect and the infrared emission from the galaxies that make up the the cosmic infrared background (CIB). We first perform a stacking analysis towards Planck-confirmed galaxy clusters. We detect infrared emission produced by dusty galaxies inside these clusters and demonstrate that the infrared emission is about 50% more extended than the tSZ effect. Modelling the emission with a Navarro-Frenk-White profile, we find that the radial profile concentration parameter is c_(500) = 1.00^(+0.18)_(-0.15). This indicates that infrared galaxies in the outskirts of clusters have higher infrared flux than cluster-core galaxies. We also study the cross-correlation between tSZ and CIB anisotropies, following three alternative approaches based on power spectrum analyses: (i) using a catalogue of confirmed clusters detected in Planck data; (ii) using an all-sky tSZ map built from Planck frequency maps; and (iii) using cross-spectra between Planckfrequency maps. With the three different methods, we detect the tSZ-CIB cross-power spectrum at significance levels of (i) 6\u03c3; (ii) 3\u03c3; and (iii) 4\u03c3. We model the tSZ-CIB cross-correlation signature and compare predictions with the measurements. The amplitude of the cross-correlation relative to the fiducial model is A_(tSZ\u2212CIB) = 1.2 \u00b1 0.3. This result is consistent with predictions for the tSZ-CIB cross-correlation assuming the best-fit cosmological model from Planck 2015 results along with the tSZ and CIB scaling relations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A23", "id_number": "CaltechAUTHORS:20190701-132745145", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-132745145", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-11-BD56-015" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527418", "primary_object": { "basename": "1509.06555.pdf", "url": "https://authors.library.caltech.edu/records/08mjd-84k07/files/1509.06555.pdf" }, "related_objects": [ { "basename": "aa27418-15.pdf", "url": "https://authors.library.caltech.edu/records/08mjd-84k07/files/aa27418-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2mwb8-crd22", "eprint_id": 60318, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:55", "lastmod": "2023-10-24 16:25:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds", "ispublished": "pub", "full_text_status": "public", "keywords": "diffuse radiation / ISM: general / radiation mechanisms: general / radio continuum: ISM / polarization / local insterstellar matter", "note": "\u00a9 2016 ESO. \n\nReceived: 22 June 2015; Accepted: 20 April 2016; Published online 20 September 2016. \n\nThis paper is dedicated to the memory of the late Professor Rodney Deane Davies CBE FRS and Professor Richard John Davis OBE, both of whom contributed greatly to the Planck project. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research was supported by an ERC Starting (Consolidator) Grant (no. 307209) and STFC Consolidated Grant (no. ST/L000768/1). We have made extensive use of the HEALPix package and the IDL astronomy library. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.\n\nPublished - aa26803-15.pdf
Submitted - 1506.06660v1.pdf
", "abstract": "We discuss the Galactic foreground emission between 20 and 100\u2009GHz based on observations by Planck and WMAP. The total intensity in this part of the spectrum is dominated by free-free and spinning dust emission, whereas the polarized intensity is dominated by synchrotron emission. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with radio recombination line templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude H\u03b1 emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (\u224830%) of H\u03b1 having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in I_\u03bd) ranging from below 20\u2009GHz to more than 50\u2009GHz. There is a strong tendency for the spinning dust component near many prominent H\u2009II regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys, particularly at 5\u201320\u2009GHz, will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck and WMAP data to make the highest signal-to-noise ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. We argue that nearly all the emission at 40deg > l > \u221290deg is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. However, it does not continue as far as the \"Fermi bubble/microwave haze\", making it less probable that these are part of the same structure. We identify a number of new faint features in the polarized sky, including a dearth of polarized synchrotron emission directly correlated with a narrow, roughly 20deg long filament seen in H\u03b1 at high Galactic latitude. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2\u03c3 upper limit of 1.6% in the Perseus region.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A25", "id_number": "CaltechAUTHORS:20150918-100209126", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-100209126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "307209" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000768/1" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526803", "primary_object": { "basename": "1506.06660v1.pdf", "url": "https://authors.library.caltech.edu/records/2mwb8-crd22/files/1506.06660v1.pdf" }, "related_objects": [ { "basename": "aa26803-15.pdf", "url": "https://authors.library.caltech.edu/records/2mwb8-crd22/files/aa26803-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/f0qyk-mnn69", "eprint_id": 60320, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:03", "lastmod": "2023-10-24 16:25:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C." }, "orcid": "0000-0002-5627-5471" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXVI. The Second Planck Catalogue of Compact Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs / cosmology: observations / radio continuum: general / submillimeter: general", "note": "\u00a9 2016 ESO. \n\nReceived: 8 July 2015; Accepted: 28 January 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and, RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. We are grateful to the H-ATLAS Executive Committee and primarily to the PIs, S. Eales and L. Dunne, for permission to use the unpublished H-ATLAS catalogue for the validation of the present catalogue. This research has made use of the \"Aladin sky atlas\" (Bonnarel et al. 2000), developed at CDS, Strasbourg Observatory, France. Part of this work was performed using the Darwin Supercomputer of the University of Cambridge High Performance Computing Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc. using Strategic Research Infrastructure Funding from the HEFCE and funding from the STFC. 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 - aa26914-15.pdf
Submitted - 1507.02058v1.pdf
", "abstract": "The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogues, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalogue. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow us to increase the number of objects in the catalogue, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC).", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A26", "id_number": "CaltechAUTHORS:20150918-104502219", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-104502219", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Higher Education Funding Council for England (HEFCE)" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526914", "primary_object": { "basename": "aa26914-15.pdf", "url": "https://authors.library.caltech.edu/records/f0qyk-mnn69/files/aa26914-15.pdf" }, "related_objects": [ { "basename": "1507.02058v1.pdf", "url": "https://authors.library.caltech.edu/records/f0qyk-mnn69/files/1507.02058v1.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Beichman, C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/nvrhy-wp979", "eprint_id": 60323, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:18", "lastmod": "2023-10-24 16:25:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Pelkonen-Veli-Matti", "name": { "family": "Pelkonen", "given": "V.-M." }, "orcid": "0000-0002-8898-1047" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXVIII. The Planck Catalogue of Galactic Cold Clumps", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: clouds / ISM: structure / local insterstellar matter / stars: formation", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 16 August 2015; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa25819-15.pdf
Submitted - 1502.01599v1.pdf
", "abstract": "We present the Planck Catalogue of Galactic Cold Clumps (PGCC), an all-sky catalogue of Galactic cold clump candidates detected by Planck. This catalogue is the full version of the Early Cold Core (ECC) catalogue, which was made available in 2011 with the Early Release Compact Source Catalogue (ERCSC) and which contained 915 high signal-to-noise sources. It is based on the Planck 48-month mission data that are currently being released to the astronomical community. The PGCC catalogue is an observational catalogue consisting exclusively of Galactic cold sources. The three highest Planck bands (857, 454, and 353 GHz) have been combined with IRAS data at 3\u2009THz to perform a multi-frequency detection of sources colder than their local environment. After rejection of possible extragalactic contaminants, the PGCC catalogue contains 13188 Galactic sources spread across the whole sky, i.e., from the Galactic plane to high latitudes, following the spatial distribution of the main molecular cloud complexes. The median temperature of PGCC sources lies between 13 and 14.5\u2009K, depending on the quality of the flux density measurements, with a temperature ranging from 5.8 to 20\u2009K after removing the sources with the top 1% highest temperature estimates. Using seven independent methods, reliable distance estimates have been obtained for 5574 sources, which allows us to derive their physical properties such as their mass, physical size, mean density, and luminosity.The PGCC sources are located mainly in the solar neighbourhood, but also up to a distance of 10.5\u2009kpc in the direction of the Galactic centre, and range from low-mass cores to large molecular clouds. Because of this diversity and because the PGCC catalogue contains sources in very different environments, the catalogue is useful for investigating the evolution from molecular clouds to cores. Finally, it also includes 54 additional sources located in the Small and Large Magellanic Clouds.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. 28", "id_number": "CaltechAUTHORS:20150918-112734674", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-112734674", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525819", "primary_object": { "basename": "1502.01599v1.pdf", "url": "https://authors.library.caltech.edu/records/nvrhy-wp979/files/1502.01599v1.pdf" }, "related_objects": [ { "basename": "aa25819-15.pdf", "url": "https://authors.library.caltech.edu/records/nvrhy-wp979/files/aa25819-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Crill, B. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/27sv3-m0n68", "eprint_id": 67836, "eprint_status": "archive", "datestamp": "2023-08-20 12:01:17", "lastmod": "2023-10-18 21:47:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Fowler-J-W", "name": { "family": "Fowler", "given": "J. W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "The bandmerged Planck Early Release Compact Source Catalogue: probing sub-structure in the molecular gas at high Galactic latitude", "ispublished": "pub", "full_text_status": "public", "keywords": "radiation mechanisms: general catalogues surveys radio continuum: galaxies", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 February 25. Received 2016 February 25. In original form 2014 August 28. First published online March 2, 2016. \n\nWe thank the referee for thoughtful comments which improved the manuscript. We also thank Dr Clive Dickinson for helpful discussions in the preparation of this paper. This research has made use of the NASA/IPAC Extragalactic Database (NED) and NASA/IPAC Infrared Science Archive, which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Some of the results in this paper have been derived using the HEALPIX (G\u00f3rski et al. 2005) package.\n\nPublished - MNRAS-2016-Chen-3619-32.pdf
Submitted - 1602.07785v1.pdf
Supplemental Material - Table4_full.zip
", "abstract": "The Planck Early Release Compact Source Catalogue (ERCSC) includes nine lists of highly reliable sources, individually extracted at each of the nine Planck frequency channels. To facilitate the study of the Planck sources, especially their spectral behaviour across the radio/infrared frequencies, we provide a 'bandmerged' catalogue of the ERCSC sources. This catalogue consists of 15 191 entries, with 79 sources detected in all nine frequency channels of Planck and 6818 sources detected in only one channel. We describe the bandmerging algorithm, including the various steps used to disentangle sources in confused regions. The multifrequency matching allows us to develop spectral energy distributions of sources between 30 and 857 GHz, in particular across the 100 GHz band, where the energetically important CO J = 1\u21920 line enters the Planck bandpass. We find \u223c3\u03c3\u20135\u03c3 evidence for contribution to the 100 GHz intensity from foreground CO along the line of sight to 147 sources with |b|>30\u2218. The median excess contribution is 4.5 \u00b1 0.9 per cent of their measured 100 GHz flux density which cannot be explained by calibration or beam uncertainties. This translates to 0.5 \u00b1 0.1 K km s^(\u22121) of CO which must be clumped on the scale of the Planck 100 GHz beam, i.e. \u223c10\u2009arcmin. If this is due to a population of low-mass (\u223c15 M_\u2299) molecular gas clumps, the total mass in these clumps may be more than 2000 M_\u2299. Further, high-spatial-resolution, ground-based observations of the high-latitude sky will help shed light on the origin of this diffuse, clumpy CO emission.", "date": "2016-06-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "458", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3619-3632", "id_number": "CaltechAUTHORS:20160610-120649776", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160610-120649776", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stw479", "primary_object": { "basename": "1602.07785v1.pdf", "url": "https://authors.library.caltech.edu/records/27sv3-m0n68/files/1602.07785v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2016-Chen-3619-32.pdf", "url": "https://authors.library.caltech.edu/records/27sv3-m0n68/files/MNRAS-2016-Chen-3619-32.pdf" }, { "basename": "Table4_full.zip", "url": "https://authors.library.caltech.edu/records/27sv3-m0n68/files/Table4_full.zip" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Chen, X.; Chary, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fgrg0-a6258", "eprint_id": 67640, "eprint_status": "archive", "datestamp": "2023-08-20 11:36:00", "lastmod": "2023-10-18 21:20:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zhou-Luwenjia", "name": { "family": "Zhou", "given": "Luwenjia" } }, { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "D\u00edaz-Santos-T", "name": { "family": "Diaz-Santos", "given": "Taino" }, "orcid": "0000-0003-0699-6083" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "Aigen" } } ] }, "title": "Spatially resolved dust emission of extremely metal-poor galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf galaxies: ISM", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 February 10. Received 2016 February 10. In original form 2015 November 19. First published online March 1, 2016. \n\nWe thank the anonymous referee for helpful suggestions that improved the quality of the paper. LZ and YS acknowledge support for this work from the National Natural Science Foundation of China (grant 11373021), the Strategic Priority Research Program 'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences (grant No. XDB09000000), and Excellent Youth Foundation of Jiangsu Scientific Committee (grant BK20150014). LZ also thanks for the support by the National Natural Science Foundation of China (Grant No. J1210039). AL is supported in part by NSF AST-1311804 and NASA NNX14AF68G. This research has made extensive use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This 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.' The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in 2003 April. We acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission.\n\nPublished - MNRAS-2016-Zhou-772-80.pdf
Submitted - 1602.05362v1.pdf
", "abstract": "We present infrared (IR) spectral energy distributions (SEDs) of individual star-forming regions in four extremely metal-poor (EMP) galaxies with metallicity Z \u2272 Z_\u2299/10 as observed by the Herschel Space Observatory. With the good wavelength coverage of the SED, it is found that these EMP star-forming regions show distinct SED shapes as compared to those of grand design Spirals and higher metallicity dwarfs: they have on average much higher f_(70\u03bcm)/f_(160\u2009\u03bcm) ratios at a given f_(160\u2009\u03bcm)/f_(250\u2009\u03bcm) ratio; single modified blackbody (MBB) fittings to the SED at \u03bb \u2265 100 \u03bcm still reveal higher dust temperatures and lower emissivity indices compared to that of Spirals, while two MBB fittings to the full SED with a fixed emissivity index (\u03b2 = 2) show that even at 100 \u03bcm, about half of the emission comes from warm (50 K) dust, in contrast to the cold (\u223c20 K) dust component. Our spatially resolved images furthermore reveal that the far-IR colours including f_(70\u2009\u03bcm)/f_(160\u2009\u03bcm), f_(160\u2009\u03bcm)/f_(250\u2009\u03bcm) and f_(250\u2009\u03bcm)/f_(350\u2009\u03bcm) are all related to the surface densities of young stars as traced by far-UV, 24 \u03bcm and star formation rates (SFRs), but not to the stellar mass surface densities. This suggests that the dust emitting at wavelengths from 70 to 350 \u03bcm is primarily heated by radiation from young stars.", "date": "2016-05-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "458", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "772-780", "id_number": "CaltechAUTHORS:20160603-084605717", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160603-084605717", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Natural Science Foundation of China", "grant_number": "11373021" }, { "agency": "Chinese Academy of Sciences", "grant_number": "XDB09000000" }, { "agency": "Jiangsu Scientific Committee Excellent Youth Foundation", "grant_number": "BK20150014" }, { "agency": "National Natural Science Foundation of China", "grant_number": "J1210039" }, { "agency": "NSF", "grant_number": "AST-1311804" }, { "agency": "NASA", "grant_number": "NNX14AF68G" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stw345", "primary_object": { "basename": "1602.05362v1.pdf", "url": "https://authors.library.caltech.edu/records/fgrg0-a6258/files/1602.05362v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2016-Zhou-772-80.pdf", "url": "https://authors.library.caltech.edu/records/fgrg0-a6258/files/MNRAS-2016-Zhou-772-80.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Zhou, Luwenjia; Shi, Yong; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/basey-98994", "eprint_id": 65033, "eprint_status": "archive", "datestamp": "2023-08-20 10:10:55", "lastmod": "2023-10-17 23:08:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick M." }, "orcid": "0000-0002-3471-981X" }, { "id": "Lanz-L", "name": { "family": "Lanz", "given": "Lauranne" }, "orcid": "0000-0002-3249-8224" }, { "id": "Nader-C", "name": { "family": "Nader", "given": "Cyril" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Superluminous Spiral Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: spiral", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 October 30; accepted 2015 December 17; published 2016 January 26. \n\nThis work was made possible by the NASA/IPAC Extragalactic Database and the NASA/ IPAC Infrared Science Archive, which are both operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We thank Joe Mazzarella, Ben Chan, Marion Schmitz, and the rest of the NED team for useful discussions and their support of this work. This publication makes use of data from the Galaxy Evolution Explorer, retrieved from the Mikulski Archive for Space Telescopes (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 provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. 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 web site is www.sdss.org. 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 publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work 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. We also make use of data from Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We thank Katey Alatalo for providing the SDSS-WISE comparison data in Figure 1(a), which is adapted from Alatalo et al. (2014). We thank Phil Hopkins and Ski Antonucci for insightful discussions that contributed to the manuscript. Finally, we thank the anonymous referee for suggesting that we analyze available bulge-disk decompositions by Simard et al. (2009), strengthening our results.\n\nPublished - Ogle_2016p109.pdf
Submitted - 1511.00659v2.pdf
", "abstract": "We report the discovery of spiral galaxies that are as optically luminous as elliptical brightest cluster galaxies, with r-band monochromatic luminosity L_r = 8\u201314L* (4.3\u20137.5 \u00d7 10^(44) erg s^(\u22121)). These super spiral galaxies are also giant and massive, with diameter D = 57\u2013134 kpc and stellar mass M_(stars) = 0.3\u20133.4 \u00d7 10^(11)M\u2299. We find 53 super spirals out of a complete sample of 1616 SDSS galaxies with redshift z < 0.3 and L_r > 8L*. The closest example is found at z = 0.089. We use existing photometry to estimate their stellar masses and star formation rates (SFRs). The SDSS and Wide-field Infrared Survey Explorer colors are consistent with normal star-forming spirals on the blue sequence. However, the extreme masses and rapid SFRs of 5\u201365 M\u2299 yr^(\u22121) place super spirals in a sparsely populated region of parameter space, above the star-forming main sequence of disk galaxies. Super spirals occupy a diverse range of environments, from isolation to cluster centers. We find four super spiral galaxy systems that are late-stage major mergers\u2014a possible clue to their formation. We suggest that super spirals are a remnant population of unquenched, massive disk galaxies. They may eventually become massive lenticular galaxies after they are cut off from their gas supply and their disks fade.", "date": "2016-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "817", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 109", "id_number": "CaltechAUTHORS:20160303-144427138", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160303-144427138", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NASA", "grant_number": "NNX09AF08G" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" }, { "agency": "University of Utah" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/817/2/109", "primary_object": { "basename": "1511.00659v2.pdf", "url": "https://authors.library.caltech.edu/records/basey-98994/files/1511.00659v2.pdf" }, "related_objects": [ { "basename": "Ogle_2016p109.pdf", "url": "https://authors.library.caltech.edu/records/basey-98994/files/Ogle_2016p109.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ogle, Patrick M.; Lanz, Lauranne; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a1njw-h5f13", "eprint_id": 49919, "eprint_status": "archive", "datestamp": "2023-08-20 10:02:55", "lastmod": "2023-10-17 22:18:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck intermediate results. XXX. The angular power spectrum of polarized dust emission at intermediate and high Galactic latitudes", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 ISM: structure \u2013 ISM: magnetic fields \u2013 polarization", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 19 September 2014; Accepted 1 December 2014; Published online 09 February 2016.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaboration. Some of the results in this paper have been derived using the HEALPix package. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.\n\nPublished - aa25034-14.pdf
Submitted - 1409_5738.pdf
", "abstract": "The polarized thermal emission from diffuse Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100\u2009GHz. In this paper we exploit the uniqueness of the Planck HFI polarization data from 100 to 353\u2009GHz to measure the polarized dust angular power spectra C_\u2113^(EE) and C_\u2113^(BB) over the multipole range 40 <\u2113< 600 well away from the Galactic plane. These measurements will bring new insights into interstellar dust physics and allow a precise determination of the level of contamination for CMB polarization experiments. Despite the non-Gaussian and anisotropic nature of Galactic dust, we show that general statistical properties of the emission can be characterized accurately over large fractions of the sky using angular power spectra. The polarization power spectra of the dust are well described by power laws in multipole, C_\u2113 \u221d \u2113_\u03b1, with exponents \u03b1^(EE,BB) = \u22122.42 \u00b1 0.02. The amplitudes of the polarization power spectra vary with the average brightness in a way similar to the intensity power spectra. The frequency dependence of the dust polarization spectra is consistent with modified blackbody emission with \u03b2_d = 1.59 and T_d = 19.6 K down to the lowest Planck HFI frequencies. We find a systematic difference between the amplitudes of the Galactic B- and E-modes, C_\u2113^(BB)/C_\u2113^(EE) = 0.5. We verify that these general properties are preserved towards high Galactic latitudes with low dust column densities. We show that even in the faintest dust-emitting regions there are no \"clean\" windows in the sky where primordial CMB B-mode polarization measurements could be made without subtraction of foreground emission. Finally, we investigate the level of dust polarization in the specific field recently targeted by the BICEP2 experiment. Extrapolation of the Planck 353\u2009GHz data to 150\u2009GHz gives a dust power", "date": "2016-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "586", "publisher": "EDP Sciences", "pagerange": "Art. No. A133", "id_number": "CaltechAUTHORS:20140923-074019006", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140923-074019006", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201425034", "primary_object": { "basename": "1409_5738.pdf", "url": "https://authors.library.caltech.edu/records/a1njw-h5f13/files/1409_5738.pdf" }, "related_objects": [ { "basename": "aa25034-14.pdf", "url": "https://authors.library.caltech.edu/records/a1njw-h5f13/files/aa25034-14.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/58472-cc358", "eprint_id": 60324, "eprint_status": "archive", "datestamp": "2023-08-20 10:03:24", "lastmod": "2023-10-24 16:26:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 ISM: magnetic fields \u2013 ISM: clouds \u2013 dust, extinction \u2013 submillimeter: ISM \u2013 infrared: ISM", "note": "\u00a9 2016 ESO. Article published by EDP Sciences. \n\nReceived 13 February 2015; Accepted 25 May 2015. Published online 09 February 2016. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.\n\nPublished - aa25896-15.pdf
Accepted Version - 1502.04123v3.pdf
", "abstract": "Within ten nearby (d < \u2009450\u2009pc) Gould belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353\u2009GHz, and the gas column density structures, quantified by the gradient of the column density, N_H. The selected regions, covering several degrees in size, are analysed at an effective angular resolution of 10\u2032 FWHM, thus sampling physical scales from 0.4 to 40\u2009pc in the nearest cloud. The column densities in the selected regions range from N_H\u2248 10^(21) to10^(23)\u2009cm^(-2), and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analysed in bins of column density using the novel statistical tool called \"histogram of relative orientations\". Throughout this study, we assume that the polarized emission observed by Planck at 353\u2009GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing N_H, from mostly parallel or having no preferred orientation to mostly perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfv\u00e9nic or sub-Alfv\u00e9nic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution.", "date": "2016-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "586", "publisher": "EDP Sciences", "pagerange": "Art. No. A138", "id_number": "CaltechAUTHORS:20150918-114746985", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-114746985", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Institut national du patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "CSIC and RES (Spain)" }, { "agency": "Tekes and CSC (Finland)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Academy of Finland" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525896", "primary_object": { "basename": "1502.04123v3.pdf", "url": "https://authors.library.caltech.edu/records/58472-cc358/files/1502.04123v3.pdf" }, "related_objects": [ { "basename": "aa25896-15.pdf", "url": "https://authors.library.caltech.edu/records/58472-cc358/files/aa25896-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3pjqq-5ys40", "eprint_id": 96864, "eprint_status": "archive", "datestamp": "2023-08-20 10:09:35", "lastmod": "2023-10-20 21:34:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck intermediate results. XXXVIII. E- and B-modes of dust polarization from the magnetized filamentary structure of the interstellar medium", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 galaxies: ISM \u2013 submillimeter: ISM \u2013 ISM: general", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 9 May 2015; Accepted 22 September 2015; Published online 09 February 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007\u22122013)/ERC grant agreement No. 267934. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa26506-15.pdf
Accepted Version - 1505.02779.pdf
", "abstract": "The quest for a B-mode imprint from primordial gravity waves on the polarization of the cosmic microwave background (CMB) requires the characterization of foreground polarization from Galactic dust. We present a statistical study of the filamentary structure of the 353 GHz Planck Stokes maps at high Galactic latitude, relevant to the study of dust emission as a polarized foreground to the CMB. We filter the intensity and polarization maps to isolate filaments in the range of angular scales where the power asymmetry between E-modes and B-modes is observed. Using the Smoothed Hessian Major Axis Filament Finder (SMAFF), we identify 259 filaments at high Galactic latitude, with lengths larger or equal to 2\u00b0 (corresponding to 3.5\u2009pc in length for a typical distance of 100\u2009pc). Thesefilaments show a preferred orientation parallel to the magnetic field projected onto the plane of the sky, derived from their polarization angles. We present mean maps of the filaments in Stokes I, Q, U, E, and B, computed by stacking individual images rotated to align the orientations of the filaments. Combining the stacked images and the histogram of relative orientations, we estimate the mean polarization fraction of the filaments to be 11%. Furthermore, we show that the correlation between the filaments and the magnetic field orientations may account for the E and B asymmetry and the C_\u2113^(TE)/C_\u2113^(EE) ratio, reported in the power spectra analysis of the Planck353\u2009GHz polarization maps. Future models of the dust foreground for CMB polarization studies will need to take into account the observed correlation between the dust polarization and the structure of interstellar matter.", "date": "2016-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "586", "publisher": "EDP Sciences", "pagerange": "Art. No. A141", "id_number": "CaltechAUTHORS:20190701-115248899", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-115248899", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526506", "primary_object": { "basename": "1505.02779.pdf", "url": "https://authors.library.caltech.edu/records/3pjqq-5ys40/files/1505.02779.pdf" }, "related_objects": [ { "basename": "aa26506-15.pdf", "url": "https://authors.library.caltech.edu/records/3pjqq-5ys40/files/aa26506-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xrjc4-jtt87", "eprint_id": 62153, "eprint_status": "archive", "datestamp": "2023-08-20 09:49:48", "lastmod": "2023-10-25 16:54:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fox-O-D", "name": { "family": "Fox", "given": "Ori D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "Joel" }, "orcid": "0000-0001-5975-290X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Andrews-J-E", "name": { "family": "Andrews", "given": "Jennifer E." }, "orcid": "0000-0003-0123-0062" }, { "id": "Bally-J", "name": { "family": "Bally", "given": "John" }, "orcid": "0000-0001-8135-6612" }, { "id": "Bond-H-E", "name": { "family": "Bond", "given": "Howard E." }, "orcid": "0000-0003-1377-7145" }, { "id": "Boyer-M-L", "name": { "family": "Boyer", "given": "Martha L." }, "orcid": "0000-0003-4850-9589" }, { "id": "Gehrz-R-D", "name": { "family": "Gehrz", "given": "R. D." }, "orcid": "0000-0003-1319-4089" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "E. Y." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Parthasarathy-M", "name": { "family": "Parthasarathy", "given": "M." } }, { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Tinyanont-S", "name": { "family": "Tinyanont", "given": "Samaporn" }, "orcid": "0000-0002-1481-4676" }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" } ] }, "title": "An Excess of Mid-Infrared Emission from the Type Iax SN 2014dt", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 October 27; accepted 2015 December 17; published 2015 December 30. \n\nThis work is based on data obtained via Program #11063 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 an award issued by JPL/Caltech. The authors thank Ryan Foley for useful discussions. We thank Peter Milne, Jacob Jencson, and Tom Prince for help with observations.\n\nPublished - Fox_2016pL13.pdf
Submitted - 1510.08070v1.pdf
", "abstract": "Supernovae Type Iax (SNe Iax) are less energetic and less luminous than typical thermonuclear explosions. A suggested explanation for the observed characteristics of this subclass is a binary progenitor system consisting of a CO white dwarf primary accreting from a helium star companion. A single-degenerate explosion channel might be expected to result in a dense circumstellar medium (CSM), although no evidence for such a CSM has yet been observed for this subclass. Here we present recent Spitzer observations of the SN Iax 2014dt obtained by the SPIRITS program nearly one year post-explosion that reveal a strong mid-IR excess over the expected fluxes of more normal SNe Ia. This excess is consistent with 10^(\u22125) M_\u2299 of newly formed dust, which would be the first time that newly formed dust has been observed to form in a Type Ia. The excess, however, is also consistent with a dusty CSM that was likely formed in pre-explosion mass-loss, thereby suggesting a single degenerate progenitor system. Compared to other SNe Ia that show significant shock interaction (SNe Ia-CSM) and interacting core-collapse events (SNe IIn), this dust shell in SN 2014dt is less massive. We consider the implications that such a pre-existing dust shell has for the progenitor system, including a binary system with a mass donor that is a red giant, a red supergiant, or an asymptotic giant branch star.", "date": "2016-01-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "816", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 13", "id_number": "CaltechAUTHORS:20151117-084214250", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151117-084214250", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "11063" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/2041-8205/816/1/L13", "primary_object": { "basename": "1510.08070v1.pdf", "url": "https://authors.library.caltech.edu/records/xrjc4-jtt87/files/1510.08070v1.pdf" }, "related_objects": [ { "basename": "Fox_2016pL13.pdf", "url": "https://authors.library.caltech.edu/records/xrjc4-jtt87/files/Fox_2016pL13.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Fox, Ori D.; Johansson, Joel; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zy44d-pkm50", "eprint_id": 63138, "eprint_status": "archive", "datestamp": "2023-08-22 16:50:27", "lastmod": "2023-10-25 23:34:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Dong-Dillon", "name": { "family": "Dong", "given": "Dillon" }, "orcid": "0000-0001-9584-2531" }, { "id": "Leroy-A-K", "name": { "family": "Leroy", "given": "Adam K." }, "orcid": "0000-0002-2545-1700" }, { "id": "Momjian-E", "name": { "family": "Momjian", "given": "Emmanuel" }, "orcid": "0000-0003-3168-5922" }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "James J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Meier-D-S", "name": { "family": "Meier", "given": "David S." }, "orcid": "0000-0001-9436-9471" }, { "id": "Ott-J", "name": { "family": "Ott", "given": "J\u00fcrgen" }, "orcid": "0000-0001-8224-1956" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Turner-J-L", "name": { "family": "Turner", "given": "Jean L." }, "orcid": "0000-0003-4625-2951" } ] }, "title": "Microwave Continuum Emission and Dense Gas Tracers in NGC 3627: Combining Jansky VLA and ALMA Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 3627); galaxies: star formation; H ii regions; ISM: molecules; radio continuum: general", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 May 24; accepted 2015 August 21; published 2015 November 5. \n\nWe would like to thank the anonymous referee for useful comments that helped to improve the content and presentation of this paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00456.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This research has made use of the NASA/IPAC Extragalactic Database (NED), as well as the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - Murphy_2015.pdf
Submitted - 1508.06284v1.pdf
", "abstract": "We present Karl G. Jansky Very Large Array Ka band (33 GHz) and Atacama Large Millimeter Array (ALMA) Band 3 (94.5 GHz) continuum images covering the nucleus and two extranuclear star-forming regions within the nearby galaxy NGC 3627 (M 66), observed as part of the Star Formation in Radio Survey. Both images achieve an angular resolution of \u227e2\", allowing us to map radio spectral indices and estimate thermal radio fractions at a linear resolution of \u227e90 pc. The thermal fraction at 33 GHz reaches unity at and around the peaks of each H ii region; the spectral index between 33 and 94.5 GHz additionally becomes both increasingly negative and positive away from the H ii region peaks, indicating an increase of non-thermal emission from diffusing cosmic-ray electrons and the possible presence of cold dust, respectively. While the ALMA observations were optimized for collecting continuum data, they also detected line emission from the J = 1 \u2192 0 transitions of HCN and HCO^+. The peaks of dense molecular gas traced by these two spectral lines are spatially offset from the peaks of the continuum emission for both extranuclear star-forming regions, indicating that our data reach an angular resolution at which one can spatially distinguish sites of recent star formation from the sites of future star formation. Finally, we find trends of decreasing dense gas fraction and velocity dispersion with increasing star formation efficiency among the regions observed, indicating that the dynamical state of the dense gas, rather than its abundance, plays a more significant role in the star formation process.", "date": "2015-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "813", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 118", "id_number": "CaltechAUTHORS:20151222-105559496", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151222-105559496", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/813/2/118", "primary_object": { "basename": "1508.06284v1.pdf", "url": "https://authors.library.caltech.edu/records/zy44d-pkm50/files/1508.06284v1.pdf" }, "related_objects": [ { "basename": "Murphy_2015.pdf", "url": "https://authors.library.caltech.edu/records/zy44d-pkm50/files/Murphy_2015.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Murphy, Eric J.; Dong, Dillon; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ye6bm-w7j14", "eprint_id": 63063, "eprint_status": "archive", "datestamp": "2023-08-20 08:42:02", "lastmod": "2023-10-25 23:29:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Lanz-L", "name": { "family": "Lanz", "given": "L." }, "orcid": "0000-0002-3249-8224" }, { "id": "Bitsakis-T", "name": { "family": "Bitsakis", "given": "T." }, "orcid": "0000-0001-5787-8242" }, { "id": "Wang-J", "name": { "family": "Wang", "given": "J." } }, { "id": "Peterson-B-W", "name": { "family": "Peterson", "given": "B. W." } }, { "id": "Lisenfeld-U", "name": { "family": "Lisenfeld", "given": "U." }, "orcid": "0000-0002-9471-5423" }, { "id": "Alatalo-K", "name": { "family": "Alatalo", "given": "K." }, "orcid": "0000-0002-4261-2326" }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "P." }, "orcid": "0000-0002-2421-1350" }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "F." } }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "M." }, "orcid": "0000-0002-9871-6490" }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Y." }, "orcid": "0000-0003-0007-2197" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Struck-C-J", "name": { "family": "Struck", "given": "C." }, "orcid": "0000-0002-6490-2156" } ] }, "title": "X-Ray Emission from the Taffy (VV254) Galaxies and Bridge", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (UGC 12914, UGC12915, VV254)", "note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 July 16; accepted 2015 September 15; published 2015 October 14. \n\nWe thank an anonymous referee for very helpful comments that improved the manuscript. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14087X, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The work is also based, in part, on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Partial support for LL, PA & KA was also provided for Herschel observations, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Partial support for K.A. was also provided by NASA through Hubble Fellowship grant #HST-HF2-51352.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. J.W. acknowledges support from NSFC grants 11443003 and 11473021.\n\nPublished - Appleton_2015.pdf
Accepted Version - 1509.05314.pdf
", "abstract": "We present the first X-ray observations of the Taffy galaxies (UGC 12914/5) with the Chandra observatory and detect soft X-ray emission in the region of the gas-rich, radio-continuum-emitting Taffy bridge. The results are compared to Herschel observations of dust and diffuse [C ii] line-emitting gas. The diffuse component of the Taffy bridge has an X-ray luminosity of L_(X(0.5-8 keV) = 5.4 \u00d7 10^(39) erg s^(\u22121), which accounts for 19% of the luminosity of the sum for the two galaxies. The total mass in hot gas is (0.8\u20131.3) \u00d7 10^8 M_\u2299, which is approximately 1% of the total (H i + H_2) gas mass in the bridge, and ~11% of the mass of warm molecular hydrogen discovered by Spitzer. The soft X-ray and dense CO-emitting gas in the bridge have offset distributions, with the X-rays peaking along the northwestern side of the bridge in the region where stronger far-IR dust and diffuse [C ii] gas is observed by Herschel. We detect nine Ultra Luminous X-ray sources in the system, the brightest of which is found in the bridge, associated with an extragalactic H ii region. We suggest that the X-ray-emitting gas has been shocked\u2014heated to high temperatures and \"splashed\" into the bridge by the collision. The large amount of gas stripped from the galaxies into the bridge and its very long gas depletion timescale (>10 Gyr) may explain why this system, unlike most major mergers, is not a powerful IR emitter.", "date": "2015-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "812", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 118", "id_number": "CaltechAUTHORS:20151218-100045145", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151218-100045145", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF2-51352.001" }, { "agency": "NASA", "grant_number": "GO3-14087X" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11443003" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11473021" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/812/2/118", "primary_object": { "basename": "1509.05314.pdf", "url": "https://authors.library.caltech.edu/records/ye6bm-w7j14/files/1509.05314.pdf" }, "related_objects": [ { "basename": "Appleton_2015.pdf", "url": "https://authors.library.caltech.edu/records/ye6bm-w7j14/files/Appleton_2015.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Appleton, P. N.; Lanz, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y6gmb-8gw42", "eprint_id": 62619, "eprint_status": "archive", "datestamp": "2023-08-22 16:27:14", "lastmod": "2023-10-25 17:17:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O. P." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Vieira-Joaquin-D", "name": { "family": "Vieira", "given": "J. D." }, "orcid": "0000-0001-7192-3871" }, { "id": "Chary-Ranga-Ram", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results XXVII. High-redshift infrared galaxy overdensity candidates and lensed sources discovered by Planck and confirmed by Herschel-SPIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: clusters: general; galaxies: evolution; galaxies: star formation; cosmology: observations large-scale structure of Universe", "note": "\u00a9 2015 EDP Sciences. \n\nReceived 11 August 2014. Accepted 12 March 2015. \n\nThe development of Planck has been supported by: ESA;\nCNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of\nthe Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaborationhttp://www.sciops.esa.int index.php?project=planck. The Herschel spacecraft was designed, built, tested, and launched under a contract\nto ESA managed by the Herschel/Planck Project team by an industrial consortium under the overall responsibility of the prime contractor Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen) responsible for the payload module and for system testing at spacecraft level, Thales Alenia Space (Turin) responsible for the service module, and Astrium (Toulouse) responsible for the telescope, with in excess of a hundred subcontractors.\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Based in part 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 Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Based in part on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, and the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la\nRecherche Scientifique of France, and the University of Hawaii. Based in part on observations carried out with the IRAM 30-m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Based in part on observations carried out with the IRAM Plateau de Bure\nInterferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Based in part on observations made at JCMT with SCUBA-2. The James Clerk Maxwell Telescope is operated by the Joint Astronomy\nCentre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research\nhas 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\nacknowledge the support from the CNES, the PNCG (Programme National de Cosmologie et Galaxies), ANR HUGE (ANR-09-BLAN-0224-HUGE) and ANR MULTIVERSE (ANR-11-BS56-015). We also acknowledge the support from R\u00e9gion Ile-de-France with DIM-ACAV. We acknowledge the Integrated Data & Operation Center (IDOC) at Institut d'Astrophysique Spatiale and\nObservatoire des Sciences de l'Univers de l'Universit\u00e9 Paris Sud (OSUPS). Support for IDOC is provided by CNRS and CNES. We acknowledge final support from ASI/INAF agreement I/072/09/0 and PRIN-INAF 2012 project \"Looking into the dust-obscured phase of galaxy formation through cosmic\nzoom lenses in the Herschel Astrophysical Large Area Survey.\" We acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, cofunded by the European Social Fund and from the Ministerio de Economia y Competitividad, project AYA2012-39475-C02-01. This research made use of matplotlib Hunter (2007), and of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. We thank E. Egami, B. Cl\u00e9ment, E. Daddi, H. J. McCracken and A. Boucaud and for fruitful\ndiscussions and helpful advice.\n\nPublished - aa24790-14.pdf
Submitted - 1503.08773v2.pdf
", "abstract": "We have used the Planck all-sky submillimetre and millimetre maps to search for rare sources distinguished by extreme brightness, a few hundred millijanskies, and their potential for being situated at high redshift. These \"cold\" Planck sources, selected using the High Frequency Instrument (HFI) directly from the maps and from the Planck Catalogue of Compact Sources (PCCS), all satisfy the criterion of having their rest-frame far-infrared peak redshifted to the frequency range 353\u2013857 GHz. This colour-selection favours galaxies in the redshift range z = 2\u20134, which we consider as cold peaks in the cosmic infrared background. With a 4.'5 beam at the four highest frequencies, our sample is expected to include overdensities of galaxies in groups or clusters, lensed galaxies, and chance line-of-sight projections. We perform a dedicated Herschel-SPIRE follow-up of 234 such Planck targets, finding a significant excess of red 350 and 500\u03bcm sources, in comparison to reference SPIRE fields. About 94% of the SPIRE sources in the Planck fields are consistent with being overdensities of galaxies peaking at 350\u03bcm, with 3% peaking at 500\u03bcm, and none peaking at 250\u03bcm. About 3% are candidate lensed systems, all 12 of which have secure spectroscopic confirmations, placing them at redshifts z> 2.2. Only four targets are Galactic cirrus, yielding a success rate in our search strategy for identifying extragalactic sources within the Planck beam of better than 98%. The galaxy overdensities are detected with high significance, half of the sample showing statistical significance above 10\u03c3. The SPIRE photometric redshifts of galaxies in overdensities suggest a peak at z \u2243 2, assuming a single common dust temperature for the sources of T_d = 35 K. Under this assumption, we derive an infrared (IR) luminosity for each SPIRE source of about 4 \u00d7 10^(12)L_\u2299, yielding star formation rates of typically 700 M_\u2299 yr^(-1). If the observed overdensities are actual gravitationally-bound structures, the total IR luminosity of all their SPIRE-detected sources peaks at 4 \u00d7 10^(13)L_\u2299, leading to total star formation rates of perhaps 7 \u00d7 10^3M_\u2299 yr^(-1) per overdensity. Taken together, these sources show the signatures of high-z (z> 2) protoclusters of intensively star-forming galaxies. All these observations confirm the uniqueness of our sample compared to reference samples and demonstrate the ability of the all-skyPlanck-HFI cold sources to select populations of cosmological and astrophysical interest for structure formation studies.", "date": "2015-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "582", "publisher": "EDP Sciences", "pagerange": "Art. No. A30", "id_number": "CaltechAUTHORS:20151204-130040093", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151204-130040093", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "CSIC, MICINN, JA, and RES (Spain)" }, { "agency": "Tekes and CSC (Finland)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PRACE (EU)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Programme National de Cosmologie et Galaxies (PNCG)" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-09-BLAN-0224-HUGE" }, { "agency": "Agence Nationale de la Recherche (ANR)", "grant_number": "ANR-11-BS56-015" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/072/09/0" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Economia y Competitividad (MINECO)", "grant_number": "AYA2012-39475-C02-01" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "European Social Fund" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national du patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Academy of Finland" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424790", "primary_object": { "basename": "1503.08773v2.pdf", "url": "https://authors.library.caltech.edu/records/y6gmb-8gw42/files/1503.08773v2.pdf" }, "related_objects": [ { "basename": "aa24790-14.pdf", "url": "https://authors.library.caltech.edu/records/y6gmb-8gw42/files/aa24790-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Aghanim, N.; Dor\u00e9, O. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2q184-ja103", "eprint_id": 60280, "eprint_status": "archive", "datestamp": "2023-08-20 01:09:16", "lastmod": "2023-10-24 16:23:08", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "Frank" }, "orcid": "0000-0002-1707-1775" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M-C", "name": { "family": "Bradford", "given": "Matt" } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. Darren" } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "Jason" }, "orcid": "0000-0001-7527-2017" }, { "id": "Goldsmith-P-F", "name": { "family": "Goldsmith", "given": "Paul" }, "orcid": "0000-0002-6622-8396" }, { "id": "Harwit-M", "name": { "family": "Harwit", "given": "Martin" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Stacey-G-J", "name": { "family": "Stacey", "given": "Gordon" } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "Joaquin" } }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min" }, "orcid": "0000-0001-7095-7543" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" } } ] }, "title": "A complete view of galaxy evolution: panchromatic luminosity functions and the generation of metals", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted on 6 Mar 2009.\n\nSubmitted - 0903.1272v1.pdf
", "abstract": "When and how did galaxies form and their metals accumulate? Over the last decade, this has moved from an archeological question to a live investigation: there is now a broad picture of the evolution of galaxies in dark matter halos: their masses, stars, metals and supermassive blackholes. Galaxies have been found and studied in which these formation processes are taking place most vigorously, all the way back in cosmic time to when the intergalactic medium (IGM) was still largely neutral. However, the details of how and why the interstellar medium (ISM) in\ndistant galaxies cools, is processed, recycled and enriched in metals by stars, and fuels active\ngalactic nuclei (AGNs) remain uncertain. In particular, the cooling of gas to fuel star formation,\nand the chemistry and physics of the most intensely active regions is hidden from view at optical\nwavelengths, but can be seen and diagnosed at mid- & far-infrared (IR) wavelengths. Rest-frame\nIR observations are important first to identify the most luminous, interesting and important\ngalaxies, secondly to quantify accurately their total luminosity, and finally to use spectroscopy to\ntrace the conditions in the molecular and atomic gas out of which stars form. In order to map out\nthese processes over the full range of environments and large-scale structures found in the\nuniverse - from the densest clusters of galaxies to the emptiest voids \u2013 we require tools for deep,\nlarge area surveys, of millions of galaxies out to z~5, and for detailed follow-up spectroscopy.\nThe necessary tools can be realized technically. Here, we outline the requirements for gathering\nthe crucial information to build, validate and challenge models of galaxy evolution.", "date": "2015-09-16", "date_type": "published", "id_number": "CaltechAUTHORS:20150916-130227932", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-130227932", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.0903.1272", "primary_object": { "basename": "0903.1272v1.pdf", "url": "https://authors.library.caltech.edu/records/2q184-ja103/files/0903.1272v1.pdf" }, "resource_type": "monograph", "pub_year": "2015", "author_list": "Blain, Andrew W.; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/haa3c-fxs78", "eprint_id": 60277, "eprint_status": "archive", "datestamp": "2023-09-15 05:07:07", "lastmod": "2023-10-23 21:13:55", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Green-J", "name": { "family": "Green", "given": "J." } }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "C." }, "orcid": "0000-0002-2951-4932" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "L." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Cutri-R-M", "name": { "family": "Cutri", "given": "R." }, "orcid": "0000-0002-0077-2305" } ] }, "title": "Wide-Field InfraRed Survey Telescope WFIRST Final Report", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - 1208.4012v1.pdf
", "abstract": "In December 2010, NASA created a Science Definition Team (SDT) for WFIRST, the Wide Field Infra-Red Survey Telescope, recommended by the Astro 2010 Decadal Survey as the highest priority for a large space mission. The SDT was chartered to work with the WFIRST Project Office at GSFC and the Program Office at JPL to produce a Design Reference Mission (DRM) for WFIRST. Part of the original charge was to produce an interim design reference mission by mid-2011. That document was delivered to NASA and widely circulated within the astronomical community. In late 2011 the Astrophysics Division augmented its original charge, asking for two design reference missions. The first of these, DRM1, was to be a finalized version of the interim DRM, reducing overall mission costs where possible. The second of these, DRM2, was to identify and eliminate capabilities that overlapped with those of NASA's James Webb Space Telescope (henceforth JWST), ESA's Euclid mission, and the NSF's ground-based Large Synoptic Survey Telescope (henceforth LSST), and again to reduce overall mission cost, while staying faithful to NWNH. This report presents both DRM1 and DRM2.", "date": "2015-09-16", "date_type": "published", "publisher": "NASA", "id_number": "CaltechAUTHORS:20150916-110407615", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-110407615", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.1208.4012", "primary_object": { "basename": "1208.4012v1.pdf", "url": "https://authors.library.caltech.edu/records/haa3c-fxs78/files/1208.4012v1.pdf" }, "resource_type": "monograph", "pub_year": "2015", "author_list": "Green, J.; Hirata, C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/2b7nr-g4v82", "eprint_id": 62536, "eprint_status": "archive", "datestamp": "2023-08-20 08:01:41", "lastmod": "2023-10-25 17:14:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Cheng-Yu-Chi", "name": { "family": "Cheng", "given": "Yu-Chi" } }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Kinoshita-Daisuke", "name": { "family": "Kinoshita", "given": "Daisuke" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas" }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: general \u2013 surveys", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 March 4; accepted 2015 April 15; published 2015 August 18.\n\nThis work uses data obtained with the 1.2 m Samuel Oschin\nTelescope at Palomar Observatory as part of the PTF, a\nscientific collaboration between the California Institute of\nTechnology (Caltech), Columbia University, Las Cumbres\nObservatory Global Telescope Network, Lawrence Berkeley\nNational Laboratory, the National Energy Research Scientific\nComputing Center, the University of Oxford, and the\nWeizmann Institute of Science (WIS).\nSome data in this work (also from the 1.2 m Oschin\nTelescope) were obtained as part of the iPTF project, a\ncollaboration among Caltech, the Kavli Institute for the Physics\nand Mathematics of the universe, Los Alamos National\nLaboratory, the Oskar Klein Centre, the University System of\nTaiwan, the University of Wisconsin Milwaukee, and WIS.\nA. Waszczak has been supported in part by the W. M. Keck\nInstitute for Space Studies (KISS) at Caltech. E.O.O. is\nincumbent of the Arye Dissentshik career development chair\nand is grateful to support by grants from the Willner Family\nLeadership Institute Ilan Gluzman (Secaucus NJ), Israeli\nMinistry of Science, Israel Science Foundation, Minerva and\nthe I-CORE Program of the Planning and Budgeting\nCommittee, and The Israel Science Foundation.\nThis work also makes use of data products from the\nWide-Field Infrared Survey Explorer, a joint project of the\nUniversity of California Los Angeles and the Jet Propulsion\nLaboratory (JPL)/Caltech, funded by NASA. This work also\nmakes use of data from NEOWISE, which is a project of JPL/\nCaltech, funded by the Planetary Science Division of NASA.\nThis work also makes use of data from the SDSS, managed\nby the Astrophysical Research Consortium for the Participating\nInstitutions and funded by the Alfred P. Sloan Foundation, the\nParticipating Institutions, the National Science Foundation, the\nUS Department of Energy, NASA, the Japanese Monbukagakusho,\nthe Max Planck Society, and the Higher Education\nCouncil for England.\nLastly, we thank an anonymous reviewer for helpful\ncomments and feedback.\n\nPublished - Waszczak_2015p75.pdf
Submitted - 1504.04041v1.pdf
", "abstract": "We fit 54,296 sparsely sampled asteroid light curves in the Palomar Transient Factory survey to a combined rotation plus phase-function model. Each light curve consists of 20 or more observations acquired in a single opposition. Using 805 asteroids in our sample that have reference periods in the literature, we find that the reliability of our fitted periods is a complicated function of the period, amplitude, apparent magnitude, and other light-curve attributes. Using the 805-asteroid ground-truth sample, we train an automated classifier to estimate (along with manual inspection) the validity of the remaining ~53,000 fitted periods. By this method we find that 9033 of our light curves (of ~8300 unique asteroids) have \"reliable\" periods. Subsequent consideration of asteroids with multiple light-curve fits indicates a 4% contamination in these \"reliable\" periods. For 3902 light curves with sufficient phase-angle coverage and either a reliable fit period or low amplitude, we examine the distribution of several phase-function parameters, none of which are bimodal though all correlate with the bond albedo and with visible-band colors. Comparing the theoretical maximal spin rate of a fluid body with our amplitude versus spin-rate distribution suggests that, if held together only by self-gravity, most asteroids are in general less dense than ~2 g cm^(\u22123), while C types have a lower limit of between 1 and 2 g cm^(\u22123). These results are in agreement with previous density estimates. For 5\u201320 km diameters, S types rotate faster and have lower amplitudes than C types. If both populations share the same angular momentum, this may indicate the two types' differing ability to deform under rotational stress. Lastly, we compare our absolute magnitudes (and apparent-magnitude residuals) to those of the Minor Planet Center's nominal (G = 0.15, rotation-neglecting) model; our phase-function plus Fourier-series fitting reduces asteroid photometric rms scatter by a factor of ~3.", "date": "2015-09", "date_type": "published", "publication": "Astronomical Journal", "volume": "150", "number": "3", "publisher": "American Astronomical Society", "pagerange": "Art. No. 75", "id_number": "CaltechAUTHORS:20151202-095604264", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151202-095604264", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Institute for Space Studies" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "NASA" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "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": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-6256/150/3/75", "primary_object": { "basename": "1504.04041v1.pdf", "url": "https://authors.library.caltech.edu/records/2b7nr-g4v82/files/1504.04041v1.pdf" }, "related_objects": [ { "basename": "Waszczak_2015p75.pdf", "url": "https://authors.library.caltech.edu/records/2b7nr-g4v82/files/Waszczak_2015p75.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Waszczak, Adam; Chang, Chan-Kao; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/m4t5f-6qh44", "eprint_id": 60287, "eprint_status": "archive", "datestamp": "2023-08-20 07:32:20", "lastmod": "2023-10-24 16:23:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ergon-M", "name": { "family": "Ergon", "given": "M." } }, { "id": "Jerkstrand-A", "name": { "family": "Jerkstrand", "given": "A." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Elias-Rosa-N", "name": { "family": "Elias-Rosa", "given": "N." }, "orcid": "0000-0002-1381-9125" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Fraser-M", "name": { "family": "Fraser", "given": "M." }, "orcid": "0000-0003-2191-1674" }, { "id": "Pastorello-A", "name": { "family": "Pastorello", "given": "A." } }, { "id": "Kotak-R", "name": { "family": "Kotak", "given": "R." }, "orcid": "0000-0001-5455-3653" }, { "id": "Taubenberger-S", "name": { "family": "Taubenberger", "given": "S." }, "orcid": "0000-0002-4265-1958" }, { "id": "Tomasella-L", "name": { "family": "Tomasella", "given": "L." } }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Benetti-S", "name": { "family": "Benetti", "given": "S." }, "orcid": "0000-0002-3256-0016" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Maund-J-R", "name": { "family": "Maund", "given": "J." }, "orcid": "0000-0003-0733-7215" }, { "id": "Smartt-S-J", "name": { "family": "Smartt", "given": "S. J." }, "orcid": "0000-0002-8229-1731" }, { "id": "Spyromilio-J", "name": { "family": "Spyromilio", "given": "J." }, "orcid": "0000-0001-6815-4055" } ] }, "title": "The Type IIb SN 2011dh: Two years of observations and modelling of the lightcurves", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual: SN 2008ax \u2013 supernovae: individual: SN 2011dh \u2013 galaxies: individual: M 51 \u2013\nsupernovae: general \u2013 supernovae: individual: SN 1993J", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived: 11 July 2014; Accepted: 9 January 2015; Published online 21 August 2015. \n\nThis work is based on observations obtained with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrof\u00edsica de Canarias; the German-Spanish Astronomical Center, Calar Alto, jointly operated by the Max-Planck-Institut f\u00fcr Astronomie Heidelberg and the Instituto de Astrof\u00edsica de Andaluc\u00eda (CSIC); the United Kingdom Infrared Telescope, operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK; the William Herschel Telescope and its service programme (proposals SW2011b21 and SW2012a02), operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias; the Copernico 1.82m Telescope and Schmidt 67/92 Telescope operated by INAF \u2013 Osservatorio Astronomico di Padova at Asiago, Italy; by the 3.6m Italian Telescopio Nazionale Galileo operated by the Fundaci\u00f3n Galileo Galilei \u2013 INAF on the island of La Palma; the Liverpool Telescope, operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias with financial support from the UK Science and Technology Facilities Council; the AlbaNova telescope operated by the Department of Astronomy at Stockholm University and funded by a grant from the Knut and Alice Wallenberg Foundation; the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias, in the island of La Palma. We acknowledge the exceptional support we got from the NOT staff throughout this campaign, we thank the Calar Alto Observatory for the allocation of the director's discretionary time and we thank Philip Dufton, Paul Dunstall, Darryl Wright and Lindsay Magill for assistance with the WHT observations. The Oskar Klein Centre is funded by the Swedish Research Council. J.S. acknowledge support by the Swedish Research Council. S.J.S. thanks European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no [291222] and STFC. A.P., L.T. and S.B. are partially supported by the PRIN-INAF 2011 with the project \"Transient Universe: from ESO Large to PESSTO\". M.F. acknowledges support by the European Union FP7 programme through ERC grant number 320360. N.E.R. acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 \"Astronomy Fellowships in Italy\" (AstroFIt). R.K. acknowledges observing time at the LT, NOT, TNG, and WHT via programme CCI-04. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. We thank Melina Bersten for providing the post-explosion density profile for the He4R270 model (B12), for inspiration and a great contribution to the understanding of SN 2011dh. We thank Peter Meikle and Dan Milisavljevic for providing spectra on SN 1993J and SN 2008ax, respectively.\n\nPublished - aa24592-14.pdf
Submitted - 1408.0731v2.pdf
", "abstract": "We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset, for which we present the observations obtained after day 100, spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732. To model the bolometric lightcurve before day 400 we use a grid of hydrodynamical SN models, which allows us to determine the errors in the derived quantities, and a bolometric correction determined with steady-state non-local thermodynamic equilibrium (NLTE) modelling. Using this method we find a helium core mass of 3.1^(+0.7)_(-0.4) M\u2299 for SN 2011dh, consistent within error bars with previous results obtained using the bolometric lightcurve before day 80. We compute bolometric and broad-band lightcurves between days 100 and 500 from spectral steady-state NLTE models, presented and discussed in a companion paper. The preferred 12 M\u2299 (initial mass) model, previously found to agree well with the observed spectra, shows a good overall agreement with the observed lightcurves, although some discrepancies exist. Time-dependent NLTE modelling shows that after day ~600 a steady-state assumption is no longer valid. The radioactive energy deposition in this phase is likely dominated by the positrons emitted in the decay of ^(56)Co, but seems insufficient to reproduce the lightcurves, and what energy source is dominating the emitted flux is unclear. We find an excess in the K and the MIR bands developing between days 100 and 250, during which an increase in the optical decline rate is also observed. A local origin of the excess is suggested by the depth of the He\u2009I 20\u2009581 \u00c5 absorption. Steady-state NLTE models with a modest dust opacity in the core (\u03c4 = 0.44), turned on during this period, reproduce the observed behaviour, but an additional excess in the Spitzer 4.5 \u03bcm band remains. Carbon-monoxide (CO) first-overtone band emission is detected at day 206, and possibly at day 89, and assuming the additional excess to bedominated by CO fundamental band emission, we find fundamental to first-overtone band ratios considerably higher than observed in SN 1987A. The profiles of the [O\u2009I] 6300 \u00c5 and Mg\u2009I] 4571 \u00c5 lines show a remarkable similarity, suggesting that these lines originate from a common nuclear burning zone (O/Ne/Mg), and using small scale fluctuations in the line profiles we estimate a filling factor of \u22720.07 for the emitting material. This paper concludes our extensive observational and modelling work on SN 2011dh. The results from hydrodynamical modelling, steady-state NLTE modelling, and stellar evolutionary progenitor analysis are all consistent, and suggest an initial mass of ~12 M\u2299 for the progenitor.", "date": "2015-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "580", "publisher": "EDP Sciences", "pagerange": "Art. No. A142", "id_number": "CaltechAUTHORS:20150916-153118277", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-153118277", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "European Research Council (ERC)", "grant_number": "291222" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "European Research Council (ERC)", "grant_number": "320360" }, { "agency": "European Research Council (ERC)", "grant_number": "267251" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201424592", "primary_object": { "basename": "1408.0731v2.pdf", "url": "https://authors.library.caltech.edu/records/m4t5f-6qh44/files/1408.0731v2.pdf" }, "related_objects": [ { "basename": "aa24592-14.pdf", "url": "https://authors.library.caltech.edu/records/m4t5f-6qh44/files/aa24592-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ergon, M.; Jerkstrand, A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/maf2t-e2q55", "eprint_id": 58570, "eprint_status": "archive", "datestamp": "2023-08-20 06:57:45", "lastmod": "2023-10-23 15:22:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Werner-M-W", "name": { "family": "Werner", "given": "M. W." } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L." }, "orcid": "0000-0002-5987-5210" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Spitzer's stellar work", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2015 American Association for the Advancement of Science.", "abstract": "In the News Feature \"After Hubble\" (24 April, p. 388), D. Clery inappropriately characterizes the Spitzer Space Telescope as \"now largely blind.\" In fact, Spitzer is alive and well and continuing to make substantial contributions to the advancement of astrophysics and to scientific preparations for the James Webb Space Telescope (JWST). The exhaustion of Spitzer's cryogen in mid-2009 left the observatory with two functioning imaging arrays at wavelengths of 3.6 and 4.5 \u00b5m. The performance of what is now called \"Warm\" Spitzer at these wavelengths matches that achieved during the cryogenic mission. Despite its small size, Spitzer is by far the most sensitive telescope, space or ground, available at these wavelengths. The science community has used Warm Spitzer for important scientific investigations, including studies of exoplanets, the early universe, variable stars to define better the cosmic distance ladder, clusters of galaxies, near-Earth asteroids, and comets. Spitzer remains very much in demand; for the past 2 years, the oversubscription for requested observing time has been the highest of the mission.", "date": "2015-06-19", "date_type": "published", "publication": "Science", "volume": "348", "number": "6241", "publisher": "American Association for the Advancement of Science", "pagerange": "1326", "id_number": "CaltechAUTHORS:20150624-083530992", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150624-083530992", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1126/science.348.6241.1326-a", "resource_type": "article", "pub_year": "2015", "author_list": "Werner, M. W.; Soifer, B. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/pkags-dre75", "eprint_id": 56847, "eprint_status": "archive", "datestamp": "2023-08-22 15:30:23", "lastmod": "2023-10-23 16:02:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Wang-Junzhi", "name": { "family": "Wang", "given": "Junzhi" } }, { "id": "Zhang-Zhi-Yu", "name": { "family": "Zhang", "given": "Zhi-Yu" }, "orcid": "0000-0002-7299-2876" }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Yu" }, "orcid": "0000-0003-0007-2197" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Gu-Qiusheng", "name": { "family": "Gu", "given": "Qiusheng" }, "orcid": "0000-0002-3890-3729" }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" } ] }, "title": "The Weak Carbon Monoxide Emission In An Extremely Metal Poor Galaxy, Sextans A", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; galaxies: ISM; submillimeter: ISM", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 January 21; accepted 2015 April 3; published 2015 April 24. \n\nBased on observations carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). \n\nWe thank the anonymous referee for constructive comments that significantly improved the paper. Y.S. acknowledges support for this work from Natural Science Foundation of China under grant 11373021 and by the Strategic Priority Research Program \"The Emergence of Cosmological Structures\" of the Chinese Academy of Sciences, grant No. XDB09000000. Y.G. is supported under grants 11390373, 11420101002, and XDB09000000. Z.Y.Z. acknowledges support from the European Research Council (ERC) in the form of an Advanced Grant, COSMICISM.\n\nPublished - Shi_2015_ApJL_804_L11.pdf
Submitted - 1504.01453v1.pdf
", "abstract": "Carbon monoxide (CO) is one of the primary coolants of gas and an easily accessible tracer of molecular gas in spiral galaxies, but it is unclear if CO plays a similar role in metal-poor dwarfs. We carried out a deep observation with IRAM 30 m to search for CO emission by targeting the brightest far-IR peak in a nearby extremely metal-poor galaxy, Sextans A, with 7% solar metallicity. A marginal signal of CO J = 1 \u2212 0 emission is seen, which is already faint enough to place a strong constraint on the conversion factor (\u0251_(CO)) from the CO luminosity to the molecular gas mass that is derived from the spatially resolved dust-mass map. The \u0251_(CO) is at least seven hundred times the Milky Way value. This indicates that CO emission is exceedingly weak in Sextans A, challenging its role as a coolant in extremely metal-poor galaxies.", "date": "2015-05-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "804", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L11", "id_number": "CaltechAUTHORS:20150421-194124894", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150421-194124894", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11373021" }, { "agency": "Chinese Academy of Sciences", "grant_number": "XDB09000000" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11390373" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11420101002" }, { "agency": "European Research Council (ERC)", "grant_number": "COSMICISM" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/804/1/L11", "primary_object": { "basename": "Shi_2015_ApJL_804_L11.pdf", "url": "https://authors.library.caltech.edu/records/pkags-dre75/files/Shi_2015_ApJL_804_L11.pdf" }, "related_objects": [ { "basename": "1504.01453v1.pdf", "url": "https://authors.library.caltech.edu/records/pkags-dre75/files/1504.01453v1.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Shi, Yong; Wang, Junzhi; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9wk8x-ar667", "eprint_id": 56933, "eprint_status": "archive", "datestamp": "2023-08-22 15:16:20", "lastmod": "2023-10-23 16:09:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Bianchi-S", "name": { "family": "Bianchi", "given": "S." }, "orcid": "0000-0002-4622-4240" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hinz-J-L", "name": { "family": "Hinz", "given": "J. L." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Wilson-C-D", "name": { "family": "Wilson", "given": "C. D." }, "orcid": "0000-0001-5817-0991" }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "A." }, "orcid": "0000-0002-5480-5686" }, { "id": "Boquien-M", "name": { "family": "Boquien", "given": "M." }, "orcid": "0000-0003-0946-6176" }, { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "K. V." }, "orcid": "0000-0002-5258-7224" }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Gil-de-Paz-A", "name": { "family": "Gil de Paz", "given": "A." }, "orcid": "0000-0001-6150-2854" }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Mu\u00f1oz-Mateos-J-C", "name": { "family": "Mu\u00f1oz-Mateos", "given": "J. C." } }, { "id": "Sandstrom-K-M", "name": { "family": "Sandstrom", "given": "K. M." }, "orcid": "0000-0002-4378-8534" }, { "id": "Sauvage-M", "name": { "family": "Sauvage", "given": "M." } }, { "id": "Vigroux-L", "name": { "family": "Vigroux", "given": "L." } }, { "id": "Zibetti-S", "name": { "family": "Zibetti", "given": "S." } } ] }, "title": "Cool dust heating and temperature mixing in nearby star-forming galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; dust, extinction; galaxies: star formation", "note": "\u00a9 2015 ESO.\n\nReceived 1 August 2014; Accepted 16 September 2014.\n\nWe dedicate this paper to the memory of Charles W. Engelbracht, whose excellence and commitment as a scientist were fundamental for this work, and without whom the SPIRE images analyzed here would not have existed. We thank the anonymous referee for concise comments which improved the clarity of the paper. S.B. and L.K.H. acknowledge support from PRIN-INAF 2012/13. B.T.D. was supported in part by NSF grant AST-1408723. Use was made of the NASA/IPAC Extragalactic Database (NED).\n\nPublished - aa24734-14.pdf
Accepted Version - 1409.5916v1.pdf
", "abstract": "Physical conditions of the interstellar medium in galaxies are closely linked to the ambient radiation field and the heating of dust grains. In order to characterize dust properties in galaxies over a wide range of physical conditions, we present here the radial surface brightness profiles of the entire sample of 61 galaxies from Key Insights into Nearby Galaxies: Far-Infrared Survey with Herschel (KINGFISH). The main goal of our work is the characterization of the grain emissivities, dust temperatures, and interstellar radiation fields (ISRFs) responsible for heating the dust. We first fit the radial profiles with exponential functions in order to compare stellar and cool-dust disk scalelengths, as measured by 3.6 \u03bcm and 250 \u03bcm surface brightnesses. Our results show that the stellar and dust scalelengths are comparable, with a mean ratio of 1.04, although several galaxies show dust-to-stellar scalelength ratios of 1.5 or more. We then fit the far-infrared spectral energy distribution (SED) in each annular region with single-temperature modified blackbodies using both variable (MBBV) and fixed (MBBF) emissivity indices \u03b2, as well as with physically motivated dust models. The KINGFISH profiles are well suited to examining trends of dust temperature T_(dust) and \u03b2 because they span a factor of ~200 in the ISRF intensity heating the bulk of the dust mass, U_(min). Results from fitting the profile SEDs suggest that, on average, T_(dust), dust optical depth \u03c4_(dust), and U_(min) decrease with radius. The emissivity index \u03b2 also decreases with radius in some galaxies, but in others is increasing, or rising in the inner regions and falling in the outer ones. Despite the fixed grain emissivity (average \u03b2 ~ 2.1) of the physically-motivated models, they are well able to accommodate flat spectral slopes with \u03b2 \u2272 1. An analysis of the wavelength variations of dust emissivities in both the data and the models shows that flatter slopes (\u03b2 \u2272 1.5) are associated with cooler temperatures, contrary to what would be expected from the usual T_(dust) \u2013 \u03b2 degeneracy. This trend is related to variations in U_(min) since \u03b2 and U_(min) are very closely linked over the entire range in U_(min) sampled by the KINGFISH galaxies: low U_(min) is associated with flat \u03b2 \u2272 1. Both these results strongly suggest that the low apparent \u03b2 values (flat slopes) in MBBV fits are caused by temperature mixing along the line of sight, rather than by intrinsic variations in grain properties. Finally, a comparison of dust models and the data show a slight ~10% excess at 500 \u03bcm for low metallicity (12 + log\u2009 (O/H) \u2272 8) and low far-infrared surface brightness (\u03a3500).", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A33", "id_number": "CaltechAUTHORS:20150423-153439902", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150423-153439902", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NSF", "grant_number": "AST-1408723" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201424734", "primary_object": { "basename": "1409.5916v1.pdf", "url": "https://authors.library.caltech.edu/records/9wk8x-ar667/files/1409.5916v1.pdf" }, "related_objects": [ { "basename": "aa24734-14.pdf", "url": "https://authors.library.caltech.edu/records/9wk8x-ar667/files/aa24734-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Hunt, L. K.; Draine, B. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9wvj8-b8a66", "eprint_id": 59384, "eprint_status": "archive", "datestamp": "2023-08-20 05:39:40", "lastmod": "2023-10-23 20:32:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 dust, extinction \u2013 ISM: magnetic fields \u2013 ISM: clouds \u2013 submillimeter: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 28 April 2014; Accepted 30 January 2015; Published online 13 April 2015. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/M CTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ ERC grant agreement no 267934 and from a joint agreement between University of S\u00e3o Paulo, Brazil, and COFECUB, France (grant nos. USP 2007.1.433.14.2 and COFECUB Uc Te 114/08). We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa24082-14.pdf
Submitted - 1405.0871v1.pdf
", "abstract": "This paper presents an overview of the polarized sky as seen by Planck HFI at 353 GHz, which is the most sensitive Planck channel for dust polarization. We construct and analyse maps of dust polarization fraction and polarization angle at 1\u00b0 resolution, taking into account noise bias and possible systematic effects. The sensitivity of the Planck HFI polarization measurements allows for the first time a mapping of Galactic dust polarized emission on large scales, including low column density regions. We find that the maximum observed dust polarization fraction is high (p_(max) = 19.8%), in particular in some regions of moderate hydrogen column density (N_H < 2 \u00d7 10^(21) cm^(-2)). The polarization fraction displays a large scatter at N_H below a few 10^(21) cm^(-2). There is a general decrease in the dust polarization fraction with increasing column density above N_H \u2243 1 \u00d7 10^(21) cm-2 and in particular a sharp drop above N_H \u2243 1.5 \u00d7 10^(22) cm^(-2). We characterize the spatial structure of the polarization angle using the angle dispersion function. We find that the polarization angle is ordered over extended areas of several square degrees, separated by filamentary structures of high angle dispersion function. These appear as interfaces where the sky projection of the magnetic field changes abruptly without variations in the column density. The polarization fraction is found to be anti-correlated with the dispersion of polarization angles. These results suggest that, at the resolution of 1\u00b0, depolarization is due mainly to fluctuations in the magnetic field orientation along the line of sight, rather than to the loss of grain alignment in shielded regions. We also compare the polarization of thermal dust emission with that of synchrotron measured with Planck, low-frequency radio data, and Faraday rotation measurements toward extragalactic sources. These components bear resemblance along the Galactic plane and in some regions such as the Fan and North Polar Spur regions. The poor match observed in other regions shows, however, that dust, cosmic-ray electrons, and thermal electrons generally sample different parts of the line of sight.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A104", "id_number": "CaltechAUTHORS:20150811-094459251", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150811-094459251", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "University of S\u00e3o Paulo", "grant_number": "USP 2007.1.433.14.2" }, { "agency": "COFECUB", "grant_number": "Uc Te 114/08" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424082", "primary_object": { "basename": "aa24082-14.pdf", "url": "https://authors.library.caltech.edu/records/9wvj8-b8a66/files/aa24082-14.pdf" }, "related_objects": [ { "basename": "1405.0871v1.pdf", "url": "https://authors.library.caltech.edu/records/9wvj8-b8a66/files/1405.0871v1.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/993xr-6xp63", "eprint_id": 96861, "eprint_status": "archive", "datestamp": "2023-08-20 05:42:57", "lastmod": "2023-10-20 21:34:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Pelkonen-Veli-Matti", "name": { "family": "Pelkonen", "given": "V.-M." }, "orcid": "0000-0002-8898-1047" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 dust, extinction \u2013 ISM: magnetic fields \u2013 ISM: clouds \u2013 infrared: ISM \u2013 submillimeter: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 28 April 2014; Accepted 4 September 2014; Published online 13 April 2015.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. Some of the results in this paper have been derived using the HEALPix package. The authors would like to thank Charles Beichman for his careful reading of the manuscript and useful comments. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. 267934.\n\nPublished - aa24086-14.pdf
Accepted Version - 1405.0872.pdf
", "abstract": "Polarized emission observed by Planck HFI at 353\u2009GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles \u03c8. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction p_(max) decreases with column density N_H in the more opaque fields with N_H> 10^(21) cm^(-2); and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction p_(max) in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A105", "id_number": "CaltechAUTHORS:20190701-105706574", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-105706574", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424086", "primary_object": { "basename": "1405.0872.pdf", "url": "https://authors.library.caltech.edu/records/993xr-6xp63/files/1405.0872.pdf" }, "related_objects": [ { "basename": "aa24086-14.pdf", "url": "https://authors.library.caltech.edu/records/993xr-6xp63/files/aa24086-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/nmk5g-1gd96", "eprint_id": 96862, "eprint_status": "archive", "datestamp": "2023-08-20 05:43:04", "lastmod": "2023-10-20 21:34:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C." }, "orcid": "0000-0002-5627-5471" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 dust, extinction \u2013 ISM: clouds \u2013 ISM: magnetic fields \u2013 submillimeter: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 28 April 2014; Accepted 3 December 2014; Published online 13 April 2015.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007\u22122013) / ERC grant agreement No. 267934. This research has made use of the SIMBAD database and the VizieR catalogue access tool, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Service.\n\nPublished - aa24087-14.pdf
Submitted - 1405.0873.pdf
", "abstract": "The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust. In addition to the information on the direction of the Galactic magnetic field, this also brings new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust, and therefore of the important dust model parameters, composition, size, and shape. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, p_V, and the optical depth in the V band to the star, \u03c4_V. Toward these stars we measure the submillimetre polarized intensity, P_S, and total intensity, I_S, in the Planck 353\u2009GHz channel. We compare the column density measure in the visible, E(B \u2212 V), with that inferred from the Planck product map of the submillimetre dust optical depth and compare the polarization direction (position angle) in the visible with that in the submillimetre. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, R_(S/V) = (P_S/I_S) / (p_V/\u03c4_V) and R_(P/p) = P_S/p_V, the latter focusing directly on the polarization properties of the aligned grain population alone. We find R_(S /V) = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and R_(P/p) = 5.4 MJy sr^(-1), with uncertainties 0.2 and 0.3 MJy sr^(-1), respectively. Our estimate of R_(S/V) is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. This estimate provides new empirical validation of many of the common underlying assumptions of the models, but is not yet very discriminating among them. However, our estimate of R_(P/p) is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, R_(P/p), indicates that changes to the optical properties in the models of the aligned grain population are required. These new diagnostics, together with the spectral dependence in the submillimetre from Planck, will be important for constraining and understanding the full complexity of the grain models, and for interpreting the Planck thermal dust polarization and refinement of the separation of this contamination of the cosmic microwave background.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A106", "id_number": "CaltechAUTHORS:20190701-110759480", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-110759480", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424087", "primary_object": { "basename": "1405.0873.pdf", "url": "https://authors.library.caltech.edu/records/nmk5g-1gd96/files/1405.0873.pdf" }, "related_objects": [ { "basename": "aa24087-14.pdf", "url": "https://authors.library.caltech.edu/records/nmk5g-1gd96/files/aa24087-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ac7wy-khp84", "eprint_id": 96863, "eprint_status": "archive", "datestamp": "2023-08-20 05:43:11", "lastmod": "2023-10-20 21:34:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XXII. Frequency dependence of thermal\u2009emission\u2009from\u2009Galactic\u2009dust\u2009in\u2009intensity and polarization", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 ISM: general \u2013 Galaxy: general \u2013 radiation mechanisms: general \u2013 submillimeter: ISM \u2013 infrared: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 28 April 2014; Accepted 9 December 2014; Published online 13 April 2015.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and J.A. (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A detailed description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa24088-14.pdf
Accepted Version - 1405.0874.pdf
", "abstract": "Planck has mapped the intensity and polarization of the sky at microwave frequencies with unprecedented sensitivity. We use these data to characterize the frequency dependence of dust emission. We make use of the Planck 353\u2009GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the Planck and WMAP data at 12 frequencies from 23 to 353\u2009GHz, over circular patches with 10\u00b0 radius. The cross-correlation analysis is performed for both intensity and polarization data in a consistent manner. The results are corrected for the chance correlation between the templates and the anisotropies of the cosmic microwave background. We use a mask that focuses our analysis on the diffuse interstellar medium at intermediate Galactic latitudes. We determine the spectral indices of dust emission in intensity and polarization between 100 and 353\u2009GHz, for each sky patch. Both indices are found to be remarkably constant over the sky. The mean values, 1.59 \u00b1 0.02 for polarization and 1.51 \u00b1 0.01 for intensity, for a mean dust temperature of 19.6\u2009K, are close, but significantly different (3.6\u03c3). We determine the mean spectral energy distribution (SED) of the microwave emission, correlated with the 353\u2009GHz dust templates, by averaging the results of the correlation over all sky patches. We find that the mean SED increases for decreasing frequencies at \u03bd< 60\u2009GHz for both intensity and polarization. The rise of the polarization SED towards low frequencies may be accounted for by a synchrotron component correlated with dust, with no need for any polarization of the anomalous microwave emission. We use a spectral model to separate the synchrotron and dust polarization and to characterize the spectral dependence of the dust polarization fraction. The polarization fraction (p) of the dust emission decreases by (21 \u00b1 6)% from 353 to 70 GHz. We discuss this result within the context of existing dust models. The decrease in p could indicate differences in polarization efficiency among components of interstellar dust (e.g., carbon versus silicate grains). Our observational results provide inputs to quantify and optimize the separation between Galactic and cosmological polarization.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A107", "id_number": "CaltechAUTHORS:20190701-112037165", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-112037165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Distributed European Infrastructure for Supercomputing Applications (DEISA)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424088", "primary_object": { "basename": "aa24088-14.pdf", "url": "https://authors.library.caltech.edu/records/ac7wy-khp84/files/aa24088-14.pdf" }, "related_objects": [ { "basename": "1405.0874.pdf", "url": "https://authors.library.caltech.edu/records/ac7wy-khp84/files/1405.0874.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. 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R." } }, { "id": "Melchiorri-A", "name": { "family": "Melchiorri", "given": "A." } }, { "id": "Mendes-L", "name": { "family": "Mendes", "given": "L." } }, { "id": "Mennella-A", "name": { "family": "Mennella", "given": "A." } }, { "id": "Migliaccio-M", "name": { "family": "Migliaccio", "given": "M." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Miville-Desch\u00eanes-Marc-Antoine", "name": { "family": "Miville-Desch\u00eanes", "given": "M.-A." }, "orcid": "0000-0002-7351-6062" }, { "id": "Moneti-A", "name": { "family": "Moneti", "given": "A." } }, { "id": "Montier-L", "name": { "family": "Montier", "given": "L." } }, { "id": "Morgante-G", "name": { "family": "Morgante", "given": "G." } }, { "id": "Mortlock-D", "name": { "family": "Mortlock", "given": "D." } }, { "id": "Moss-A", "name": { "family": "Moss", "given": "A." } }, { "id": "Munshi-D", "name": { "family": "Munshi", "given": "D." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. 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W., IV" } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Pagano-L", "name": { "family": "Pagano", "given": "L." } }, { "id": "Pajot-F", "name": { "family": "Pajot", "given": "F." } }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Paoletti-D", "name": { "family": "Paoletti", "given": "D." } }, { "id": "Partridge-B", "name": { "family": "Partridge", "given": "B." } }, { "id": "Pasian-F", "name": { "family": "Pasian", "given": "F." } }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "G." } }, { "id": "Pearson-Timothy-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Perdereau-O", "name": { "family": "Perdereau", "given": "O." } }, { "id": "Perotto-L", "name": { "family": "Perotto", "given": "L." } }, { "id": "Pettorino-V", "name": { "family": "Pettorino", "given": "V." } }, { "id": "Piacentini-Francesco", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Piat-M", "name": { "family": "Piat", "given": "M." } }, { "id": "Pietrobon-D", "name": { "family": "Pietrobon", "given": "D." } }, { "id": "Plaszczynski-S", "name": { "family": "Plaszczynski", "given": "S." } }, { "id": "Pointecouteau-E", "name": { "family": "Pointecouteau", "given": "E." } }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Ponthieu-N", "name": { "family": "Ponthieu", "given": "N." } }, { "id": "Pratt-G-W", "name": { "family": "Pratt", "given": "G. W." } }, { "id": "Prunet-S", "name": { "family": "Prunet", "given": "S." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Puget-J-L", "name": { "family": "Puget", "given": "J.-L." } }, { "id": "Rachen-J-P", "name": { "family": "Rachen", "given": "J. P." } }, { "id": "Reach-William-T", "name": { "family": "Reach", "given": "W. T." }, "orcid": "0000-0001-8362-4094" }, { "id": "Rebolo-Rafael", "name": { "family": "Rebolo", "given": "R." }, "orcid": "0000-0003-3767-7085" }, { "id": "Reinecke-M", "name": { "family": "Reinecke", "given": "M." } }, { "id": "Remazeilles-M", "name": { "family": "Remazeilles", "given": "M." } }, { "id": "Renault-C", "name": { "family": "Renault", "given": "C." } }, { "id": "Renzi-A", "name": { "family": "Renzi", "given": "A." } }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Ristorcelli-I", "name": { "family": "Ristorcelli", "given": "I." } }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rossetti-M", "name": { "family": "Rossetti", "given": "M." } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "G." } }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Rubi\u00f1o-Martin-J-A", "name": { "family": "Rubi\u00f1o-Martin", "given": "J. A." } }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Sandri-M", "name": { "family": "Sandri", "given": "M." } }, { "id": "Santos-D", "name": { "family": "Santos", "given": "D." } }, { "id": "Savelainen-M", "name": { "family": "Savelainen", "given": "M." } }, { "id": "Savini-G", "name": { "family": "Savini", "given": "G." } }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Sheehy-C-D", "name": { "family": "Sheehy", "given": "C. D." } }, { "id": "Spencer-L-D", "name": { "family": "Spencer", "given": "L. D." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Stolyarov-V", "name": { "family": "Stolyarov", "given": "V." } }, { "id": "Sudiwala-R", "name": { "family": "Sudiwala", "given": "R." } }, { "id": "Sunyaev-R-A", "name": { "family": "Sunyaev", "given": "R. A." } }, { "id": "Sutton-D", "name": { "family": "Sutton", "given": "D." } }, { "id": "Suur-Uski-A-S", "name": { "family": "Suur-Uski", "given": "A.-S." } }, { "id": "Sygnet-J-F", "name": { "family": "Sygnet", "given": "J.-F." } }, { "id": "Tauber-J-A", "name": { "family": "Tauber", "given": "J. A." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } }, { "id": "Terenzi-L", "name": { "family": "Terenzi", "given": "L." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Toffolatti-L", "name": { "family": "Toffolatti", "given": "L." } }, { "id": "Tolan-J-E", "name": { "family": "Tolan", "given": "J. E." } }, { "id": "Tomasi-M", "name": { "family": "Tomasi", "given": "M." } }, { "id": "Tristram-M", "name": { "family": "Tristram", "given": "M." } }, { "id": "Tucci-M", "name": { "family": "Tucci", "given": "M." } }, { "id": "Turner-A-D", "name": { "family": "Turner", "given": "A. D." } }, { "id": "Valenziano-L", "name": { "family": "Valenziano", "given": "L." } }, { "id": "Valiviita-J", "name": { "family": "Valiviita", "given": "J." } }, { "id": "Van-Tent-B", "name": { "family": "Van Tent", "given": "B." } }, { "id": "Vibert-L", "name": { "family": "Vibert", "given": "L." } }, { "id": "Vielva-P", "name": { "family": "Vielva", "given": "P." } }, { "id": "Vieregg-A-G", "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Villa-F", "name": { "family": "Villa", "given": "F." } }, { "id": "Wade-L-A", "name": { "family": "Wade", "given": "L. A." } }, { "id": "Wandelt-Benjamin-D", "name": { "family": "Wandelt", "given": "B. D." }, "orcid": "0000-0002-5854-8269" }, { "id": "Watson-R", "name": { "family": "Watson", "given": "R." } }, { "id": "Weber-A-C", "name": { "family": "Weber", "given": "A. C." } }, { "id": "Wehus-I-K", "name": { "family": "Wehus", "given": "I. K." } }, { "id": "White-M", "name": { "family": "White", "given": "M." } }, { "id": "White-S-D-M", "name": { "family": "White", "given": "S. D. M." } }, { "id": "Willmert-J", "name": { "family": "Willmert", "given": "J." } }, { "id": "Wong-C-L", "name": { "family": "Wong", "given": "C. L." } }, { "id": "Yoon-K-W", "name": { "family": "Yoon", "given": "K. W." } }, { "id": "Yvon-D", "name": { "family": "Yvon", "given": "D." } }, { "id": "Zacchei-A", "name": { "family": "Zacchei", "given": "A." } }, { "id": "Zonca-A", "name": { "family": "Zonca", "given": "A." } } ] }, "title": "A Joint Analysis of BICEP2/Keck Array and Planck Data", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 American Physical Society. \n\n(Received 21 January 2015; published 9 March 2015) \n\nBICEP2 was supported by the U.S. National Science Foundation under Grants No. ANT-0742818 and No. ANT-1044978 (Caltech and Harvard) and No. ANT-0742592 and No. ANT-1110087 (Chicago and Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The Keck Array project was supported by the National Science Foundation under Grants No. ANT-1145172 (Harvard), No. ANT-1145143 (Minnesota) and No. ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. The Planck Collaboration acknowledges the support of the following: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found in Ref. [52].\n\nPublished - PhysRevLett.114.101301.pdf
Submitted - 1502.00612v1.pdf
", "abstract": "We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400\u2009\u2009deg2 patch of sky centered on RA 0 h, Dec. \u221257.5\u00b0. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2\u2009\u2009\u03bcK deg in Q and U at 143 GHz). We detect 150\u00d7353 cross-correlation in B modes at high significance. We fit the single- and cross-frequency power spectra at frequencies \u2265150\u2009\u2009GHz to a lensed-\u039bCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous Planck analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally, we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r0.05<0.12 at 95% confidence. Marginalizing over dust and r, lensing B modes are detected at 7.0\u03c3 significance.", "date": "2015-03-09", "date_type": "published", "publication": "Physical Review Letters", "volume": "114", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 101301", "id_number": "CaltechAUTHORS:20150205-194356590", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150205-194356590", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT- 1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "CSIC and RES (Spain)" }, { "agency": "Tekes and CSC (Finland)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "PRACE (EU)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Academy of Finland" }, { "agency": "European Research Council (ERC)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.1103/PhysRevLett.114.101301", "primary_object": { "basename": "1502.00612v1.pdf", "url": "https://authors.library.caltech.edu/records/bv7yz-e4e53/files/1502.00612v1.pdf" }, "related_objects": [ { "basename": "PhysRevLett.114.101301.pdf", "url": "https://authors.library.caltech.edu/records/bv7yz-e4e53/files/PhysRevLett.114.101301.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Aghanim, N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gccxy-55773", "eprint_id": 60296, "eprint_status": "archive", "datestamp": "2023-08-20 05:00:32", "lastmod": "2023-10-24 16:24:10", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jain-B", "name": { "family": "Jain", "given": "B." } }, { "id": "Spergel-D-N", "name": { "family": "Spergel", "given": "D." }, "orcid": "0000-0002-5151-0006" }, { "id": "Bean-R", "name": { "family": "Bean", "given": "R." } }, { "id": "Connolly-A-J", "name": { "family": "Connolly", "given": "A." } }, { "id": "Dell'Antonio-I-P", "name": { "family": "Dell'Antonio", "given": "I." } }, { "id": "Frieman-J-A", "name": { "family": "Frieman", "given": "J." } }, { "id": "Gawiser-E", "name": { "family": "Gawiser", "given": "E." } }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "N." } }, { "id": "Gladney-L", "name": { "family": "Gladney", "given": "L." } }, { "id": "Heitmann-K", "name": { "family": "Heitmann", "given": "K." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "C." }, "orcid": "0000-0002-2951-4932" }, { "id": "Ho-S", "name": { "family": "Ho", "given": "S." } }, { "id": "Ivezi\u0107-\u017d", "name": { "family": "Ivezi\u0107", "given": "\u017d." }, "orcid": "0000-0001-5250-2633" }, { "id": "Jarvis-M-J", "name": { "family": "Jarvis", "given": "M." }, "orcid": "0000-0001-7039-9078" }, { "id": "Kahn-S", "name": { "family": "Kahn", "given": "S." } }, { "id": "Kalirai-J-S", "name": { "family": "Kalirai", "given": "J." }, "orcid": "0000-0001-9690-4159" }, { "id": "Kim-A", "name": { "family": "Kim", "given": "A." } }, { "id": "Lupton-R", "name": { "family": "Lupton", "given": "R." } }, { "id": "Mandelbaum-R", "name": { "family": "Mandelbaum", "given": "R." }, "orcid": "0000-0003-2271-1527" }, { "id": "Marshall-P-J", "name": { "family": "Marshall", "given": "P." } }, { "id": "Newman-J-A", "name": { "family": "Newman", "given": "J. A." }, "orcid": "0000-0001-8684-2222" }, { "id": "Perlmutter-S", "name": { "family": "Perlmutter", "given": "S." } }, { "id": "Postman-Marc", "name": { "family": "Postman", "given": "M." }, "orcid": "0000-0002-9365-7989" }, { "id": "Rhodes-J-D", "name": { "family": "Rhodes", "given": "J." }, "orcid": "0000-0002-4485-8549" }, { "id": "Straus-M-A", "name": { "family": "Strauss", "given": "M. A." } }, { "id": "Tyson-J-A", "name": { "family": "Tyson", "given": "J. A." } }, { "id": "Walkowics-L", "name": { "family": "Walkowicz", "given": "L." } }, { "id": "Wood-Vasey-W-M", "name": { "family": "Wood-Vasey", "given": "W. M." } } ] }, "title": "The Whole is Greater than the Sum of the Parts: Optimizing the Joint Science Return from LSST, Euclid and WFIRST", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted on 30 Jan 2015 (v1), last revised 19 Feb 2015 (this version, v2). February 20, 2015.\n\nThe resources required to achieve this additional science are outside of what is currently budgeted for\nLSST by NSF and DOE, and for WFIRST (or Euclid) by NASA. Funding for this science would most\nnaturally emerge from coordination among all agencies involved, and would be closely orchestrated scientifically\nand programmatically to optimize science returns. A possible model would be to identify members\nof the science teams of each project who would work together on the joint analysis. The analysis team would\nideally be coupled with an experienced science center acting as a focal point for the implementation, and\nsimultaneously preparing the public release and documentation for broadest access by the community.\n\nSubmitted - 1501.07897v2.pdf
", "abstract": "The focus of this report is on the opportunities enabled by the combination of LSST, Euclid and WFIRST, the optical surveys that will be an essential part of the next decade's astronomy. The sum of these surveys has the potential to be significantly greater than the contributions of the individual parts. As is detailed in this report, the combination of these surveys should give us multi-wavelength high-resolution images of galaxies and broadband data covering much of the stellar energy spectrum. These stellar and galactic data have the potential of yielding new insights into topics ranging from the formation history of the Milky Way to the mass of the neutrino. However, enabling the astronomy community to fully exploit this multi-instrument data set is a challenging technical task: for much of the science, we will need to combine the photometry across multiple wavelengths with varying spectral and spatial resolution. We identify some of the key science enabled by the combined surveys and the key technical challenges in achieving the synergies.", "date": "2015-02-19", "date_type": "published", "id_number": "CaltechAUTHORS:20150917-081449249", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-081449249", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "LSST" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.48550/arXiv.1501.07897", "primary_object": { "basename": "1501.07897v2.pdf", "url": "https://authors.library.caltech.edu/records/gccxy-55773/files/1501.07897v2.pdf" }, "resource_type": "monograph", "pub_year": "2015", "author_list": "Jain, B.; Spergel, D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/m6mhr-6cg72", "eprint_id": 55779, "eprint_status": "archive", "datestamp": "2023-08-22 14:56:03", "lastmod": "2023-10-20 23:10:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Herrera-Camus-R", "name": { "family": "Herrera-Camus", "given": "R." }, "orcid": "0000-0002-2775-0595" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" } ] }, "title": "[C II] 158 \u03bcm Emission as a Star Formation Tracer", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; galaxies: star formation; infrared: galaxies; ISM: structure", "note": "\u00a9 2015 American Astronomical Society. Received 2014 July 3; accepted 2014 September 20; published 2015 February 2.\n\nWe thank the referee for constructive and valuable comments on the paper. R.H.C. acknowledges support from a Fulbright-CONICYT grant. A.D.B. acknowledges partial support from a CAREER grant NSF-AST0955836, from NSF-AST1139998, from NASA-JPL 1373858, and from a Research Corporation for Science Advancement Cottrell Scholar award. We thank B. Weiner for providing [C ii] and FIR fluxes for his sample of LIRGs in advance of publication. We also thank T. Diaz-Santos for providing the areas used to measure the surface brightness of the galaxies in the GOALS sample in advance of publication. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France);MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the\nfunding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. This work is based (in part) on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. The National Radio Astronomy Observatory is a facility of the National\nScience Foundation operated under cooperative agreement by Associated Universities, Inc. 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\nWe wish to dedicate this study to the memory of our colleague Dr. Charles \"Chad\" Engelbracht for his numerous contributions to space-based far-infrared astronomy that made this work possible, as well as that of many other researchers employing Spitzer and Herschel observations.\n\nPublished - 0004-637X_800_1_1.pdf
Submitted - 1409.7123v1.pdf
", "abstract": "The [C II] 157.74 \u03bcm transition is the dominant coolant of the neutral interstellar gas, and has great potential as a star formation rate (SFR) tracer. Using the Herschel KINGFISH sample of 46 nearby galaxies, we investigate the relation of [C II] surface brightness and luminosity with SFR. We conclude that [C II] can be used for measurements of SFR on both global and kiloparsec scales in normal star-forming galaxies in the absence of strong active galactic nuclei (AGNs). The uncertainty of the \u03a3_([C II]) \u2013 \u03a3_(SFR) calibration is \u00b10.21 dex. The main source of scatter in the correlation is associated with regions that exhibit warm IR colors, and we provide an adjustment based on IR color that reduces the scatter. We show that the color-adjusted \u03a3_([C II]) \u2013 \u03a3_(SFR) correlation is valid over almost five orders of magnitude in \u03a3_(SFR), holding for both normal star-forming galaxies and non-AGN luminous infrared galaxies. Using [C II] luminosity instead of surface brightness to estimate SFR suffers from worse systematics, frequently underpredicting SFR in luminous infrared galaxies even after IR color adjustment (although this depends on the SFR measure employed). We suspect that surface brightness relations are better behaved than the luminosity relations because the former are more closely related to the local far-UV field strength, most likely the main parameter controlling the efficiency of the conversion of far-UV radiation into gas heating. A simple model based on Starburst99 population-synthesis code to connect SFR to [C II] finds that heating efficiencies are 1%-3% in normal galaxies.", "date": "2015-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "800", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 1", "id_number": "CaltechAUTHORS:20150316-101053602", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150316-101053602", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Fulbright Foundation" }, { "agency": "NSF", "grant_number": "AST0955836" }, { "agency": "NSF", "grant_number": "AST1139998" }, { "agency": "NASA-JPL", "grant_number": "1373858" }, { "agency": "Cottrell Scholar of Research Corporation" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/800/1/1", "primary_object": { "basename": "0004-637X_800_1_1.pdf", "url": "https://authors.library.caltech.edu/records/m6mhr-6cg72/files/0004-637X_800_1_1.pdf" }, "related_objects": [ { "basename": "1409.7123v1.pdf", "url": "https://authors.library.caltech.edu/records/m6mhr-6cg72/files/1409.7123v1.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Herrera-Camus, R.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1whmh-3vm22", "eprint_id": 60293, "eprint_status": "archive", "datestamp": "2023-08-20 04:10:40", "lastmod": "2024-01-13 16:25:00", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "The Palomar Transient Factory: High Quality Realtime Data Processing in a Cost-Constrained Environment", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2015 Astronomical Society of the Pacific.\n\nPublished - 495-0197.pdf
Submitted - 1501.06007v1.pdf
", "abstract": "The Palomar Transient Factory (PTF) is a synoptic sky survey in operation since 2009. PTF utilizes a 7.1 square degree camera on the Palomar 48-inch Schmidt telescope to survey the sky primarily at a single wavelength (R-band) at a rate of 1000-3000 square degrees a night. The data are used to detect and study transient and moving objects such as gamma ray bursts, supernovae and asteroids, as well as variable phenomena such as quasars and Galactic stars. The data processing system at IPAC handles realtime processing and detection of transients, solar system object processing, high photometric precision processing and light curve generation, and long-term archiving and curation. This was developed under an extremely limited budget profile in an unusually agile development environment. Here we discuss the mechanics of this system and our overall development approach. Although a significant scientific installation in of itself, PTF also serves as the prototype for our next generation project, the Zwicky Transient Facility (ZTF). Beginning operations in 2017, ZTF will feature a 50 square degree camera which will enable scanning of the entire northern visible sky every night. ZTF in turn will serve as a stepping stone to the Large Synoptic Survey Telescope (LSST), a major NSF facility scheduled to begin operations in the early 2020s.", "date": "2015", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "197-206", "id_number": "CaltechAUTHORS:20150917-072916631", "isbn": "9781583818749", "book_title": "Astronomical Data Analysis Software and Systems XXIV", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-072916631", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "contributors": { "items": [ { "id": "Taylor-A-R", "name": { "family": "Taylor", "given": "A. R." } }, { "id": "Rosolowsky-E", "name": { "family": "Rosolowsky", "given": "E." } } ] }, "doi": "10.48550/arXiv.1501.06007", "primary_object": { "basename": "1501.06007v1.pdf", "url": "https://authors.library.caltech.edu/records/1whmh-3vm22/files/1501.06007v1.pdf" }, "related_objects": [ { "basename": "495-0197.pdf", "url": "https://authors.library.caltech.edu/records/1whmh-3vm22/files/495-0197.pdf" } ], "resource_type": "book_section", "pub_year": "2015", "author_list": "Surace, Jason; Laher, Russ; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jdn9d-3pg44", "eprint_id": 53080, "eprint_status": "archive", "datestamp": "2023-08-22 14:25:57", "lastmod": "2023-10-19 14:31:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kirkpatrick-Allison", "name": { "family": "Kirkpatrick", "given": "Allison" } }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "Alexandra" }, "orcid": "0000-0001-8592-2706" }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "Itziar" }, "orcid": "0000-0002-6590-3994" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Monta\u00f1a-A", "name": { "family": "Monta\u00f1a", "given": "Alfredo" }, "orcid": "0000-0003-4229-381X" }, { "id": "Narayanan-G", "name": { "family": "Narayanan", "given": "Gopal" } }, { "id": "Schloerb-F-P", "name": { "family": "Schloerb", "given": "F. Peter" } }, { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Vega-Olga", "name": { "family": "Vega", "given": "Olga" } }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "Min S." }, "orcid": "0000-0001-7095-7543" } ] }, "title": "Early Science with the Large Millimeter Telescope: Exploring the Effect of AGN Activity on the Relationships between Molecular Gas, Dust, and Star Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: ISM; galaxies: starburst", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 12 July 2014; accepted for publication 14 October 2014; published 14 November 2014.\n\nWe thank the anonymous referee for the helpful comments which have improved the clarity of this work. This work would not have been possible without the long-term financial support from the Mexican Science and Technology Funding Agency, CONACYT (Consejo Nacional de Ciencia y Tecnolog\u00eda) during the construction and early operational phase of the Large Millimeter Telescope Alfonso Serrano, as well as support from the US National Science Foundation via the University Radio Observatory program, the Instituto Nacional de Astrof\u00edsica, \u00d3ptica y Electr\u00f3nica (INAOE) and the University of Massachusetts (UMASS). The UMass LMT group acknowledges support from NSF URO and ATI grants (AST-0096854 and AST-0704966) for the LMT project and the construction of the RSR. A.K. would like to acknowledge support from a William Bannick Student Travel Grant. We are grateful to all the LMT observers from Mexico and UMass who took data for this project. 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, and the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. 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 - 0004-637X_796_2_135.pdf
Submitted - 1411.1065v1.pdf
", "abstract": "The molecular gas, H_2, that fuels star formation in galaxies is difficult to observe directly. As such, the ratio of L_IR to L'_CO is an observational estimate of the star formation rate compared with the amount of molecular gas available to form stars, which is related to the star formation efficiency and the inverse of the gas consumption\ntimescale. We test what effect an IR luminous active galactic nucleus (AGN) has on the ratio L_IR/L'_CO in a sample of 24 intermediate redshift galaxies from the 5 mJy Unbiased Spitzer Extragalactic Survey (5MUSES). We obtain new CO(1\u20130) observations with the Redshift Search Receiver on the Large Millimeter Telescope. We diagnose the\npresence and strength of an AGN using Spitzer IRS spectroscopy. We find that removing the AGN contribution\nto L^(tot)_IR results in a mean L^(SF)_IR/L'_CO for our entire sample consistent with the mean L_IR/L'_CO derived for a large sample of star forming galaxies from z \u223c 0\u20133.We also include in our comparison the relative amount of polycyclic aromatic hydrocarbon emission for our sample and a literature sample of local and high-redshift ultra luminous infrared galaxies and find a consistent trend between L_6.2/L^(SF)_IR and L^(SF)_IR/L'CO, such that small dust grain emission decreases with increasing L^(SF)_IR/L'_CO for both local and high-redshift dusty galaxies.", "date": "2014-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "796", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 135", "id_number": "CaltechAUTHORS:20141222-101405419", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141222-101405419", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)" }, { "agency": "INAOE" }, { "agency": "University of Massachusetts" }, { "agency": "NSF", "grant_number": "AST-0096854" }, { "agency": "NSF", "grant_number": "AST-0704966" }, { "agency": "William Bannick Student Travel Grant" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/796/2/135", "primary_object": { "basename": "1411.1065v1.pdf", "url": "https://authors.library.caltech.edu/records/jdn9d-3pg44/files/1411.1065v1.pdf" }, "related_objects": [ { "basename": "0004-637X_796_2_135.pdf", "url": "https://authors.library.caltech.edu/records/jdn9d-3pg44/files/0004-637X_796_2_135.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Kirkpatrick, Allison; Pope, Alexandra; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/76tne-hae05", "eprint_id": 96852, "eprint_status": "archive", "datestamp": "2023-08-20 03:34:43", "lastmod": "2023-10-20 21:34:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Matsumura-Tomotake", "name": { "family": "Matsumura", "given": "T." } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. I. Overview of products and scientific results", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 space vehicles: instruments \u2013 instrumentation: detectors", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 21 March 2013; Accepted 17 May 2014; Published online 29 October 2014.\n\nPlanck is too large a project to allow full acknowledgement of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via Instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's UK Planck Project, based at JPL and involving scientists at many UK institutions, contributes significantly to the efforts of these two Consortia. A third Consortium, led by H. U. Norgaard-Nielsen and supported by the Danish Natural Research Council, contributed to the reflector programme. The author list for this paper has been selected by the Planck Science Team from the Planck Collaboration, and is composed of individuals from all of the above entities who have made multi-year contributions to the development of the mission. It does not pretend to be inclusive of all contributions to Planck. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at (http://www.rssd.esa.int/index.php?project=PLANCK& page=Planck_ Collaboration). The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, and JA (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).\n\nPublished - aa21529-13.pdf
Submitted - 1303.5062.pdf
", "abstract": "The European Space Agency's Planck satellite, dedicated to studying the early Universe and its subsequent evolution, was launched 14 May 2009 and has been scanning the microwave and submillimetre sky continuously since 12 August 2009. In March 2013, ESA and the Planck Collaboration released the initial cosmology products based on the first 15.5\u2009months of Planck data, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the mission and its performance, the processing, analysis, and characteristics of the data, the scientific results, and the science data products and papers in the release. The science products include maps of the cosmic microwave background (CMB) and diffuse extragalactic foregrounds, a catalogue of compact Galactic and extragalactic sources, and a list of sources detected through the Sunyaev-Zeldovich effect. The likelihood code used to assess cosmological models against the Planck data and a lensing likelihood are described. Scientific results include robust support for the standard six-parameter \u039bCDM model of cosmology and improved measurements of its parameters, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for these parameters and others derived from them are significantly different from those previously determined. Several large-scale anomalies in the temperature distribution of the CMB, first detected by WMAP, are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at greater than 25\u03c3. Planck finds no evidence for non-Gaussianity in the CMB. Planck's results agree well with results from the measurements of baryon acoustic oscillations. Planck finds a lower Hubble constant than found in some more local measures. Some tension is also present between the amplitude of matter fluctuations (\u03c38) derived from CMB data and that derived from Sunyaev-Zeldovich data. The Planck and WMAP power spectra are offset from each other by an average level of about 2% around the first acoustic peak. Analysis of Planck polarization data is not yet mature, therefore polarization results are not released, although the robust detection of E-mode polarization around CMB hot and cold spots is shown graphically.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A1", "id_number": "CaltechAUTHORS:20190701-084039975", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-084039975", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321529", "primary_object": { "basename": "1303.5062.pdf", "url": "https://authors.library.caltech.edu/records/76tne-hae05/files/1303.5062.pdf" }, "related_objects": [ { "basename": "aa21529-13.pdf", "url": "https://authors.library.caltech.edu/records/76tne-hae05/files/aa21529-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/s33jy-jpn50", "eprint_id": 96853, "eprint_status": "archive", "datestamp": "2023-08-20 03:34:53", "lastmod": "2023-10-20 21:34:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. VI. High Frequency Instrument data processing", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis \u2013 cosmic background radiation \u2013 cosmology: observations \u2013 surveys", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 26 March 2013; Accepted 22 July 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration.\n\nPublished - aa21570-13.pdf
Accepted Version - 1303.5067.pdf
", "abstract": "We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857GHz with an angular resolution ranging from 9.\u03017 to 4.\u03016. The detector noise per (effective) beam solid angle is respectively, 10, 6 , 12, and 39\u2009\u03bcK in the four lowest HFI frequency channels (100\u2212353GHz) and 13 and 14\u2009kJy sr^(-1) in the 545 and 857\u2009GHz channels. Relative to the 143\u2009GHz channel, these two high frequency channels are calibrated to within 5% and the 353\u2009GHz channel to the percent level. The 100 and 217\u2009GHz channels, which together with the 143\u2009GHz channel determine the high-multipole part of the CMB power spectrum (50 <\u2113 < 2500), are calibrated relative to 143\u2009GHz to better than 0.2%.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A6", "id_number": "CaltechAUTHORS:20190701-085818699", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-085818699", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321570", "primary_object": { "basename": "1303.5067.pdf", "url": "https://authors.library.caltech.edu/records/s33jy-jpn50/files/1303.5067.pdf" }, "related_objects": [ { "basename": "aa21570-13.pdf", "url": "https://authors.library.caltech.edu/records/s33jy-jpn50/files/aa21570-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rm1w3-fgf92", "eprint_id": 96851, "eprint_status": "archive", "datestamp": "2023-08-20 03:34:34", "lastmod": "2023-10-20 21:34:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. VIII. HFI photometric calibration and mapmaking", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 surveys \u2013 methods: data analysis", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 21 March 2013; Accepted 8 March 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=PlanckCollaboration.\n\nPublished - aa21538-13.pdf
Submitted - 1303.5069.pdf
", "abstract": "This paper describes the methods used to produce photometrically calibrated maps from the Planck High Frequency Instrument (HFI) cleaned, time-ordered information. HFI observes the sky over a broad range of frequencies, from 100 to 857\u2009\u2009GHz. To obtain the best calibration accuracy over such a large range, two different photometric calibration schemes have to be used. The 545 and 857\u2009GHz data are calibrated by comparing flux-density measurements of Uranus and Neptune with models of their atmospheric emission. The lower frequencies (below 353\u2009\u2009GHz) are calibrated using the solar dipole. A component of this anisotropy is time-variable, owing to the orbital motion of the satellite in the solar system. Photometric calibration is thus tightly linked to mapmaking, which also addresses low-frequency noise removal. By comparing observations taken more than one year apart in the same configuration, we have identified apparent gain variations with time. These variations are induced by non-linearities in the read-out electronics chain. We have developed an effective correction to limit their effect on calibration. We present several methods to estimate the precision of the photometric calibration. We distinguish relative uncertainties (between detectors, or between frequencies) and absolute uncertainties. Absolute uncertainties lie in the range from 0.54% to 10% from 100 to 857\u2009\u2009GHz. We describe the pipeline used to produce the maps from the HFI timelines, based on the photometric calibration parameters, and the scheme used to set the zero level of the maps a posteriori. We also discuss the cross-calibration between HFI and the SPIRE instrument on board Herschel. Finally we summarize the basic characteristics of the set of HFI maps included in the 2013 Planck data release.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A8", "id_number": "CaltechAUTHORS:20190701-075622398", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-075622398", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321538", "primary_object": { "basename": "1303.5069.pdf", "url": "https://authors.library.caltech.edu/records/rm1w3-fgf92/files/1303.5069.pdf" }, "related_objects": [ { "basename": "aa21538-13.pdf", "url": "https://authors.library.caltech.edu/records/rm1w3-fgf92/files/aa21538-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/265xd-cxd57", "eprint_id": 96859, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:43", "lastmod": "2023-10-20 21:34:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abergel-A", "name": { "family": "Abergel", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XI. All-sky model of thermal dust emission", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis \u2013 ISM: general \u2013 dust, extinction \u2013 infrared: ISM \u2013 submillimeter: ISM \u2013 opacity", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 4 December 2013; Accepted 4 September 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. 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 Monbuk agakusho, 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, 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. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa23195-13.pdf
Accepted Version - 1312.1300.pdf
", "abstract": "This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857\u2009GHz, and IRAS 100 \u03bcm data. Using a modified blackbody fit to the data we present all-sky maps of the dust optical depth, temperature, and spectral index over the 353\u20133000\u2009GHz range. This model is a good representation of the IRAS and Planck data at 5\u2032 between 353 and 3000\u2009GHz (850 and 100 \u03bcm). It shows variations of the order of 30% compared with the widely-used model of Finkbeiner, Davis, and Schlegel. The Planck data allow us to estimate the dust temperature uniformly over the whole sky, down to an angular resolution of 5\u2032, providing an improved estimate of the dust optical depth compared to previous all-sky dust model, especially in high-contrast molecular regions where the dust temperature varies strongly at small scales in response to dust evolution, extinction, and/or local production of heating photons. An increase of the dust opacity at 353\u2009GHz, \u03c4_(353)/N_H, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, T_(obs), that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H\u2009I column densities lower than 10^(20)\u2009cm^(-2) that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between \u03c4_(353)/N_H and T_(obs) while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields. This effect is compatible with the view that, in the diffuse ISM, T_(obs) responds to spatial variations of the dust opacity, due to variations of dust properties, in addition to (small) variations of the radiation field strength. The implication is that in the diffuse high-latitude ISM \u03c4_(353) is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of \u03c4_(353) with dust extinction estimated using colour excess measurements on stars is strong. To estimate Galactic E(B\u2212 V) in extragalactic fields at high latitude we develop a new method based on the thermal dust radiance, instead of the dust optical depth, calibrated to E(B \u2212 V) using reddening measurements of quasars deduced from Sloan Digital Sky Survey data.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A11", "id_number": "CaltechAUTHORS:20190701-102824126", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-102824126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201323195", "primary_object": { "basename": "1312.1300.pdf", "url": "https://authors.library.caltech.edu/records/265xd-cxd57/files/1312.1300.pdf" }, "related_objects": [ { "basename": "aa23195-13.pdf", "url": "https://authors.library.caltech.edu/records/265xd-cxd57/files/aa23195-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Abergel, A.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/qmf7j-v0192", "eprint_id": 96854, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:02", "lastmod": "2023-10-20 21:34:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R. R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XII. Diffuse component separation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 26 March 2013; Accepted 18 December 2013; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The authors acknowledge the support provided by the Advanced Computing and e-Science team at IFCA. This work made use of the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa21580-13.pdf
Submitted - 1303.5072.pdf
", "abstract": "Planck has produced detailed all-sky observations over nine frequency bands between 30 and 857 GHz. These observations allow robust reconstruction of the primordial cosmic microwave background (CMB) temperature fluctuations over nearly the full sky, as well as new constraints on Galactic foregrounds, including thermal dust and line emission from molecular carbon monoxide (CO). This paper describes the component separation framework adopted by Planck for many cosmological analyses, including CMB power spectrum determination and likelihood construction on large angular scales, studies of primordial non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe effect, gravitational lensing, and searches for topological defects. We test four foreground-cleaned CMB maps derived using qualitatively different component separation algorithms. The quality of our reconstructions is evaluated through detailed simulations and internal comparisons, and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to \u2113 = 2000. The parameter constraints on \u039bCDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis. We choose two of the CMB maps for specific scientific goals. We also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission. The component maps are found to provide a faithful representation of the sky, as evaluated by simulations, with the largest bias seen in the CO component at 3%. For the low-frequency component, the spectral index varies widely over the sky, ranging from about \u03b2 = \u22124 to \u2212 2. Considering both morphology and prior knowledge of the low frequencycomponents, the index map allows us to associate a steep spectral index (\u03b2< \u22123.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of \u03b2> \u22122.3 with strong free-free emission, and intermediate values with synchrotron emission.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A12", "id_number": "CaltechAUTHORS:20190701-091146023", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-091146023", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321580", "primary_object": { "basename": "1303.5072.pdf", "url": "https://authors.library.caltech.edu/records/qmf7j-v0192/files/1303.5072.pdf" }, "related_objects": [ { "basename": "aa21580-13.pdf", "url": "https://authors.library.caltech.edu/records/qmf7j-v0192/files/aa21580-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/f0k4w-rq416", "eprint_id": 96855, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:11", "lastmod": "2023-10-20 21:34:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XIV. Zodiacal emission", "ispublished": "pub", "full_text_status": "public", "keywords": "zodiacal dust \u2013 interplanetary medium \u2013 cosmic background radiation", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 25 March 2013; Accepted 4 March 2014; Published online 29 October 2014.\n\nThis paper benefited from exchanges with Dale Fixsen, Tom Kelsall and Janet Weiland. We acknowledge the IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for this work. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration.\n\nPublished - aa21562-13.pdf
Submitted - 1303.5074.pdf
", "abstract": "The Planck satellite provides a set of all-sky maps at nine frequencies from 30\u2009GHz to 857\u2009GHz. Planets, minor bodies, and diffuse interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through different columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model \u2013 a diffuse cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are different from those in the diffuse cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A14", "id_number": "CaltechAUTHORS:20190701-092236114", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-092236114", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321562", "primary_object": { "basename": "1303.5074.pdf", "url": "https://authors.library.caltech.edu/records/f0k4w-rq416/files/1303.5074.pdf" }, "related_objects": [ { "basename": "aa21562-13.pdf", "url": "https://authors.library.caltech.edu/records/f0k4w-rq416/files/aa21562-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a1jcx-ecf68", "eprint_id": 96856, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:20", "lastmod": "2023-10-20 21:34:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XV. CMB power spectra and likelihood", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmological parameters \u2013 cosmology: observations \u2013 methods: data analysis", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 26 March 2013; Accepted 5 May 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of the CLASS Boltzmann code (Lesgourgues 2011) and the Monte Python package (Audren et al. 2013) in earlier stages of this work. The likelihood code and some of the validation work was built on the library pmclib from the CosmoPMC package (Kilbinger et al. 2011). This research used resources of the IN2P3 Computer Center (http://cc.in2p3.fr) as well as of the Planck-HFI data processing centre infrastructures hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES.\n\nPublished - aa21573-13.pdf
Submitted - 1303.5075.pdf
", "abstract": "This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, \u2113, covering 2 \u2264 \u2113 \u2264 2500. The main source of uncertainty at \u2113 \u2272 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher \u2113s. For \u2113 < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At \u2113 \u2265 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high-\u2113 cross-spectra with residuals below a few \u03bcK^2 at \u2113 \u2272 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit \u039bCDM cosmology is in excellent agreement with preliminary PlanckEE and TE polarisation spectra. We find that the standard \u039bCDM cosmology is well constrained by Planck from the measurements at \u2113 \u2272 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4\u03c3 deviation from scale invariance, n_s = 1. Increasing the multipole range beyond \u2113 \u2243 1500 does not increase our accuracy for the \u039bCDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the \u039bCDM framework. Finally, we report a tension between the Planck best-fit \u039bCDM model and the low-\u2113 spectrum in the form of a power deficit of 5\u201310% at \u2113 \u2272 40, with a statistical significance of 2.5\u20133\u03c3. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A15", "id_number": "CaltechAUTHORS:20190701-095024014", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-095024014", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321573", "primary_object": { "basename": "1303.5075.pdf", "url": "https://authors.library.caltech.edu/records/a1jcx-ecf68/files/1303.5075.pdf" }, "related_objects": [ { "basename": "aa21573-13.pdf", "url": "https://authors.library.caltech.edu/records/a1jcx-ecf68/files/aa21573-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zp3n1-aam71", "eprint_id": 96857, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:27", "lastmod": "2023-10-20 21:34:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XXIII. Isotropy and statistics of the CMB", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 cosmology: miscellaneous", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 21 March 2013; Accepted 11 January 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of resources from the Norewegian national super computing facilities NOTUR. The modal and KSW bispectrum estimator analysis was performed on the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. We further acknowledge the computer resources and technical assistance provided by the Spanish Supercomputing Network nodes at Universidad de Cantabria and Universidad Polit\u00e9cnica de Madrid as well as by the Advanced Computing and e-Science team at IFCA. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa21534-13.pdf
Accepted Version - 1303.5083.pdf
", "abstract": "The two fundamental assumptions of the standard cosmological model \u2013 that the initial fluctuations are statistically isotropic and Gaussian \u2013 are rigorously tested using maps of the cosmic microwave background (CMB) anisotropy from the Planck satellite. The detailed results are based on studies of four independent estimates of the CMB that are compared to simulations using a fiducial \u039bCDM model and incorporating essential aspects of the Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice, and frequency dependence. Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (about 3\u03c3). However, we find little evidence of non-Gaussianity, with the exception of a few statistical signatures that seem to be associated with specific anomalies. In particular, we find that the quadrupole-octopole alignment is also connected to a low observed variance in the CMB signal. A power asymmetry is now found to persist on scales corresponding to about \u2113 = 600 and can be described in the low-\u2113 regime by a phenomenological dipole modulation model. However, any primordial power asymmetry is strongly scale-dependent and does not extend toarbitrarily small angular scales. Finally, it is plausible that some of these features may be reflected in the angular power spectrum of the data, which shows a deficit of power on similar scales. Indeed, when the power spectra of two hemispheres defined by a preferred direction are considered separately, one shows evidence of a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity violation and phase correlations also detected in the data. Although these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A23", "id_number": "CaltechAUTHORS:20190701-100009602", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-100009602", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321534", "primary_object": { "basename": "1303.5083.pdf", "url": "https://authors.library.caltech.edu/records/zp3n1-aam71/files/1303.5083.pdf" }, "related_objects": [ { "basename": "aa21534-13.pdf", "url": "https://authors.library.caltech.edu/records/zp3n1-aam71/files/aa21534-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fg01x-gs803", "eprint_id": 96858, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:34", "lastmod": "2023-10-20 21:34:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "id": "Pr\u00e9zeau-Gary", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-Michael-D", "name": { "family": "Seiffert", "given": "M. D." }, "orcid": "0000-0002-7536-9393" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XXVII. Doppler boosting of the CMB: Eppur si muove", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 reference systems \u2013 relativistic processes", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 23 March 2013; Accepted 3 January 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. Some of the results in this paper have been derived using the HEALPix package. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. We acknowledge support from the Science and Technology Facilities Council [grant number ST/I000976/1].\n\nPublished - aa21556-13.pdf
Accepted Version - 1303.5087.pdf
", "abstract": "Our velocity relative to the rest frame of the cosmic microwave background (CMB) generates a dipole temperature anisotropy on the sky which has been well measured for more than 30 years, and has an accepted amplitude of v/c = 1.23 \u00d7 10^(-3), or v = 369. In addition to this signal generated by Doppler boosting of the CMB monopole, our motion also modulates and aberrates the CMB temperature fluctuations (as well as every other source of radiation at cosmological distances). This is an order 10^(-3) effect applied to fluctuations which are already one part in roughly 10^5, so it is quite small. Nevertheless, it becomes detectable with the all-sky coverage, high angular resolution, and low noise levels of the Planck satellite. Here we report a first measurement of this velocity signature using the aberration and modulation effects on the CMB temperature anisotropies, finding a component in the known dipole direction, (l,b) = (264\u00b0,48\u00b0), of 384 km s^(-1) \u00b1 78 km s^(-1) (stat.) \u00b1 115 km s^(-1) (syst.). This is a significant confirmation of the expected velocity.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A27", "id_number": "CaltechAUTHORS:20190701-101108014", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-101108014", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321556", "primary_object": { "basename": "aa21556-13.pdf", "url": "https://authors.library.caltech.edu/records/fg01x-gs803/files/aa21556-13.pdf" }, "related_objects": [ { "basename": "1303.5087.pdf", "url": "https://authors.library.caltech.edu/records/fg01x-gs803/files/1303.5087.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Aghanim, N.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/swarg-2yg47", "eprint_id": 51431, "eprint_status": "archive", "datestamp": "2023-08-20 03:22:20", "lastmod": "2023-10-18 16:22:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" }, { "id": "Gao-Yu", "name": { "family": "Gao", "given": "Yu" }, "orcid": "0000-0003-0007-2197" }, { "id": "Wang-Junzhi", "name": { "family": "Wang", "given": "Junzhi" } }, { "id": "Zhang-Zhi-Yu", "name": { "family": "Zhang", "given": "Zhi-Yu" }, "orcid": "0000-0002-7299-2876" }, { "id": "Gu-Qiusheng", "name": { "family": "Gu", "given": "Qiusheng" }, "orcid": "0000-0002-3890-3729" } ] }, "title": "Inefficient star formation in extremely metal poor galaxies", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 Macmillan Publishers Limited.\n\nReceived 15 April 2014; Accepted 29 August 2014; Published online 15 October 2014.\n\nY.S. acknowledges support for this work from the Natural Science\nFoundation of China (NSFC), grant 11373021, the Strategic Priority Research Program\n'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences\n(CAS), grant XDB09000000, and Nanjing University grant 985. Y.G. acknowledges\nsupport from the NSFC (grants 11173059 and 11390373) and from the CAS Program\n(grant XDB09000000). J.W. was supported by the National 973 programme (grant\n2012CB821805) and by the NSFC (grant 11173013). Z.-Y.Z. acknowledges support\nfrom the European Research Council (ERC) in the form of advanced grant COSMICISM.\nQ.G. was supported by the NSFC (11273015 and 11133001) and by the National 973\nprogramme (grant 2013CB834905). We thank F. Bigiel for making his data points\navailable to plot contours in Fig. 3, S. P. C. Peters for making available his HI gas map of\nESO 146-G14 to us, and L. Piazzo for help in Herschel data reduction. Herschel is an\nESA space observatory with science instruments provided by European-led Principal\nInvestigator consortia and with important participation from NASA. This work was\nsupported in part by the Spitzer Space Telescope, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology, under a contract with\nNASA. It was also supported in part by a NASA Herschel grant (OT2_yshi_3) issued by\nJPL/Caltech.\n\nAuthor Contributions:\nY.S. led the Herschel proposal, Herschel data reduction and the\nwriting of the manuscript. L.A. helped develop Herschel observations and helped in the\nwriting of the manuscript. G.H. and S.S. assisted in the Herschel proposal. All authors\ndiscussed and commented on the manuscript.\n\nSubmitted - 1410.5504v1.pdf
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", "abstract": "The first galaxies contain stars born out of gas with few or no 'metals' (that is, elements heavier than helium). The lack of metals is expected to inhibit efficient gas cooling and star formation, but this effect has yet to be observed in galaxies with an oxygen abundance (relative to hydrogen) below a tenth of that of the Sun. Extremely metal poor nearby galaxies may be our best local laboratories for studying in detail the conditions that prevailed in low metallicity galaxies at early epochs. Carbon monoxide emission is unreliable as a tracer of gas at low metallicities, and while dust has been used to trace gas in low-metallicity galaxies, low spatial resolution in the far-infrared has typically led to large uncertainties. Here we report spatially resolved infrared observations of two galaxies with oxygen abundances below ten per cent of the solar value, and show that stars formed very inefficiently in seven star-forming clumps in these galaxies. The efficiencies are less than a tenth of those found in normal, metal rich galaxies today, suggesting that star formation may have been very inefficient in the early Universe.", "date": "2014-10-16", "date_type": "published", "publication": "Nature", "volume": "514", "number": "7522", "publisher": "Nature Publishing Group", "pagerange": "335-338", "id_number": "CaltechAUTHORS:20141107-104925647", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141107-104925647", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11373021" }, { "agency": "Chinese Academy of Sciences (CAS)", "grant_number": "XDB09000000" }, { "agency": "Nanjing University", "grant_number": "985" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11173059" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11390373" }, { "agency": "National 973 programme", "grant_number": "2012CB821805" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11173013" }, { "agency": "European Research Council (ERC)" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11273015" }, { "agency": "Natural Science Foundation of China (NSFC)", "grant_number": "11133001" }, { "agency": "National 973 programme", "grant_number": "2013CB834905" }, { "agency": "Spitzer Space Telescope" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Herschel", "grant_number": "OT2_yshi_3" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature13820", "primary_object": { "basename": "nature13820-st3.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-st3.jpg" }, "related_objects": [ { "basename": "nature13820-st4.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-st4.jpg" }, { "basename": "nature13820-st5.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-st5.jpg" }, { "basename": "nature13820-st6.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-st6.jpg" }, { "basename": "1410.5504v1.pdf", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/1410.5504v1.pdf" }, { "basename": "nature13820-sf1.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-sf1.jpg" }, { "basename": "nature13820-st1.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-st1.jpg" }, { "basename": "nature13820-st2.jpg", "url": "https://authors.library.caltech.edu/records/swarg-2yg47/files/nature13820-st2.jpg" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Shi, Yong; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/275cb-t3c96", "eprint_id": 48770, "eprint_status": "archive", "datestamp": "2023-08-20 01:38:52", "lastmod": "2023-10-17 20:25:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Jackson-E", "name": { "family": "Jackson", "given": "Ed" } }, { "id": "Desai-V", "name": { "family": "Desai", "given": "Vandana" }, "orcid": "0000-0002-1340-0543" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi" }, "orcid": "0000-0002-5619-4938" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom" } }, { "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": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hamam-N", "name": { "family": "Hamam", "given": "Nouhad" } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Mi-Wei", "name": { "family": "Mi", "given": "Wei" } }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "Steve" }, "orcid": "0000-0001-5668-3507" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry" }, "orcid": "0000-0002-7064-5424" }, { "id": "Hale-D-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger" } }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } } ] }, "title": "IPAC Image Processing and Data Archiving for the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 Astronomical Society of the Pacific. \n\nReceived 2014 April 04; accepted 2014 May 28; published 2014 July 10. \n\nE. O. O. is incumbent of the Arye Dissentshik career development chair and is gratefully supported by grants from the Israeli Ministry of Science, the Israeli Centers of Research Excellence (I-CORE) Program of the Planning and Budgeting Committee, and the Israel Science Foundation (grant No. 1829/12). We wish to thank Dave Shupe, Trey Roby, Loi Ly, Winston Yang, Rick Ebert, Rich Hoban, Hector Wong, and Jack Lampley for valuable contributions to the project. PTF is a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. This work made use of Montage, 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. Montage is maintained by the NASA/\nIPAC Infrared Science Archive. This project makes use of data from the Sloan Digital Sky Survey, managed by the Astrophysical Research Consortium for the Participating Institutions and funded by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Council for England. This research has made use of the VizieR catalog access tool, Centre de Donn\u00e9es (CDS), Strasbourg, France. Our pipelines use many free software packages from other institutions and past projects (see Table 12), for which we are indebted.\n\nPublished - 677351.pdf
Submitted - 1404.1953v3.pdf
", "abstract": "The Palomar Transient Factory (PTF) is a multiepochal robotic survey of the northern sky that acquires data for the scientific study of transient and variable astrophysical phenomena. The camera and telescope provide for wide-field imaging in optical bands. In the five years of operation since first light on 2008 December 13, images taken with Mould-R and SDSS-g\u2032 camera filters have been routinely acquired on a nightly basis (weather permitting), and two different H\u03b1 filters were installed in 2011 May (656 and 663 nm). The PTF image-processing and data-archival program at the Infrared Processing and Analysis Center (IPAC) is tailored to receive and reduce the data, and, from it, generate and preserve astrometrically and photometrically calibrated images, extracted source catalogs, and co-added reference images. Relational databases have been deployed to track these products in operations and the data archive. The fully automated system has benefited by lessons learned from past IPAC projects and comprises advantageous features that are potentially incorporable into other ground-based observatories. Both off-the-shelf and in-house software have been utilized for economy and rapid development. The PTF data archive is curated by the NASA/IPAC Infrared Science Archive (IRSA). A state-of-the-art custom Web interface has been deployed for downloading the raw images, processed images, and source catalogs from IRSA. Access to PTF data products is currently limited to an initial public data release (M81, M44, M42, SDSS Stripe 82, and the Kepler Survey Field). It is the intent of the PTF collaboration to release the full PTF data archive when sufficient funding becomes available.", "date": "2014-07", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "126", "number": "941", "publisher": "Astronomical Society of the Pacific", "pagerange": "674-710", "id_number": "CaltechAUTHORS:20140821-102815016", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140821-102815016", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science (Israel)" }, { "agency": "Israeli Centers of Research Excellence (I-CORE) Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "NASA", "grant_number": "NCC5-626" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Council for England" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/677351", "primary_object": { "basename": "1404.1953v3.pdf", "url": "https://authors.library.caltech.edu/records/275cb-t3c96/files/1404.1953v3.pdf" }, "related_objects": [ { "basename": "677351.pdf", "url": "https://authors.library.caltech.edu/records/275cb-t3c96/files/677351.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Laher, Russ R.; Surace, Jason; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7a89x-88s10", "eprint_id": 96860, "eprint_status": "archive", "datestamp": "2023-08-20 01:18:02", "lastmod": "2023-10-20 21:34:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abergel-A", "name": { "family": "Abergel", "given": "A." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction \u2013 submillimeter: ISM \u2013 local insterstellar matter \u2013 infrared: diffuse background \u2013 cosmic background radiation", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 18 December 2013; Accepted 29 January 2014; Published online 11 June 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The Parkes Radio Telescope is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement n\u00b0 267934.\n\nPublished - aa23270-13.pdf
Accepted Version - 1312.5446.pdf
", "abstract": "The dust-Hi correlation is used to characterize the emission properties of dust in the diffuse interstellar medium (ISM) from far infrared wavelengths to microwave frequencies. The field of this investigation encompasses the part of the southern sky best suited to study the cosmic infrared and microwave backgrounds. We cross-correlate sky maps from Planck, the Wilkinson Microwave Anisotropy Probe (WMAP), and the diffuse infrared background experiment (DIRBE), at 17 frequencies from 23 to 3000 GHz, with the Parkes survey of the 21 cm line emission of neutral atomic hydrogen, over a contiguous area of 7500 deg^2 centred on the southern Galactic pole. We present a general methodology to study the dust-Hi correlation over the sky, including simulations to quantify uncertainties. Our analysis yields four specific results. (1) We map the temperature, submillimetre emissivity, and opacity of the dust per H-atom. The dust temperature is observed to be anti-correlated with the dust emissivity and opacity. We interpret this result as evidence of dust evolution within the diffuse ISM. The mean dust opacity is measured to be (7.1 \u00b1 0.6) \u00d7 10^(-27) cm^2 H^(-1) \u00d7 (\u03bd/ 353 GHz)^(1.53 \u00b1 0.03) for 100 \u2264 \u03bd \u2264 353 GHz. This is a reference value to estimate hydrogen column densities from dust emission at submillimetre and millimetre wavelengths. (2) We map the spectral index \u03b2mm of dust emission at millimetre wavelengths (defined here as \u03bd \u2264 353 GHz), and find it to be remarkably constant at \u03b2_(mm) = 1.51 \u00b1 0.13. We compare it with the far infrared spectral index \u03b2_(FIR) derived from greybody fits at higher frequencies, and find a systematic difference, \u03b2_(mm) \u2013 \u03b2_(FIR) = \u2212 0.15, which suggests that the dust spectral energy distribution (SED) flattens at \u03bd \u2264 353 GHz. (3) We present spectral fits of the microwave emission correlated with Hi from 23 to 353 GHz, which separate dust and anomalous microwave emission (AME). We show that the flattening of the dust SED can be accounted for with an additional component with a blackbody spectrum. This additional component, which accounts for (26 \u00b1 6)% of the dust emission at 100 GHz, could represent magnetic dipole emission. Alternatively, it could account for an increasing contribution of carbon dust, or a flattening of the emissivity of amorphous silicates, at millimetre wavelengths. These interpretations make different predictions for the dust polarization SED. (4) We analyse the residuals of the dust-Hi correlation. We identify a Galactic contribution to these residuals, which we model with variations of the dust emissivity on angular scales smaller than that of our correlation analysis. This model of the residuals is used to quantify uncertainties of the CIB power spectrum in a companion Planck paper.", "date": "2014-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "566", "publisher": "EDP Sciences", "pagerange": "Art. No. A55", "id_number": "CaltechAUTHORS:20190701-104222513", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-104222513", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201323270", "primary_object": { "basename": "aa23270-13.pdf", "url": "https://authors.library.caltech.edu/records/7a89x-88s10/files/aa23270-13.pdf" }, "related_objects": [ { "basename": "1312.5446.pdf", "url": "https://authors.library.caltech.edu/records/7a89x-88s10/files/1312.5446.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Abergel, A.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/yxyxr-fqb29", "eprint_id": 97092, "eprint_status": "archive", "datestamp": "2023-08-20 00:51:14", "lastmod": "2023-10-20 23:02:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Tibbs-C-T", "name": { "family": "Tibbs", "given": "C. T." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XV. A study of anomalous microwave emission in Galactic clouds", "ispublished": "pub", "full_text_status": "public", "keywords": "HII regions \u2013 radiation mechanisms: general \u2013 radio continuum: ISM \u2013 submillimeter: ISM", "note": "\u00a9 2014 ESO. Article published by EDP Sciences. \n\nReceived 5 September 2013; Accepted 19 February 2014; Published online 20 May 2014. \n\nWe thank the anonymous referee for providing useful comments. We thank Justin Jonas for providing the 2326\u2009MHz HartRAO map. We acknowledge the use of the MPIfR Survey Sampler website at http://www.mpifr-bonn.mpg.de/survey.html and the Legacy Archive for Microwave Background Data Analysis (LAMBDA); support for LAMBDA is provided by the NASA Office of Space Science. 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. This research also makes use of the SIMBAD database, operated at the CDS, Strasbourg, France. We acknowledge the use of NASA's SkyView facility (http://skyview.gsfc.nasa.gov) located at NASA Goddard Space Flight Center. C.D. acknowledges an STFC Advanced Fellowship, an EU Marie-Curie IRG grant under the FP7, and an ERC Starting Grant (No. 307209). The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration.\n\nPublished - aa22612-13.pdf
Accepted Version - 1309.1357.pdf
Erratum - aa22612e-13.pdf
", "abstract": "Anomalous microwave emission (AME) is believed to be due to electric dipole radiation from small spinning dust grains. The aim of this paper is a statistical study of the basic properties of AME regions and the environment in which they emit. We used WMAP and Planck maps, combined with ancillary radio and IR data, to construct a sample of 98 candidate AME sources, assembling SEDs for each source using aperture photometry on 1\u00b0-smoothed maps from 0.408\u2009GHz up to 3000\u2009GHz. Each spectrum is fitted with a simple model of free-free, synchrotron (where necessary), cosmic microwave background (CMB), thermal dust, and spinning dust components. We find that 42 of the 98 sources have significant (>5\u03c3) excess emission at frequencies between 20 and 60\u2009GHz. An analysis of the potential contribution of optically thick free-free emission from ultra-compact H\u2009II regions, using IR colour criteria, reduces the significant AME sample to 27 regions. The spectrum of the AME is consistent with model spectra of spinning dust. Peak frequencies are in the range 20\u221235\u2009GHz except for the California nebula (NGC\u20091499), which appears to have a high spinning dust peak frequency of (50 \u00b1 17)\u2009GHz. The AME regions tend to be more spatially extended than regions with little or no AME. The AME intensity is strongly correlated with the sub-millimetre/IR flux densities and comparable to previous AME detections in the literature. AME emissivity, defined as the ratio of AME to dust optical depth, varies by an order of magnitude for the AME regions. The AME regions tend to be associated with cooler dust in the range 14\u221220\u2009K and an average emissivity index, \u03b2_d, of +1.8, while the non-AME regions are typically warmer, at 20\u221227\u2009K. In agreement with previous studies, the AME emissivity appears to decrease with increasing column density. This supports the idea of AME originating from small grains that are known to be depleted in dense regions, probably due to coagulation onto larger grains. We also find a correlation between the AME emissivity (and to a lesser degree the spinning dust peak frequency) and the intensity of the interstellar radiation field, G_0. Modelling of this trend suggests that both radiative and collisional excitation are important for the spinning dust emission. The most significant AME regions tend to have relatively less ionized gas (free-free emission), although this could be a selection effect. The infrared excess, a measure of the heating of dust associated with H\u2009II regions, is typically >4 for AME sources, indicating that the dust is not primarily heated by hot OB stars. The AME regions are associated with known dark nebulae and have higher 12 \u03bcm/25 \u03bcm ratios. The emerging picture is that the bulk of the AME is coming from the polycyclic aromatic hydrocarbons and small dust grains from the colder neutral interstellar medium phase.", "date": "2014-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "565", "publisher": "EDP Sciences", "pagerange": "Art. No. A103", "id_number": "CaltechAUTHORS:20190712-103904402", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190712-103904402", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "European Research Council (ERC)", "grant_number": "307209" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MICINN)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201322612", "primary_object": { "basename": "1309.1357.pdf", "url": "https://authors.library.caltech.edu/records/yxyxr-fqb29/files/1309.1357.pdf" }, "related_objects": [ { "basename": "aa22612-13.pdf", "url": "https://authors.library.caltech.edu/records/yxyxr-fqb29/files/aa22612-13.pdf" }, { "basename": "aa22612e-13.pdf", "url": "https://authors.library.caltech.edu/records/yxyxr-fqb29/files/aa22612e-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9qy7h-f0t74", "eprint_id": 46120, "eprint_status": "archive", "datestamp": "2023-08-22 12:00:09", "lastmod": "2023-10-26 18:42:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "Georgios E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "D\u00edaz-Santos-T", "name": { "family": "D\u00edaz-Santos", "given": "Tanio" }, "orcid": "0000-0003-0699-6083" }, { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" } ] }, "title": "A Two-parameter Model for the Infrared/Submillimeter/Radio Spectral Energy Distributions of Galaxies and Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: active; galaxies: star formation; infrared: ISM", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 November 25; accepted 2014 February 6; published 2014 March 6. \n\nWe appreciate helpful discussions with Adam Myers, Mike Brotherton, Zhaohui Shang, Allison Kirkpatrick, Emeric Le Floc'h, and James Mullaney. Support for this work, part of the Spitzer Space Telescope Legacy Science Program 40539, was provided by NASA and issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We gratefully acknowledge NASA's support for the construction, operation, and science analysis for the Galaxy Evolution Explorer (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 Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the\nU.S. Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. 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.\n\nPublished - 0004-637X_784_1_83.pdf
Accepted Version - 1402.1495.pdf
", "abstract": "A two-parameter semi-empirical model is presented for the spectral energy distributions of galaxies with contributions to their infrared-submillimeter-radio emission from both star formation and accretion disk-powered activity. This model builds upon a previous one-parameter family of models for star-forming galaxies, and includes an update to the mid-infrared emission using an average template obtained from Spitzer Space Telescope observations of normal galaxies. Star-forming/active galactic nucleus (AGN) diagnostics based on polycyclic aromatic hydrocarbon equivalent widths and broadband infrared colors are presented, and example mid-infrared AGN fractional contributions are estimated from model fits to the Great Observatories All-Sky LIRG Survey sample of nearby U/LIRGS and the Five mJy Unbiased Spitzer Extragalactic Survey sample of 24 \u03bcm selected sources at redshifts 0 \u227e z \u227e 4.", "date": "2014-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "784", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 83", "id_number": "CaltechAUTHORS:20140606-102341805", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140606-102341805", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "40539" }, { "agency": "NASA/JPL/Caltech", "grant_number": "1407" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "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": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/784/1/83", "primary_object": { "basename": "0004-637X_784_1_83.pdf", "url": "https://authors.library.caltech.edu/records/9qy7h-f0t74/files/0004-637X_784_1_83.pdf" }, "related_objects": [ { "basename": "1402.1495.pdf", "url": "https://authors.library.caltech.edu/records/9qy7h-f0t74/files/1402.1495.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Dale, Daniel A.; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ay86r-tr229", "eprint_id": 46257, "eprint_status": "archive", "datestamp": "2023-08-22 11:56:40", "lastmod": "2023-10-26 19:37:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wong-O-Ivy", "name": { "family": "Wong", "given": "O. Ivy" } }, { "id": "Kenney-J-D-P", "name": { "family": "Kenney", "given": "Jeffrey D. P." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "The Search for Shock-excited H_2 in Virgo Spirals Experiencing Ram Pressure Stripping", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: individual (NGC 4330, NGC 4402, NGC 4501, NGC 4522); galaxies: interactions; intergalactic medium", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 May 12; accepted 2014 January 23; published 2014 February 21.\n\nThis work is based in part on observations made with\nthe Spitzer Space Telescope, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology under\na contract with NASA. Support for this work was provided\nby NASA through a grant (R09078) issued by JPL/Caltech.\nO.I.W. is the recipient of a Super Science Fellowship from\nthe Australian Research Council. The authors also thank the\nanonymous referee for the constructive comments which have\ngreatly improved this paper.\n\nPublished - 0004-637X_783_2_109.pdf
Submitted - 1401.6223v2.pdf
", "abstract": "We investigate the presence of shock-excited H_2 in four Virgo cluster galaxies that show clear evidence of ongoing ram pressure stripping. Mid-infrared spectral mapping of the rotational H_2 emission lines were performed using the Infrared Spectrograph on board the Spitzer Space Telescope. We target four regions along the leading side of galaxies where the intracluster medium appears to be pushing back the individual galaxy's interstellar medium. For comparison purposes, we also study two regions on the trailing side of these galaxies: a region within an edge-on disk and an extraplanar star-forming region. We find a factor of 2.6 excess of warm H_2/PAH in our sample relative to the observed fractions in other nearby galaxies. We attribute the H_2/PAH excess to contributions of shock-excited H_2 which is likely to have been triggered by ongoing ram pressure interaction in our sample galaxies. Ram pressure driven shocks may also be responsible for the elevated ratios of [Fe\u2009ii]/[Ne\u2009ii] found in our sample.", "date": "2014-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "783", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 109", "id_number": "CaltechAUTHORS:20140613-080122045", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140613-080122045", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "R09078" }, { "agency": "Australian Research Council" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/783/2/109", "primary_object": { "basename": "0004-637X_783_2_109.pdf", "url": "https://authors.library.caltech.edu/records/ay86r-tr229/files/0004-637X_783_2_109.pdf" }, "related_objects": [ { "basename": "1401.6223v2.pdf", "url": "https://authors.library.caltech.edu/records/ay86r-tr229/files/1401.6223v2.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Wong, O. Ivy; Kenney, Jeffrey D. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8fq6n-74f30", "eprint_id": 43250, "eprint_status": "archive", "datestamp": "2023-08-22 10:54:58", "lastmod": "2023-10-25 23:23:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" } ] }, "title": "The Mid-infrared Light Curve of Nearby Core-collapse Supernova SN 2011dh (PTF 11eon)", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter; galaxies: individual (M51); infrared: ISM; supernovae: individual (SN2011dh)", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 May 8; accepted 2013 September 26; published 2013 November 7. \n\nWe acknowledge the anonymous referee and Eli Dwek for helpful comments. This work was supported and 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. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grants from the Israeli Ministry of Science and the I-CORE Program. Work by A.G.-Y. and his group is supported by grants from the BSF, ISF, GIF and Minerva, the EU/FP7 via an ERC grant, and the Kimmel award for innovative investigation.\n\nPublished - 2041-8205_778_1_L19.pdf
Accepted Version - 1309.4891.pdf
", "abstract": "We present Spitzer observations at 3.6 and 4.5 \u03bcm of the supernova SN 2011dh (PTF 11eon) in M51 from 18 days to 625 days after explosion. The mid-infrared emission peaks at 24 days after explosion at a few \u00d710^7 L_\u2609, and decays more slowly than the visible-light bolometric luminosity. The infrared color temperature cools for the first 90 days and then is constant. Simple numerical models of a thermal echo can qualitatively reproduce the early behavior. At late times, the mid-IR light curve cannot be explained by a simple thermal echo model, suggesting additional dust heating or line emission mechanisms. We also propose that thermal echoes can serve as effective probes to uncover supernovae in heavily obscured environments, and speculate that under the right conditions, integrating the early epoch of the mid-infrared light curve may constrain the total energy in the shock breakout flash.", "date": "2013-11-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "778", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L19", "id_number": "CaltechAUTHORS:20140107-140223826", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140107-140223826", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Minerva" }, { "agency": "European Research Council (ERC)" }, { "agency": "Kimmel Award" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/2041-8205/778/1/L19", "primary_object": { "basename": "1309.4891.pdf", "url": "https://authors.library.caltech.edu/records/8fq6n-74f30/files/1309.4891.pdf" }, "related_objects": [ { "basename": "2041-8205_778_1_L19.pdf", "url": "https://authors.library.caltech.edu/records/8fq6n-74f30/files/2041-8205_778_1_L19.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Helou, George; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/04v31-wjb66", "eprint_id": 41529, "eprint_status": "archive", "datestamp": "2023-08-22 10:48:39", "lastmod": "2023-10-24 23:48:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" } ] }, "title": "A Joint Model of X-Ray and Infrared Backgrounds. II. Compton-thick Active Galactic Nucleus Abundance", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: nuclei", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 January 23; accepted 2013 July 20; published 2013 October 8. \n\nWe thank the anonymous referee for helpful comments that have improved the paper significantly. The work is supported through the Spitzer 5MUSES Legacy Program 40539. The authors acknowledge support by NASA through awards issued by JPL/Caltech. Online calculators of the model are available at http://5muses.ipac.caltech.edu/5muses/EBL_model/index.html.\n\nPublished - Shi_2013_ApJ_777_6.pdf
Accepted Version - 1309.1202v1.pdf
", "abstract": "We estimate the abundance of Compton-thick (CT) active galactic nuclei (AGNs) based on our joint model of X-ray and infrared backgrounds. At L_(rest2-10keV) > 10^(42) erg s^(\u20131), the CT AGN density predicted by our model is a few \u00d710^(\u20134) Mpc^(\u20133) from z = 0 up to z = 3. CT AGNs with higher luminosity cuts (>10^(43), 10^(44), and 10^(45) erg s^(\u20131)) peak at higher redshift and show a rapid increase in number density from z = 0 to z ~ 2-3. The CT AGN to all AGN ratio appears to be low (2%-5%) at f_(2-10keV) > 10^(\u201315) erg s^(\u20131) cm^(\u20132) but rises rapidly toward fainter flux levels. The CT AGNs account for ~38% of the total accreted supermassive black hole mass and contribute ~25% of the cosmic X-ray background spectrum at 20 keV. Our model predicts that the majority (90%) of luminous and bright CT AGNs (L_(rest2-10keV) > 10^(44) erg s^(\u20131) or f_(2-10 keV) > 10^(\u201315) erg s^(\u20131) cm^(\u20132)) have detectable hot dust 5-10 \u03bcm emission, which we associate with a dusty torus. The fraction drops for fainter objects, to around 30% at L_(rest2-10keV) > 10^(42) erg s^(\u20131) or f_(2-10keV) > 10^(\u201317) erg s^(\u20131) cm^(\u20132). Our model confirms that heavily obscured AGNs (N_(HI) > 10^(23) cm^(\u20132)) can be separated from unobscured and mildly obscured ones (N_(HI) < 10^(23) cm^(\u20132)) in the plane of observed frame X-ray hardness versus mid-IR/X-ray ratio.", "date": "2013-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "777", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 6", "id_number": "CaltechAUTHORS:20130925-122421418", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130925-122421418", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Spitzer 5MUSES Legacy Program", "grant_number": "40539" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/777/1/6", "primary_object": { "basename": "1309.1202v1.pdf", "url": "https://authors.library.caltech.edu/records/04v31-wjb66/files/1309.1202v1.pdf" }, "related_objects": [ { "basename": "Shi_2013_ApJ_777_6.pdf", "url": "https://authors.library.caltech.edu/records/04v31-wjb66/files/Shi_2013_ApJ_777_6.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Shi, Yong; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5v2k0-sv027", "eprint_id": 43274, "eprint_status": "archive", "datestamp": "2023-08-19 21:41:53", "lastmod": "2023-10-25 23:24:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G. E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Hurley-P", "name": { "family": "Hurley", "given": "P." } }, { "id": "Alonso-Herrero-A", "name": { "family": "Alonso-Herrero", "given": "A." }, "orcid": "0000-0001-6794-2519" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S." } }, { "id": "Charmandaris-V", "name": { "family": "Charmandaris", "given": "V." }, "orcid": "0000-0002-2688-1956" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dai-Y-Sophia", "name": { "family": "Dai", "given": "Y. Sophia" }, "orcid": "0000-0002-7928-416X" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "id": "Feltre-A", "name": { "family": "Feltre", "given": "A." } }, { "id": "Hatziminaoglou-E", "name": { "family": "Hatziminaoglou", "given": "E." } }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Morrison-G-E", "name": { "family": "Morrison", "given": "G." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M." }, "orcid": "0000-0002-6689-6271" }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Shi-Y", "name": { "family": "Shi", "given": "Y." } } ] }, "title": "Mid- to far-infrared properties of star-forming galaxies and active galactic nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: active, galaxies: starburst, galaxies: star formation, infrared: galaxies", "note": "\u00a9 2013 ESO. Article published by EDP Sciences. \n\nReceived 8 July 2013. Accepted 23 August 2013. Published online 22 October 2013. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nGEM acknowledges support from the John Fell Oxford University Press (OUP) Research Fund and the University of Oxford. A.A.-H. acknowledges funding through the Universidad de Cantabria August G.\nLinares Programme. VC acknowledges partial support from the EU FP7 Grant PIRSES-GA-20120316788. This paper uses data from Herschel's photometer SPIRE. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA).\n\nPublished - aa22226-13.pdf
Submitted - 1309.3922v1.pdf
", "abstract": "We study the mid- to far-IR properties of a 24 \u03bcm-selected flux-limited sample (S_(24)> 5\u2009mJy) of 154 intermediate redshift (\u27e8 z \u27e9 ~ 0.15), infrared luminous galaxies, drawn from the 5 Milli-Jansky Unbiased Spitzer Extragalactic Survey. By combining existing mid-IR spectroscopy and new Herschel SPIRE submm photometry from the Herschel Multi-tiered Extragalactic Survey, we derived robust total infrared luminosity (L_(IR)) and dust mass (M_(dust)) estimates and infered the relative contribution of the AGN to the infrared energy budget of the sources. We found that the total (8\u22121000 \u03bcm) infrared emission of galaxies with weak 6.2 \u03bcm PAH emission (EW_(6.2) \u2264 0.2 \u03bcm) is dominated by AGN activity, while for galaxies with EW_(6.2)> 0.2 \u03bcm more than 50% of the L_(IR) arises from star formation. We also found that for galaxies detected in the 250\u2013500 \u03bcm Herschel bands an AGN has a statistically insignificant effect on the temperature of the cold dust and the far-IR colours of the host galaxy, which are primarily shaped by star formation activity. For star-forming galaxies we reveal an anti-correlation between the L_(IR)-to-rest-frame 8 \u03bcm luminosity ratio, IR8 \u2261 L_(IR)/L_8\u2009 and the strength of PAH features. We found that this anti-correlation is primarily driven by variations in the PAHs emission, and not by variations in the 5\u221215 \u03bcm mid-IR continuum emission. Using the [Ne\u2009iii]/[Ne\u2009ii] line ratio as a tracer of the hardness of the radiation field, we confirm that galaxies with harder radiation fields tend to exhibit weaker PAH features, and found that they have higher IR8 values and higher dust-mass-weighted luminosities (L_(IR)/M_(dust)), the latter being a proxy for the dust temperature (T_d). We argue that these trends originate either from variations in the environment of the star-forming regions or are caused by variations in the age of the starburst. Finally, we provide scaling relations that will allow estimating L_(IR), based on single-band observations with the mid-infrared instrument, on board the upcoming James Webb Space Telescope.", "date": "2013-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "558", "publisher": "EDP Sciences", "pagerange": "Art. No. A136", "id_number": "CaltechAUTHORS:20140108-140820993", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140108-140820993", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "John Fell Oxford University Press (OUP) Research Fund" }, { "agency": "University of Oxford" }, { "agency": "Universidad de Cantabria August G. Linares Programme" }, { "agency": "European Research Council (ERC)", "grant_number": "PIRSES-GA-20120316788" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201322226", "primary_object": { "basename": "1309.3922v1.pdf", "url": "https://authors.library.caltech.edu/records/5v2k0-sv027/files/1309.3922v1.pdf" }, "related_objects": [ { "basename": "aa22226-13.pdf", "url": "https://authors.library.caltech.edu/records/5v2k0-sv027/files/aa22226-13.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Magdis, G. E.; Rigopoulou, D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/h23t6-cdg05", "eprint_id": 38803, "eprint_status": "archive", "datestamp": "2023-08-22 09:20:38", "lastmod": "2023-10-23 23:29:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Li-Yiming", "name": { "family": "Li", "given": "Yiming" } }, { "id": "Crocker-A-F", "name": { "family": "Crocker", "given": "Alison F." }, "orcid": "0000-0001-8513-4945" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Wilson-C-D", "name": { "family": "Wilson", "given": "Christine D." }, "orcid": "0000-0001-5817-0991" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Brandl-B-R", "name": { "family": "Brandl", "given": "Bernhard R." } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "B. D." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "K." }, "orcid": "0000-0002-5258-7224" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "B." }, "orcid": "0000-0002-9768-0246" }, { "id": "Hao-C-N", "name": { "family": "Hao", "given": "C.-N." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hinz-J-L", "name": { "family": "Hinz", "given": "J." } }, { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Krause-O", "name": { "family": "Krause", "given": "O." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sauvage-M", "name": { "family": "Sauvage", "given": "M." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" } ] }, "title": "Star Formation Rates in Resolved Galaxies: Calibrations with Near- and Far-infrared Data for NGC 5055 and NGC 6946", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; H II regions; infrared: galaxies; infrared: ISM; ISM: structure", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2012 November 12; accepted 2013 April 4; published 2013 April 26. \n\nBased on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, and the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. \n\nThis work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Partial support for this work was provided by NASA through the award 1369560 issued by JPL/Caltech. This work has also been partially supported by the NASA\u2013ADAP grant NNX10AD08G. The research of C.D.W. is supported by grants from the Natural Sciences and Engineering Research Council of Canada. The authors would like to thank Daniel Devost for the WIRCam observations with RUNID 07AD86 for NGC 5055 and 07BD91 for NGC 6946. \n\nThis work 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 authors thank an anonymous referee for valuable comments that have helped improve this paper.\n\nPublished - 0004-637X_768_2_180.pdf
Accepted Version - 1304.1541.pdf
", "abstract": "We use the near-infrared Br\u03b3 hydrogen recombination line as a reference star formation rate (SFR) indicator to test the validity and establish the calibration of the Herschel/PACS 70 \u03bcm emission as a SFR tracer for sub-galactic regions in external galaxies. Br\u03b3 offers the double advantage of directly tracing ionizing photons and of being relatively insensitive to the effects of dust attenuation. For our first experiment, we use archival Canada-France-Hawaii Telescope Br\u03b3 and Ks images of two nearby galaxies: NGC 5055 and NGC 6946, which are also part of the Herschel program KINGFISH (Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel). We use the extinction corrected Br\u03b3 emission to derive the SFR(70) calibration for H II regions in these two galaxies. A comparison of the SFR(70) calibrations at different spatial scales, from 200 pc to the size of the whole galaxy, reveals that about 50% of the total 70 \u03bcm emission is due to dust heated by stellar populations that are unrelated to the current star formation. We use a simple model to qualitatively relate the increase of the SFR(70) calibration coefficient with decreasing region size to the star formation timescale. We provide a calibration for an unbiased SFR indicator that combines the observed H\u03b1 with the 70 \u03bcm emission, also for use in H II regions. We briefly analyze the PACS 100 and 160 \u03bcm maps and find that longer wavelengths are not as good SFR indicators as 70 \u03bcm, in agreement with previous results. We find that the calibrations show about 50% difference between the two galaxies, possibly due to effects of inclination.", "date": "2013-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "768", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 180", "id_number": "CaltechAUTHORS:20130605-085927165", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130605-085927165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "1369560" }, { "agency": "NASA", "grant_number": "NNX10AD08G" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/768/2/180", "primary_object": { "basename": "1304.1541.pdf", "url": "https://authors.library.caltech.edu/records/h23t6-cdg05/files/1304.1541.pdf" }, "related_objects": [ { "basename": "0004-637X_768_2_180.pdf", "url": "https://authors.library.caltech.edu/records/h23t6-cdg05/files/0004-637X_768_2_180.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Li, Yiming; Crocker, Alison F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/63d56-f1g65", "eprint_id": 38941, "eprint_status": "archive", "datestamp": "2023-08-19 19:41:00", "lastmod": "2023-10-24 14:53:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Boquien-M", "name": { "family": "Boquien", "given": "M." }, "orcid": "0000-0003-0946-6176" }, { "id": "Brandl-B-R", "name": { "family": "Brandl", "given": "B." } }, { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "K. V." }, "orcid": "0000-0002-5258-7224" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "B." }, "orcid": "0000-0002-9768-0246" }, { "id": "Hao-C-N", "name": { "family": "Hao", "given": "C.-N." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hinz-J-L", "name": { "family": "Hinz", "given": "J. L." } }, { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Johnson-B-D", "name": { "family": "Johnson", "given": "B. D." } }, { "id": "Li-Yiming", "name": { "family": "Li", "given": "Y." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sandstrom-K-M", "name": { "family": "Sandstrom", "given": "K." }, "orcid": "0000-0002-4378-8534" }, { "id": "Skibba-R-A", "name": { "family": "Skibba", "given": "R. A." } }, { "id": "Tabatabaei-F-S", "name": { "family": "Tabatabaei", "given": "F. S." } } ] }, "title": "Calibration of the total infrared luminosity of nearby galaxies from Spitzer and Herschel bands", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction\n galaxies: ISM\n submillimetre: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 February 18. Received 2013 February 12; in original form 2012 December 15. First published online: March 20, 2013. \n\nWe would like to thank the referee for his/her careful reading of the paper and a helpful report. We would like to thank M. Pereira-Santaella for providing us with the SPIRE flux densities and TIR luminosities of his sources. PACS has been developed by MPE (Germany); UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by BMVIT (Austria), ESAPRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL,\nUKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). This research has also 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 - MNRAS-2013-Galametz-1956-86.pdf
Accepted Version - 1302.4363.pdf
", "abstract": "When combined with infrared observations with the Spitzer telescope (3 to 160\u2009\u03bcm), the Herschel Space Observatory now fully samples the thermal dust emission up to 500\u2009\u03bcm and enables us to better estimate the total infrared-submm energy budget (L_(TIR)) of nearby galaxies. We present new empirical calibrations to estimate resolved and integrated total infrared luminosities from Spitzer and Herschel bands used as monochromatic or combined tracers. We base our calibrations on resolved elements of nearby galaxies (3 to 30\u2009Mpc) observed with Herschel. We perform a resolved spectral energy distribution (SED) modelling of these objects using the Draine & Li dust models and investigate the influence of the addition of Spectral and Photometric Imaging Receiver (SPIRE) measurements in the estimation of L_(TIR). We find that using data up to 250\u2009\u03bcm leads to local L_(TIR) values consistent with those obtained with a complete coverage (up to 500\u2009\u03bcm) within \u00b110 per cent for most of our resolved elements. We then study the distribution of energy in the resolved SEDs of our galaxies. The bulk of energy (30\u201350 per cent) is contained in the [70\u2013160\u2009\u03bcm] band. The [24\u201370\u2009\u03bcm] fraction decreases with increasing metallicity. The [160\u20131100\u2009\u03bcm]submillimetre band can account for up to 25 per cent of the L_(TIR) in metal-rich galaxies. We investigate the correlation between the total infrared (TIR) surface brightnesses/luminosities and monochromatic Spitzer and Herschel surface brightnesses/luminosities. The three Photodetector Array Camera and Spectrometer (PACS) bands can be used as reliable monochromatic estimators of the L_(TIR), the 100\u2009\u03bcm band being the most reliable monochromatic tracer. There is also a strong correlation between the SPIRE 250\u2009\u03bcm and L_(TIR), although with more scatter than for the PACS relations. We also study the ability of our monochromatic relations to reproduce integrated L_(TIR) of nearby galaxies as well as L_(TIR) of z \u223c 1\u20133 sources. Finally, we provide calibration coefficients that can be used to derive TIR surface brightnesses/luminosities from a combination of Spitzer and Herschel surface brightnesses/fluxes and analyse the associated uncertainties.", "date": "2013-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "431", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1956-1986", "id_number": "CaltechAUTHORS:20130613-100124435", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130613-100124435", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt313", "primary_object": { "basename": "1302.4363.pdf", "url": "https://authors.library.caltech.edu/records/63d56-f1g65/files/1302.4363.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Galametz-1956-86.pdf", "url": "https://authors.library.caltech.edu/records/63d56-f1g65/files/MNRAS-2013-Galametz-1956-86.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Galametz, M.; Kennicutt, R. C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/snhcc-nv271", "eprint_id": 38978, "eprint_status": "archive", "datestamp": "2023-08-22 09:02:33", "lastmod": "2023-10-24 14:55:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tabatabaei-F-S", "name": { "family": "Tabatabaei", "given": "F. S." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Beck-R", "name": { "family": "Beck", "given": "R." } }, { "id": "Groves-B-A", "name": { "family": "Groves", "given": "B." }, "orcid": "0000-0002-9768-0246" }, { "id": "Meidt-S-E", "name": { "family": "Meidt", "given": "S. E." }, "orcid": "0000-0002-6118-4048" }, { "id": "Krause-M", "name": { "family": "Krause", "given": "M." } }, { "id": "Rix-H-W", "name": { "family": "Rix", "given": "H.-W." }, "orcid": "0000-0003-4996-9069" }, { "id": "Sandstrom-K-M", "name": { "family": "Sandstrom", "given": "K." }, "orcid": "0000-0002-4378-8534" }, { "id": "Crocker-A-F", "name": { "family": "Crocker", "given": "A. F." }, "orcid": "0000-0001-8513-4945" }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Wilson-C-D", "name": { "family": "Wilson", "given": "C. D." }, "orcid": "0000-0001-5817-0991" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B." }, "orcid": "0000-0002-0846-936X" }, { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D." }, "orcid": "0000-0002-5782-9093" }, { "id": "Dumas-G", "name": { "family": "Dumas", "given": "G." } }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Hinz-J-L", "name": { "family": "Hinz", "given": "J." } }, { "id": "Kreckel-K", "name": { "family": "Kreckel", "given": "K." }, "orcid": "0000-0001-6551-3091" }, { "id": "Montiel-E", "name": { "family": "Montiel", "given": "E." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } } ] }, "title": "A detailed study of the radio-FIR correlation in NGC 6946 with Herschel-PACS/SPIRE from KINGFISH", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual: NGC 6946; radio continuum: ISM; ISM: magnetic fields; infrared: ISM; galaxies: star formation", "note": "\u00a9 2013 ESO. Article published by EDP Sciences. \n\nReceived: 17 August 2012. Accepted: 22 January 2013. Published online 15 March 2013. \n\nWe are grateful to A. Ferguson for kindly providing us with the H\u03b1 data. The combined molecular and atomic gas data were kindly provided by F. Walter. F.S.T. acknowledges the support by the DFG via the grant TA 801/1-1.\n\nPublished - aa20249-12.pdf
Accepted Version - 1301.6884.pdf
", "abstract": "We derive the distribution of the synchrotron spectral index across NGC\u20096946 and investigate the correlation between the radio continuum (synchrotron) and far-infrared (FIR) emission using the KINGFISH Herschel-PACS and SPIRE data. The radio-FIR correlation is studied as a function of star formation rate, magnetic field strength, radiation field strength, and the total gas surface density. The synchrotron emission follows both star-forming regions and the so-called magnetic arms present in the inter-arm regions. The synchrotron spectral index is steepest along the magnetic arms (\u03b1_n ~ 1), while it is flat in places of giant Hii regions and in the center of the galaxy (\u03b1_n ~ 0.6\u22120.7). The map of \u03b1_n provides observational evidence for aging and energy loss of cosmic ray electrons (CREs) propagating in the disk of the galaxy. Variations in the synchrotron-FIR correlation across the galaxy are shown to be a function of both star formation and magnetic field strength. We find that the synchrotron emission correlates better with cold rather than with warm dust emission, when the diffuse interstellar radiation field is the main heating source of dust. The synchrotron-FIR correlation suggests a coupling between the magnetic field and the gas density. NGC\u20096946 shows a power-law behavior between the total (turbulent) magnetic field strength B and the star formation rate surface density \u03a3_(SFR) with an index of 0.14\u2009(0.16) \u00b1 0.01. This indicates an efficient production of the turbulent magnetic field with the increasing gas turbulence expected in actively star forming regions. Moreover, it is suggested that the B-\u03a3_(SFR) power law index is similar for the turbulent and the total fields in normal galaxies. On the other hand, for galaxies interacting with the cluster environment this index is steeper for turbulent magnetic fields than it is for the total magnetic fields. The scale-by-scale analysis of the synchrotron-FIR correlation indicates that the ISM affects the propagation of old/diffused CREs, resulting in a diffusion coefficient of D_0 = 4.6 \u00d7 10^(28)\u2009cm^2\u2009s^(-1) for 2.2\u2009GeV CREs.", "date": "2013-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "552", "publisher": "EDP Sciences", "pagerange": "Art. No. A19", "id_number": "CaltechAUTHORS:20130619-083510282", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130619-083510282", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TA 801/1-1" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201220249", "primary_object": { "basename": "1301.6884.pdf", "url": "https://authors.library.caltech.edu/records/snhcc-nv271/files/1301.6884.pdf" }, "related_objects": [ { "basename": "aa20249-12.pdf", "url": "https://authors.library.caltech.edu/records/snhcc-nv271/files/aa20249-12.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Tabatabaei, F. S.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/azfra-neg38", "eprint_id": 105641, "eprint_status": "archive", "datestamp": "2023-08-22 08:50:31", "lastmod": "2024-01-15 17:05:06", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Min-Wei", "name": { "family": "Min", "given": "Wei" }, "orcid": "0000-0003-2570-3557" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "S." }, "orcid": "0000-0001-5668-3507" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "D." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Palomar Transient Factory Data Archive", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Relational Database; Disk Storage; Public Release; Image Metadata; Demilitarize Zone", "note": "\u00a9 2013 Springer-Verlag Berlin Heidelberg.", "abstract": "The Palomar Transient Factory (PTF) is a multi-epoch robotic survey of the northern sky for the scientific study of transient astronomical phenomena. The camera and telescope provide for wide-field imaging in two optical bands. The system has been in operation since December 2008. The image data are sent to the Infrared Processing and Analysis Center (IPAC) for processing and archiving. The archived science products are astrometrically and photometrically calibrated images, extracted source catalogs, and coadded reference images. Relational databases track these products in operations and the data archive. The fully automated system has benefited by lessons learned from past IPAC projects and comprises advantageous features that are potentially incorporable into other ground-based observatories. Both off-the-shelf and in-house software have been utilized for economy and rapid development. The PTF data archive is curated by the NASA/IPAC Infrared Science Archive (IRSA). A state-of-the-art custom web interface has been deployed for downloading the raw images, processed images, and source catalogs from IRSA. A public release of this science-rich archive is planned.", "date": "2013-03", "date_type": "published", "publisher": "Springer", "place_of_pub": "Berlin", "pagerange": "67-70", "id_number": "CaltechAUTHORS:20200929-132408274", "isbn": "978-3-642-37133-2", "book_title": "Databases in Networked Information Systems", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200929-132408274", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "contributors": { "items": [ { "id": "Madaan-A", "name": { "family": "Madaan", "given": "Aastha" } }, { "id": "Kikuchi-S", "name": { "family": "Kikuchi", "given": "Shinji" } }, { "id": "Bhalla-S", "name": { "family": "Bhalla", "given": "Subhash" } } ] }, "doi": "10.1007/978-3-642-37134-9_5", "resource_type": "book_section", "pub_year": "2013", "author_list": "Min, Wei; Laher, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fzwey-hxw34", "eprint_id": 37422, "eprint_status": "archive", "datestamp": "2023-08-22 08:41:20", "lastmod": "2023-10-23 17:26:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel" }, "orcid": "0000-0002-5782-9093" } ] }, "title": "A Joint Model of the X-Ray and Infrared Extragalactic Backgrounds. I. Model Construction and First Results", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: evolution; galaxies: luminosity function, mass function", "note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2012 July 30; accepted 2012 November 10; published 2013 January 22.\n\nWe thank the anonymous referee for detailed and constructive\ncomments. We thank Matthieu Bethermin for careful reading\nand comments. The work is supported through the Spitzer\n5MUSES Legacy Program 40539. The authors acknowledge\nsupport by NASA through awards issued by JPL/Caltech.\n\nPublished - 0004-637X_764_1_28.pdf
", "abstract": "We present an extragalactic population model of the cosmic background light to interpret the rich high-quality survey data in the X-ray and IR bands. The model incorporates star formation and supermassive black hole (SMBH) accretion in a co-evolution scenario to fit simultaneously 617 data points of number counts, redshift distributions, and local luminosity functions (LFs) with 19 free parameters. The model has four main components, the total IR LF, the SMBH accretion energy fraction in the IR band, the star formation spectral energy distribution (SED), and the unobscured SMBH SED extinguished with a H I column density distribution. As a result of the observational uncertainties about the star formation and SMBH SEDs, we present several variants of the model. The best-fit reduced \u03c72 reaches as small as 2.7-2.9 of which a significant amount (>0.8) is contributed by cosmic variances or caveats associated with data. Compared to previous models, the unique result of this model is to constrain the SMBH energy fraction in the IR band that is found to increase with the IR luminosity but decrease with redshift up to z ~ 1.5; this result is separately verified using aromatic feature equivalent-width data. The joint modeling of X-ray and mid-IR data allows for improved constraints on the obscured active galactic nucleus (AGN), especially the Compton-thick AGN population. All variants of the model require that Compton-thick AGN fractions decrease with the SMBH luminosity but increase with redshift while the type 1 AGN fraction has the reverse trend.", "date": "2013-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "764", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 28", "id_number": "CaltechAUTHORS:20130308-134657854", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130308-134657854", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Spitzer 5MUSES Legacy Program", "grant_number": "40539" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/764/1/28", "primary_object": { "basename": "0004-637X_764_1_28.pdf", "url": "https://authors.library.caltech.edu/records/fzwey-hxw34/files/0004-637X_764_1_28.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Shi, Yong; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gzqaj-ydq70", "eprint_id": 36319, "eprint_status": "archive", "datestamp": "2023-08-22 07:57:53", "lastmod": "2023-10-20 23:00:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Bremseth-J", "name": { "family": "Bremseth", "given": "J." } }, { "id": "Mason-B-S", "name": { "family": "Mason", "given": "B. S." } }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "J. J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Turner-J-L", "name": { "family": "Turner", "given": "J. L." }, "orcid": "0000-0003-4625-2951" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" } ] }, "title": "The Star Formation in Radio Survey: GBT 33 GHz Observations of Nearby Galaxy Nuclei and Extranuclear Star-forming Regions", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic rays; galaxies: nuclei; H II regions; radio continuum: general; stars: formation", "note": "\u00a9 2012 American Astronomical Society. Received 2012 July 13; accepted 2012 October 10; published 2012 November 30. We thank the anonymous referee for useful suggestions that\nhelped improve the presentation of the paper. E.J.M. thanks C. Leitherer and M. Seibert for useful discussions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - 0004-637X_761_2_97.pdf
", "abstract": "We present 33 GHz photometry of 103 galaxy nuclei and extranuclear star-forming complexes taken with the Green Bank Telescope as part of the Star Formation in Radio Survey. Among the sources without evidence for an active galactic nucleus, and also having lower frequency radio data, we find a median thermal fraction at 33 GHz of \u224876% with a dispersion of \u224824%. For all sources resolved on scales \u227e0.5 kpc, the thermal fraction is even larger, being \u227390%. This suggests that the rest-frame 33 GHz emission provides a sensitive measure of the ionizing photon rate from young star-forming regions, thus making it a robust star formation rate (SFR) indicator. Taking the 33 GHz SFRs as a reference, we investigate other empirical calibrations relying on different combinations of warm 24 \u03bcm dust, total infrared (IR; 8-1000 \u03bcm), H\u03b1 line, and far-UV continuum emission. The recipes derived here generally agree with others found in the literature, albeit with a large dispersion that most likely stems from a combination of effects. Comparing the 33 GHz to total IR flux ratios as a function of the radio spectral index, measured between 1.7 and 33 GHz, we find that the ratio increases as the radio spectral index flattens which does not appear to be a distance effect. Consequently, the ratio of non-thermal to total IR emission appears relatively constant, suggesting only moderate variations in the cosmic-ray electron injection spectrum and ratio of synchrotron to total cooling processes among star-forming complexes. Assuming that this trend solely arises from an increase in the thermal fraction sets a maximum on the scatter of the non-thermal spectral indices among the star-forming regions of \u03c3_\u03b1 NT \u227e0.13.", "date": "2012-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "761", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 97", "id_number": "CaltechAUTHORS:20130111-105248992", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130111-105248992", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/761/2/97", "primary_object": { "basename": "0004-637X_761_2_97.pdf", "url": "https://authors.library.caltech.edu/records/gzqaj-ydq70/files/0004-637X_761_2_97.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Murphy, E. J.; Bremseth, J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a1gnw-apw71", "eprint_id": 36060, "eprint_status": "archive", "datestamp": "2023-08-22 07:53:09", "lastmod": "2023-10-20 22:11:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kim-Ji-Hoon", "name": { "family": "Kim", "given": "Ji Hoon" } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "Myungshin" }, "orcid": "0000-0002-8537-6714" }, { "id": "Lee-Hyung-Mok", "name": { "family": "Lee", "given": "Hyung-Mok" }, "orcid": "0000-0003-4412-7161" }, { "id": "Lee-Myung-Gyoon", "name": { "family": "Lee", "given": "Myung Gyoon" } }, { "id": "Jun-Hyunsung-David", "name": { "family": "Jun", "given": "Hyunsung David" }, "orcid": "0000-0003-1470-5901" }, { "id": "Nakagawa-Takao", "name": { "family": "Nakagawa", "given": "Takao" } }, { "id": "Matsuhara-Hideo", "name": { "family": "Matsuhara", "given": "Hideo" } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "Takehiko" } }, { "id": "Oyabu-Shinki", "name": { "family": "Oyabu", "given": "Shinki" } }, { "id": "Takagi-Toshinobu", "name": { "family": "Takagi", "given": "Toshinobu" } }, { "id": "Inami-Hanae", "name": { "family": "Inami", "given": "Hanae" }, "orcid": "0000-0003-4268-0393" }, { "id": "Ohyama-Youichi", "name": { "family": "Ohyama", "given": "Youichi" }, "orcid": "0000-0001-9490-3582" }, { "id": "Yamada-Rika", "name": { "family": "Yamada", "given": "Rika" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" } ] }, "title": "The 3.3 \u03bcm Polycyclic Aromatic Hydrocarbon Emission as a Star Formation Rate Indicator", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: ISM; galaxies: starburst; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 December 8; accepted 2012 September 29; published 2012 November 15. \n\nThe authors sincerely appreciate the anonymous referee's helpful comments and suggestions to improve the quality of this paper. They also thank Yanling Wu for her work leading to this paper. This work was supported by a Korean Research Foundation (KRF) grant funded by the Korean government (MEST), No. 2010\u20130000712. This research is based on observations with AKARI, a JAXA project with the participation of ESA.\n\nPublished - 0004-637X_760_2_120.pdf
", "abstract": "Polycyclic aromatic hydrocarbon (PAH) emission features dominate the mid-infrared spectra of star-forming galaxies and can be useful to calibrate star formation rates (SFRs) and diagnose ionized states of grains. However, the PAH 3.3 \u03bcm feature has not been studied as much as other PAH features since it is weaker than others and resides outside of Spitzer capability. In order to detect and calibrate the 3.3 \u03bcm PAH emission and investigate its potential as an SFR indicator, we carried out an AKARI mission program, AKARI mJy Unbiased Survey of Extragalactic Sources (AMUSES), and compared its sample with various literature samples. We obtained 2-5 \u03bcm low-resolution spectra of 20 flux-limited galaxies with mixed spectral energy distribution classes, which yielded the detection of the 3.3 \u03bcm PAH emission from 3 out of 20 galaxies. For the combined sample of AMUSES and literature samples, the 3.3 \u03bcm PAH luminosities correlate with the infrared luminosities of star-forming galaxies, albeit with a large scatter (1.5 dex). The correlation appears to break down at the domain of ultraluminous infrared galaxies (ULIRGs), and the power of the 3.3 \u03bcm PAH luminosity as a proxy for the infrared luminosity is hampered at log[L P_(AH3.3) erg^(\u20131) s^(\u20131)] > ~42.0. Possible origins for this deviation in the correlation are discussed, including contributions from active galactic nuclei and strongly obscured young stellar objects, and the destruction of PAH molecules in ULIRGs.", "date": "2012-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "760", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 120", "id_number": "CaltechAUTHORS:20121219-145701379", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121219-145701379", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Research Foundation of Korea" }, { "agency": "Ministry of Education, Science and Technology (Korea)", "grant_number": "2010-0000712" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/760/2/120", "primary_object": { "basename": "0004-637X_760_2_120.pdf", "url": "https://authors.library.caltech.edu/records/a1gnw-apw71/files/0004-637X_760_2_120.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Kim, Ji Hoon; Im, Myungshin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7za61-6y883", "eprint_id": 35895, "eprint_status": "archive", "datestamp": "2023-08-22 07:11:49", "lastmod": "2023-10-20 21:54:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dib-S", "name": { "family": "Dib", "given": "Sami" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Moore-T-J-T", "name": { "family": "Moore", "given": "Toby J. T." } }, { "id": "Urquhart-J-S", "name": { "family": "Urquhart", "given": "James S." } }, { "id": "Dariush-A-A", "name": { "family": "Dariush", "given": "Ali" } } ] }, "title": "The Lesser Role of Shear in Galactic Star Formation: Insight from the Galactic Ring Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; ISM: clouds; ISM: molecules; stars: formation", "note": "\u00a9 2012 American Astronomical Society. Received 2012 January 31; accepted 2012 August 31; published 2012 October 8. We are very grateful to the referee for a thoughtful report\nwhich helped us improve both the content of the paper and\nthe presentation of the results. We also thank Samuel Boissier\nand Ruixiang Chang for useful discussions. S.D. acknowledges\nsupport from the Science and Technology Facilities Council\n(STFC) grant ST/H00307X/1 and a Santander Mobility Award.\nT.J.T.M. is supported in part by STFC grant ST/001847/1.\nThis publication makes use of molecular line data from\nthe Boston University-FCRAO Galactic Ring Survey (GRS).\nThe GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National\nScience Foundation under grants AST-9800334, AST-0098562,\nand AST-0100793. This paper made use of information from the\nRedMSX Source survey database at www.ast.leeds.ac.uk/RMS\nwhich was constructed with support from the STFC. Partial support for this work was provided by NASA through the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology.\n\nPublished - 0004-637X_758_2_125.pdf
", "abstract": "We analyze the role played by shear in regulating star formation in the Galaxy on the scale of individual molecular clouds. The clouds are selected from the ^(13)CO J = 1-0 line of the Galactic Ring Survey. For each cloud, we estimate the shear parameter which describes the ability of density perturbations to grow within the cloud. We find that for almost all molecular clouds considered, there is no evidence that shear is playing a significant role in opposing the effects of self-gravity. We also find that the shear parameter of the clouds does not depend on their position in the Galaxy. Furthermore, we find no correlations between the shear parameter of the clouds with several indicators of their star formation activity. No significant correlation is found between the shear parameter and the star formation efficiency of the clouds which is measured using the ratio of the massive young stellar objects luminosities, measured in the Red MSX survey, to the cloud mass. There are also no significant correlations between the shear parameter and the fraction of their mass that is found in denser clumps which is a proxy for their clump formation efficiency, nor with their level of fragmentation expressed in the number of clumps per unit mass. Our results strongly suggest that shear is playing only a minor role in affecting the rates and efficiencies at which molecular clouds convert their gas into dense cores and thereafter into stars.", "date": "2012-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "758", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 125", "id_number": "CaltechAUTHORS:20121210-104018358", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121210-104018358", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/H00307X/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/001847/1" }, { "agency": "NSF", "grant_number": "AST-9800334" }, { "agency": "NSF", "grant_number": "AST-0098562" }, { "agency": "NSF", "grant_number": "AST-0100793" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA Spitzer Space Telescope" }, { "agency": "Santander Mobility Award" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/758/2/125", "primary_object": { "basename": "0004-637X_758_2_125.pdf", "url": "https://authors.library.caltech.edu/records/7za61-6y883/files/0004-637X_758_2_125.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Dib, Sami; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/906kt-8m993", "eprint_id": 35214, "eprint_status": "archive", "datestamp": "2023-08-22 06:51:45", "lastmod": "2023-10-20 15:51:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: NGC 628 and NGC 6946", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: abundances; galaxies: general; galaxies: ISM; infrared: galaxies; ISM: general", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2012 March 14; accepted 2012 June 19; published 2012 August 23.\n\nWe are grateful to R. H. Lupton for availability of the SM\ngraphics program, and to the anonymous referee for helpful\nsuggestions.\nThis research was supported in part by JPL grants 1329088\nand 1373687, and by NSF grant AST1008570.\n\nPublished - 0004-637X_756_2_138.pdf
", "abstract": "We characterize the dust in NGC 628 and NGC 6946, two nearby spiral galaxies in the KINGFISH sample. With data from 3.6 \u03bcm to 500 \u03bcm, dust models are strongly constrained. Using the Draine & Li dust model (amorphous silicate and carbonaceous grains), for each pixel in each galaxy we estimate (1) dust mass surface density, (2) dust mass fraction contributed by polycyclic aromatic hydrocarbons, (3) distribution of starlight intensities heating the dust, (4) total infrared (IR) luminosity emitted by the dust, and (5) IR luminosity originating in regions with high starlight intensity. We obtain maps for the dust properties, which trace the spiral structure of the galaxies. The dust models successfully reproduce the observed global and resolved spectral energy distributions (SEDs). The overall dust/H mass ratio is estimated to be 0.0082 \u00b1 0.0017 for NGC 628, and 0.0063 \u00b1 0.0009 for NGC 6946, consistent with what is expected for galaxies of near-solar metallicity. Our derived dust masses are larger (by up to a factor of three) than estimates based on single-temperature modified blackbody fits. We show that the SED fits are significantly improved if the starlight intensity distribution includes a (single intensity) \"delta function\" component. We find no evidence for significant masses of cold dust (T \u2272 12 K). Discrepancies between PACS and MIPS photometry in both low and high surface brightness areas result in large uncertainties when the modeling is done at PACS resolutions, in which case SPIRE, MIPS70, and MIPS160 data cannot be used. We recommend against attempting to model dust at the angular resolution of PACS.", "date": "2012-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "756", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 138", "id_number": "CaltechAUTHORS:20121031-140206376", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121031-140206376", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL", "grant_number": "1329088" }, { "agency": "JPL", "grant_number": "1373687" }, { "agency": "NSF", "grant_number": "AST1008570" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/756/2/138", "primary_object": { "basename": "0004-637X_756_2_138.pdf", "url": "https://authors.library.caltech.edu/records/906kt-8m993/files/0004-637X_756_2_138.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Aniano, G.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/j65n9-0av68", "eprint_id": 34992, "eprint_status": "archive", "datestamp": "2023-08-19 11:56:43", "lastmod": "2023-10-19 23:36:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "D." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" }, { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "J. C." }, "orcid": "0000-0003-2192-5371" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P." }, "orcid": "0000-0002-3389-0586" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Pickles-A-J", "name": { "family": "Pickles", "given": "A." } }, { "id": "Ag\u00fceros-M-A", "name": { "family": "Ag\u00fceros", "given": "M." }, "orcid": "0000-0001-7077-3664" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "L." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "The Palomar Transient Factory photometric catalog 1.0", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomical Techniques", "note": "\u00a9 2012 The Astronomical Society of the Pacific.\n\nReceived 2012 February 28; accepted 2012 June 05; published 2012 August 29.\n\nWe thank an anonymous referee for constructive comments.\nThis article is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. E. O. O. is the incumbent of the Arye Dissentshik career development chair and is grateful for support via a grant from the Israeli Ministry\nof Science, and the Helen Kimmel Center for Planetary Science. S. R. K. and his group are partially supported by NSF grant AST-0507734.\n\nPublished - 666978.pdf
", "abstract": "We constructed a photometrically calibrated catalog of non-variable sources from the Palomar Transient Factory (PTF) observations. The first version of this catalog presented here, the PTF photometric catalog 1.0, contains calibrated R_PTF-filter magnitudes for \u22482.1 \u00d7 10^7 sources brighter than magnitude 19, over an area of \u224811,233 deg^2. The magnitudes are provided in the PTF photometric system, and the color of a source is required in order to convert these magnitudes into other magnitude systems. We estimate that the magnitudes in this catalog have a typical accuracy of about 0.02 mag with respect to magnitudes from the Sloan Digital Sky Survey. The median repeatability of our catalog's magnitudes for stars between 15 and 16 mag, is about 0.01 mag and it is over 0.03 mag for 95% of the sources in this magnitude range. The main goal of this catalog is to provide reference magnitudes for photometric calibration of visible light observations. Subsequent versions of this catalog, which will be published incrementally online, will be extended to cover a larger sky area and will also include g_PTF-filter magnitudes, as well as variability and proper-motion information.", "date": "2012-08", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "124", "number": "918", "publisher": "Astronomical Society of the Pacific", "pagerange": "854-860", "id_number": "CaltechAUTHORS:20121019-135732936", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121019-135732936", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science (Israel)" }, { "agency": "Helen Kimmel Center for Planetary Science" }, { "agency": "NSF", "grant_number": "AST-0507734" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/666978", "primary_object": { "basename": "666978.pdf", "url": "https://authors.library.caltech.edu/records/j65n9-0av68/files/666978.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Ofek, E. O.; Laher, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/e4ddt-fff19", "eprint_id": 34358, "eprint_status": "archive", "datestamp": "2023-08-19 11:34:36", "lastmod": "2023-10-19 14:51:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Gorjian-V", "name": { "family": "Gorjian", "given": "Varoujan" } }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Fowler-J-W", "name": { "family": "Fowler", "given": "John W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" } ] }, "title": "Aperture Photometry Tool", "ispublished": "pub", "full_text_status": "public", "keywords": "Data Analysis and Techniques", "note": "\u00a9 2012 Astronomical Society of the Pacific. Received 2010 March 29; accepted 2012 May 24; published 2012 July 10. We thank the beta testers. In particular, Tom Jarrett, Seppo\nLaine, Alberto Crespo-Noriega, Bill Reach, Jeonghee Rho, and\nNancy Silbermann made numerous helpful suggestions. Inga\nSaathoff conducted invaluable beta testing in Germany. We\nare also grateful to Xiuqin Wu, Trey Roby, Loi Ly, and Booth\nHartley for generous expert Java programming help and the use\nof some of their Java classes.We also thank BenneW. Holwerda\nfor his insightful suggestions and manuscript corrections. Aperture\nPhotometry Tool's motto Inviso notitia and logo are copyright \u00a9 2012 by the California Institute of Technology.\n\nPublished - 666883.pdf
", "abstract": "Aperture Photometry Tool (APT) is software for astronomers and students interested in manually exploring the photometric qualities of astronomical images. It is a graphical user interface (GUI) designed to allow the image data associated with aperture photometry calculations for point and extended sources to be visualized and, therefore, more effectively analyzed. The finely tuned layout of the GUI, along with judicious use of color-coding and alerting, is intended to give maximal user utility and convenience. Simply mouse-clicking on a source in the displayed image will instantly draw a circular or elliptical aperture and sky annulus around the source and will compute the source intensity and its uncertainty, along with several commonly used measures of the local sky background and its variability. The results are displayed and can be optionally saved to an aperture-photometry-table file and plotted on graphs in various ways using functions available in the software. APT is geared toward processing sources in a small number of images and is not suitable for bulk processing a large number of images, unlike other aperture photometry packages (e.g., SExtractor). However, APT does have a convenient source-list tool that enables calculations for a large number of detections in a given image. The source-list tool can be run either in automatic mode to generate an aperture photometry table quickly or in manual mode to permit inspection and adjustment of the calculation for each individual detection. APT displays a variety of useful graphs with just the push of a button, including image histogram, x and y aperture slices, source scatter plot, sky scatter plot, sky histogram, radial profile, curve of growth, and aperture-photometry-table scatter plots and histograms. APT has many functions for customizing the calculations, including outlier rejection, pixel \"picking\" and \"zapping,\" and a selection of source and sky models. The radial-profile-interpolation source model, which is accessed via the radial-profile-plot panel, allows recovery of source intensity from pixels with missing data and can be especially beneficial in crowded fields.", "date": "2012-07", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "124", "number": "917", "publisher": "Astronomical Society of the Pacific", "pagerange": "737-763", "id_number": "CaltechAUTHORS:20120925-135301558", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120925-135301558", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/666883", "primary_object": { "basename": "666883.pdf", "url": "https://authors.library.caltech.edu/records/e4ddt-fff19/files/666883.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Laher, Russ R.; Gorjian, Varoujan; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7j2br-pwk41", "eprint_id": 34357, "eprint_status": "archive", "datestamp": "2023-08-19 11:34:30", "lastmod": "2023-10-19 14:51:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Gorjian-V", "name": { "family": "Gorjian", "given": "Varoujan" } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Fowler-J-W", "name": { "family": "Fowler", "given": "John W." } }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl" }, "orcid": "0000-0003-4072-169X" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Mattingly-S", "name": { "family": "Mattingly", "given": "Sean" } }, { "id": "Jackson-E", "name": { "family": "Jackson", "given": "Ed" } }, { "id": "Hacopeans-E", "name": { "family": "Hacopeans", "given": "Eugean" } }, { "id": "Hamam-N", "name": { "family": "Hamam", "given": "Nouhad" } }, { "id": "Groom-S-L", "name": { "family": "Groom", "given": "Steve" }, "orcid": "0000-0001-5668-3507" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry" }, "orcid": "0000-0002-7064-5424" }, { "id": "Mi-Wei", "name": { "family": "Mi", "given": "Wei" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "Julian C." }, "orcid": "0000-0003-2192-5371" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." } }, { "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" } }, { "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": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" } ] }, "title": "Aperture Photometry Tool Versus SExtractor for Noncrowded Fields", "ispublished": "pub", "full_text_status": "public", "keywords": "Data Analysis and Techniques", "note": "\u00a9 2012 Astronomical Society of the Pacific. Received 2010 March 29; accepted 2012 April 27; published 2012 June 18. This work is based in part on images acquired by the Palomar\nTransient Factory; in part on archival data obtained with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under a contract with\nthe National Aeronautics and Space Administration (NASA); and\nin part on observations made with the NASA/ESA Hubble Space\nTelescope and obtained from the Hubble Legacy Archive, which\nis a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating\nFacility (ST-ECF/ESA), and the Canadian Astronomy Data\nCentre (CADC/NRC/CSA). This research made use of\nMontage, funded by NASA's Earth Science Technology Office,\nComputation Technologies Project, under cooperative agreement NCC5-626 between NASA and the California Institute of\nTechnology. Montage is maintained by the NASA/IPAC Infrared\nScience Archive.\n\nPublished - 666507.pdf
", "abstract": "Outputs from new software program Aperture Photometry Tool (APT) are compared with similar outputs from SExtractor for sources extracted from R-band optical images acquired by the Palomar Transient Factory (PTF), infrared mosaics constructed from Spitzer Space Telescope images, and a processed visible/near-infrared image from the Hubble Legacy Archive (HLA). Two large samples from the PTF images are studied, each containing around 3 \u00d7 10^3 sources from noncrowded fields. The median values of source-intensity relative percentage differences between the two software programs, computed separately for two PTF samples, are +0.13% and +0.17%, with corresponding statistical dispersions of 1.43% and 1.84%, respectively. For the Spitzer mosaics, a similar large sample of extracted sources for each of channels 1\u20134 of Spitzer's Infrared Array Camera (IRAC) are analyzed with two different sky annulus sizes, and we find that the median and modal values of source-intensity relative percentage differences between the two software programs are between -0.5% and +2.0%, and the corresponding statistical dispersions range from 1.4 to 6.7%, depending on the Spitzer IRAC channel and sky annulus. The results for the HLA image are mixed, as might be expected for a moderately crowded field. The comparisons for the three different kinds of images show that there is generally excellent agreement between APT and SExtractor. Differences in source-intensity uncertainty estimates for the PTF images amount to less than 3% for the PTF sources, and these are potentially caused by SExtractor's omission of the sky background uncertainty term in the formula for source-intensity uncertainty, as well as differing methods of sky background estimation.", "date": "2012-07", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "124", "number": "917", "publisher": "Astronomical Society of the Pacific", "pagerange": "764-781", "id_number": "CaltechAUTHORS:20120925-132848017", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120925-132848017", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NCC5-626" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/666507", "primary_object": { "basename": "666507.pdf", "url": "https://authors.library.caltech.edu/records/7j2br-pwk41/files/666507.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Laher, Russ R.; Rebull, Luisa M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dtbwb-gdx02", "eprint_id": 30088, "eprint_status": "archive", "datestamp": "2023-08-22 05:52:14", "lastmod": "2023-10-17 15:17:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" } ] }, "title": "A Study of Heating and Cooling of the ISM in NGC 1097 with Herschel-PACS and Spitzer-IRS", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 1097); galaxies: ISM; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2012 The American Astronomical Society. \n\nReceived 2011 November 28; accepted 2012 March 28; published 2012 May 16. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nWe thank Gregory Brunner and Sebastian Haan for the code used to construct the Spitzer-IRS maps. We also thank Dario Fadda and Jeff Jacobson for software support. This work is partially based on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). Data presented in this paper were analyzed using The Herschel Interactive Processing Environment (HIPE), a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia.\n\nPublished - Beir\u00e3o_2012_ApJ_751_144.pdf
Submitted - A9R97ED.pdf
", "abstract": "NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst ring, a strong large-scale bar, and an active nucleus. We present a detailed study of the spatial variation of the far-infrared (FIR) [C II]158 \u03bcm and [O I]63 \u03bcm lines and mid-infrared H_2 emission lines as tracers of gas cooling, and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the photoelectric heating, using Herschel-PACS and Spitzer-IRS infrared spectral maps. We focus on the nucleus and the ring, and two star-forming regions (Enuc N and Enuc S). We estimated a photoelectric gas heating efficiency ([C II]158 \u03bcm+[O I]63 \u03bcm)/PAH in the ring about 50% lower than in Enuc N and S. The average 11.3/7.7 \u03bcm PAH ratio is also lower in the ring, which may suggest a larger fraction of ionized PAHs, but no clear correlation with [C II]158 \u03bcm/PAH(5.5-14 \u03bcm) is found. PAHs in the ring are responsible for a factor of two more [C II]158 \u03bcm and [O I]63 \u03bcm emission per unit mass than PAHs in the Enuc S. spectral energy distribution (SED) modeling indicates that at most 25% of the FIR power in the ring and Enuc S can come from high-intensity photodissociation regions (PDRs), in which case G_0 ~ 10^(2.3) and n_H ~ 10^(3.5) cm^(\u20133) in the ring. For these values of G_0 and n_H, PDR models cannot reproduce the observed H2 emission. Much of the H2 emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.", "date": "2012-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "751", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 144", "id_number": "CaltechAUTHORS:20120416-075343247", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120416-075343247", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/751/2/144", "primary_object": { "basename": "A9R97ED.pdf", "url": "https://authors.library.caltech.edu/records/dtbwb-gdx02/files/A9R97ED.pdf" }, "related_objects": [ { "basename": "Beir\u00e3o_2012_ApJ_751_144.pdf", "url": "https://authors.library.caltech.edu/records/dtbwb-gdx02/files/Beir\u00e3o_2012_ApJ_751_144.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Beir\u00e3o, P.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/p4bqv-jpz06", "eprint_id": 31817, "eprint_status": "archive", "datestamp": "2023-08-22 05:42:00", "lastmod": "2023-10-17 21:22:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Peterson-B-W", "name": { "family": "Peterson", "given": "B. W." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "P." }, "orcid": "0000-0002-2421-1350" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Cluver-M-E", "name": { "family": "Cluver", "given": "M. E." }, "orcid": "0000-0002-9871-6490" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Struck-C-J", "name": { "family": "Struck", "given": "C." }, "orcid": "0000-0002-6490-2156" }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "F." } } ] }, "title": "Detection of Powerful Mid-IR H_2 Emission in the Bridge between the Taffy Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (UGC 12914, UGC 12915); galaxies: interactions; intergalactic medium", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 January 21; accepted 2012 March 11; published 2012 April 30.\n\nB.W.P. thanks the IPAC Visiting Graduate Student Fellowship (from 2009 September to 2010 March) for supporting this work. We also thank Jim Condon for providing a digital copy of the 20 cm radio data and the anonymous referee for many insightful comments that greatly improved this manuscript. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech) under NASA contract. 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. Facility: Spitzer\n\nPublished - Peterson2012p18391Astrophys_J.pdf
", "abstract": "We report the detection of strong, resolved emission from warm H_2 in the Taffy galaxies and bridge. Relative to the continuum and faint polyclic aromatic hydrocarbon (PAH) emission, the H_2 emission is the strongest in the connecting bridge, approaching L(H_2)/L(PAH 8 \u03bcm) = 0.1 between the two galaxies, where the purely rotational lines of H_2 dominate the mid-infrared spectrum in a way very reminiscent of the group-wide shock in the interacting group Stephan's Quintet (SQ). The surface brightness in the 0-0 S(0) and S(1) H_2 lines in the bridge is more than twice that observed at the center of the SQ shock. We observe a warm H2 mass of 4.2 \u00d7 10^8 M_\u2609 in the bridge, but taking into account the unobserved bridge area, the total warm mass is likely to be twice this value. We use excitation diagrams to characterize the warm molecular gas, finding an average surface mass of ~5 \u00d7 10^6 M_\u2609 kpc^(\u20132) and typical excitation temperatures of 150-175 K. H_2 emission is also seen in the galaxy disks, although there the emission is more consistent with normal star-forming galaxies. We investigate several possible heating mechanisms for the bridge gas but favor the conversion of kinetic energy from the head-on collision via turbulence and shocks as the main heating source. Since the cooling time for the warm H_2 is short (~5000 yr), shocks must be permeating the molecular gas in the bridge region in order to continue heating the H_2.", "date": "2012-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "751", "number": "1", "publisher": "American Astronomical Society", "pagerange": "11", "id_number": "CaltechAUTHORS:20120605-123347820", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120605-123347820", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "IPAC Visiting Graduate Student Fellowship" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/751/1/11", "primary_object": { "basename": "Peterson2012p18391Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/p4bqv-jpz06/files/Peterson2012p18391Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Peterson, B. W.; Appleton, P. N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xx6qn-6tw44", "eprint_id": 31768, "eprint_status": "archive", "datestamp": "2023-08-22 05:41:33", "lastmod": "2023-10-17 21:07:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Davies-J-E", "name": { "family": "Davies", "given": "J. E." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Bertincourt-B", "name": { "family": "Bertincourt", "given": "B." } }, { "id": "Seymour-N", "name": { "family": "Seymour", "given": "N." }, "orcid": "0000-0003-3506-5536" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Ultraluminous Star-forming Galaxies and Extremely Luminous Warm Molecular Hydrogen Emission at z = 2.16 in the PKS 1138\u201326 Radio Galaxy Protocluster", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (PKS 1138\u201326); galaxies: formation; galaxies: high-redshift", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 November 23; accepted 2012 March 13; published 2012 April 30. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. This work benefited greatly from the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. N.S. is a recipient of an Australian Research Council Future Fellowship.\n\nPublished - Ogle2012p18394Astrophys_J.pdf
Submitted - 1203.3019v1.pdf
", "abstract": "A deep Spitzer Infrared Spectrograph map of the PKS 1138\u201326 galaxy protocluster reveals ultraluminous polycyclic aromatic hydrocarbon (PAH) emission from obscured star formation in three protocluster galaxies, including H\u03b1-emitter (HAE) 229, HAE 131, and the central Spiderweb Galaxy. Star formation rates of ~500-1100 M_\u2609 yr^(\u20131) are estimated from the 7.7 \u03bcm PAH feature. At such prodigious formation rates, the galaxy stellar masses will double in 0.6-1.1 Gyr. We are viewing the peak epoch of star formation for these protocluster galaxies. However, it appears that extinction of H\u03b1 is much greater (up to a factor of 40) in the two ULIRG HAEs compared to the Spiderweb. This may be attributed to different spatial distributions of star formation-nuclear star formation in the HAEs versus extended star formation in accreting satellite galaxies in the Spiderweb. We find extremely luminous mid-IR rotational line emission from warm molecular hydrogen in the Spiderweb Galaxy, with L(H_2 0-0 S(3)) = 1.4 \u00d7 10^(44) erg s^(\u20131) (3.7 \u00d7 10^(10) L_\u2609), ~20 times more luminous than any previously known H2 emission galaxy (MOHEG). Depending on the temperature, this corresponds to a very large mass of >9 \u00d7 10^(6)-2 \u00d7 10^9 M_\u2609 of T > 300 K molecular gas, which may be heated by the PKS 1138\u201326 radio jet, acting to quench nuclear star formation. There is >8 times more warm H_2 at these temperatures in the Spiderweb than what has been seen in low-redshift (z < 0.2) radio galaxies, indicating that the Spiderweb may have a larger reservoir of molecular gas than more evolved radio galaxies. This is the highest redshift galaxy yet in which warm molecular hydrogen has been directly detected.", "date": "2012-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "751", "number": "1", "publisher": "American Astronomical Society", "pagerange": "13", "id_number": "CaltechAUTHORS:20120601-100532323", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120601-100532323", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Australian Research Council" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/751/1/13", "primary_object": { "basename": "1203.3019v1.pdf", "url": "https://authors.library.caltech.edu/records/xx6qn-6tw44/files/1203.3019v1.pdf" }, "related_objects": [ { "basename": "Ogle2012p18394Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/xx6qn-6tw44/files/Ogle2012p18394Astrophys_J.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Ogle, P.; Davies, J. E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/5z1sc-6ye03", "eprint_id": 31715, "eprint_status": "archive", "datestamp": "2023-08-22 05:40:01", "lastmod": "2023-10-17 20:19:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Porter-T-A", "name": { "family": "Porter", "given": "T. A." } }, { "id": "Moskalenko-I-V", "name": { "family": "Moskalenko", "given": "I. V." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Strong-A-W", "name": { "family": "Strong", "given": "A. W." }, "orcid": "0000-0003-3799-5489" } ] }, "title": "Characterizing Cosmic-Ray Propagation in Massive Star-forming Regions: The Case of 30 Doradus and the Large Magellanic Cloud", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic rays; galaxies: individual (LMC); gamma rays: galaxies; H II regions; infrared: galaxies; radio continuum: galaxies; stars: formation", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2012 January 24; accepted 2012 March 7; published 2012 April 24.\n\nWe thank the anonymous referee for useful suggestions that helped to improve the content and presentation of this paper. E. J. M. thanks Annie Hughes for both providing us with radio maps and for useful discussions which greatly helped shape the paper. We are grateful to the SAGE team for producing high quality data sets used in this study. T.A.P. and E.J.M. acknowledge support via NASA grant NNX10AE78G. I.V.M. acknowledges support via NASA grant NNX09AC15G. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d' \u00c9tudes Spatiales in France. 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. This research has additionally made use of the NASA/IPAC Extragalactic Database (NED), which is also operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.\n\nPublished - Murphy2012p18284Astrophys_J.pdf
", "abstract": "Using infrared, radio, and \u03b3-ray data, we investigate the propagation characteristics of cosmic-ray (CR) electrons and nuclei in the 30 Doradus (30 Dor) star-forming region in the Large Magellanic Cloud (LMC) using a phenomenological model based on the radio-far-infrared correlation within galaxies. Employing a correlation analysis, we derive an average propagation length of ~100-140 pc for ~3 GeV CR electrons resident in 30 Dor from consideration of the radio and infrared data. Assuming that the observed \u03b3-ray emission toward 30 Dor is associated with the star-forming region, and applying the same methodology to the infrared and \u03b3-ray data, we estimate a ~20 GeV propagation length of 200-320 pc for the CR nuclei. This is approximately twice as large as for ~3 GeV CR electrons, corresponding to a spatial diffusion coefficient that is ~4 times higher, scaling as (R/GV)\u03b4 with \u03b4 \u2248 0.7-0.8 depending on the smearing kernel used in the correlation analysis. This value is in agreement with the results found by extending the correlation analysis to include ~70 GeV CR nuclei traced by the 3-10 GeV \u03b3-ray data (\u03b4 \u2248 0.66 \u00b1 0.23). Using the mean age of the stellar populations in 30 Dor and the results from our correlation analysis, we estimate a diffusion coefficient D_R \u2248 (0.9-1.0) \u00d7 10^(27)(R/GV)0.7 cm^(2) s^(\u20131). We compare the values of the CR electron propagation length and surface brightness for 30 Dor and the LMC as a whole with those of entire disk galaxies. We find that the trend of decreasing average CR propagation distance with increasing disk-averaged star formation activity holds for the LMC, and extends down to single star-forming regions, at least for the case of 30 Dor.", "date": "2012-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "750", "number": "2", "publisher": "American Astronomical Society", "pagerange": "126", "id_number": "CaltechAUTHORS:20120530-114858153", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120530-114858153", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX10AE78G" }, { "agency": "NASA", "grant_number": "NNX09AC15G" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" } ] }, "doi": "10.1088/0004-637X/750/2/126", "primary_object": { "basename": "Murphy2012p18284Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/5z1sc-6ye03/files/Murphy2012p18284Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Murphy, E. J.; Porter, T. A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/sv9rv-yat28", "eprint_id": 29853, "eprint_status": "archive", "datestamp": "2023-08-22 05:07:53", "lastmod": "2023-10-24 22:30:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "Kevin V." }, "orcid": "0000-0002-5258-7224" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" } ] }, "title": "Resolving the Far-IR Line Deficit: Photoelectric Heating and Far-IR Line Cooling in NGC 1097 and NGC 4559", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 1097, NGC 4559); galaxies: ISM; ISM: lines and bands", "note": "\u00a9 2012 American Astronomical Society. Received 2011 November 11; accepted 2012 January 2; published 2012 February 15. \nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\nPACS has been developed by a consortium of institutes\nled by MPE (Germany) and including UVIE (Austria); KU\nLeuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA\n(Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy);\nand IAC (Spain). This development has been supported by the\nfunding agencies BMVIT (Austria), ESA-PRODEX (Belgium),\nCEA/CNES (France), DLR (Germany), ASI/INAF (Italy),\nand CICYT/MCYT (Spain). HIPE is a joint development by\nthe Herschel Science Ground Segment Consortium, consisting\nof ESA, the NASA Herschel Science Center, and the HIFI,\nPACS, and SPIRE consortia. This work is based (in part) on\nobservations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA.\nSupport for this work was provided by NASA through an\naward issued by JPL/Caltech. This research has made use\nof 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.\n\nPublished - Croxall2012p17550Astrophys_J.pdf
", "abstract": "The physical state of interstellar gas and dust is dependent on the processes which heat and cool this medium. To probe heating and cooling of the interstellar medium over a large range of infrared surface brightness, on sub-kiloparsec scales, we employ line maps of [C II] 158 \u03bcm, [O I] 63 \u03bcm, and [N II] 122 \u03bcm in NGC 1097 and NGC 4559, obtained with the Photodetector Array Camera & Spectrometer on board Herschel. We matched new observations to existing Spitzer Infrared Spectrograph data that trace the total emission of polycyclic aromatic hydrocarbons (PAHs). We confirm at small scales in these galaxies that the canonical measure of photoelectric heating efficiency, ([C II] + [O I])/TIR, decreases as the far-infrared (far-IR) color, \u03bd_f \u03bd(70 \u03bcm) \u03bdf_\u03bd(100 \u03bcm), increases. In contrast, the ratio of far-IR cooling to total PAH emission, ([C II] + [O I])/PAH, is a near constant ~6% over a wide range of far-IR color, 0.5 < \u03bdf_\u03bd(70 \u03bcm) \u03bdf_\u03bd(100 \u03bcm) \u227e 0.95. In the warmest regions, where \u03bdf_\u03bd(70 \u03bcm) \u03bdf_\u03bd(100 \u03bcm) \u2273 0.95, the ratio ([C II] + [OI])/PAH drops rapidly to 4%. We derived representative values of the local ultraviolet radiation density, G_0, and the gas density, n_H, by comparing our observations to models of photodissociation regions. The ratio G_0/n_H, derived from fine-structure lines, is found to correlate with the mean dust-weighted starlight intensity, langUrang, derived from models of the IR spectral energy distribution. Emission from regions that exhibit a line deficit is characterized by an intense radiation field, indicating that small grains are susceptible to ionization effects. We note that there is a shift in the 7.7/11.3 \u03bcm PAH ratio in regions that exhibit a deficit in ([C II] + [O I])/PAH, suggesting that small grains are ionized in these environments.", "date": "2012-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "747", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 81", "id_number": "CaltechAUTHORS:20120327-074624584", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120327-074624584", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/747/1/81", "primary_object": { "basename": "Croxall2012p17550Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/sv9rv-yat28/files/Croxall2012p17550Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Croxall, Kevin V.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9hf49-qjg19", "eprint_id": 29933, "eprint_status": "archive", "datestamp": "2023-08-22 04:44:56", "lastmod": "2023-10-24 22:35:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" } ] }, "title": "Herschel Far-Infrared and Submillimeter Photometry for the Kingfish Sample of Nearby Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; infrared: ISM; ISM: general", "note": "\u00a9 2012 American Astronomical Society. Received 2011 October 25; accepted 2011 December 4; published 2012 January 4. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia\nand with important participation from NASA. IRAF, the\nImage Reduction and Analysis Facility, has been developed by\nthe National Optical Astronomy Observatories and the Space\nTelescope Science Institute.\n\nPublished - Dale2012p17613Astrophys_J.pdf
", "abstract": "New far-infrared and submillimeter photometry from the Herschel Space Observatory is presented for 61 nearby galaxies from the Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel (KINGFISH) sample. The spatially integrated fluxes are largely consistent with expectations based on Spitzer far-infrared photometry and extrapolations to longer wavelengths using popular dust emission models. Dwarf irregular galaxies are notable exceptions, as already noted by other authors, as their 500 \u03bcm emission shows evidence for a submillimeter excess. In addition, the fraction of dust heating attributed to intense radiation fields associated with photodissociation regions is found to be (21 \u00b1 4)% larger when Herschel data are included in the analysis. Dust masses obtained from the dust emission models of Draine & Li are found to be on average nearly a factor of two higher than those based on single-temperature modified blackbodies, as single blackbody curves do not capture the full range of dust temperatures inherent to any galaxy. The discrepancy is largest for galaxies exhibiting the coolest far-infrared colors.", "date": "2012-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "745", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 95", "id_number": "CaltechAUTHORS:20120402-101320344", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120402-101320344", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/745/1/95", "primary_object": { "basename": "Dale2012p17613Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/9hf49-qjg19/files/Dale2012p17613Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Dale, D. A.; Appleton, P. N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vend7-55232", "eprint_id": 42915, "eprint_status": "archive", "datestamp": "2023-08-19 09:27:41", "lastmod": "2023-10-25 23:08:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "D." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "J. C." }, "orcid": "0000-0003-2192-5371" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P." }, "orcid": "0000-0002-3389-0586" }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "J." } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Ag\u00fceros-M-A", "name": { "family": "Ag\u00fceros", "given": "M." }, "orcid": "0000-0001-7077-3664" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "L." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "The Palomar Transient Factory Photometric Calibration", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 The Astronomical Society of the Pacific.\n\nReceived 2011 August 21; accepted 2011 December 5; published 2012 January 30.\n\nWe thank Andrew Pickles and an anonymous referee for\nuseful comments on the article. This article is based on observations\nobtained with the Samuel Oschin Telescope as part of\nthe Palomar Transient Factory project, a scientific collaboration\nbetween the California Institute of Technology, Columbia\nUniversity, Las Cumbres Observatory, the Lawrence Berkeley\nNational Laboratory, the National Energy Research Scientific\nComputing Center, the University of Oxford, and theWeizmann\nInstitute of Science. E. O. O. is supported by an Einstein fellowship\nand NASA grants. S. R. K. and his group are partially supported\nby the NSF grant AST-0507734. S. B. C. acknowledges\ngenerous financial assistance from Gary and Cynthia Bengier,\nthe Richard and Rhoda Goldman Fund, NASA/Swift grants\nNNX10AI21G and GO-7100028, the TABASGO Foundation,\nand NSF grant AST-0908886.\n\nPublished - 664065.pdf
Submitted - 1112.4851v1.pdf
", "abstract": "The Palomar Transient Factory (PTF) provides multiple epoch imaging for a large fraction of the celestial sphere. Here, we describe the photometric calibration of the PTF data products that allows the PTF magnitudes to be related to other magnitude systems. The calibration process utilizes Sloan Digital Sky Survey (SDSS) r \u223c 16 mag point-source objects as photometric standards. During photometric conditions, this allows us to solve for the extinction coefficients and color terms and to estimate the camera illumination correction. This also enables the calibration of fields that are outside the SDSS footprint. We test the precision and repeatability of the PTF photometric calibration. Given that PTF is observing in a single filter each night, we define a PTF calibrated magnitude system for the R band and g band. We show that, in this system, \u224859% (47%) of the photometrically calibrated PTF R-band (g-band) data achieve a photometric precision of 0.02\u20130.04 mag and have color terms and extinction coefficients that are close to their average values. Given the objects' color, the PTF magnitude system can be converted to other systems. Moreover, a night-by-night comparison of the calibrated magnitudes of individual stars observed on multiple nights shows that they are consistent to a level of \u22480.02 mag. Most of the data that were taken under nonphotometric conditions can be calibrated relative to other epochs of the same sky footprint obtained during photometric conditions. We provide a concise guide describing how to use the PTF photometric-calibration data products, as well as the transformations between the PTF magnitude system and the SDSS and Johnson-Cousins systems.", "date": "2012-01", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "124", "number": "911", "publisher": "Astronomical Society of the Pacific", "pagerange": "62-73", "id_number": "CaltechAUTHORS:20131210-082130611", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131210-082130611", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Einstein Fellowship" }, { "agency": "NSF", "grant_number": "AST-0507734" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "GO-7100028" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/664065", "primary_object": { "basename": "1112.4851v1.pdf", "url": "https://authors.library.caltech.edu/records/vend7-55232/files/1112.4851v1.pdf" }, "related_objects": [ { "basename": "664065.pdf", "url": "https://authors.library.caltech.edu/records/vend7-55232/files/664065.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Ofek, E. O.; Laher, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ms78e-0hk61", "eprint_id": 29127, "eprint_status": "archive", "datestamp": "2023-08-19 08:47:49", "lastmod": "2023-10-24 18:22:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "KINGFISH\u2014Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel: Survey Description and Image Atlas", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxies", "note": "\u00a9 2011 Astronomical Society of the Pacific.\n\nReceived 2011 September 21; accepted 2011 November 14; published 2011 December 21.\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\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 - Kennicutt2011p16992Publ_Astron_Soc_Pac.pdf
", "abstract": "The KINGFISH project (Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel) is an imaging and spectroscopic survey of 61 nearby (d < 30 Mpc) galaxies, chosen to cover a wide range of galaxy properties and local interstellar medium (ISM) environments found in the nearby universe. Its broad goals are to characterize the ISM of present-day galaxies, the heating and cooling of their gaseous and dust components, and to better understand the physical processes linking star formation and the ISM. KINGFISH is a direct descendant of the Spitzer Infrared Nearby Galaxies Survey (SINGS), which produced complete Spitzer imaging and spectroscopic mapping and a comprehensive set of multiwavelength ancillary observations for the sample. The Herschel imaging consists of complete maps for the galaxies at 70, 100, 160, 250, 350, and 500 \u03bcm. The spectral line imaging of the principal atomic ISM cooling lines ([O I] 63 \u03bcm, [O III] 88 \u03bcm, [N II] 122,205 \u03bcm, and [C II] 158 \u03bcm) covers the subregions in the centers and disks that already have been mapped in the mid-infrared with Spitzer. The KINGFISH and SINGS multiwavelength data sets combined provide panchromatic mapping of the galaxies sufficient to resolve individual star-forming regions, and tracing the important heating and cooling channels of the ISM, across a wide range of local extragalactic ISM environments. This article summarizes the scientific strategy for KINGFISH, the properties of the galaxy sample, the observing strategy, and data processing and products. It also presents a combined Spitzer and Herschel image atlas for the KINGFISH galaxies, covering the wavelength range 3.6\u2013500 \u03bcm. All imaging and spectroscopy data products will be released to the Herschel user-generated product archives.", "date": "2011-12", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "123", "number": "910", "publisher": "Astronomical Society of the Pacific", "pagerange": "1347-1369", "id_number": "CaltechAUTHORS:20120203-115828066", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120203-115828066", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/663818", "primary_object": { "basename": "Kennicutt2011p16992Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/ms78e-0hk61/files/Kennicutt2011p16992Publ_Astron_Soc_Pac.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Kennicutt, R. C.; Appleton, P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/726ev-70142", "eprint_id": 85229, "eprint_status": "archive", "datestamp": "2023-08-19 08:50:37", "lastmod": "2023-10-18 17:59:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Matsumura-Tomotake", "name": { "family": "Matsumura", "given": "Tomotake" } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga-Ram" }, "orcid": "0000-0001-7583-0621" }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 ESO. \n\nReceived: 10 January 2011. Accepted: 29 June 2011. \n\nThe Planck HFI instrument (http://hfi.planck.fr/) was designed and built by an international consortium of laboratories, universities and institutes, with important contributions from the industry, under the leadership of the PI institute, IAS at Orsay, France. It was funded in particular by CNES, CNRS, NASA, STFC and ASI. The authors extend their gratitude to the numerous engineers and scientists, who have contributed to the design, development, construction or evaluation of the HFI instrument. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/index.php?project=PLANCK\\&page=Planck_Collaboration. The Planck Collaboration acknowledges financial support from: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC and MICINN (Spain); Tekes and AoF (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); Swiss Funding Agency (Switzerland); Norwegian Funding Agency (Norway); and FCT/MCTES (Portugal).\n\nPublished - aa16487-11.pdf
Submitted - 1101.2039.pdf
", "abstract": "The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10\u2032 (100 GHz), 7\u2032 (143 GHz), and 5\u2032 (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6\u22122.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.", "date": "2011-12", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "536", "number": "12", "publisher": "EDP Sciences", "pagerange": "Art. No. A4", "id_number": "CaltechAUTHORS:20180309-110837130", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180309-110837130", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Finnish Funding Agency for Technology and Innovation" }, { "agency": "Academy of Finland" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "Swiss Funding Agencies" }, { "agency": "Norwegian Funding Agency" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck HFI Core Team" ] }, "doi": "10.1051/0004-6361/201116487", "primary_object": { "basename": "1101.2039.pdf", "url": "https://authors.library.caltech.edu/records/726ev-70142/files/1101.2039.pdf" }, "related_objects": [ { "basename": "aa16487-11.pdf", "url": "https://authors.library.caltech.edu/records/726ev-70142/files/aa16487-11.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/3hfvn-c7r56", "eprint_id": 25347, "eprint_status": "archive", "datestamp": "2023-08-22 03:27:59", "lastmod": "2023-10-24 15:48:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "J. J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Turner-J-L", "name": { "family": "Turner", "given": "J. L." }, "orcid": "0000-0003-4625-2951" }, { "id": "Aniano-G", "name": { "family": "Aniano", "given": "G." }, "orcid": "0000-0001-9015-2654" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "A. D." }, "orcid": "0000-0002-5480-5686" }, { "id": "Brandl-B-R", "name": { "family": "Brandl", "given": "B. R." } }, { "id": "Croxall-K-V", "name": { "family": "Croxall", "given": "K. V." }, "orcid": "0000-0002-5258-7224" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Donovan-Meyer-J-L", "name": { "family": "Donovan Meyer", "given": "J. L." }, "orcid": "0000-0002-3106-7676" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C." } }, { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Hao-C-N", "name": { "family": "Hao", "given": "C.-N." } }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Skibba-R", "name": { "family": "Skibba", "given": "R." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J.-D. T." }, "orcid": "0000-0003-1545-5078" } ] }, "title": "Calibrating Extinction-Free Star Formation Rate Diagnostics with 33 GHz Free-Free Emission in NGC 6946", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic rays; galaxies: individual (NGC 6946); H_(II) regions; infrared: general; radio continuum: general; stars: formation", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 February 9; accepted 2011 May 24; published 2011 August 4. We thank the referee, T. Takeuchi, for useful suggestions that helped to improve the content and presentation of this paper. E.J.M. thanks the Observatories of the Carnegie Institution of Washington, where the final version of this paper was written. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We are grateful to the SINGS team for producing high-quality data sets used in this study. This work is based in part on observations made with the SST, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - Murphy2011p15740Astrophys_J.pdf
", "abstract": "Using free-free emission measured in the Ka band (26-40 GHz) for 10 star-forming regions in the nearby galaxy NGC 6946, including its starbursting nucleus, we compare a number of star formation rate (SFR) diagnostics that are typically considered to be unaffected by interstellar extinction. These diagnostics include non-thermal radio (i.e., 1.4 GHz), total infrared (IR; 8-1000 \u03bcm), and warm dust (i.e., 24 \u03bcm) emission, along with hybrid indicators that attempt to account for obscured and unobscured emission from star-forming regions including H\u03b1 + 24 \u03bcm and UV + IR measurements. The assumption is made that the 33 GHz free-free emission provides the most accurate measure of the current SFR. Among the extranuclear star-forming regions, the 24 \u03bcm, H\u03b1 + 24 \u03bcm, and UV + IR SFR calibrations are in good agreement with the 33 GHz free-free SFRs. However, each of the SFR calibrations relying on some form of dust emission overestimates the nuclear SFR by a factor of ~2 relative to the 33 GHz free-free SFR. This is more likely the result of excess dust heating through an accumulation of non-ionizing stars associated with an extended episode of star formation in the nucleus rather than increased competition for ionizing photons by dust. SFR calibrations using the non-thermal radio continuum yield values which only agree with the 33 GHz free-free SFRs for the nucleus and underestimate the SFRs from the extranuclear star-forming regions by an average factor of ~2 and ~4-5 before and after subtracting local background emission, respectively. This result likely arises from the cosmic-ray (CR) electrons decaying within the starburst region with negligible escape, whereas the transient nature of star formation in the young extranuclear star-forming complexes allows for CR electrons to diffuse significantly further than dust-heating photons, resulting in an underestimate of the true SFR. Finally, we find that the SFRs estimated using the total 33 GHz flux density appear to agree well with those estimated using free-free emission due to the large thermal fractions present at these frequencies even when local diffuse backgrounds are not removed. Thus, rest-frame 33 GHz observations may act as a reliable method to measure the SFRs of galaxies at increasingly high redshift without the need of ancillary radio data to account for the non-thermal emission.", "date": "2011-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "737", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 67", "id_number": "CaltechAUTHORS:20110914-114524691", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110914-114524691", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/737/2/67", "primary_object": { "basename": "Murphy2011p15740Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/3hfvn-c7r56/files/Murphy2011p15740Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Murphy, E. J.; Condon, J. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ye3tv-xa290", "eprint_id": 24995, "eprint_status": "archive", "datestamp": "2023-08-22 03:25:50", "lastmod": "2023-10-24 15:31:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Elmegreen-D-M", "name": { "family": "Elmegreen", "given": "Debra Meloy" }, "orcid": "0000-0002-1392-3520" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Doyle-Trisha", "name": { "family": "Mizusawa", "given": "Trisha" }, "orcid": "0000-0001-7182-5307" } ] }, "title": "Grand Design and Flocculent Spirals in the Spitzer Survey of Stellar Structure in Galaxies (S^(4)G)", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: photometry; galaxies: spiral; galaxies: structure; infrared: galaxies", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2011 March 22; accepted 2011 May 26; published 2011 July 26.\n\nWe are grateful to the dedicated staff at the Spitzer Science Center for their help and support in planning and execution of this Exploration Science program. We also gratefully acknowledge support from NASA JPL/Spitzer grant RSA1374189 provided for the S4G project. D.M.E. gratefully acknowledges Vassar College for student support for Andrew Yau, and thanks NASA/JPL/Caltech for grant 1368024. E.A. and A.B. thank the Centre National d'Etudes Spatiales for financial support. This research is based in part on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract\nwith NASA, and has made use of the NASA/IPAC Extragalactic\nDatabase (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. D.M.E. thanks Fred Chromey for writing the script to transform images into polar coordinates. We thank the referee for helpful comments on statistics.\n\nPublished - Elmegreen2011p15549Astrophys_J.pdf
", "abstract": "Spiral arm properties of 46 galaxies in the Spitzer Survey of Stellar Structure in Galaxies (S^(4)G) were measured at 3.6 \u03bcm, where extinction is small and the old stars dominate. The sample includes flocculent, multiple arm, and grand design types with a wide range of Hubble and bar types. We find that most optically flocculent galaxies are also flocculent in the mid-IR because of star formation uncorrelated with stellar density waves, whereas multiple arm and grand design galaxies have underlying stellar waves. Arm-interarm contrasts increase from flocculent to multiple arm to grand design galaxies and with later Hubble types. Structure can be traced further out in the disk than in previous surveys. Some spirals peak at mid-radius while others continuously rise or fall, depending on Hubble and bar type. We find evidence for regular and symmetric modulations of the arm strength in NGC 4321. Bars tend to be long, high amplitude, and flat-profiled in early-type spirals, with arm contrasts that decrease with radius beyond the end of the bar, and they tend to be short, low amplitude, and exponential-profiled in late Hubble types, with arm contrasts that are constant or increase with radius. Longer bars tend to have larger amplitudes and stronger arms.", "date": "2011-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "737", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 32", "id_number": "CaltechAUTHORS:20110823-102753742", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110823-102753742", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA JPL/Spitzer", "grant_number": "RSA1374189" }, { "agency": "Vassar College" }, { "agency": "NASA/JPL/Caltech", "grant_number": "1368024" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/737/1/32", "primary_object": { "basename": "Elmegreen2011p15549Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/ye3tv-xa290/files/Elmegreen2011p15549Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Elmegreen, Debra Meloy; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/aeeqb-d6h65", "eprint_id": 23977, "eprint_status": "archive", "datestamp": "2023-08-22 02:55:03", "lastmod": "2023-10-23 20:12:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wu-Yanling", "name": { "family": "Wu", "given": "Yanling" } }, { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Papovich-C", "name": { "family": "Papovich", "given": "Casey" }, "orcid": "0000-0001-7503-8482" }, { "id": "Rahman-N", "name": { "family": "Rahman", "given": "Nurur" } }, { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi M." } }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" } ] }, "title": "The Mid-infrared Luminosity Function at z < 0.3 from 5MUSES: Understanding the Star Formation/Active Galactic Nucleus Balance from a Spectroscopic View", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: luminosity function, mass function; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 December 7; accepted 2011 April 1; published 2011 May 24. We thank J.-S. Huang, V. Charmandaris, H. Fu, and E.\nLe Floc'h for insightful discussion. This work was based on\nobservations made with the Spitzer Space Telescope, which is\noperated by JPL/Caltech under a contract with NASA. The\nobservations are associated with the Spitzer Legacy Program\n40539. The authors acknowledge support by NASA through\nawards issued by JPL/Caltech. This research has made use\nof the NASA/IPAC Extragalactic Database (NED) which is\noperated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - Wu2011p14087Astrophys_J.pdf
", "abstract": "We present rest-frame 15 and 24 \u03bcm luminosity functions (LFs) and the corresponding star-forming LFs at z < 0.3 derived from the 5MUSES sample. Spectroscopic redshifts have been obtained for ~98% of the objects and the median redshift is ~0.12. The 5-35 \u03bcm Infrared Spectrograph spectra allow us to estimate accurately the luminosities and build the LFs. Using a combination of starburst and quasar templates, we quantify the star formation (SF) and active galactic nucleus (AGN) contributions in the mid-IR spectral energy distribution. We then compute the SF LFs at 15 and 24 \u03bcm, and compare with the total 15 and 24 \u03bcm LFs. When we remove the contribution of AGNs, the bright end of the LF exhibits a strong decline, consistent with the exponential cutoff of a Schechter function. Integrating the differential LF, we find that the fractional contribution by SF to the energy density is 58% at 15 \u03bcm and 78% at 24 \u03bcm, while it goes up to ~86% when we extrapolate our mid-IR results to the total IR luminosity density. We confirm that the AGNs play more important roles energetically at high luminosities. Finally, we compare our results with work at z ~ 0.7 and confirm that evolution on both luminosity and density is required to explain the difference in the LFs at different redshifts.", "date": "2011-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "734", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 40", "id_number": "CaltechAUTHORS:20110610-142036267", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110610-142036267", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/734/1/40", "primary_object": { "basename": "Wu2011p14087Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/aeeqb-d6h65/files/Wu2011p14087Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Wu, Yanling; Shi, Yong; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4nr1y-1rk90", "eprint_id": 23924, "eprint_status": "archive", "datestamp": "2023-08-22 02:53:43", "lastmod": "2023-10-23 20:09:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Wu-Yanling", "name": { "family": "Wu", "given": "Yanling" } }, { "id": "Papovich-C", "name": { "family": "Papovich", "given": "Casey" }, "orcid": "0000-0001-7503-8482" }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" } ] }, "title": "Extended Schmidt Law: Role of Existing Stars in Current Star Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst; ISM: atoms; ISM: molecules; stars: formation", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 December 8; accepted 2011 March 22; published 2011 May 9. We thank the anonymous referee for the detailed and constructive\ncomments.We also thank Daniel Dale, Leslie K. Hunt,\nEva Schinnerer, and Bruce G. Elmegreen for careful reading and\ncomments. The work is supported through the Spitzer 5MUSES\nLegacy Program 40539. The authors acknowledge support by\nNASA through awards issued by JPL/Caltech. This work was\nbased on observations made with the Spitzer Space Telescope,\nwhich is operated by JPL/Caltech under a contract with NASA.\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\nwith the National Aeronautics and Space Administration. Funding\nfor 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\nNational Aeronautics and Space Administration, the Japanese\nMonbukagakusho, the Max Planck Society, and the Higher Education\nFunding Council for England. The SDSS Web site is\nhttp://www.sdss.org/.\n\nPublished - Shi2011p14041Astrophys_J.pdf
", "abstract": "We propose an \"extended Schmidt law\" with explicit dependence of the star formation efficiency (SFE = SFR/M _(gas)) on the stellar mass surface density (\u03a3_(star)). This relation has a power-law index of 0.48 \u00b1 0.04 and a 1\u03c3 observed scatter on the SFE of 0.4 dex, which holds over five orders of magnitude in the stellar density for individual global galaxies, including various types and especially the low-surface-brightness (LSB) galaxies that deviate significantly from the Kennicutt-Schmidt (KS) law. When applying it to regions of a sample of 12 spiral galaxies at sub-kiloparsec resolution, the extended Schmidt law not only holds for LSB regions but also shows significantly smaller scatters both within and across galaxies compared with the KS law. We argue that this new relation points to the role of existing stars in regulating the SFE, thus better encoding the star formation physics. Comparison with physical models of star formation recipes shows that the extended Schmidt law can be reproduced by some models including gas free fall in a stellar-gravitational potential and pressure-supported star formation. By implementing this new law into the analytic model of gas accretion in \u039bCDM, we show that it can reproduce the observed main sequence of star-forming galaxies (a relation between the SFR and stellar mass) from z = 0 up to z = 2.", "date": "2011-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "733", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 87", "id_number": "CaltechAUTHORS:20110607-093056335", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110607-093056335", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Spitzer 5MUSES Legacy Program", "grant_number": "40539" }, { "agency": "NASA/JPL/Caltech" }, { "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": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/733/2/87", "primary_object": { "basename": "Shi2011p14041Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/4nr1y-1rk90/files/Shi2011p14041Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Shi, Yong; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/z5h2k-s3581", "eprint_id": 23554, "eprint_status": "archive", "datestamp": "2023-08-19 06:27:28", "lastmod": "2023-10-23 19:44:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Shim-Hyunjin", "name": { "family": "Shim", "given": "H." } } ] }, "title": "Spectroscopically Selected Spitzer 24 \u03bcm Active Galactic Nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active, infrared: galaxies, techniques: spectroscopic", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2010 May 23; accepted 2011 February 17; published 2011 April 11. \n\nWe thank the anonymous referee for the detailed and insightful\ncomments that contributed greatly to the paper. This work\nis based (in part) on observations made with the Spitzer Space\nTelescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under a contract with NASA.\nSome of the data presented herein 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 the National Aeronautics and Space Administration.\nThe Observatory was made possible by the generous\nfinancial support of the W.M. Keck Foundation. Support for\nthis work was provided by NASA through JPL/Caltech contract\n1287611. M.I. acknowledges the support from the Creative\nResearch Initiative program, No. 2010-0000712 of the Korea\nScience and Engineering Foundation (KOSEF) funded by the\nKorea government (MEST). The analysis pipeline used to reduce\nthe DEIMOS data was developed by the DEEP2 group at UC Berkeley with support from NSF grant AST-0071048.\nFinally, we wish to recognize and acknowledge the significant\ncultural role and reverence that the summit of Mauna Kea has\nwithin the indigenous Hawaiian community. We are grateful for\nthe opportunity to conduct observations from this mountain.\n\nPublished - Choi2011p13685Astrophys_J.pdf
", "abstract": "We investigate the active galactic nucleus (AGN) sub-population of a 24 \u03bcm flux-limited galaxy sample in the Spitzer Extragalactic First Look Survey. Using deep Keck optical spectroscopy and a series of emission-line diagnostics, we identify AGN-dominated systems over broad redshift 0 < z < 3.5 and luminosity 9 < log (L_(TIR)) < 14 ranges, with sample means of = 0.85 and log <(L_(TIR))> = 11.5. We find that down to the flux limits of our Spitzer MIPS sample (f_(24) > 200 \u03bcJy), 15%-20% of sources exhibit strong AGN signatures in their optical spectra. At this flux limit, the AGN population accounts for as much as 25%-30% of the integrated 24 \u03bcm flux. This corresponds to an MIR AGN contribution \u22482-3 \u00d7 greater than that found in ISOCAM 15 \u03bcm studies that used X-ray AGN identifications. Based on our spectroscopically selected AGN sample, we also investigate the merits of Infrared Array Camera (IRAC) color selection for AGN identification. Our comparison reveals that although there is considerable overlap, a significant fraction of spectroscopic AGNs are not identifiable based on their MIR colors alone. Both the measured completeness and reliability of the IRAC color selections are found to be strongly dependent on the MIR flux limit. Finally, our spectroscopic AGN sample implies as much as a 3 \u00d7 higher AGN surface density at high redshift (z > 1.2) than that of recent optical surveys at comparable optical flux limits, suggestive of a population of heavily obscured, optical/UV reddened AGNs.", "date": "2011-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "732", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 21", "id_number": "CaltechAUTHORS:20110504-132254073", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110504-132254073", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "1287611" }, { "agency": "Ministry of Education, Science and Technology (Korea)", "grant_number": "2010-0000712" }, { "agency": "NSF", "grant_number": "AST-0071048" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/732/1/21", "primary_object": { "basename": "Choi2011p13685Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/z5h2k-s3581/files/Choi2011p13685Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Choi, P. I.; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9qjvj-1kf76", "eprint_id": 23770, "eprint_status": "archive", "datestamp": "2023-08-22 02:33:41", "lastmod": "2023-10-23 19:55:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mao-Minnie-Y", "name": { "family": "Mao", "given": "Minnie Y." } }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "Minh T." } }, { "id": "Norris-R-P", "name": { "family": "Norris", "given": "Ray P." }, "orcid": "0000-0002-4597-1906" }, { "id": "Dickinson-Mark-E", "name": { "family": "Dickinson", "given": "Mark" }, "orcid": "0000-0001-5414-5131" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "Dave T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Monkiewicz-Jacqueline-A", "name": { "family": "Monkiewicz", "given": "Jacqueline A." } } ] }, "title": "No Evidence for Evolution in the Far-infrared\u2013Radio Correlation out to z ~ 2 in the Extended Chandra Deep Field South", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: evolution; Galaxy: formation; infrared: galaxies; radio continuum: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 November 2; accepted 2011 February 15; published 2011 March 25. We thank our anonymous referee whose insightful comments\nhelped improve this paper. We thank Neal Miller for providing the radio data. M.Y.M. was supported by the IPAC Visiting Graduate Research Fellowship Program for this work. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - Mao2011p13843Astrophys_J.pdf
", "abstract": "We investigate the 70 \u03bcm far-infrared-radio correlation (FRC) of star-forming galaxies in the Extended Chandra Deep Field South (ECDFS) out to z > 2. We use 70 \u03bcm data from the Far-Infrared Deep Extragalactic Legacy Survey (FIDEL), which comprises the most sensitive (~0.8 mJy rms) and extensive far-infrared deep field observations using MIPS on the Spitzer Space Telescope, and 1.4 GHz radio data (~8 \u03bcJy beam^(\u20131) rms) from the Very Large Array. In order to quantify the evolution of the FRC, we use both survival analysis and stacking techniques, which we find give similar results. We also calculate the FRC using total infrared luminosity and rest-frame radio luminosity, q TIR, and find that q TIR is constant (within 0.22) over the redshift range 0-2. We see no evidence for evolution in the FRC at 70 \u03bcm, which is surprising given the many factors that are expected to change this ratio at high redshifts.", "date": "2011-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "731", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 79", "id_number": "CaltechAUTHORS:20110524-080345301", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110524-080345301", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "IPAC Visiting Graduate Student Fellowship Program" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/731/2/79", "primary_object": { "basename": "Mao2011p13843Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/9qjvj-1kf76/files/Mao2011p13843Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Mao, Minnie Y.; Huynh, Minh T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/73kpf-5bx62", "eprint_id": 23343, "eprint_status": "archive", "datestamp": "2023-08-22 02:27:50", "lastmod": "2023-10-23 19:01:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "Michel" } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi" } }, { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Heckman-T-M", "name": { "family": "Heckman", "given": "Tim" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "HST/NICMOS Imaging of Bright High-redshift 24 \u03bcm Selected Galaxies: Merging Properties", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; infrared: galaxies", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 July 12; accepted 2010 December 30; published 2011 March 14.\n\nWe are grateful to M. Elitzer and L. Armus for insightful\ndiscussions about various aspects of mid-IR spectroscopy as\nwell as to J. Lotz on aspects of automated classification. We are very much obliged toward J. Kartaltepe for kindly sharing her results ahead of publication and for providing us with helpful information. We thank P. Hopkins for providing us data from his simulations. We are grateful to V. Fadeyev and C. Peng for their help with their improved NICMOS pipeline and GALFIT softwares, respectively. We would like to extend our thanks to the referee for his/her comments that helped improve this paper. M.Z. acknowledges support from the HST GO grant 11142. \n\nFacilities: HST (NICMOS), Spitzer (IRS, MIPS)\n\nPublished - Zamojski2011p13404Astrophys_J.pdf
", "abstract": "We present new results on the physical nature of infrared-luminous sources at 0.5 < z < 2.8 as revealed by HST/NICMOS imaging and Infrared Spectrograph mid-infrared spectroscopy. Our sample consists of 134 galaxies selected at 24 \u03bcm with a flux of S(24 \u03bcm)>0.9 mJy. We find many (~60%) of our sources to possess an important bulge and/or central point source component, most of which reveal additional underlying structures after subtraction of a best-fit S\u00e9rsic (or S\u00e9rsic+PSF) profile. Based on visual inspection of the NIC2 images and their residuals, we estimate that ~80% of all our sources are mergers. We calculate lower and upper limits on the merger fraction to be 62% and 91%, respectively. At z < 1.5, we observe objects in early (pre-coalescence) merging stages to be mostly disk and star formation dominated, while we find mergers to be mainly bulge dominated and active galactic nucleus (AGN)-starburst composites during coalescence and then AGN dominated in late stages. This is analogous to what is observed in local ULIRGs. At z \u2265 1.5, we find a dramatic rise in the number of objects in pre-coalescence phases of merging, despite an increase in the preponderance of AGN signatures in their mid-IR spectra and luminosities above 10^(12.5) L_\u2609. We further find the majority of mergers at those redshifts to retain a disk-dominated profile during coalescence. We conclude that, albeit still driven by mergers, these high-z ULIRGs are substantially different in nature from their local counterparts and speculate that this is likely due to their higher gas content. Finally, we observe obscured (\u03c4_(9.7) \u03bcm>3.36) quasars to live in faint and compact hosts and show that these are likely high-redshift analogs of local dense-core mergers. We find late-stage mergers to possess predominantly unobscured AGN spectra, but do not observe other morphological classes to carry any specific combination of \u03c4_(9.7) \u03bcm and polycyclic aromatic hydrocarbon (PAH) equivalent width. This suggests a high degree of variation in the PAH emission and silicate absorption properties of these mergers, and possibly throughout the merging process itself.", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 125", "id_number": "CaltechAUTHORS:20110415-095543716", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110415-095543716", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO 11142" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/730/2/125", "primary_object": { "basename": "Zamojski2011p13404Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/73kpf-5bx62/files/Zamojski2011p13404Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Zamojski, Michel; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://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" }, "resource_type": "article", "pub_year": "2011", "author_list": "Kasliwal, Mansi M.; Kulkarni, Shri R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6syph-rq478", "eprint_id": 21894, "eprint_status": "archive", "datestamp": "2023-08-19 04:32:52", "lastmod": "2023-10-23 15:28:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Doyle-T-F", "name": { "family": "Mizusawa", "given": "Trisha" }, "orcid": "0000-0001-7182-5307" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "Thomas H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "Patrick" }, "orcid": "0000-0002-3471-981X" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi" }, "orcid": "0000-0002-5619-4938" } ] }, "title": "The Spitzer Survey of Stellar Structure in Galaxies (S^4G)", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The Astronomical Society of the Pacific. Received 2010 April 22; accepted 2010 October 6; published 2010 December 2. The authors thank the referee for useful comments and suggestions\nthat greatly helped improve this article. We are also\ngrateful to the dedicated staff at the Spitzer Science Center\nfor their support and help with the planning and execution of this legacy exploration program. K. S. would like to thank\nL. Armus, E. Bell, S. Carey, E. Churchwell, M. Dickinson,\nG. Helou, N. Scoville, and J. Stauffer for sharing their experiences\nin leading large teams. A. G. d. P. and J. C. M. M. are\npartially financed by the Spanish Programa Nacional de Astronom\u00eda\ny Astrof\u00edsica under grants AyA2006-02358 and\nAyA2009-10368. A. G. d. P. is also financed by the Spanish\nRam\u00f3n y Cajal program. J. C. M. M. acknowledges the receipt\nof a Formaci\u00f3n del Profesorado Universitario fellowship. E. L.\nand H. S. acknowledge support from the Academy of Finland.\nK. M. D. is supported by a National Science Foundation (NSF)\nAstronomy and Astrophysics Postdoctoral Fellowship under\naward AST-0802399. D. M. E. acknowledges support from\nthe Spitzer Science Center from NASA grant JPL RSA-1368024. R. B. acknowledges support from NSF grant AST\n05-07140. E. A. and A. B. thank the Centre National d'Etudes\nSpatiales and ANR-06-BLAN-0172 for support. K. L. M. acknowledges\nfunding from the Peter and Patricia Gruber Foundation\nas the 2008 IAU Fellow, from the University of\nPortsmouth, and from the South East Physics Network. This\nwork is based on observations and archival data obtained with\nthe Spitzer Space Telescope, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology under a\ncontract with NASA. Support for this work was provided by\nNASA. We gratefully acknowledge support from NASA JPL/Spitzer grant RSA 1374189 provided for the S^4G project.\n\nPublished - Sheth2010p12393Publ_Astron_Soc_Pac.pdf
", "abstract": "The Spitzer Survey of Stellar Structure in Galaxies (S^4G) is an Exploration Science Legacy Program\napproved for the Spitzer post\u2013cryogenic mission. It is a volume-, magnitude-, and size-limited (d < 40 Mpc,\n|b|> 30\u00b0,m_(Bcorr) < 15:5, and D_(25) > 1') survey of 2331 galaxies using the Infrared Array Camera (IRAC) at 3.6 and\n4.5 \u03bcm. Each galaxy is observed for 240 s and mapped to \u2265 1:5 \u00d7 D_(25). The final mosaicked images have a typical\n1 \u03c3 rms noise level of 0.0072 and 0:0093 MJy sr^-1 at 3.6 and 4.5 \u03bcm, respectively. Our azimuthally averaged surface\nbrightness profile typically traces isophotes at \u03bc_(3.6\u03bcm (AB)(1\u03c3) ~ 27 mag arcsec^(-2), equivalent to a stellar mass surface\ndensity of ~1 M_\u2299pc^(-2). S^4G thus provides an unprecedented data set for the study of the distribution of mass\nand stellar structures in the local universe. This large, unbiased, and extremely deep sample of all Hubble types from\ndwarfs to spirals to ellipticals will allow for detailed structural studies, not only as a function of stellar mass, but also\nas a function of the local environment. The data from this survey will serve as a vital testbed for cosmological\nsimulations predicting the stellar mass properties of present-day galaxies. This article introduces the survey and\ndescribes the sample selection, the significance of the 3.6 and 4.5 \u03bcm bands for this study, and the data collection\nand survey strategies. We describe the S^4G data analysis pipeline and present measurements for a first set of galaxies,\nobserved in both the cryogenic and warm mission phases of Spitzer. For every galaxy we tabulate the galaxy\ndiameter, position angle, axial ratio, inclination at \u03bc_(3.6\u03bcm)(AB) = 25:5, and 26:5 mag arcsec^(-2) (equivalent to\n\u2248\u03bc_B(AB) = 27:2 and 28:2 mag arcsec^(-2), respectively). These measurements will form the initial S^4G catalog\nof galaxy properties. We also measure the total magnitude and the azimuthally averaged radial profiles of ellipticity,\nposition angle, surface brightness, and color. Finally, using the galaxy-fitting code GALFIT, we deconstruct each\ngalaxy into its main constituent stellar components: the bulge/spheroid, disk, bar, and nuclear point source, where\nnecessary. Together, these data products will provide a comprehensive and definitive catalog of stellar structures,\nmass, and properties of galaxies in the nearby universe and will enable a variety of scientific investigations, some of\nwhich are highlighted in this introductory S^4G survey paper.", "date": "2010-12", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "122", "number": "898", "publisher": "Astronomical Society of the Pacific", "pagerange": "1397-1414", "id_number": "CaltechAUTHORS:20110126-084714506", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110126-084714506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nacional de Astronomia y Astrofisica", "grant_number": "AyA2006-02358" }, { "agency": "Nacional de Astronomia y Astrofisica", "grant_number": "AyA2009-10368" }, { "agency": "Ramon y Cajal programme" }, { "agency": "Formacion del Profesorado Universitario" }, { "agency": "Academy of Finland" }, { "agency": "NSF", "grant_number": "AST-0802399" }, { "agency": "NSF", "grant_number": "AST 05-07140" }, { "agency": "NASA", "grant_number": "RSA-1368024" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "University of Portsmouth" }, { "agency": "South East Physics Network" }, { "agency": "NASA", "grant_number": "RSA 1374189" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-06-BLAN-0172" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/657638", "primary_object": { "basename": "Sheth2010p12393Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/6syph-rq478/files/Sheth2010p12393Publ_Astron_Soc_Pac.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Sheth, Kartik; Mizusawa, Trisha; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/22bnk-hsx95", "eprint_id": 21226, "eprint_status": "archive", "datestamp": "2023-08-19 04:19:07", "lastmod": "2023-10-20 23:51:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wu-Yanling", "name": { "family": "Wu", "given": "Yanling" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Cormier-D", "name": { "family": "Cormier", "given": "Diane" } }, { "id": "Shi-Yong", "name": { "family": "Shi", "given": "Yong" }, "orcid": "0000-0002-8614-6275" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel" }, "orcid": "0000-0002-5782-9093" }, { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi" } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" }, { "id": "Papovich-C", "name": { "family": "Papovich", "given": "Casey" }, "orcid": "0000-0001-7503-8482" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce" }, "orcid": "0000-0002-0846-936X" }, { "id": "Rahman-N", "name": { "family": "Rahman", "given": "Nurur" } }, { "id": "Stierwalt-S", "name": { "family": "Stierwalt", "given": "Sabrina" }, "orcid": "0000-0002-2596-8531" }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Lagache-G", "name": { "family": "Lagache", "given": "G." } } ] }, "title": "Infrared luminosities and aromatic features in the 24 \u03bcm flux-limited sample of 5muses", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active, galaxies: starburst, infrared: galaxies, surveys", "note": "\u00a9 2010 The American Astronomical Society. Received 2010 May 25; accepted 2010 September 2; published 2010 October 15. We thank the anonymous referee whose comments have\nhelped to improve this paper. This work was based on observations\nmade with the Spitzer Space Telescope, which is operated\nby JPL/Caltech under a contract with NASA. The observations\nare associated with the Spitzer Legacy Program 40539. The authors\nacknowledge support by NASA through awards issued\nby JPL/Caltech. 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 - Wu2010p12058Astrophys_J.pdf
", "abstract": "We study a 24 \u03bcm selected sample of 330 galaxies observed with the infrared spectrograph for the 5 mJy Unbiased\nSpitzer Extragalactic Survey. We estimate accurate total infrared luminosities by combining mid-IR spectroscopy\nand mid-to-far infrared photometry, and by utilizing newempirical spectral templates from Spitzer data. The infrared luminosities of this sample range mostly from 10^9 L_\u2299 to 10^(13.5) L_\u2299,with 83% in the range 10^(10) L_\u2299 < L_(IR) < 10^(12) L_\u2299. The redshifts range from 0.008 to 4.27, with a median of 0.144. The equivalent widths of the 6.2 \u03bcm aromatic feature have a bimodal distribution, probably related to selection effects. We use the 6.2\u03bcm polycyclic aromatic hydrocarbon equivalent width (PAH EW) to classify our objects as starburst (SB)-dominated (44%), SB-AGN composite (22%), and active galactic nucleus (AGN)-dominated (34%). The high EW objects (SB-dominated) tend to have steeper mid-IR to far-IR spectral slopes and lower L_(IR) and redshifts. The low EW objects (AGN-dominated) tend to have less steep spectral slopes and higher L_(IR) and redshifts. This dichotomy leads to a gross correlation between EW and slope, which does not hold within either group. AGN-dominated sources tend to have lower log(L_(PAH7.7 \u03bcm)/L_(PAH11.3 \u03bcm)) ratios than star-forming galaxies, possibly due to preferential destruction of the smaller aromatics by the AGN. The log(L_(PAH7.7 \u03bcm)/L_(PAH11.3 \u03bcm)) ratios for star-forming galaxies are lower in our sample than the ratios measured from the nuclear spectra of nearby normal galaxies, most probably indicating a difference in the ionization state or grain size distribution between the nuclear regions and the entire galaxy. Finally, we provide a calibration relating the monochromatic continuum or aromatic feature luminosity to L_(IR) for different types of objects.", "date": "2010-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "723", "number": "1", "publisher": "American Astronomical Society", "pagerange": "895-914", "id_number": "CaltechAUTHORS:20101208-080506134", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101208-080506134", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/723/1/895", "primary_object": { "basename": "Wu2010p12058Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/22bnk-hsx95/files/Wu2010p12058Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Wu, Yanling; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/erk5d-z0r24", "eprint_id": 20196, "eprint_status": "archive", "datestamp": "2023-08-19 03:44:34", "lastmod": "2023-10-20 22:19:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bhattacharya-B", "name": { "family": "Bhattacharya", "given": "B." } }, { "id": "Noriega-Crespo-A", "name": { "family": "Noriega-Crespo", "given": "A." }, "orcid": "0000-0002-6296-8960" }, { "id": "Penprase-B-E", "name": { "family": "Penprase", "given": "B. E." } }, { "id": "Meadows-V-S", "name": { "family": "Meadows", "given": "V. S." } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Looper-D", "name": { "family": "Looper", "given": "D." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Giorgini-J-D", "name": { "family": "Giorgini", "given": "J. D." } }, { "id": "Granvik-M", "name": { "family": "Granvik", "given": "M." }, "orcid": "0000-0002-5624-1888" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Hagen-A", "name": { "family": "Hagen", "given": "A." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Reach-W-T", "name": { "family": "Reach", "given": "W. T." }, "orcid": "0000-0001-8362-4094" }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "L. M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Mid-infrared Photometric Analysis of Main Belt Asteroids: A Technique for Color-Color Differentiation from Background Astrophysical Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: general \u2013 techniques: photometric", "note": "\u00a9 2010. The American Astronomical Society. All rights reserved. Received 2009 May 12; accepted 2010 June 16; published 2010 August 6. The authors acknowledge the late S. Tyler, whose enthusiastic\npresence is missed by the FLS-EPC team. During his years\nat the Spitzer Science Center, Mr. Tyler assisted in data analysis\nfor this project. The authors also thank the anonymous referee for helpful comments. B.B. thanks Dr. Tom Jarrett for providing\nvaluable feedback, and the FLS-EPC team acknowledges\nProfessor Jim Elliot for developing the original concept of the\nsolar system First Look Survey. This work is based upon observations\nmade with the Spitzer Space Telescope, operated by JPL,\nCaltech, and funded under NASA contract 1407. Additional\nwork is funded by the NASA Herschel Science Center, operated\nby JPL, Caltech.\n\nPublished - Bhattacharya2010p11429Astrophys_J.pdf
", "abstract": "The Spitzer Space Telescope routinely detects asteroids in astrophysical observations near the ecliptic plane. For the galactic or extragalactic astronomer, these solar system bodies can introduce appreciable uncertainty into the source identification process. We discuss an infrared color discrimination tool that may be used to distinguish between solar system objects and extrasolar sources. We employ four Spitzer Legacy data sets, the First Look Survey-Ecliptic Plane Component (FLS-EPC), SCOSMOS, SWIRE, and GOODS. We use the Standard Thermal Model to derive FLS-EPC main belt asteroid (MBA) diameters of 1-4 km for the numbered asteroids in our sample and note that several of our solar system sources may have fainter absolute magnitude values than previously thought. A number of the MBAs are detected at flux densities as low as a few tens of \u03bcJy at 3.6 \u03bcm. As the FLS-EPC provides the only 3.6-24.0 \u03bcm observations of individual asteroids to date, we are able to use this data set to carry out a detailed study of asteroid color in comparison to astrophysical sources observed by SCOSMOS, SWIRE, and GOODS. Both SCOSMOS and SWIRE have identified a significant number of asteroids in their data, and we investigate the effectiveness of using relative color to distinguish between asteroids and background objects. We find a notable difference in color in the IRAC 3.6-8.0 mm and MIPS 24 \u03bcm bands between the majority of MBAs, stars, galaxies, and active galactic nuclei, though this variation is less significant when comparing fluxes in individual bands. We find median colors for the FLS-EPC asteroids to be [F(5.8/3.6), F(8.0/4.5), F(24/8)] = (4.9 \u00b1 1.8, 8.9 \u00b1 7.4, 6.4 \u00b1 2.3). Finally, we consider the utility of this technique for other mid-infrared observations that are sensitive to near-Earth objects, MBAs, and trans-Neptunian objects. We consider the potential of using color to differentiate between solar system and background sources for several space-based observatories, including Warm Spitzer, Herschel, and WISE.", "date": "2010-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "720", "number": "1", "publisher": "American Astronomical Society", "pagerange": "114-129", "id_number": "CaltechAUTHORS:20100928-115506218", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100928-115506218", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA Herschel Science Center" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/720/1/114", "primary_object": { "basename": "Bhattacharya2010p11429Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/erk5d-z0r24/files/Bhattacharya2010p11429Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Bhattacharya, B.; Noriega-Crespo, A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0mc7m-w6046", "eprint_id": 71635, "eprint_status": "archive", "datestamp": "2023-08-19 03:31:11", "lastmod": "2024-01-13 20:17:39", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Holmes-W-A", "name": { "family": "Holmes", "given": "Warren" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" } ] }, "title": "The background-limited infrared-submillimeter spectrograph (BLISS) for SPICA: a design study", "ispublished": "unpub", "full_text_status": "public", "keywords": "Bolometer, TES, Far-IR Spectroscopy, Grating", "note": "\u00a9 2010 SPIE.\n\nWe thank Jeremy Hodis and Jonathan Kawamura at JPL for help with the WaFIRS spectrometer measurements.\n\nPublished - 77310S_1.pdf
", "abstract": "We are developing the Background-Limited Infrared-Submillimeter Spectrograph (BLISS) for SPICA to provide a breakthrough capability for far-IR survey spectroscopy. SPICAs large cold aperture allows mid-IR to submm observations which are limited only by the natural backgrounds, and BLISS is designed to operate near this fundamental limit. BLISS-SPICA is 6 orders of magnitude faster than the spectrometers on Herschel and SOFIA in obtaining full-band spectra. It enables spectroscopy of dust-obscured galaxies at all epochs back to the rst billion years after the Big Bang (redshift 6), and study of all stages of planet formation in circumstellar disks. BLISS covers 35 - 433 microns range in ve or six wavelength bands, and couples two 2 sky positions simultaneously. The instrument is cooled to 50 mK for optimal sensitivity with an on-board refrigerators. The detector package is 4224 silicon-nitride micro-mesh leg-isolated bolometers with superconducting transition-edge-sensed (TES) thermistors, read out with a cryogenic time-domain multiplexer. All technical elements of BLISS have heritage in mature scientic instruments, and many have own. We report on our design study in which we are optimizing performance while accommodating SPICAs constraints, including the stringent cryogenic mass budget. In particular, we present our progress in the optical design and waveguide spectrometer prototyping. A companion paper in Conference 7741 (Beyer et al.) discusses in greater detail the progress in the BLISS TES bolometer development.", "date": "2010-08-10", "date_type": "published", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_pub": "Bellingham, WA", "pagerange": "Art. No. 77310S", "id_number": "CaltechAUTHORS:20161031-160552623", "isbn": "978-0-81948-221-1", "book_title": "Space Telescopes and Instrumentation 2010: Optical, Infrared, and Millimeter Wave", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161031-160552623", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Oschmann-J-M-Jr", "name": { "family": "Oschmann", "given": "Jacobus M., Jr." } }, { "id": "Clampin-M-C", "name": { "family": "Clampin", "given": "Mark C." } }, { "id": "MacEwen-H-A", "name": { "family": "MacEwen", "given": "Howard A." } } ] }, "corp_creators": { "items": [ "BLISS Study Team" ] }, "doi": "10.1117/12.857779", "primary_object": { "basename": "77310S_1.pdf", "url": "https://authors.library.caltech.edu/records/0mc7m-w6046/files/77310S_1.pdf" }, "resource_type": "book_section", "pub_year": "2010", "author_list": "Bradford, C. M.; Bock, James; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/68a6p-71d54", "eprint_id": 19602, "eprint_status": "archive", "datestamp": "2023-08-22 00:34:08", "lastmod": "2023-10-20 21:11:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Lagache-Guilaine", "name": { "family": "Lagache", "given": "Guilaine" }, "orcid": "0000-0003-1492-2519" }, { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "Dieter" }, "orcid": "0000-0003-0291-9582" }, { "id": "Wuyts-S", "name": { "family": "Wuyts", "given": "Stijn" } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Marcillac-D", "name": { "family": "Marcillac", "given": "Delphine" } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "Karina" }, "orcid": "0000-0001-8183-1460" }, { "id": "Spoon-H-W-W", "name": { "family": "Spoon", "given": "Henrik W. W." }, "orcid": "0000-0002-8712-369X" }, { "id": "Veilleux-S", "name": { "family": "Veilleux", "given": "Sylvain" }, "orcid": "0000-0002-3158-6820" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew" }, "orcid": "0000-0001-7489-5167" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Ultra-deep Mid-infrared Spectroscopy of Luminous Infrared Galaxies at z ~ 1 and z ~ 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2009 December 21; accepted 2010 June 14; published 2010 July 20.\n\nThis research made use of Tiny Tim/Spitzer, developed by\nJohn Krist for the Spitzer Science Center. The Center is managed \nby the California Institute of Technology under a contract \nwith NASA. We are grateful to Haojing Yan for providing \nus the reduced NICMOS H-band stamp images for some of \nour sources. We thank P. Capak for helpful discussions. We \nare grateful to the anonymous referee for the detailed reading \nof the paper and for many ideas and suggestions to improve \nthe quality of the paper. Support for this work was provided \nby NASA through an award issued by JPL/Caltech. S. Wuyts \nacknowledges support from the W. M. Keck Foundation.\n\nPublished - Fadda2010p11129Astrophys_J.pdf
Submitted - 1006.2873v1.pdf
", "abstract": "We present ultra-deep mid-infrared spectra of 48 infrared-luminous galaxies in the GOODS-south field obtained with the Infrared Spectrograph on the Spitzer Space Telescope. These galaxies are selected among faint infrared sources (0.14-0.5 mJy at 24 \u03bcm) in two redshift bins (0.76-1.05 and 1.75-2.4) to sample the major contributors to the cosmic infrared background at the most active epochs. We estimate redshifts for 92% of the sample using polycyclic aromatic (PAH) and Si absorption features obtaining, in particular, eight new redshifts difficult to measure from ground-based observations. Only a few of these galaxies (5% at z ~ 1 and 12% at z ~ 2) have their total infrared luminosity dominated by emission from active galactic nuclei (AGNs). The averaged mid-IR spectrum of the z ~ 1 luminous infrared galaxies (LIRGs) is a very good match to the averaged spectrum of local starbursts. The averaged spectrum of the z ~ 2 ultra-luminous infrared galaxies (ULIRGs), because of a deeper Si absorption, is better fitted by the averaged spectrum of H II-like local ULIRGs. Combining this sample with other published data, we find that 6.2 \u03bcm PAH equivalent widths (EW) reach a plateau of ~ 1 \u03bcm for L 24 \u03bcm \u227e 10^(11) L_\u2299. At higher luminosities, EW_(6.2 \u03bcm) anti-correlates with L _(24 \u03bcm). Intriguingly, high-z ULIRGs and sub-millimeter galaxies (SMGs) lie above the local EW_(6.2 \u03bcm)-L_(24 \u03bcm) relationship suggesting that, at a given luminosity, high-z ULIRGs have AGN contributions to their dust emission lower than those of local counterparts. A quantitative analysis of their morphology shows that most of the luminous IR galaxies have morphologies similar to those of IR-quiet galaxies at the same redshift. All z ~ 2 ULIRGs of our sample are IR-excess BzK galaxies and most of them have L_(FIR)/L_(1600 \u00c5) ratios higher than those of starburst galaxies at a given UV slope. The \"IR excess\" is mostly due to strong 7.7 \u03bcm PAH emission and underestimation of UV dust extinction. On the basis of the AGN-powered L_(6 \u03bcm) continuum measured directly from the mid-IR spectra, we estimate an average intrinsic X-ray AGN luminosity of L_(2\u201310 keV) = (0.1\u00b1 0.6)\u00d7 10^(43) erg s^(\u20131), a value substantially lower than the prediction by Daddi et al.", "date": "2010-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "719", "number": "1", "publisher": "American Astronomical Society", "pagerange": "425-450", "id_number": "CaltechAUTHORS:20100823-143138995", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100823-143138995", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/719/1/425", "primary_object": { "basename": "1006.2873v1.pdf", "url": "https://authors.library.caltech.edu/records/68a6p-71d54/files/1006.2873v1.pdf" }, "related_objects": [ { "basename": "Fadda2010p11129Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/68a6p-71d54/files/Fadda2010p11129Astrophys_J.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Fadda, Dario; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4kf2c-znn98", "eprint_id": 21034, "eprint_status": "archive", "datestamp": "2023-08-19 03:00:42", "lastmod": "2023-10-20 23:42:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Far-infrared line imaging of the starburst ring in NGC 1097 with the Herschel/PACS spectrometer", "ispublished": "pub", "full_text_status": "public", "keywords": "photon-dominated region, infrared: galaxies, galaxies: Seyfert, galaxies: starburst, techniques: imaging spectroscopy, galaxies: individual: NGC 1097", "note": "\u00a9 2010 ESO. Received 30 March 2010, Accepted 3 May 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based [in part] on observations made with\nHerschel, a European Space Agency Cornerstone Mission with significant participation\nby NASA. Support for this work was provided by NASA through an\naward issued by JPL/Caltech. PACS has been developed by a consortium of\ninstitutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL,\nIMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT,\nOAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been\nsupported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium),\nCEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain).\nData presented in this paper were analyzed using The Herschel Interactive\nProcessing Environment (HIPE), a joint development by the Herschel Science\nGround Segment Consortium, consisting of ESA, the NASA Herschel Science\nCenter, and the HIFI, PACS and SPIRE consortia. We would like to thank Dario\nFadda and Jeff Jacobson for software support and Hanae Inami for the help on\nthe velocity diagram.\n\nPublished - Beirao2010p11876Astron_Astrophys.pdf
", "abstract": "NGC 1097 is a nearby SBb galaxy with a Seyfert nucleus and a bright starburst ring. We study the physical properties of the interstellar medium (ISM) in the ring using spatially resolved far-infrared spectral maps of the circumnuclear starburst ring of NGC 1097, obtained with the PACS spectrometer on board the Herschel Space Observatory. In particular, we map the important ISM cooling and diagnostic emission lines of [OI] 63 \u03bcm, [OIII] 88 \u03bcm, [NII] 122 \u03bcm, [CII] 158 \u03bcm and [NII] 205 \u03bcm. We observe that in the [OI] 63 \u03bcm, [OIII] 88 \u03bcm, and [NII] 122 \u03bcm line maps, the emission is enhanced in clumps along the NE part of the ring. We observe evidence of rapid rotation in the circumnuclear ring, with a rotation velocity of ~220 km s^(\u22121) (inclination uncorrected) measured in all lines. The [OI] 63 \u03bcm/[CII] 158 \u03bcm ratio varies smoothly throughout the central region, and is enhanced on the northeastern part of the ring, which may indicate a stronger radiation field. This enhancement coincides with peaks in the [OI] 63 \u03bcm and [OIII] 88 \u03bcm maps. Variations of the [NII] 122 \u03bcm/[NII] 205 \u03bcm ratio correspond to a range in the ionized gas density between 150 and 400 cm^(\u22123).", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L60", "id_number": "CaltechAUTHORS:20101129-100014152", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101129-100014152", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific Experiments (PRODEX) (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICT)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014592", "primary_object": { "basename": "Beirao2010p11876Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/4kf2c-znn98/files/Beirao2010p11876Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Beir\u00e3o, P.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/n6t09-xsf98", "eprint_id": 20944, "eprint_status": "archive", "datestamp": "2023-08-22 00:15:17", "lastmod": "2023-10-20 23:36:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sandstrom-K-M", "name": { "family": "Sandstrom", "given": "K." }, "orcid": "0000-0002-4378-8534" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Beir\u00e3o-P", "name": { "family": "Beir\u00e3o", "given": "P." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" } ] }, "title": "Mapping far-IR emission from the central kiloparsec of NGC\u20091097", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; galaxies: star formation; galaxies: individual: NGC 1097; dust, extinction", "note": "\u00a9 2010 ESO.\n\nReceived 30 March 2010; Accepted 29 April 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nThe authors thank R. Beck for the radio continuum data\nand P.-Y. Hsieh for the CO data. K.S. would like to thank G. van de Ven and L. Burtscher for useful discussions. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany);\nINAF- IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESAPRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).\n\nPublished - Sandstrom2010p11884Astron_Astrophys.pdf
", "abstract": "Using photometry of NGC 1097 from the Herschel PACS (Photodetector Array Camera and Spectrometer) instrument, we study the resolved properties of thermal dust continuum emission from a circumnuclear starburst ring with a radius ~900 pc. These observations are the first to resolve the structure of a circumnuclear ring at wavelengths that probe the peak (i.e. \u03bb ~ 100 \u03bcm) of the dust spectral energy distribution. The ring dominates the far-infrared (far-IR) emission from the galaxy \u2013 the high angular resolution of PACS allows us to isolate the ring's contribution and we find it is responsible for 75, 60 and 55% of the total flux of NGC 1097 at 70, 100 and 160 \u03bcm, respectively. We compare the far-IR structure of the ring to what is seen at other wavelengths and identify a sequence of far-IR bright knots that correspond to those seen in radio and mid-IR images. The mid- and far-IR band ratios in the ring vary by less than \u00b120% azimuthally, indicating modest variation in the radiation field heating the dust on ~600 pc scales. We explore various explanations for the azimuthal uniformity in the far-IR colors of the ring including a lack of well-defined age gradients in the young stellar cluster population, a dominant contribution to the far-IR emission from dust heated by older (>10 Myr) stars and/or a quick smoothing of local enhancements in dust temperature due to the short orbital period of the ring. Finally, we improve previous limits on the far-IR flux from the inner ~600 pc of NGC 1097 by an order of magnitude, providing a better estimate of the total bolometric emission arising from the active galactic nucleus and its associated central starburst.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. NO. L59", "id_number": "CaltechAUTHORS:20101122-112011285", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101122-112011285", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency-PROgramme for the Development of scientific EXperiments (ESA-PRODEX) (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Ministerio de Ciencia y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014583", "primary_object": { "basename": "Sandstrom2010p11884Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/n6t09-xsf98/files/Sandstrom2010p11884Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Sandstrom, K.; Appleton, P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/76wkv-jhe18", "eprint_id": 18548, "eprint_status": "archive", "datestamp": "2023-08-21 23:55:51", "lastmod": "2023-10-20 16:30:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C. L." }, "orcid": "0000-0001-6647-3861" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Oesch-P-A", "name": { "family": "Oesch", "given": "P." }, "orcid": "0000-0001-5851-6649" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Smol\u010di\u0107-V", "name": { "family": "Smol\u010di\u0107", "given": "V." }, "orcid": "0000-0002-3893-8614" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" } ] }, "title": "No Evolution in the IR\u2013Radio Relation for IR-luminous Galaxies at z < 2 in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: evolution; infrared: galaxies; radio continuum: galaxies; surveys", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2010 January 12; accepted 2010 March 22; published 2010 April 12.\n\nPartly based on observations collected at the European Organization for\nAstronomical Research in the Southern Hemisphere, Chile, ESO program\nID 175.A-0839.\n\nM.T.S. acknowledges DFG-funding (grant SCHI 536/3-2)\nand thanks Gianni Zamorani and Rob Ivison for reading and\ncommenting on the manuscript.\nThis work is partly based on observations made with the\nSpitzer Space Telescope, which is operated by NASA/JPL/\nCaltech. The National Radio Astronomy Observatory (NRAO)\nis operated by Associated Universities, Inc., under cooperative\nagreement with the National Science Foundation.\nFacilities: VLA, Spitzer (IRAC, MIPS), VLT:Melipal,\nSubaru (SuprimeCam)\n\nPublished - Sargent2010p10083Astrophys_J_Lett.pdf
", "abstract": "Previous observational studies of the infrared (IR)-radio relation out to high redshift employed any detectable star-forming systems at a given redshift within the restricted area of cosmological survey fields. Consequently, the evolution inferred relies on a comparison between the average IR/radio properties of (1) very IR-luminous high-z sources and (2) more heterogeneous low(er)-z samples that often lack the strongest IR emitters. In this Letter, we consider populations of objects with comparable luminosities over the last 10 Gyr by taking advantage of deep IR (especially Spitzer 24 \u03bcm) and Very Large Array 1.4 GHz observations of the COSMOS field. Consistent with recent model predictions, both Ultra Luminous Infrared Galaxies and galaxies on the bright end of the evolving IR luminosity function do not display any change in their average IR/radio ratios out to z ~ 2 when corrected for bias. Uncorrected data suggested ~0.3 dex of positive evolution.", "date": "2010-05-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "714", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L190-L195", "id_number": "CaltechAUTHORS:20100603-113404879", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100603-113404879", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "SCHI 536/3-2" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/714/2/L190", "primary_object": { "basename": "Sargent2010p10083Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/76wkv-jhe18/files/Sargent2010p10083Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Sargent, M. T.; Schinnerer, E.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ryz2d-4n764", "eprint_id": 17639, "eprint_status": "archive", "datestamp": "2023-08-21 23:20:46", "lastmod": "2023-10-20 00:05:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "J. J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Turner-J-L", "name": { "family": "Turner", "given": "J. L." }, "orcid": "0000-0003-4625-2951" }, { "id": "Beck-R", "name": { "family": "Beck", "given": "R." } }, { "id": "Mason-B-S", "name": { "family": "Mason", "given": "B. S." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" } ] }, "title": "The Detection of Anomalous Dust Emission in the Nearby Galaxy NGC 6946", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (NGC 6946); radiation mechanisms: thermal; radio continuum: general", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 2 (2010 February 1); received 2009 October 27; accepted for publication 2009 December 14;\npublished 2010 January 11.\n\nWe thank the anonymous referee for useful suggestions that\nhelped to improve the content and presentation of this Letter. E.J.M. thanks William Reach and Roberta Paladini for stimulating discussions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We are grateful to the SINGS team for producing high-quality data sets used in this study. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - Murphy2010p7153Astrophys_J_Lett.pdf
", "abstract": "We report on the Ka-band (26-40 GHz) emission properties for 10 star-forming regions in the nearby galaxy NGC 6946. From a radio spectral decomposition, we find that the 33 GHz flux densities are typically dominated by thermal (free-free) radiation. However, we also detect excess Ka-band emission for an outer-disk star-forming region relative to what is expected given existing radio, submillimeter, and infrared data. Among the 10 targeted regions, measurable excess emission at 33 GHz is detected for half of them, but in only one region is the excess found to be statistically significant (\u22487\u03c3). We interpret this as the first likely detection of so-called \"anomalous\" dust emission outside of the Milky Way. We find that models explaining this feature as the result of dipole emission from rapidly rotating ultrasmall grains are able to reproduce the observations for reasonable interstellar medium conditions. While these results suggest that the use of Ka-band data as a measure of star formation activity in external galaxies may be complicated by the presence of anomalous dust, it is unclear how significant a factor this will be for globally integrated measurements as the excess emission accounts for \u227210% of the total Ka-band flux density from all 10 regions.", "date": "2010-02-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "709", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L108-L113", "id_number": "CaltechAUTHORS:20100303-095251524", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100303-095251524", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/2041-8205/709/2/L108", "primary_object": { "basename": "Murphy2010p7153Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/ryz2d-4n764/files/Murphy2010p7153Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Murphy, E. J.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/fwhqj-53584", "eprint_id": 17084, "eprint_status": "archive", "datestamp": "2023-08-19 00:39:41", "lastmod": "2023-10-19 22:47:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rau-A", "name": { "family": "Rau", "given": "Arne" }, "orcid": "0000-0001-5990-6243" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David" }, "orcid": "0000-0002-5741-3047" }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "George S." }, "orcid": "0000-0002-0603-3087" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "Derek B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "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": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Reach-W-T", "name": { "family": "Reach", "given": "William T." }, "orcid": "0000-0001-8362-4094" }, { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael" } }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "Andrew J." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Helfand-D-J", "name": { "family": "Helfand", "given": "David J." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" } ] }, "title": "Exploring the Optical Transient Sky with the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2009 Astronomical Society of the Pacific.\n\nReceived 2008 November 28; accepted 2009 July 13; published 2009 October 5.\n\nThis paper is based on observations obtained with the\nSamuel Oschin Telescope and the 60 inch telescope at the\nPalomar Observatory as part of the Palomar Transient Factory\nproject, a scientific collaboration between the California\nInstitute of Technology, Columbia University, Las Cumbres\nObservatory, the Lawrence Berkeley National Laboratory, the\nNational Energy Research Scientific Computing Center, the\nUniversity of Oxford, and the Weizmann Institute of Science.\nS. R. K. and his group were partially supported by NSF grant\nAST-0507734. J. S. B. and his group were partially supported\nby a Hellman Family Grant, a Sloan Foundation Fellowship,\nNSF/DDDAS-TNRP grant CNS-0540352, and a continuing\ngrant from DOE/SciDAC. TheWeizmann Institute PTF partnership\nis supported by an ISF equipment grant to A. G., whose\nactivity is further supported by a Marie Curie IRG grant from\nthe EU, and by the Minerva Foundation, the Benoziyo Center\nfor Astrophysics, a research grant from Peter and Patricia\nGruber Awards, and the William Z. and Eda Bess Novick\nNew Scientists Fund at the Weizmann Institute. E. O. O. thanks\nNASA for partial support through grants HST-GO-11104.01-A,\nNNX08AM04G, 07-GLAST1-0023, and HST-AR-11766.01-A. A. V. F. and his group are grateful for funding from\nNSF grant AST-0607485, DOE/SciDAC grant DE-FC02-06ER41453, DOE grant DE-FG02-08ER41563, the TABASGO\nFoundation, Gary and Cynthia Bengier, the Sylvia and Jim\nKatzman Foundation, and the Richard and Rhoda Goldman\nFund. S. G. D. and A. A. M. were supported in part by NSF\ngrants AST-0407448 and CNS-0540369, and also by the Ajax\nFoundation. The National Energy Research Scientific Computing\nCenter, which is supported by the Office of Science of the\nU.S. Department of Energy under Contract No. DE-AC02-05CH11231, has provided resources for this project by supporting\nstaff and providing computational resources and data\nstorage. L. B.'s research is supported by the NSF via grants\nPHY 05-51164 and AST 07-07633. M. S. acknowledges\nsupport from the Royal Society and the University of Oxford\nFell Fund.\n\nPublished - Rau2009p6625Publ_Astron_Soc_Pac.pdf
", "abstract": "The Palomar Transient Factory (PTF) is a wide-field experiment designed to investigate the optical transient and variable sky on time scales from minutes to years. PTF uses the CFH12k mosaic camera, with a field of view of 7.9 deg^2 and a plate scale of 1\u2033 pixel^(-1), mounted on the Palomar Observatory 48 inch Samuel Oschin Telescope. The PTF operation strategy is devised to probe the existing gaps in the transient phase space and to search for theoretically predicted, but not yet detected, phenomena, such as fallback supernovae, macronovae, .Ia supernovae, and the orphan afterglows of gamma-ray bursts. PTF will also discover many new members of known source classes, from cataclysmic variables in their various avatars to supernovae and active galactic nuclei, and will provide important insights into understanding galactic dynamics (through RR Lyrae stars) and the solar system (asteroids and near-Earth objects). The lessons that can be learned from PTF will be essential for the preparation of future large synoptic sky surveys like the Large Synoptic Survey Telescope. In this article we present the scientific motivation for PTF and describe in detail the goals and expectations for this experiment.", "date": "2009-12", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "121", "number": "886", "publisher": "Astronomical Society of the Pacific", "pagerange": "1334-1351", "id_number": "CaltechAUTHORS:20100106-135303416", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100106-135303416", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0507734" }, { "agency": "Hellman Family" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "CNS-0540352" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Minerva Foundation" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "William Z. and Eda Bess Novick New Scientists Fund at the Weizmann Institute" }, { "agency": "NASA", "grant_number": "HST-GO-11104.01-A" }, { "agency": "NASA", "grant_number": "NNX08AM04G" }, { "agency": "NASA", "grant_number": "07-GLAST1-0023" }, { "agency": "NASA", "grant_number": "HST-AR-11766.01-A" }, { "agency": "NSF", "grant_number": "AST-0607485" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FC02-06ER41453" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-08ER41563" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NSF", "grant_number": "AST-0407448" }, { "agency": "NSF", "grant_number": "CNS-0540369" }, { "agency": "Ajax Foundation" }, { "agency": "NSF", "grant_number": "PHY05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Royal Society" }, { "agency": "University of Oxford Fell Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/605911", "primary_object": { "basename": "Rau2009p6625Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/fwhqj-53584/files/Rau2009p6625Publ_Astron_Soc_Pac.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Rau, Arne; Kulkarni, Shrinivas R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8xnwe-sk143", "eprint_id": 17105, "eprint_status": "archive", "datestamp": "2023-08-19 00:39:57", "lastmod": "2023-10-19 22:49:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Brown-T-M", "name": { "family": "Brown", "given": "Tim" }, "orcid": "0000-0002-1793-9968" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David" }, "orcid": "0000-0002-5741-3047" }, { "id": "Croner-E-E", "name": { "family": "Croner", "given": "Ernest" } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. George" }, "orcid": "0000-0002-0603-3087" }, { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "Julian" }, "orcid": "0000-0003-2192-5371" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "Derek B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Hale-D-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Haman-N", "name": { "family": "Haman", "given": "Nouhad" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Henning-J-R", "name": { "family": "Henning", "given": "John" } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Jacobsen-J", "name": { "family": "Jacobsen", "given": "Janet" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Mattingly-S", "name": { "family": "Mattingly", "given": "Sean" } }, { "id": "McKenna-D-L", "name": { "family": "McKenna", "given": "Dan" } }, { "id": "Pickles-A", "name": { "family": "Pickles", "given": "Andrew" } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "Gustavo" } }, { "id": "Rau-A", "name": { "family": "Rau", "given": "Arne" }, "orcid": "0000-0001-5990-6243" }, { "id": "Rosing-W", "name": { "family": "Rosing", "given": "Wayne" } }, { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger" } }, { "id": "Starr-D", "name": { "family": "Starr", "given": "Dan" } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Velur-V", "name": { "family": "Velur", "given": "Viswa" } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "Jeff" } } ] }, "title": "The Palomar Transient Factory: System Overview, Performance, and First Results", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 University of Chicago Press.\n\nReceived 2009 June 30; accepted 2009 September 29; published 2009 November 12.\n\nThis paper is based on observations obtained with the\nSamuel Oschin Telescope and the 60 inch Telescope at the\nPalomar Observatory as part of the Palomar Transient Factory\nproject, a scientific collaboration between the California Institute\nof Technology, Columbia University, Las Cumbres Observatory,\nthe Lawrence Berkeley National Laboratory, the\nNational Energy Research Scientific Computing Center, the\nUniversity of Oxford, and the Weizmann Institute of Science.\nS. R. K. and his group were partially supported by the NSF\ngrant AST-0507734. J. S. B. and his group were partially supported\nby a Hellman Family Grant, a Sloan Foundation Fellowship,\nNSF/DDDAS-TNRP grant CNS-0540352, and a\ncontinuing grant from DOE/SciDAC. T. B., A. P., W. R. and\nD. A. H. are supported by the TABASGO foundation and\nthe Las Cumbres Observatory Global Telescope Network.\nThe Weizmann Institute PTF partnership is supported by an\nISF equipment grant to A. G. A. G.'s activity is further supported\nby a Marie Curie IRG grant from the EU, and by the\nMinerva Foundation, Benoziyo Center for Astrophysics, a research\ngrant from Peter and Patricia Gruber Awards, and the\nWilliam Z. and Eda Bess Novick New Scientists Fund at the\nWeizmann Institute. E. O. O. acknowledges partial support from\nNASA through grants HST-GO-11104.01-A; NNX08AM04G;\n07-GLAST1-0023; and HST-AR-11766.01-A. A. V. F. and his\ngroup are grateful for funding from NSF grant AST\u20130607485,\nDOE/SciDAC grant DE-FC02-06ER41453, DOE grant DE-FG02-08ER41563, the TABASGO Foundation, Gary and\nCynthia Bengier, and the Sylvia and Jim Katzman Foundation. S. G. D. and A. A. M. were supported in part by NSF grants\nAST-0407448 and CNS-0540369, and also by the Ajax Foundation.\nThe National Energy Research Scientific Computing\nCenter, which is supported by the Office of Science of the\nU.S. Department of Energy under Contract No. DE-AC02-05CH11231, has provided resources for this project by supporting\nstaff and providing computational resources and data\nstorage. A. V. F. and his group are grateful for funding from\nNSF grant AST\u20130607485, DOE/SciDAC grant DE-FC02-06ER41453, DOE grant DE-FG02-08ER41563, the TABASGO\nFoundation, Gary and Cynthia Bengier, the Richard and\nRhoda Goldman Fund, and the Sylvia and Jim Katzman Foundation.\nL. B.'s research is supported by the NSF via grants\nPHY 05-51164 and AST 07-07633. M. S. acknowledges support\nfrom the Royal Society and the University of Oxford Fell\nFund.\n\nPublished - Law2009p6633Publ_Astron_Soc_Pac.pdf
", "abstract": "The Palomar Transient Factory (PTF) is a fully-automated, wide-field survey aimed at a systematic exploration of the optical transient sky. The transient survey is performed using a new 8.1 square degree camera installed on the 48 inch Samuel Oschin telescope at Palomar Observatory; colors and light curves for detected transients are obtained with the automated Palomar 60 inch telescope. PTF uses 80% of the 1.2 m and 50% of the 1.5 m telescope time. With an exposure of 60 s the survey reaches a depth of m_(g\u2032) \u2248 21.3 and m_R \u2248 20.6 (5\u03c3, median seeing). Four major experiments are planned for the five-year project: (1) a 5 day cadence supernova search; (2) a rapid transient search with cadences between 90 s and 1 day; (3) a search for eclipsing binaries and transiting planets in Orion; and (4) a 3\u03c0 sr deep H-alpha survey. PTF provides automatic, real-time transient classification and follow-up, as well as a database including every source detected in each frame. This paper summarizes the PTF project, including several months of on-sky performance tests of the new survey camera, the observing plans, and the data reduction strategy. We conclude by detailing the first 51 PTF optical transient detections, found in commissioning data.", "date": "2009-12", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "121", "number": "886", "publisher": "Astronomical Society of the Pacific", "pagerange": "1395-1408", "id_number": "CaltechAUTHORS:20100108-092743274", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100108-092743274", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0507734" }, { "agency": "Hellman Family" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "CNS-0540352" }, { "agency": "TABASGO Foundation" }, { "agency": "Las Cumbres Observatory Global Telescope Network" }, { "agency": "International Science Foundation" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Minerva Foundation" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Peter and Patricia Gruber Awards" }, { "agency": "William Z. and Eda Bess Novick New Scientists Fund at the Weizmann Institute" }, { "agency": "NASA", "grant_number": "HST-GO-11104.01-A" }, { "agency": "NASA", "grant_number": "NNX08AM04G" }, { "agency": "NASA", "grant_number": "07-GLAST1-0023" }, { "agency": "NASA", "grant_number": "HST-AR-11766.01-A" }, { "agency": "NSF", "grant_number": "AST\u20130607485" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FC02-06ER41453" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-08ER41563" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "NSF", "grant_number": "AST-0407448" }, { "agency": "NSF", "grant_number": "CNS-0540369" }, { "agency": "Ajax Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02- 05CH11231" }, { "agency": "NSF", "grant_number": "AST\u20130607485" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FC02- 06ER41453" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-08ER41563" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Royal Society" }, { "agency": "University of Oxford Fell Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/648598", "primary_object": { "basename": "Law2009p6633Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/8xnwe-sk143/files/Law2009p6633Publ_Astron_Soc_Pac.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Law, Nicholas M.; Kulkarni, Shrinivas R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/88psz-vas76", "eprint_id": 16620, "eprint_status": "archive", "datestamp": "2023-08-21 22:39:28", "lastmod": "2023-10-19 22:25:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bertincourt-B", "name": { "family": "Bertincourt", "given": "B." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Lagache-G", "name": { "family": "Lagache", "given": "G." } }, { "id": "Brooke-T-Y", "name": { "family": "Brooke", "given": "T." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J-D." }, "orcid": "0000-0003-1545-5078" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D." }, "orcid": "0000-0002-5782-9093" }, { "id": "Harwit-M", "name": { "family": "Harwit", "given": "M." } }, { "id": "Puget-J-L", "name": { "family": "Puget", "given": "J-L." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } } ] }, "title": "A Spitzer Unbiased Ultradeep Spectroscopic Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: starburst; infrared: galaxies", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 January 6; accepted 2009 September 10; published 2009 October 7.\nWe thank Aaron Stephen for help with the X-ray data. This\nwork is based on observation obtained with the Spitzer Space\nTelescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under NASA contract 1407.\nSupport for this work was provided by NASA through an award\nissued by JPL/Caltech, as well as the French National Agency\nfor Research under programs ANR-06-BLAN-0170 and ANR-05-BLAN-0289-02. This research has made use of the NASA/IPAC Extragalactic Database which is operated by JPL/Caltech,\nunder contract with NASA.\nFacilities: Spitzer (IRS).\n\nPublished - Bertincourt2009p6230Astrophys_J.pdf
", "abstract": "We carried out an unbiased, spectroscopic survey using the low-resolution module of the infrared spectrograph (IRS) onboard Spitzer targeting two 2.6 square arcminute regions in the GOODS-North field. The IRS was used in a spectral mapping mode with 5 hr of effective integration time per pixel. One region was covered between 14 and 21 \u03bcm and the other between 20 and 35 \u03bcm. We extracted spectra for 45 sources. About 84% of the sources have reported detections by GOODS at 24 \u03bcm, with a median f_\u03bd(24 \u03bcm) ~ 100 \u03bcJy. All but one source are detected in all four IRAC bands, 3.6 to 8 \u03bcm. We use a new cross-correlation technique to measure redshifts and estimate IRS spectral types; this was successful for ~60% of the spectra. Fourteen sources show significant polycyclic aromatic hydrocarbon emission, four mostly SiO absorption, eight present mixed spectral signatures (low PAH and/or SiO) and two show a single line in emission. For the remaining 17, no spectral features were detected. Redshifts range from z ~ 0.2 to z ~ 2.2, with a median of 1. IR luminosities are roughly estimated from 24 \u03bcm flux densities, and have median values of 2.2 \u00d7 10^(11) L_\u2299 and 7.5 \u00d7 10^(11) L_\u2299 at z ~ 1 and z ~ 2, respectively. This sample has fewer active galactic nuclei than previous faint samples observed with the IRS, which we attribute to the fainter luminosities reached here.", "date": "2009-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "705", "number": "1", "publisher": "American Astronomical Society", "pagerange": "68-88", "id_number": "CaltechAUTHORS:20091109-092443054", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091109-092443054", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-06-BLAN-0170" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-05-BLAN-0289-02" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/705/1/68", "primary_object": { "basename": "Bertincourt2009p6230Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/88psz-vas76/files/Bertincourt2009p6230Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Bertincourt, B.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0tn0d-dv250", "eprint_id": 16561, "eprint_status": "archive", "datestamp": "2023-08-19 00:26:48", "lastmod": "2023-10-19 22:22:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "M. T." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Afonso-Luis-A", "name": { "family": "Afonso-Luis", "given": "A." } }, { "id": "Bhattacharya-Bidushi", "name": { "family": "Bhattacharya", "given": "B." } }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A. M." }, "orcid": "0000-0002-6610-2048" }, { "id": "Lee-Nicolas", "name": { "family": "Lee", "given": "Nicholas" }, "orcid": "0000-0001-5500-1324" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Sargent-M-T", "name": { "family": "Sargent", "given": "M. T." }, "orcid": "0000-0003-1033-9684" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Spitzer 70 and 160 \u03bcm Observations of the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: starburst \u2013 infrared: galaxies", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2009 February 17; accepted 2009 August 15; published 2009 September 22. \n\nWe thank our colleagues associated with the Spitzer mission who have made these observations possible. This work is based 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 an award issued by JPL/Caltech.\n\nPublished - Frayer2009p6233Astron_J.pdf
Accepted Version - 0902.3273.pdf
", "abstract": "We present Spitzer 70 and 160 \u03bcm observations of the COSMOS Spitzer survey (S-COSMOS). The data processing techniques are discussed for the publicly released products consisting of images and source catalogs. We present accurate 70 and 160 \u03bcm source counts of the COSMOS field and find reasonable agreement with measurements in other fields and with model predictions. The previously reported counts for GOODS-North and the extragalactic First Look Survey are updated with the latest calibration, and counts are measured based on the large area SWIRE survey to constrain the bright source counts. We measure an extragalactic confusion noise level of \u03c3_c = 9.4 \u00b1 3.3 mJy (q = 5) for the MIPS 160 \u03bcm band based on the deep S-COSMOS data and report an updated confusion noise level of \u03c3_c = 0.35 \u00b1 0.15 mJy (q = 5) for the MIPS 70 \u03bcm band.", "date": "2009-11", "date_type": "published", "publication": "Astronomical Journal", "volume": "138", "number": "5", "publisher": "American Astronomical Society", "pagerange": "1261-1270", "id_number": "CaltechAUTHORS:20091103-130946829", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091103-130946829", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-6256/138/5/1261", "primary_object": { "basename": "Frayer2009p6233Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/0tn0d-dv250/files/Frayer2009p6233Astron_J.pdf" }, "related_objects": [ { "basename": "0902.3273.pdf", "url": "https://authors.library.caltech.edu/records/0tn0d-dv250/files/0902.3273.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Frayer, D. T.; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y8a70-c6y45", "eprint_id": 15304, "eprint_status": "archive", "datestamp": "2023-08-21 22:06:31", "lastmod": "2023-10-18 21:38:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi M." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Zamojski-M-A", "name": { "family": "Zamojski", "given": "Michel" } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce" }, "orcid": "0000-0002-0846-936X" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David" }, "orcid": "0000-0003-1924-1122" } ] }, "title": "The ~0.9 mJy Sample: A Mid-Infrared Spectroscopic Catalog of 150 Infrared-Luminous, 24 \u03bcm Selected Galaxies at 0.3 \u2264 z \u2264 3.5", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: active; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: interactions; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2009. The American Astronomical Society. Received 2009 April 21; accepted 2009 June 29; published 2009 July 29.\nThis work was based on observations made with the Spitzer\nSpace Telescope, which is operated by JPL/Caltech under a\ncontract with NASA, and on observations made with the NASA/\nESA Hubble Space Telescope, obtained at the Space Telescope\nScience Institute, which is operated by the Association of\nUniversities for Research in Astronomy, Incorporated, under\nNASA contract NAS5-26555. The observations are associated\nwith the Spitzer programs 20629 and 40025, and the HST\nprogram 11142. The authors acknowledge support by NASA\nthrough awards issued by JPL/Caltech and through the grant\nHST-GO-11142.06-A awarded by the Space Telescope Science\nInstitute.\n\nPublished - Dasyra2009p5726Astrophys_J.pdf
", "abstract": "We present a catalog of mid-infrared (MIR) spectra of 150 infrared (IR) luminous galaxies in the Spitzer extragalactic first look survey obtained with the IR spectrograph on board the Spitzer Space Telescope. The sample is selected to be brighter than ~0.9 mJy at 24 \u03bcm and it has a redshift distribution in the range [0.3, 3.5], with a peak at z = 1. It primarily comprises ultraluminous IR galaxies (ULIRGs) at z \u2273 1 and luminous IR galaxies at z < 1, as estimated from their monochromatic rest-frame 14 \u03bcm luminosities. The number of sources with spectra that are dominated by an active galactic nucleus (AGN) continuum is 49, while 39 sources have strong, star formation related features. For this classification, we used the equivalent width (EW) of the 11.3 \u03bcm polycyclic aromatic hydrocarbon (PAH) feature. Several intermediate and high z starbursts have higher PAH EW than local ULIRGs, which could be indicative of an elevated star formation activity. Moreover, an increase in the AGN activity is observed with increasing z and luminosity, based on the decreasing EW of PAHs and the increasing [Ne III]/ [Ne II] ratio. Spectral stacking leads to the detection of weak features such as the 3.3 \u03bcm PAH, the H_2 0-0 S(1) and S(3) lines, and the [Ne V] line. We observe differences in the flux ratios of PAHs in the stacked spectra of IR-luminous galaxies with redshift or luminosity, which cannot be attributed to extinction effects since both the depth and the profile of the silicate absorption feature at 9.7 \u03bcm remain the same at z < 1 and z \u2265 1. When placing the observed galaxies on IR color-color diagrams, we find that the wedge defining AGNs comprises most sources with continuum-dominated spectra, but also contains many starbursts and sources with strong silicate absorption at 9.7 \u03bcm. The comparison of the 11.3 \u03bcm PAH EW and the H-band effective radius, measured from Hubble Space Telescope data, indicates that sources with EWs \u2265 2 \u03bcm, are typically more extended than ~3 kpc. However, there is no strong correlation between the MIR spectral type and the near-IR extent of the sources.", "date": "2009-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "701", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1123-1146", "id_number": "CaltechAUTHORS:20090825-141510421", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090825-141510421", "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": "HST-GO-11142.06-A" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/701/2/1123", "primary_object": { "basename": "Dasyra2009p5726Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/y8a70-c6y45/files/Dasyra2009p5726Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Dasyra, Kalliopi M.; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vxc6j-fnw53", "eprint_id": 14913, "eprint_status": "archive", "datestamp": "2023-08-21 21:52:57", "lastmod": "2023-10-18 20:22:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bot-C", "name": { "family": "Bot", "given": "Caroline" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Latter-W-B", "name": { "family": "Latter", "given": "William B." } }, { "id": "Puget-J", "name": { "family": "Puget", "given": "J\u00e9r\u00e9mie" } }, { "id": "Schneider-S", "name": { "family": "Schneider", "given": "Stephen" } }, { "id": "Terzian-Y", "name": { "family": "Terzian", "given": "Yervant" } } ] }, "title": "A Search for Dust Emission in the Leo Intergalactic Cloud", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: ISM; intergalactic medium; ISM: clouds; ISM: individual (Leo cloud)", "note": "\u00a9 2009. The American Astronomical Society. Print publication: Issue 2 (2009 August).\nReceived 2008 November 10, accepted for publication 2009 May 17\nPublished 2009 June 29.\nThis work is based on observations made with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under a contract with\nNASA. This 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\nwith the National Aeronautics and Space Administration. We\nwould like to thank M. Fouesneau and D. Thilker for their help\non the estimate of the UV radiation field from the star-forming\nregion with evolutionary synthesis models.\n\nPublished - Bot2009p5113Astron_J.pdf
", "abstract": "We present a search for infrared dust emission associated with the Leo cloud, a large intergalactic cloud in the M96 group. Mid-infrared and far-infrared images were obtained with the InfraRed Array Camera and the Multiband Imaging Photometer for Spitzer on the Spitzer Space Telescope. Our analysis of these maps is done at each wavelength relative to the H I spatial distribution. We observe a probable detection at 8 \u03bcm and a marginal detection at 24 \u03bcm associated with the highest H I column densities in the cloud. At 70 and 160 \u03bcm, upper limits on the dust emission are deduced. The level of the detection is low so that the possibility of a fortuitous cirrus clump or of an overdensity of extragalactic sources along the line of sight cannot be excluded. If this detection is confirmed, the quantities of dust inferred imply a dust-to-gas ratio in the intergalactic cloud up to a few times solar but no less than 1/20 solar. A confirmed detection would therefore exclude the possibility that the intergalactic cloud has a primordial origin. Instead, this large intergalactic cloud could therefore have been formed through interactions between galaxies in the group.", "date": "2009-08", "date_type": "published", "publication": "Astronomical Journal", "volume": "138", "number": "2", "publisher": "American Astronomical Society", "pagerange": "452-458", "id_number": "CaltechAUTHORS:20090810-084634970", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090810-084634970", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-6256/138/2/452", "primary_object": { "basename": "Bot2009p5113Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/vxc6j-fnw53/files/Bot2009p5113Astron_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Bot, Caroline; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8rjse-0r946", "eprint_id": 24334, "eprint_status": "archive", "datestamp": "2023-08-21 21:59:17", "lastmod": "2024-01-13 05:17:53", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi M." } }, { "id": "Peterson-B-M", "name": { "family": "Peterson", "given": "Bradley M." } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "Linda J." }, "orcid": "0000-0002-1485-9401" }, { "id": "Netzer-H", "name": { "family": "Netzer", "given": "Hagai" } }, { "id": "Ho-Luis-C", "name": { "family": "Ho", "given": "Luis C." }, "orcid": "0000-0001-6947-5846" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "Dieter" }, "orcid": "0000-0003-0291-9582" }, { "id": "Davies-R", "name": { "family": "Davies", "given": "Richard" } }, { "id": "Watson-L", "name": { "family": "Watson", "given": "Linda" } } ] }, "title": "On the Relation Between Black Hole Mass and Velocity Dispersion in Type 1 and Type 2 AGN", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: nuclei; galaxies: kinematics and dynamics; (galaxies:) quasars: emission lines; infrared: galaxies; instrumentation: adaptive optics", "note": "\u00a9 2010 International Astronomical Union. Published online: 03 June 2010.\n\nPublished - Dasyra2010p14501Co-Evolution_Of_Central_Black_Holes_And_Galaxies.pdf
Submitted - 1001.4370v1.pdf
", "abstract": "We present results from infrared spectroscopic projects that aim to test the relation\nbetween the mass of a black hole M_(BH) and the velocity dispersion of the stars in its host-galaxy\nbulge. We demonstrate that near-infrared, high-resolution spectroscopy assisted by adaptive\noptics is key in populating the high-luminosity end of the relation. We show that the velocity\ndispersions of mid-infrared, high-ionization lines originating from gas in the narrow-line region\nof the active galactic nucleus follow the same relation. This result provides a way of inferring\nMBH estimates for the cosmologically significant population of obscured, type 2 AGN that can\nbe applicable to data from spectrographs on next-generation infrared telescopes.", "date": "2009-08", "date_type": "published", "publisher": "Cambridge University Press", "place_of_pub": "New York, NY", "pagerange": "172-176", "id_number": "CaltechAUTHORS:20110707-093531555", "isbn": "978-0-521-76502-2", "book_title": "Co-Evolution of Central Black Holes and Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110707-093531555", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Peterson-B-M", "name": { "family": "Peterson", "given": "B. M." } }, { "id": "Somerville-R-S", "name": { "family": "Somerville", "given": "R. S." } }, { "id": "Storchi-Bergmann-T", "name": { "family": "Storchi-Bergmann", "given": "T." } } ] }, "doi": "10.1017/S1743921310006113", "primary_object": { "basename": "Dasyra2010p14501Co-Evolution_Of_Central_Black_Holes_And_Galaxies.pdf", "url": "https://authors.library.caltech.edu/records/8rjse-0r946/files/Dasyra2010p14501Co-Evolution_Of_Central_Black_Holes_And_Galaxies.pdf" }, "related_objects": [ { "basename": "1001.4370v1.pdf", "url": "https://authors.library.caltech.edu/records/8rjse-0r946/files/1001.4370v1.pdf" } ], "resource_type": "book_section", "pub_year": "2009", "author_list": "Dasyra, Kalliopi M.; Peterson, Bradley M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/eq685-56551", "eprint_id": 14049, "eprint_status": "archive", "datestamp": "2023-08-21 21:12:54", "lastmod": "2023-10-18 16:04:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bot-C", "name": { "family": "Bot", "given": "Caroline" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "Fran\u00e7ois" } }, { "id": "Lagache-G", "name": { "family": "Lagache", "given": "Guilaine" } }, { "id": "Miville-Deschenes-M-A", "name": { "family": "Miville-Deschenes", "given": "Marc-Antoine" } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce" }, "orcid": "0000-0002-0846-936X" }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter" }, "orcid": "0000-0002-5236-3896" } ] }, "title": "Serendipity observations of far infrared cirrus emission in the Spitzer Infrared Nearby Galaxies Survey: analysis of far-infrared correlations", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: clouds; infrared: ISM", "note": "\u00a92009 The American Astronomical Society.\nReceived 2008 October 13; accepted 2009 January 13; published 2009 March 31.\nWe would like to thank our referee M. Rowan-Robinson for\nhis useful and interesting comments and A. Efstathiou for his helpwith their cirrusmodel. We are also grateful to L. Cambr\u00e9sy for useful discussions and work on upper limit for extinction in our fields.\nFacilities: Spitzer.\n\nPublished - Bot2009p1478Astrophys_J.pdf
", "abstract": "We present an analysis of far-infrared (FIR) dust emission from diffuse cirrus clouds. This study is based on\nserendipitous observations at 160 \u03bcm at high-galactic latitude with the Multiband Imaging Photometer onboard\nthe Spitzer Space Telescope by the Spitzer Infrared Nearby Galaxies Survey. These observations are complemented\nwith IRIS data at 100 and 60 \u03bcm and constitute one of the most sensitive and unbiased samples of FIR observations\nat a small scale of diffuse interstellar clouds. Outside regions dominated by the cosmic infrared background fluctuations, we observe a substantial scatter in the 160/100 colors from cirrus emission. We compared the 160/100 color variations to 60/100 colors in the same fields and find a trend of decreasing 60/100 with increasing 160/100. This trend cannot be accounted for by current dust models by changing solely the interstellar radiation field. It requires a significant change of dust properties such as grain size distribution or emissivity or a mixing of clouds in different physical conditions along the line of sight. These variations are important as a potential confusing foreground for extragalactic studies.", "date": "2009-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "695", "number": "1", "publisher": "American Astronomical Society", "pagerange": "469-478", "id_number": "CaltechAUTHORS:20090422-150618966", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090422-150618966", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/695/1/469", "primary_object": { "basename": "Bot2009p1478Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/eq685-56551/files/Bot2009p1478Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Bot, Caroline; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vchm7-d0v62", "eprint_id": 14356, "eprint_status": "archive", "datestamp": "2023-08-21 21:10:51", "lastmod": "2023-10-18 16:48:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Kenney-J-D-P", "name": { "family": "Kenney", "given": "J. D. P." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Chung-A", "name": { "family": "Chung", "given": "A." } }, { "id": "Howell-J-H", "name": { "family": "Howell", "given": "J. H." } } ] }, "title": "Environmental effects in clusters: modified far-infrared-radio relations within Virgo Cluster galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic rays; galaxies: clusters: individual (Virgo); galaxies: interactions; galaxies: ISM; infrared: galaxies; radio continuum: galaxies", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2008 June 9; accepted 2009 January 5; published 2009 March 24.\nWe thank the anonymous referee for their useful suggestions\nthat helped to improve the content and presentation of this\npaper. We are grateful to the SINGS team for producing high\nquality data sets used in this study. This work is based in part\non observations made with the SST, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology under\na contract with NASA. Support for this work was provided by\nNASA through an award issued by JPL/Caltech. The National Radio Astronomy Observatory is a facility of the National\nScience Foundation operated under cooperative agreement by\nAssociated Universities, Inc.\n\nPublished - Murphy2009p1378Astrophys_J.pdf
", "abstract": "We present a study on the effects of the intracluster medium (ICM) on the interstellar medium (ISM) of 10 Virgo Cluster galaxies using Spitzer far-infrared (FIR) and Very Large Array radio continuum imaging. Relying on the FIR-radio correlation within normal galaxies, we use our infrared data to create model radio maps, which we compare to the observed radio images. For six of our sample galaxies, we find regions along their outer edges that are highly deficient in the radio compared with our models. We also detect FIR emission slightly beyond the observed radio disk along these outer edges. We believe these observations are the signatures of ICM ram pressure. For NGC 4522, we find the radio-deficit region to lie just exterior to a region of high radio polarization and flat radio spectral index, although the total 20 cm radio continuum in this region does not appear strongly enhanced. These characteristics seem consistent for other galaxies with radio polarization data in the literature. The strength of the radio deficit is inversely correlated with the time since peak pressure as inferred from stellar population studies and gas-stripping simulations, consistent with the strength of the radio deficit being a good indicator of the strength of the current ram pressure. We also find that galaxies having local radio deficits appear to have enhanced global radio fluxes. Our preferred physical picture is that the observed radio-deficit regions arise from the ICM wind sweeping away cosmic-ray (CR) electrons and the associated magnetic field, thereby creating synchrotron tails as observed for some of our galaxies. We propose that CR particles are also reaccelerated by ICM-driven shocklets behind the observed radio-deficit regions which, in turn, enhances the remaining radio disk brightness. The high radio polarization and lack of precisely coincident enhancement in the total synchrotron power for these regions suggest shearing, and possibly mild compression of the magnetic field, as the ICM wind drags and stretches the leading edge of the ISM.", "date": "2009-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "694", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1435-1451", "id_number": "CaltechAUTHORS:20090603-092811594", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090603-092811594", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/694/2/1435", "primary_object": { "basename": "Murphy2009p1378Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/vchm7-d0v62/files/Murphy2009p1378Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Murphy, E. J.; Kenney, J. D. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/92a6w-dax60", "eprint_id": 15186, "eprint_status": "archive", "datestamp": "2023-08-21 21:01:15", "lastmod": "2023-10-18 21:03:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Schlawin-E-A", "name": { "family": "Schlawin", "given": "E. A." }, "orcid": "0000-0001-8291-6490" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Cohen-S-A", "name": { "family": "Cohen", "given": "S. A." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Johnson-L-C", "name": { "family": "Johnson", "given": "L. C." } }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Staudaher-S", "name": { "family": "Staudaher", "given": "S." } }, { "id": "Bot-C", "name": { "family": "Bot", "given": "C." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "S." }, "orcid": "0000-0002-9226-5350" } ] }, "title": "The Spitzer Infrared Nearby Galaxies Survey: A High-Resolution Spectroscopy Anthology", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; galaxies: active; galaxies: jets", "note": "\u00a9 2009. The American Astronomical Society. Print publication: Issue 2 (2009 March 10). Received 2008 September 10, accepted for publication 2008 December 3.\nPublished 2009 March 10. Rajib Ganguly, Brent Groves, and Phil Maloney graciously\nhelped with comparisons of the data to theoretical models.\nWe are grateful for the helpful suggestions provided\nby the referee. Support for this work, part of the Spitzer\nSpace Telescope Legacy Science Program, was provided by\nNASA through Contract Number 1224769 issued by the Jet\nPropulsion Laboratory, California Institute of Technology under\nNASA contract 1407. This research has made use of\nthe NASA/IPAC Extragalactic Database which is operated\nby JPL/Caltech, under contract with NASA. This publication\nmakes use of data products from the Two Micron All Sky\nSurvey, which is a joint project of the University of Massachusetts\nand the Infrared Processing and Analysis Center/\nCalifornia Institute of Technology, funded by theNational Aeronautics\nand Space Administration and the National Science\nFoundation.\n\nPublished - Dale2009p1041Astrophys_J.pdf
", "abstract": "High-resolution mid-infrared spectra are presented for 155 nuclear and extranuclear regions from the Spitzer Infrared Nearby Galaxies Survey (SINGS). The fluxes for nine atomic forbidden and three molecular hydrogen mid-infrared emission lines are also provided, along with upper limits in key lines for infrared-faint targets. The SINGS sample shows a wide range in the ratio of [S III] 18.71 \u03bcm/[S III] 33.48 \u03bcm, but the average ratio of the ensemble indicates a typical interstellar electron density of 300-400 cm^(\u20133) on ~23\" \u00d7 15\" scales and 500-600 cm^(\u20133) using ~11\" \u00d7 9\" apertures, independent of whether the region probed is a star-forming nuclear, a star-forming extranuclear, or an active galactic nuclei (AGN) environment. Evidence is provided that variations in gas-phase metallicity play an important role in driving variations in radiation field hardness, as indicated by [Ne III] 15.56 \u03bcm/[Ne II] 12.81 \u03bcm, for regions powered by star formation. Conversely, the radiation hardness for galaxy nuclei powered by accretion around a massive black hole is independent of metal abundance. Furthermore, for metal-rich environments AGN are distinguishable from star-forming regions by significantly larger [Ne III] 15.56 \u03bcm/[Ne II] 12.81 \u03bcm ratios. Finally, [Fe II] 25.99 \u03bcm/[Ne II] 12.81 \u03bcm versus [Si II] 34.82 \u03bcm/[S III] 33.48 \u03bcm also provides an empirical method for discerning AGN from normal star-forming sources. However, similar to [Ne III] 15.56 \u03bcm/[Ne II] 12.81 \u03bcm, these mid-infrared line ratios lose their AGN/star-formation diagnostic powers for very low metallicity star-forming systems with hard radiation fields.", "date": "2009-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "693", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1821-1834", "id_number": "CaltechAUTHORS:20090820-103557386", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090820-103557386", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/693/2/1821", "primary_object": { "basename": "Dale2009p1041Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/92a6w-dax60/files/Dale2009p1041Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Dale, D. A.; Smith, J. D. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/r2bcz-rx685", "eprint_id": 14915, "eprint_status": "archive", "datestamp": "2023-08-21 20:55:20", "lastmod": "2023-10-18 20:22:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "F." } }, { "id": "Maillard-J-P", "name": { "family": "Maillard", "given": "J. P." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" }, { "id": "Falgarone-E", "name": { "family": "Falgarone", "given": "E." } }, { "id": "Lagache-Guilaine", "name": { "family": "Lagache", "given": "G." }, "orcid": "0000-0003-1492-2519" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Wakker-B-P", "name": { "family": "Wakker", "given": "B. P." } }, { "id": "Bressan-A", "name": { "family": "Bressan", "given": "A." } }, { "id": "Cernicharo-J", "name": { "family": "Cernicharo", "given": "J." } }, { "id": "Charmandaris-V", "name": { "family": "Charmandaris", "given": "V." }, "orcid": "0000-0002-2688-1956" }, { "id": "Drissen-L", "name": { "family": "Drissen", "given": "L." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Henning-T", "name": { "family": "Henning", "given": "T." } }, { "id": "Lim-Tanya-L", "name": { "family": "Lim", "given": "T. L." } }, { "id": "Valentjin-E-A", "name": { "family": "Valentjin", "given": "E. A." } }, { "id": "Abergel-A", "name": { "family": "Abergel", "given": "A." } }, { "id": "Le-Bourlot-J", "name": { "family": "Le Bourlot", "given": "J." } }, { "id": "Bouzit-M", "name": { "family": "Bouzit", "given": "M." } }, { "id": "Cabrit-S", "name": { "family": "Cabrit", "given": "S." } }, { "id": "Combes-F", "name": { "family": "Combes", "given": "F." }, "orcid": "0000-0003-2658-7893" }, { "id": "Deharveng-J-M", "name": { "family": "Deharveng", "given": "J. M." } }, { "id": "Desmet-P", "name": { "family": "Desmet", "given": "P." } }, { "id": "Dole-H", "name": { "family": "Dole", "given": "H." } }, { "id": "Dumesnil-C", "name": { "family": "Dumesnil", "given": "C." } }, { "id": "Dutrey-A", "name": { "family": "Dutrey", "given": "A." } }, { "id": "Fourmond-J-J", "name": { "family": "Fourmond", "given": "J. J." } }, { "id": "Gavila-E", "name": { "family": "Gavila", "given": "E." } }, { "id": "Grang\u00e9-R", "name": { "family": "Grang\u00e9", "given": "R." } }, { "id": "Gry-C", "name": { "family": "Gry", "given": "C." } }, { "id": "Guillard-P", "name": { "family": "Guillard", "given": "P." }, "orcid": "0000-0002-2421-1350" }, { "id": "Guilloteau-S", "name": { "family": "Guilloteau", "given": "S." } }, { "id": "Habart-E", "name": { "family": "Habart", "given": "E." } }, { "id": "Huet-B", "name": { "family": "Huet", "given": "B." } }, { "id": "Joblin-C", "name": { "family": "Joblin", "given": "C." } }, { "id": "Langer-M", "name": { "family": "Langer", "given": "M." } }, { "id": "Longval-Yu-Ying", "name": { "family": "Longval", "given": "Y." } }, { "id": "Madden-S-C", "name": { "family": "Madden", "given": "S. C." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Miville-Desch\u00eanes-M-A", "name": { "family": "Miville-Desch\u00eanes", "given": "M. A." } }, { "id": "Pineau-des-For\u00eats-G", "name": { "family": "Pineau des For\u00eats", "given": "G." } }, { "id": "Pointecouteau-E", "name": { "family": "Pointecouteau", "given": "E." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Tresse-L", "name": { "family": "Tresse", "given": "L." } }, { "id": "Verstraete-L", "name": { "family": "Verstraete", "given": "L." } }, { "id": "Viallefond-F", "name": { "family": "Viallefond", "given": "F." } }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Jorgensen-J", "name": { "family": "Jorgensen", "given": "J." } }, { "id": "Bouwman-J", "name": { "family": "Bouwman", "given": "J." } }, { "id": "Carmona-A", "name": { "family": "Carmona", "given": "A." } }, { "id": "Krause-O", "name": { "family": "Krause", "given": "O." } }, { "id": "Baruffolo-A", "name": { "family": "Baruffolo", "given": "A." } }, { "id": "Bonoli-C", "name": { "family": "Bonoli", "given": "C." } }, { "id": "Bortoletto-F", "name": { "family": "Bortoletto", "given": "F." } }, { "id": "Danese-L", "name": { "family": "Danese", "given": "L." } }, { "id": "Granato-G-L", "name": { "family": "Granato", "given": "G. L." } }, { "id": "Pernechele-C", "name": { "family": "Pernechele", "given": "C." } }, { "id": "Rampazzo-R", "name": { "family": "Rampazzo", "given": "R." }, "orcid": "0000-0001-5318-9183" }, { "id": "Silva-L", "name": { "family": "Silva", "given": "L." } }, { "id": "De-Zotti-G", "name": { "family": "de Zotti", "given": "G." }, "orcid": "0000-0003-2868-2595" }, { "id": "Pardo-J-R", "name": { "family": "Pardo", "given": "J." } }, { "id": "Spaans-M", "name": { "family": "Spaans", "given": "M." } }, { "id": "van-der-Tak-F-F-S", "name": { "family": "van der Tak", "given": "F. F. S." } }, { "id": "Wild-W-J", "name": { "family": "Wild", "given": "W." } }, { "id": "Ferlet-M-J", "name": { "family": "Ferlet", "given": "M. J." } }, { "id": "Ramsay-Howat-S-K", "name": { "family": "Ramsay Howat", "given": "S. K." } }, { "id": "Smith-M-D", "name": { "family": "Smith", "given": "M. D." } }, { "id": "Swinyard-B-M", "name": { "family": "Swinyard", "given": "B." } }, { "id": "Wright-G-S", "name": { "family": "Wright", "given": "G. S." } }, { "id": "Joncas-G", "name": { "family": "Joncas", "given": "G." } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Davis-C-J", "name": { "family": "Davis", "given": "C. J." } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Goldsmith-P-F", "name": { "family": "Goldsmith", "given": "P. F." }, "orcid": "0000-0002-6622-8396" }, { "id": "Mainzer-A-K", "name": { "family": "Mainzer", "given": "A. K." } }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Rinehart-S-A", "name": { "family": "Rinehart", "given": "S. A." } }, { "id": "Stacey-G-J", "name": { "family": "Stacey", "given": "G. J." } }, { "id": "Tielens-A-G-G-M", "name": { "family": "Tielens", "given": "A. G. G. M." } } ] }, "title": "The molecular hydrogen explorer H2EX", "ispublished": "pub", "full_text_status": "public", "keywords": "Star formation; Galaxies; ISM; Disks; Astronomical instrumentation", "note": "\u00a9 2009 Springer Science. Received: 31 October 2007 / Accepted: 3 June 2008 / Published online: 16 July 2008.\nThe authors gratefully acknowledge help and advices from Ren\u00e9 Laureijs at\nESA who, as former H2EX PI, was the early initiator of the new H2EX mission. The preparation\nof the proposal was supported by the Centre National d'\u00c9tudes Spatiales (CNES).\n\nPublished - Boulanger2009p1091Exp_Astron.pdf
Submitted - 0805.3109v1.pdf
", "abstract": "The Molecular Hydrogen Explorer, H2EX, was proposed in response to the ESA 2015 - 2025 Cosmic Vision Call as a medium class space mission with NASA and CSA participations. The mission, conceived to understand the formation of galaxies, stars and planets from molecular hydrogen, is designed to observe the first rotational lines of the H_2 molecule (28.2, 17.0, 12.3 and 9.7 \u03bcm) over a wide field, and at high spectral resolution. H2EX can provide an inventory of warm (\u2265 100 K) molecular gas in a broad variety of objects, including nearby young star clusters, galactic molecular clouds, active galactic nuclei, local and distant galaxies. The rich array of molecular, atomic and ionic lines, as well as solid state features available in the 8 to 29 \u03bcm spectral range brings additional science dimensions to H2EX. We present the optical and mechanical design of the H2EX payload based on an innovative Imaging Fourier Transform Spectrometer fed by a 1.2m telescope. The 20'\u00d720' field of view is imaged on two 1024\u00d71024 Si:As detectors. The maximum resolution of 0.032 cm^(\u22121) (full width at half maximum) means a velocity resolution of 10 kms^(\u22121) for the 0 \u2013 0 S(3) line at 9.7 \u03bcm. This instrument offers the large field of view necessary to survey extended emission in the Galaxy and local Universe galaxies as well as to perform unbiased extragalactic and circumstellar disks surveys. The high spectral resolution makes H_2EX uniquely suited to study the dynamics of H2 in all these environments. The mission plan is made of seven wide-field spectro-imaging legacy programs, from the cosmic web to galactic young star clusters, within a nominal two years mission. The payload has been designed to re-use the Planck platform and passive cooling design.", "date": "2009-03", "date_type": "published", "publication": "Experimental Astronomy", "volume": "23", "number": "1", "publisher": "Springer", "pagerange": "277-302", "id_number": "CaltechAUTHORS:20090810-090018904", "issn": "0922-6435", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090810-090018904", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1007/s10686-008-9108-7", "primary_object": { "basename": "0805.3109v1.pdf", "url": "https://authors.library.caltech.edu/records/r2bcz-rx685/files/0805.3109v1.pdf" }, "related_objects": [ { "basename": "Boulanger2009p1091Exp_Astron.pdf", "url": "https://authors.library.caltech.edu/records/r2bcz-rx685/files/Boulanger2009p1091Exp_Astron.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Boulanger, F.; Maillard, J. P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ttxz3-zp726", "eprint_id": 12696, "eprint_status": "archive", "datestamp": "2023-08-22 13:11:08", "lastmod": "2023-10-17 20:26:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brauher-J-R", "name": { "family": "Brauher", "given": "James R." } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "A Compendium of Far-Infrared Line and Continuum Emission for 227 Galaxies Observed by the Infrared Space Observatory", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared galaxies; ISM - interstellar matter", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2008 March 25, accepted for publication 2008 May 19. Print publication: Issue 2 (2008 October). \n\nWe thank several people for their contributions: Harold Corwin for reclassifying the galaxies in this sample according to the RC3 catalog; Steve Lord, Tom Jarrett, and Alessandra Contursi for helpful discussions; Heather Maynard for her suggestions and support; and Pat Patterson and Niles McElveney for assistance with the preparation of the manuscript. We appreciate the constructive comments made by the anonymous referee. The data for this project are based on observations with the Infrared Space Observatory, an ESA project with instruments funded by ESA member states (especially the PI countries: France, Germany, the Netherlands, and the United Kingdom) with the participation of ISAS and NASA. The ISO Spectral Analysis Package (ISAP) is a joint development by the LWS and SWS Instrument Teams and Data Centers. Contributing institutes are CESR, IAS, IPAC, MPE, RAL, and SRON. This research has made use of the NASA/IPAC Extragalactic Database that is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). This work has made use of data services of the InfraRed Science Archive (IRSA) at the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration (NASA).\n\nPublished - BRAapjss08.pdf
", "abstract": "Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory. The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or H II regions: [O III] 52 \u03bcm, [N III] 57 \u03bcm, [O I] 63 \u03bcm, [O III] 88 \u03bcm, [N II] 122 \u03bcm, [O I] 145 \u03bcm, and [C II] 158 \u03bcm. Molecular lines such as OH at 53, 79, 84, 119, and 163 \u03bcm, and H2O at 58, 66, 75, 101, and 108 \u03bcm are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [C II] 158 \u03bcm and an unidentified line near 74 \u03bcm in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170 \u03bcm are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75\" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.", "date": "2008-10", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "178", "number": "2", "publisher": "American Astronomical Society", "pagerange": "280-301", "id_number": "CaltechAUTHORS:BRAapjss08", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BRAapjss08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/590249", "primary_object": { "basename": "BRAapjss08.pdf", "url": "https://authors.library.caltech.edu/records/ttxz3-zp726/files/BRAapjss08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Brauher, James R.; Dale, Daniel A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6bk35-hx498", "eprint_id": 13438, "eprint_status": "archive", "datestamp": "2023-08-22 13:03:27", "lastmod": "2023-10-17 23:53:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "M. D." } }, { "id": "Bot-C", "name": { "family": "Bot", "given": "C." } }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "A." } }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } } ] }, "title": "The relations among 8, 24 and 160 mu m dust emission within nearby spiral galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; infrared: galaxies", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS. \nAccepted 2008 June 11. Received 2008 May 30; in original form 2008 March 13.\nThis work was funded by STFC. BTD was supported in part by NSF\ngrant AST04-06883. AL is supported in part by the Spitzer Theory\nPrograms and NSF grant AST 07-07866.\n\nPublished - BENmnras08.pdf
", "abstract": "We investigate the relations among the stellar continuum-subtracted 8 \u00b5m polycyclic aromatic hydrocarbon (PAH 8 \u00b5m) emission, 24 \u00b5m hot dust emission and 160 \u00b5m cold dust emission in 15 nearby face-on spiral galaxies in the Spitzer Infrared Nearby Galaxies Survey sample. The relation between PAH 8 and 24 \u00b5m emission measured in ~2 kpc regions is found to exhibit a significant amount of scatter, and strong spatial variations are observed in the (PAH 8 \u00b5m)/24 \u00b5m surface brightness ratio. In particular, the (PAH 8 \u00b5m)/24 \u00b5m surface brightness ratio is observed to be high in the diffuse interstellar medium and low in bright star-forming regions and other locations with high 24 \u00b5m surface brightness. PAH 8 \u00b5m emission is found to be well-correlated with 160 \u00b5m emission on spatial scales of ~2 kpc, and the (PAH 8 \u00b5m)/160 \u00b5m surface brightness ratio is generally observed to increase as the 160 \u00b5m surface brightness increases. These results suggest that the PAHs are associated with the diffuse, cold dust that produces most of the 160 \u00b5m emission in these galaxies, and the variations in the (PAH 8 \u00b5m)/160 \u00b5m ratio may generally be indicative of either the intensity or the spectrum of the interstellar radiation field that is heating both the PAHs and the diffuse interstellar dust.", "date": "2008-09-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "389", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "629-650", "id_number": "CaltechAUTHORS:BENDOmnras08", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BENDOmnras08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NSF", "grant_number": "AST 04-06883" }, { "agency": "NSF", "grant_number": "AST 07-07866" }, { "agency": "Spitzer Theory Programs" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2008.13567.x", "primary_object": { "basename": "BENmnras08.pdf", "url": "https://authors.library.caltech.edu/records/6bk35-hx498/files/BENmnras08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Bendo, G. J.; Draine, B. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dt3vx-6db96", "eprint_id": 13371, "eprint_status": "archive", "datestamp": "2023-08-22 12:53:52", "lastmod": "2023-10-17 23:50:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "Baruch T." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Werner-M", "name": { "family": "Werner", "given": "Michael" } } ] }, "title": "The Spitzer view of the extragalactic universe", "ispublished": "pub", "full_text_status": "public", "keywords": "aromatic emission hands; far-infrared background; infrared astronomy; massive high-redshift galaxies; star formation history; ultraluminous infrared galaxies", "note": "\u00a9 2008 Annual Reviews.\nWe wish to acknowledge all the people whose work we have been able to cite, as well as those\nresearchers whose work we were unable to cite because of lack of space, and we thank many members\nof the Spitzer community for providing suggestions and preprints. It is especially appropriate\nto acknowledge the instrument teams whose beautiful handiwork has led to the spectacular results\nwe have described\u2014the IRAC team led by Giovanni Fazio, the IRS team led by James Houck,\nand the MIPS team led by George Rieke. We thank E. van Dishoeck, B. Brandl, R. Genzel, G.\nRieke, and G. Neugebauer for commenting on the manuscript. We also thank Marilyn Morgan,\nMary Young, and Jim Jackson for editorial assistance, and Caroline Bot for assistance in preparing\nFigure 13. This work was supported by the National Aeronautics and Space Administration\n(NASA). Part of this work was carried out at the Jet Propulsion Laboratory, California Institute\nof Technology, under a contract with NASA.\n\nPublished - SOIaraa08.pdf
", "abstract": "The Spitzer Space Telescope was launched in August 2003. Scientists from around the world have applied its orders-of-magnitude gain in imaging and spectroscopic capability to a wide array of topics in extragalactic research. Spitzer studies have found massive galaxies at redshifts greater than 6, resolved the cosmic background at 200 \u03bcm > \u03bb > 20 \u03bcm into the dusty infrared-luminous galaxies that comprise it, directly detected dust-enshrouded star formation, and measured the star formation history of the universe to z > 3. In this review we examine a small fraction of the extragalactic studies from Spitzer that have been conducted in its first three years of operations.", "date": "2008-09", "date_type": "published", "publication": "Annual Review of Astronomy and Astrophysics", "volume": "46", "publisher": "Annual Reviews", "pagerange": "201-240", "id_number": "CaltechAUTHORS:SOIaraa08", "issn": "0066-4146", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SOIaraa08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1146/annurev.astro.46.060407.145144", "primary_object": { "basename": "SOIaraa08.pdf", "url": "https://authors.library.caltech.edu/records/dt3vx-6db96/files/SOIaraa08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Soifer, Baruch T.; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/n9yay-50g80", "eprint_id": 14241, "eprint_status": "archive", "datestamp": "2023-08-22 12:45:49", "lastmod": "2023-10-18 16:25:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "Dieter" }, "orcid": "0000-0003-0291-9582" }, { "id": "Steffen-A", "name": { "family": "Steffen", "given": "Aaron" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Huynh-Minh-T", "name": { "family": "Huynh", "given": "Minh" } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David" }, "orcid": "0000-0003-1924-1122" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "Philip" } }, { "id": "Tacconi-Linda-J", "name": { "family": "Tacconi", "given": "Linda" }, "orcid": "0000-0002-1485-9401" }, { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi" } } ] }, "title": "Spitzer mid-infrared spectroscopy of infrared luminous galaxies at z ~ 2. III. far-IR to radio properties and optical spectral diagnostics", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; infrared: galaxies; quasars: general; radio continuum: galaxies", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2008 January 20, accepted for publication 2008 May 1.\nWe are grateful to the anonymous referee for a careful reading of our manuscript and detailed comments that greatly increased the clarity and presentation of this paper. We wish to thank Mark Lacy, Eric Murphy, Lee Armus, and Bruce Partridge for useful discussions. We are grateful to Alexandra Pope for providing us with the average SMG SED template and to Alejo Martinez-Sansigre for providing us with the optical spectrum of MIPS 22204. We are grateful to D. Stern and G. Becker for allowing us to use their\nsoftware tools to reduce the Keck spectra. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of\nTechnology under contract with NASA. Support for this work\nwas provided by NASA through an award issued by JPL/Caltech.\nThis work includes observations made with IRAM, which is\nsupported by INSU/CNRS (France), MPG (Germany), and IGN\n(Spain). Some of the data presented herein were obtained at the\nW. M. Keck Observatory, which is operated as a scientific partnership\namong the California Institute of Technology, the University\nof California, and theNationalAeronautics and SpaceAdministration.\nTheObservatorywasmade possible by the generous financial\nsupport of theW. M. Keck Foundation. Lastly, this work includes\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), theAustralianResearchCouncil (Australia),CNPq(Brazil),\nand SECYT (Argentina).\n\nPublished - SAJapj08.pdf
", "abstract": "We present the FIR, millimeter, and radio photometry and optical and NIR spectroscopy of a sample of 48 z ~ 1\u20133 Spitzer-selected ULIRGs with IRS MIR spectra. Our goals are to compute their bolometric emission and to determine both the presence and relative strength of their AGN and starburst components. We find that strong-PAH sources tend to have higher MIPS 160 \u03bcm and MAMBO 1.2 mm fluxes than weak-PAH sources. The depth of the 9.7 \u03bcm silicate feature does not affect MAMBO detectability. We fit the far-IR SEDs of our sample and find an average LIR ~ 7 \u00d7 10^(12)L_\u2609 for our z > 1.5 sources. Our spectral decomposition suggests that strong-PAH sources typically have ~20%-30% AGN fractions of L_(IR). The weak-PAH sources by contrast tend to have \u226570% AGN fractions, with a few sources having comparable contributions of AGN and starbursts. The optical line diagnostics support the presence of AGNs in the bulk of the weak-PAH sources. With one exception, our sources are narrow-line sources, show no obvious correspondence between the available optical extinction and the silicate feature depth, and, in two cases, show some evidence for outflows. Radio AGNs are present in both strong- and weak-PAH sources. This is supported by our sample's FIR-to-radio ratios (q) being consistently below the average value of 2.34 for local star-forming galaxies. We use survival analysis to include the lower limits given by the radio-undetected sources, arriving at (q) = 2.07 \u00b1 0.01 for our z > 1.5 sample. In total, radio and, where available, optical line diagnostics support the presence of AGNs in 57% of the z > 1.5 sources, independent of IR-based diagnostics. For higher z sources, the AGN luminosities alone are estimated to be >10^(12) L_\u2609, which, supported by the available [O III] luminosities, implies that the bulk of our sources host obscured quasars.", "date": "2008-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "683", "number": "2", "publisher": "University of Chicago Press", "pagerange": "659-682", "id_number": "CaltechAUTHORS:20090517-185509708", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090517-185509708", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max Planck Gesellschaft" }, { "agency": "Instituto Geografico Nacional (IGN)" }, { "agency": "University of California" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" }, { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "National Research Council of Canada" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)" }, { "agency": "Australian Research Council" }, { "agency": "Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq)" }, { "agency": "Secretaria de Ciencia y Tecnologia (SECYT)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/589914", "primary_object": { "basename": "SAJapj08.pdf", "url": "https://authors.library.caltech.edu/records/n9yay-50g80/files/SAJapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Sajina, Anna; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rv7pt-t6202", "eprint_id": 13696, "eprint_status": "archive", "datestamp": "2023-08-22 11:58:08", "lastmod": "2023-10-18 00:05:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "Kalliopi M." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Colbert-J-W", "name": { "family": "Colbert", "given": "James" } } ] }, "title": "HST NICMOS imaging of z ~ 2, 24 \u00b5m-selected ultraluminous infrared galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: interactions; infrared: galaxies", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 July 19; accepted 2008 February 6.\nK. D. wishes to thank Lee Armus and Lisa Storrie-Lombardi\nfor useful discussions. This work is based on observations made\nwith the NASA/ESA Hubble Space Telescope, obtained from the\ndata archive at the Space Telescope Science Institute (STScI).\nSTScI is operated by the Association of Universities for Research\nin Astronomy (AURA), Inc., under NASA contract NAS5-26555.\nIt is also based in part on observations made with the Spitzer Space\nTelescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under a contract with NASA.\nSupport for this work was provided by NASA through an award\nissued by JPL, Caltech.\n\nPublished - DASapj08.pdf
", "abstract": "We present Hubble Space Telescope NICMOSH-band imaging of 33 ultraluminous infrared galaxies (ULIRGs) at z ~ 2 that were selected from the 24 \u00b5m catalog of the Spitzer Extragalactic First Look Survey. The images reveal that at least 17 of the 33 objects are associated with interactions. Up to one-fifth of the sources in our sample could be minor mergers, whereas only two systems are merging binaries with luminosity ratio \u2264 3 : 1, which is characteristic of local ULIRGs. The rest-frame optical luminosities of the sources are of the order 10^(10)-10^(11) L\u2299 and their effective radii range from 1.4 to 4.9 kpc. The most compact sources are either those with a strong active nucleus continuum or those with a heavy obscuration in the mid-infrared regime, as determined from Spitzer Infrared Spectrograph data. The luminosity of the 7.7 \u00b5m feature produced by polycyclic aromatic hydrocarbon molecules varies significantly among compact systems, whereas it is typically large for extended systems. A bulge-to-disk decomposition performed for the six brightest (m_H < 20) sources in our sample indicates that they are best fit by disklike profiles with small or negligible bulges, unlike the bulge-dominated remnants of local ULIRGs. Our results provide evidence that the interactions associated with ultraluminous infrared activity at z ~ 2 can differ from those at z ~ 0.", "date": "2008-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "680", "number": "1", "publisher": "American Astronomical Society", "pagerange": "232-245", "id_number": "CaltechAUTHORS:DASapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:DASapj08", "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": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/587447", "primary_object": { "basename": "DASapj08.pdf", "url": "https://authors.library.caltech.edu/records/rv7pt-t6202/files/DASapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Dasyra, Kalliopi M.; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/46bga-5qd98", "eprint_id": 13396, "eprint_status": "archive", "datestamp": "2023-08-22 11:44:40", "lastmod": "2023-10-17 23:52:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kenney-J-D-P", "name": { "family": "Kenney", "given": "J. D. P." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Braun-R", "name": { "family": "Braun", "given": "R." } } ] }, "title": "Connecting far-infrared and radio morphologies of disk galaxies: Cosmic-ray electron diffusion after star formation episodes", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic rays; infrared: galaxies; radio continuum: galaxies", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 July 4; accepted 2008 January 30.\nWe wish to thank the referee, Don Cox, for his insightful\ncomments, which have greatly improved the paper. E. J. M. is\nindebted to Eric Slezak for his highly constructive comments and\ncritical remarks that helped guide the technical aspects of the\nwavelet decomposition. E. J. M. would also like to thank other\nmembers of the Spitzer Infrared Nearby Galaxies Survey (SINGS)\nteam for their invaluable contributions to the work presented here,\nespecially those of R. C. Kennicutt Jr., D. Calzetti, K. D. Gordon,\nC. W. Engelbracht, and G. Bendo. As part of the Spitzer Space\nTelescope Legacy Science Program, support was provided by\nNASA through contract 1224769 issued by the Jet Propulsion\nLaboratory, California Institute of Technology under NASA contract\n1407. E. J. M. also acknowledges support for this work provided\nby the Spitzer Science Center Visiting Graduate Student\nprogram. This research has made use of the NASA/IPAC Extragalactic\nDatabase, which is operated by JPL/Caltech, under contract\nwith NASA. This publication makes use of data products\nfrom the Two Micron All Sky Survey, which is a joint project of\nthe University of Massachusetts and IPAC/Caltech, funded by\nNASA and the National Science Foundation.\n\nPublished - MURapj08.pdf
", "abstract": "We present results on the ISM properties of 29 galaxies based on a comparison of Spitzer far-infrared and Westerbork Synthesis Radio Telescope radio continuum imagery. Of these 29 galaxies, 18 are close enough to resolve at \u227e\n to 1 kpc scales at 70 \u00b5m and 22 cm. We extend the approach of our earlier work of smoothing infrared images to approximate cosmic-ray (CR) electron spreading and thus largely reproduce the appearance of radio images. Using a wavelet analysis, we decompose each 70 \u00b5m image into one component containing the star-forming structures and a second one for the diffuse disk. The components are smoothed separately, and their combination compared to a free-free corrected 22 cm radio image; the scale lengths are then varied to best match the radio and smoothed infrared images. We find that late-type spirals having high amounts of ongoing star formation benefit most from the two-component method. We also find that the disk component dominates for galaxies having low star formation activity, whereas the structure component dominates at high star formation activity. We propose that this result arises from an age effect rather than from differences in CR electron diffusion due to varying ISM parameters. The bulk of the CR electron population in actively star-forming galaxies is significantly younger than that in less active galaxies due to recent episodes of enhanced star formation; these galaxies are observed within ~10^8 yr since the onset of the most recent star formation episode. The sample irregulars have anomalously low best-fit scale lengths for their surface brightnesses compared to the rest of the sample spirals, which we attribute to enhanced CR electron escape.", "date": "2008-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "678", "number": "2", "publisher": "American Astronomical Society", "pagerange": "828-850", "id_number": "CaltechAUTHORS:MURapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:MURapj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "Spitzer Science Center Visiting Graduate Student Program" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/587123", "primary_object": { "basename": "MURapj08.pdf", "url": "https://authors.library.caltech.edu/records/46bga-5qd98/files/MURapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Murphy, E. J.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ckjps-59e93", "eprint_id": 13692, "eprint_status": "archive", "datestamp": "2023-08-22 11:17:21", "lastmod": "2023-10-18 00:05:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brunner-G", "name": { "family": "Brunner", "given": "Gregory" } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Wolfire-M-G", "name": { "family": "Wolfire", "given": "Mark" }, "orcid": "0000-0003-0030-9510" }, { "id": "Vogel-S-N", "name": { "family": "Vogel", "given": "Stuart" } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "Eva" }, "orcid": "0000-0002-3933-7677" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Dufour-R", "name": { "family": "Dufour", "given": "Reginald" } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David" }, "orcid": "0000-0003-1545-5078" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" } ] }, "title": "Warm molecular gas in M51 : mapping the excitation temperature and mass of H_2 with the Spitzer infrared spectrograph", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (M51); galaxies: ISM; ISM: molecules", "note": "\u00a9 2008 The American Astronomical Society.\nReceived 2007 July 13; accepted 2007 October 10.\nThe author graciously acknowledges the Spitzer Science Center\nVisiting Graduate Student Fellowship program and committee\nfor providing support for this research. The author would\nlike to specifically acknowledge the program coordinators, Phil\nAppleton and Alberto Noriega-Crepso. The authors would also\nlike to thank the anonymous referee who helped to clarify our\nresults and improve our discussion. Partial support for the completion\nand preparation for publication of this study by the author\nwas provided by AURA grant GO10822.1 to Rice University.\n\nPublished - BRUapj08.pdf
", "abstract": "We have mapped the warm molecular gas traced by the H_2 S(0)-H_2 S(5) pure rotational mid-infrared emission lines over a radial strip across the nucleus and disk of M51 (NGC 5194) using the Infrared Spectrograph (IRS) on the Spitzer Space Telescope. The six H_2 lines have markedly different emission distributions. We obtained the H_2 temperature and surface density distributions by assuming a two-temperature model: a warm (T = 100\u2013300 K) phase traced by the low J [S(0)-S(2)] lines and a hot phase (T = 400\u20131000 K) traced by the high J [S(2)-S(5)] lines. The lowest molecular gas temperatures are found within the spiral arms (T ~ 155 K), while the highest temperatures are found in the inter-arm regions (T > 700 K). The warm gas surface density reaches a maximum of 11 M\u2299 pc^(\u22122) in the northwest spiral arm, whereas the hot gas surface density peaks at 0.24 M\u2299 pc^(\u22122) at the nucleus. The spatial offset between the peaks in the different phases suggests that the warm phase is more efficiently heated by star formation activity and the hot phase is more efficiently heated by nuclear activity. The warm H_2 is found in the dust lanes of M51 and is generally spatially coincident with the cold molecular gas traced by CO emission, consistent with excitation of the warm phase in dense photodissociation regions. The hot H_2 is most prominent in the nuclear region. Here, the hot H_2 coincides with [O IV] (25.89 \u03bcm) and X-ray emission indicating that shocks and/or X-rays are responsible for exciting this phase.", "date": "2008-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "675", "number": "1", "publisher": "American Astronomical Society", "pagerange": "316-329", "id_number": "CaltechAUTHORS:BRUapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BRUapj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO10822.1" }, { "agency": "Association of Universities for Research in Astronomy (AURA)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/524348", "primary_object": { "basename": "BRUapj08.pdf", "url": "https://authors.library.caltech.edu/records/ckjps-59e93/files/BRUapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Brunner, Gregory; Sheth, Kartik; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/a8sna-wkc51", "eprint_id": 14298, "eprint_status": "archive", "datestamp": "2023-08-19 22:09:53", "lastmod": "2023-10-18 16:27:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dasyra-K-M", "name": { "family": "Dasyra", "given": "K. M." } }, { "id": "Ho-Luis-C", "name": { "family": "Ho", "given": "L. C." }, "orcid": "0000-0001-6947-5846" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Ogle-P-M", "name": { "family": "Ogle", "given": "P." }, "orcid": "0000-0002-3471-981X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Peterson-B-M", "name": { "family": "Peterson", "given": "B. M." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Netzer-H", "name": { "family": "Netzer", "given": "H." } }, { "id": "Sturm-E", "name": { "family": "Sturm", "given": "E." } } ] }, "title": "High-ionization mid-infrared lines as black hole mass and bolometric luminosity indicators in active galactic nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active\u2014galaxies: kinematics and dynamics\u2014galaxies: nuclei\u2014galaxies: Seyfert\u2014infrared: galaxies\u2014quasars: emission lines", "note": "\u00a9 2008. The American Astronomical Society. \n\nReceived 2007 October 26; accepted 2007 December 19; published 2008 January 22. \n\nThis work was based on observations made with the Spitzer Space Telescope and was supported by NASA through an award issued by JPL/Caltech.\n\nPublished - DASapjl08.pdf
", "abstract": "We present relations of the black hole mass and the optical luminosity with the velocity dispersion and the luminosity of the [Ne v] and the [O iv] high-ionization lines in the mid-infrared (MIR) for 28 reverberation-mapped active galactic nuclei. We used high-resolution Spitzer Infrared Spectrograph and Infrared Space Observatory\nShort Wavelength Spectrometer data to fit the profiles of these MIR emission lines that originate from the narrow-line region of the nucleus. We find that the lines are often resolved and that the velocity dispersion of [Ne v] and [O iv] follows a relation similar to that between the black hole mass and the bulge stellar velocity dispersion found for local galaxies. The luminosity of the [Ne v] and the [O iv] lines in these sources is correlated\nwith that of the optical 5100 continuum and with the black hole mass. Our results provide a means to derive \u00b0A black hole properties in various types of active galactic nuclei, including highly obscured systems.", "date": "2008-02-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "674", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L9-L12", "id_number": "CaltechAUTHORS:20090526-101228585", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090526-101228585", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/528843", "primary_object": { "basename": "DASapjl08.pdf", "url": "https://authors.library.caltech.edu/records/a8sna-wkc51/files/DASapjl08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Dasyra, K. M.; Ho, L. C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mwxq3-vfz52", "eprint_id": 19212, "eprint_status": "archive", "datestamp": "2023-08-19 21:46:39", "lastmod": "2024-01-12 23:57:37", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "Nanyao" }, "orcid": "0000-0002-8948-1044" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Global Star Formation and Mid-Infrared Emission Features in Galaxies", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2008 Astronomical Society of the Pacific.\n\nPublished - Lu2008p8837Second_Annual_Spitzer_Science_Center_Conference_Infrared_Diagnostics_Of_Galaxy_Evolution.pdf
", "abstract": "In view of the controversy as to whether the global aromatic features in emission (AFEs) can be used as a robust tracer of the current star formation in normal galaxies, we have constructed a simple two-temperature dust emission model consisting of a cold (diffuse) component of 20K and a warm component associated with star-forming regions. Based on a large sample of star-forming galaxies with available homogeneous IRAS infrared and SCUBA sub-mm fluxes, we show that both these dust components contribute to the global AFE emission. Only for very active star-forming galaxies (e.g., with IRAS f_\u03bd(60 \u03bcm)/f_\u03bd(100 \u03bcm) > 0.6), does the star-forming component become dominant. We show that our model predictions are consistent with the Spitzer archival data in the case of the nearby galaxy NGC6946.", "date": "2008", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "46-49", "id_number": "CaltechAUTHORS:20100728-095411952", "isbn": "978-1-58381-325-6", "book_title": "The Second Annual Spitzer Science Center Conference: Infrared Diagnostics of Galaxy Evolution", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100728-095411952", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga-Ram" } }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry I." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" } } ] }, "primary_object": { "basename": "Lu2008p8837Second_Annual_Spitzer_Science_Center_Conference_Infrared_Diagnostics_Of_Galaxy_Evolution.pdf", "url": "https://authors.library.caltech.edu/records/mwxq3-vfz52/files/Lu2008p8837Second_Annual_Spitzer_Science_Center_Conference_Infrared_Diagnostics_Of_Galaxy_Evolution.pdf" }, "resource_type": "book_section", "pub_year": "2008", "author_list": "Lu, Nanyao and Helou, George" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vxs0r-sqw12", "eprint_id": 19155, "eprint_status": "archive", "datestamp": "2023-08-19 21:45:27", "lastmod": "2024-01-12 23:52:46", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pesenson-M-Z", "name": { "family": "Pesenson", "given": "Meyer" } }, { "id": "Roby-W", "name": { "family": "Roby", "given": "William" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "McCollum-B", "name": { "family": "McCollum", "given": "Bruce" } }, { "id": "Ly-Loi", "name": { "family": "Ly", "given": "Loi" } }, { "id": "Wu-Xiuqin", "name": { "family": "Wu", "given": "Xiuqin" } }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "Seppo" }, "orcid": "0000-0003-1250-8314" }, { "id": "Hartley-B", "name": { "family": "Hartley", "given": "Booth" } } ] }, "title": "Image Processing Application for Cognition (IPAC) - Traditional and Emerging Topics in Image Processing in Astronomy", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2008 Astronomical Society of the Pacific.\nM. Pesenson would like to thank W. Reach, A. Noriega-Crespo, J. Chavez, J. Ingalls and S. Carey for helpful discussions. The\nauthors would also like to thank R. Molloy and S. Tyler for helpful discussions.\nThis work is based on observations made with the Spitzer Space Telescope, which\nis operated by the Jet Propulsion Laboratory, California Institute of Technology,\nunder a contract with NASA.\n\nPublished - Pesenson2008p8719Astronomical_Data_Analysis_Software_And_Systems_Xvii.pdf
", "abstract": "A new application framework for advanced image processing for\nastronomy is presented. It implements standard two-dimensional operators,\nand recent developments in the field of non-astronomical image processing (IP),\nas well as original algorithms based on nonlinear partial differential equations\n(PDE). These algorithms are especially well suited for multi-scale astronomical\nimages since they increase signal to noise ratio without smearing localized and\ndiffuse objects. The visualization component is based on the extensive tools that\nwe developed for Spitzer Space Telescope's observation planning tool Spot and\narchive retrieval tool Leopard. It contains many common features, combines images in new and unique ways and interfaces with many astronomy data archives.\nBoth interactive and batch mode processing are incorporated. In the interactive\nmode, the user can set up simple processing pipelines, and monitor and visualize the resulting images from each step of the processing stream. The system\nis platform-independent and has an open architecture that allows extensibility\nby addition of plug-ins. This presentation addresses astronomical applications\nof traditional topics of IP (image enhancement, image segmentation) as well as\nemerging new topics like automated image quality assessment (QA) and feature extraction, which have potential for shaping future developments in the\nfield. Our application framework embodies a novel synergistic approach based\non integration of image processing, image visualization and image QA (iQA).", "date": "2008", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "97-106", "id_number": "CaltechAUTHORS:20100722-092800249", "isbn": "978-1-58381-658-5", "book_title": "Astronomical Data Analysis Software and Systems XVII", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100722-092800249", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Argyle-R-W", "name": { "family": "Argyle", "given": "R. W." } }, { "id": "Bunclark-P-S", "name": { "family": "Bunclark", "given": "P. S." } }, { "id": "Lewis-J-R", "name": { "family": "Lewis", "given": "J. R." } } ] }, "primary_object": { "basename": "Pesenson2008p8719Astronomical_Data_Analysis_Software_And_Systems_Xvii.pdf", "url": "https://authors.library.caltech.edu/records/vxs0r-sqw12/files/Pesenson2008p8719Astronomical_Data_Analysis_Software_And_Systems_Xvii.pdf" }, "resource_type": "book_section", "pub_year": "2008", "author_list": "Pesenson, Meyer; Roby, William; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x4gtw-psw19", "eprint_id": 19165, "eprint_status": "archive", "datestamp": "2023-08-19 21:45:40", "lastmod": "2024-01-12 23:52:55", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" } ] }, "title": "NGC1377: An Extragalactic Proto-Starburst", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 2008 Astronomical Society of the Pacific.\n\nPublished - Roussel2008p8836Second_Annual_Spitzer_Science_Center_Conference_Infrared_Diagnostics_Of_Galaxy_Evolution.pdf
", "abstract": "NGC1377 is the archetype of a class of galaxies called nascent starbursts, selected by their very high infrared to radio continuum flux ratios and their high dust temperatures. This nearby galaxy is an ideal test case to refine the understanding of the mechanisms of the infrared-radio correlation of star-forming galaxies; to characterize the physical conditions of an embedded starburst at its very onset; and to gain a better knowledge of the activity of a class of ultraluminous galaxies sharing the main infrared-radio properties of NGC1377. We present new data on NGC1377 obtained as part of the Spitzer Infrared Nearby Galaxies Survey (SINGS) Legacy program and discuss briefly our interpretation of the combined optical, infrared and radio properties.", "date": "2008", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "297-300", "id_number": "CaltechAUTHORS:20100722-120151278", "isbn": "978-1-58381-325-6", "book_title": "2nd Spitzer Conference: Infrared Diagnostics of Galaxy Evolution", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100722-120151278", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga-Ram" } }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry I." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" } } ] }, "corp_creators": { "items": [ "SINGS Team" ] }, "primary_object": { "basename": "Roussel2008p8836Second_Annual_Spitzer_Science_Center_Conference_Infrared_Diagnostics_Of_Galaxy_Evolution.pdf", "url": "https://authors.library.caltech.edu/records/x4gtw-psw19/files/Roussel2008p8836Second_Annual_Spitzer_Science_Center_Conference_Infrared_Diagnostics_Of_Galaxy_Evolution.pdf" }, "resource_type": "book_section", "pub_year": "2008", "author_list": "Roussel, H.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/xyjak-jbj57", "eprint_id": 17553, "eprint_status": "archive", "datestamp": "2023-08-22 10:41:38", "lastmod": "2023-10-19 23:59:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David J." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Bendo-G", "name": { "family": "Bendo", "given": "George" } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Prescott-M-K-M", "name": { "family": "Prescott", "given": "Moire K. M." } }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael W." } }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "Michele D." } }, { "id": "Bot-C", "name": { "family": "Bot", "given": "Caroline" } }, { "id": "Brinks-E", "name": { "family": "Brinks", "given": "Elias" }, "orcid": "0000-0002-7758-9699" }, { "id": "de-Blok-E", "name": { "family": "de Blok", "given": "Erwin" } }, { "id": "de-Mello-D", "name": { "family": "de Mello", "given": "Dulia" } }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "Martin" } }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "John" } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" } ] }, "title": "Star Formation in NGC 5194 (M51a). II. The Spatially Resolved Star Formation Law", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : evolution; galaxies : individual (M51a, NGC 5194); galaxies : ISM; HII regions; infrared : galaxies; stars : formation", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 April 29; accepted 2007 August 7.\nWe would like to acknowledge valuable discussions with a\nnumber of colleagues, including Ayesha Begum, Hsiao-WenChen,\nCathie Clarke, Crystal Martin, Phil Solomon, and Art Wolfe. We\nthank the anonymous referee for a careful reading of the manuscript.\nThis work is based in part on observations made with the\nSpitzer Space Telescope, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under a contract\nwith NASA. Support for this work was provided by NASA through\nan award issued by JPL/Caltech.\n\nPublished - KENapj07.pdf
", "abstract": "We have studied the relationship between the star formation rate (SFR), surface density, and gas surface density in the spiral galaxy M51a (NGC 5194), using multiwavelength data obtained as part of the Spitzer Infrared Nearby Galaxies Survey (SINGS). We introduce a new SFR index based on a linear combination of H\u03b1 emission-line and 24 \u03bcm continuum luminosities, which provides reliable extinction-corrected ionizing fluxes and SFR densities over a wide range of dust attenuations. The combination of these extinction-corrected SFR densities with aperture synthesis H I and CO maps has allowed us to probe the form of the spatially resolved star formation law on scales of 0.5-2 kpc. We find that the resolved SFR versus gas surface density relation is well represented by a Schmidt power law, which is similar in form and dispersion to the disk-averaged Schmidt law. We observe a comparably strong correlation of the SFR surface density with the molecular gas surface density, but no significant correlation with the surface density of atomic gas. The best-fitting slope of the Schmidt law varies from N = 1.37 to 1.56, with zero point and slope that change systematically with the spatial sampling scale. We tentatively attribute these variations to the effects of areal sampling and averaging of a nonlinear intrinsic star formation law. Our data can also be fitted by an alternative parameterization of the SFR surface density in terms of the ratio of gas surface density to local dynamical time, but with a considerable dispersion.", "date": "2007-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "671", "number": "1", "publisher": "American Astronomical Society", "pagerange": "333-348", "id_number": "CaltechAUTHORS:20100222-113208974", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-113208974", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/522300", "primary_object": { "basename": "KENapj07.pdf", "url": "https://authors.library.caltech.edu/records/xyjak-jbj57/files/KENapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Kennicutt, Robert C., Jr.; Calzetti, Daniela; et el." }, { "id": "https://authors.library.caltech.eduhttps://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" }, "resource_type": "article", "pub_year": "2007", "author_list": "Thilker, David A.; Boissier, Samuel; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gmjhm-47342", "eprint_id": 17724, "eprint_status": "archive", "datestamp": "2023-08-22 10:25:52", "lastmod": "2023-10-20 00:10:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "M. D." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Bot-C", "name": { "family": "Bot", "given": "C." } } ] }, "title": "Warm Molecular Hydrogen in the Spitzer SINGS Galaxy Sample", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; infrared: galaxies; infrared: ISM; ISM: lines and bands; ISM: molecules; surveys", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 November 10); received 2007 February 18; accepted for publication 2007 July 3.\n\nSupport for this work, part of the Spitzer Space Telescope Legacy\nScience Program, was provided by NASA through an award\nissued by the Jet Propulsion Laboratory, California Institute of\nTechnology under NASA contract 1407. We thank the referee for\na careful review and valued suggestions, and Adam Leroy for a\nuseful discussion.\n\nPublished - ROUapj07.pdf
", "abstract": "Results on the properties of warm molecular hydrogen in 57 normal galaxies are derived from measurements of H_2 rotational transitions, obtained as part of SINGS. This study extends previous extragalactic surveys of emission lines of H_2 to fainter and more common systems (L_(FIR) = 10^(7)-6 \u00d7 10^(10) L_\u2609). The 17 \u03bcm S(1) transition is securely detected in the nuclear regions of 86% of galaxies with stellar masses above 10^(9.5) M_\u2609. The derived column densities of warm H_2 (T \u2265 100 K), although averaged over kiloparsec-scale areas, are commensurate with values observed in resolved photodissociation regions. They amount to between 1% and >30% of the total H_2. The power emitted in the three lowest energy transitions is on average 30% of the power of the bright [Si II] cooling line (34.8 \u03bcm) and about 4 \u00d7 10^(-4) of the total infrared power for star-forming galaxies, which is consistent with excitation in PDRs. The fact that the H_2 line intensities scale tightly with the aromatic band emission, even though the average radiation field intensity varies by a factor of 10, can also be understood if both tracers originate predominantly in PDRs, either dense or diffuse. Many of the 25 LINER/Seyfert targets strongly depart from the rest of the sample, in having warmer excited H_2 and excess H_2 rotational power with respect to the dust emission. We propose a threshold in H_2-to-aromatic band power ratios, allowing the identification of low-luminosity AGNs by an excess H_2 excitation. A dominant contribution from shock heating is favored in these objects. Finally, we detect in nearly half the star-forming targets nonequilibrium ortho-to-para ratios, consistent with the effects of FUV pumping combined with incomplete ortho-para thermalization, or possibly nonequilibrium photodissociation fronts.", "date": "2007-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "669", "number": "2", "publisher": "American Astronomical Society", "pagerange": "959-981", "id_number": "CaltechAUTHORS:20100311-113933068", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100311-113933068", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "1407" } ] }, "doi": "10.1086/521667", "primary_object": { "basename": "ROUapj07.pdf", "url": "https://authors.library.caltech.edu/records/gmjhm-47342/files/ROUapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Roussel, H.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/wrnyn-egp55", "eprint_id": 13969, "eprint_status": "archive", "datestamp": "2023-08-22 10:13:27", "lastmod": "2023-10-18 16:00:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Prescott-M-K-M", "name": { "family": "Prescott", "given": "Moire K. M." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "George J." } }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "Brent A." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David J." } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice C." }, "orcid": "0000-0002-2278-9407" }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "John" } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "Thomas H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Akiyama-Sanae", "name": { "family": "Akiyama", "given": "Sanae" } }, { "id": "Sosey-M-L", "name": { "family": "Sosey", "given": "Megan L." } } ] }, "title": "The incidence of highly obscured star-forming regions in SINGS galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; galaxies: photometry; H II regions; stars: formation", "note": "\u00a9 2007 American Astronomical Society.\nPrint publication: Issue 1 (2007 October 10); received 2007 February 18; accepted for publication 2007 June 21.\nWe are grateful to Kristian Finlator and Christy Tremonti for many thoughtful discussions. M. P. was supported by an NSF Graduate Research Fellowship. 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\nwith NASA. Support for this work was provided by NASA\nthrough an award issued by JPL/Caltech. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under contract with\nthe National Aeronautics and Space Administration.\nThis publication makes use of data products from the Two\nMicron 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.\n\nPublished - PREapj07.pdf
", "abstract": "Using the new capabilities of Spitzer and extensive multiwavelength data from SINGS, it is now possible to study the infrared properties of star formation in nearby galaxies down to scales equivalent to large H II regions. We are therefore able to determine what fraction of large, infrared-selected star-forming regions in normal galaxies are highly obscured and address how much of the star formation we miss by relying solely on the optical portion of the spectrum. Employing a new empirical method for deriving attenuations of infrared-selected star-forming regions, we investigate the statistics of obscured star formation on 500 pc scales in a sample of 38 nearby galaxies. We find that the median attenuation is 1.4 mag in H\u03b1 and that there is no evidence for a substantial subpopulation of uniformly highly obscured star-forming regions. The regions in the highly obscured tail of the attenuation distribution (AH\u03b1 \u2273 3) make up only ~4% of the sample of nearly 1800 regions, although very embedded infrared sources on the much smaller scales and lower luminosities of compact and ultracompact H II regions are almost certainly present in greater numbers. The highly obscured cases in our sample are generally the bright, central regions of galaxies with high overall attenuation but are not otherwise remarkable. We also find that a majority of the galaxies show decreasing radial trends in H\u03b1 attenuation. The small fraction of highly obscured regions seen in this sample of normal, star-forming galaxies suggests that on 500 pc scales the timescale for significant dispersal or breakup of nearby, optically thick dust clouds is short relative to the lifetime of a typical star-forming region.", "date": "2007-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "668", "number": "1", "publisher": "American Astronomical Society", "pagerange": "182-202", "id_number": "CaltechAUTHORS:20090414-111750090", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090414-111750090", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/521071", "primary_object": { "basename": "PREapj07.pdf", "url": "https://authors.library.caltech.edu/records/wrnyn-egp55/files/PREapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Prescott, Moire K. M.; Kennicutt, Robert C., Jr.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8tery-z7156", "eprint_id": 16726, "eprint_status": "archive", "datestamp": "2023-08-19 21:01:22", "lastmod": "2023-10-19 22:30:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" } ] }, "title": "Spectral Mapping Reconstruction of Extended Sources", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2007 The Astronomical Society of the Pacific.\nReceived 2007 June 5; accepted 2007 August 21; published 2007 October 25.\nThe authors thank the staff of the IRS instrument support\nteam at the Spitzer Science Center, California Institute of Technology\u2014\nwith special thanks to Phil Appleton, Carl Grillmair,\nDavid Shupe, Pat Morris, Sergio Fajardo-Acosta, Patrick Ogle,\nJim Ingalls, Harry Teplitz, and Patrick Ogle\u2014for substantial\ncontinuing support and advice regarding all aspects of telescope\ncontrol, instrument calibration, pipeline behavior, and more.\nWe are also indebted to the IRS instrument team at Cornell\nUniversity\u2014in particular Jim Houck, Vassilis Charmandaris, Jeff Van Cleve, Keven Uchida, Greg Sloan, Sarah Higdon, and\nDaniel Devost\u2014for much helpful advice, discussions, calibration\nassistance, and insight into the instrument. Michael Cushing\nprovided helpful discussions regarding aspects of the algorithm\ndesign. Support for this work, part of the Spitzer Space\nTelescope Legacy Science Program, was provided by NASA\nthrough contract 1224769 issued by JPL/Caltech under contract\n1407.\n\nPublished - SMIpasp07.pdf
", "abstract": "Three\u2010dimensional spectroscopy of extended sources is typically performed with dedicated integral field spectrographs. We describe a method of reconstructing full spectral cubes, with two spatial and one spectral dimension, from rastered spectral mapping observations employing a single slit in a traditional slit spectrograph. When the background and image characteristics are stable, as is often achieved in space, the use of traditional long slits for integral field spectroscopy can substantially reduce instrument complexity over dedicated integral field designs, without loss of mapping efficiency\u2014particularly compelling when a long\u2010slit mode for single unresolved source follow\u2010up is separately required. We detail a custom flux\u2010conserving cube reconstruction algorithm, discuss issues of extended\u2010source flux calibration, and describe CUBISM, a tool that implements these methods for spectral maps obtained with the Spitzer Space Telescope's Infrared Spectrograph.", "date": "2007-10", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "119", "number": "860", "publisher": "Astronomical Society of the Pacific", "pagerange": "1133-1144", "id_number": "CaltechAUTHORS:20091117-094901174", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-094901174", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/522634", "primary_object": { "basename": "SMIpasp07.pdf", "url": "https://authors.library.caltech.edu/records/8tery-z7156/files/SMIpasp07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Smith, J. D. T.; Armus, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x557c-c6x57", "eprint_id": 16504, "eprint_status": "archive", "datestamp": "2023-08-22 09:59:15", "lastmod": "2023-10-19 22:18:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "C." }, "orcid": "0000-0003-2685-4488" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Kewley-L-J", "name": { "family": "Kewley", "given": "L." }, "orcid": "0000-0001-8152-3943" }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } }, { "id": "Sosey-M-L", "name": { "family": "Sosey", "given": "M." } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G. X." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G." } }, { "id": "Bot-C", "name": { "family": "Bot", "given": "C." } }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T." }, "orcid": "0000-0002-4939-734X" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "A." } }, { "id": "Meyer-M", "name": { "family": "Meyer", "given": "M." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Prescott-M-K-M", "name": { "family": "Prescott", "given": "M." } }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "M. W." } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "M. D." } }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" } ] }, "title": "The Calibration of Mid-Infrared Star Formation Rate Indicators", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : interactions; galaxies : ISM; galaxies : starburst; ISM : structure", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 May 1; accepted 2007 May 22.\nThe authors would like to acknowledge the anonymous referee\nfor the speedy report and for the many constructive comments\nthat have helped improve the manuscript. This work has\nbeen partially supported by the NASA HST grant GO-9360 and\nby the JPL, Caltech, contract 1224667. It is part of SINGS, The\nSpitzer Infrared Nearby Galaxies Survey, one of the Spitzer\nSpace Telescope Legacy Science Programs. This work has made\nuse of the NASA/IPAC Extragalactic Database (NED), which is\noperated by the Jet Propulsion Laboratory, California Institute of\nTechnology, under contract with the National Aeronautics and\nSpace Administration.\n\nPublished - CALapj07.pdf
", "abstract": "With the goal of investigating the degree to which the MIR emission traces the SFR, we analyze Spitzer 8 and 24 \u03bcm data of star-forming regions in a sample of 33 nearby galaxies with available HST NICMOS images in the Pa\u03b1 (1.8756 \u03bcm) emission line. The galaxies are drawn from the SINGS sample and cover a range of morphologies and a factor ~10 in oxygen abundance. Published data on local low-metallicity starburst galaxies and LIRGs are also included in the analysis. Both the stellar continuum-subtracted 8 \u03bcm emission and the 24 \u03bcm emission correlate with the extinction-corrected Pa\u03b1 line emission, although neither relationship is linear. Simple models of stellar populations and dust extinction and emission are able to reproduce the observed nonlinear trend of the 24 \u03bcm emission versus number of ionizing photons, including the modest deficiency of 24 \u03bcm emission in the low-metallicity regions, which results from a combination of decreasing dust opacity and dust temperature at low luminosities. Conversely, the trend of the 8 \u03bcm emission as a function of the number of ionizing photons is not well reproduced by the same models. The 8 \u03bcm emission is contributed, in larger measure than the 24 \u03bcm emission, by dust heated by nonionizing stellar populations, in addition to the ionizing ones, in agreement with previous findings. Two SFR calibrations, one using the 24 \u03bcm emission and the other using a combination of the 24 \u03bcm and H\u03b1 luminosities (Kennicutt and coworkers), are presented. No calibration is presented for the 8 \u03bcm emission because of its significant dependence on both metallicity and environment. The calibrations presented here should be directly applicable to systems dominated by ongoing star formation.", "date": "2007-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "666", "number": "2", "publisher": "American Astronomical Society", "pagerange": "870-895", "id_number": "CaltechAUTHORS:20091028-075614201", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091028-075614201", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-9360" }, { "agency": "NASA/JPL/Caltech", "grant_number": "1224667" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/520082", "primary_object": { "basename": "CALapj07.pdf", "url": "https://authors.library.caltech.edu/records/x557c-c6x57/files/CALapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Calzetti, D.; Kennicutt, R. C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rzhjp-de478", "eprint_id": 17715, "eprint_status": "archive", "datestamp": "2023-08-22 09:53:44", "lastmod": "2023-10-20 00:10:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "M." }, "orcid": "0000-0001-7116-9303" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Brooke-T", "name": { "family": "Brooke", "given": "T." } }, { "id": "Bhattacharya-B", "name": { "family": "Bhattacharya", "given": "B." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J. S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Barnes-J-E", "name": { "family": "Barnes", "given": "J. E." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P." }, "orcid": "0000-0003-3578-6843" }, { "id": "Carilli-C-L", "name": { "family": "Carilli", "given": "C." }, "orcid": "0000-0001-6647-3861" }, { "id": "Carollo-C-Marcella", "name": { "family": "Carollo", "given": "C. M." }, "orcid": "0000-0003-1624-7609" }, { "id": "Comastri-A", "name": { "family": "Comastri", "given": "A." }, "orcid": "0000-0003-3451-9970" }, { "id": "Daddi-Emanuele", "name": { "family": "Daddi", "given": "E." }, "orcid": "0000-0002-3331-9590" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "M." } }, { "id": "Fall-S-M", "name": { "family": "Fall", "given": "S. M." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Giavalisco-M", "name": { "family": "Giavalisco", "given": "M." }, "orcid": "0000-0002-7831-8751" }, { "id": "Hasinger-G", "name": { "family": "Hasinger", "given": "G." }, "orcid": "0000-0002-0797-0646" }, { "id": "Impey-C-D", "name": { "family": "Impey", "given": "C." } }, { "id": "Koekemoer-A-M", "name": { "family": "Koekemoer", "given": "A." }, "orcid": "0000-0002-6610-2048" }, { "id": "Le-F\u00e8vre-O", "name": { "family": "Le F\u00e8vre", "given": "O." }, "orcid": "0000-0001-5891-2596" }, { "id": "Lilly-S-J", "name": { "family": "Lilly", "given": "S." }, "orcid": "0000-0002-6423-3597" }, { "id": "Liu-Michael-C", "name": { "family": "Liu", "given": "M. C." }, "orcid": "0000-0003-2232-7664" }, { "id": "McCracken-H-J", "name": { "family": "McCracken", "given": "H. J." }, "orcid": "0000-0002-9489-7765" }, { "id": "Mobasher-B", "name": { "family": "Mobasher", "given": "B." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "A." }, "orcid": "0000-0002-7093-7355" }, { "id": "Rich-M", "name": { "family": "Rich", "given": "M." } }, { "id": "Schinnerer-E", "name": { "family": "Schinnerer", "given": "E." }, "orcid": "0000-0002-3933-7677" }, { "id": "Shopbell-P-L", "name": { "family": "Shopbell", "given": "P. L." } }, { "id": "Taniguchi-Yoshiaki", "name": { "family": "Taniguchi", "given": "Y." }, "orcid": "0000-0003-2247-3741" }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Urry-C-M", "name": { "family": "Urry", "given": "C. M." }, "orcid": "0000-0002-0745-9792" }, { "id": "Williams-J-P", "name": { "family": "Williams", "given": "J. P." }, "orcid": "0000-0001-5058-695X" } ] }, "title": "S-COSMOS: The Spitzer Legacy Survey of the Hubble Space Telescope ACS 2 deg^2 COSMOS Field I: Survey Strategy and First Analysis", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: formation; infrared: galaxies; large-scale structure of universe; surveys", "note": "\u00a9 2007 American Astronomical Society. \n\nPrint publication: Issue 1 (2007 September); received 2006 August 28; accepted for publication 2007 January 9. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through contract 1278386 issued by the JPL. It is a pleasure to acknowledge the hospitality provided by the Aspen Center for Physics where the majority of this paper was written. Additional information on the S-COSMOS Legacy Survey is available from the main COSMOSWeb site 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. We thank Guilaine Lagache for useful comments on power spectra measurements. We would also like to thank the referee for comments and suggestions which helped clarify our presentation. \n\nFacilities: HST (ACS), Spitzer (IRAC), Spitzer (MIPS)\n\nPublished - SANapjss07.pdf
", "abstract": "The COSMOS Spitzer survey (S-COSMOS) is a Legacy program (Cycles 2+3) designed to carry out a uniform deep survey of the full 2 deg^2 COSMOS field in all seven Spitzer bands (3.6, 4.5, 5.6, 8.0, 24.0, 70.0, and 160.0 \u03bcm). This paper describes the survey parameters, mapping strategy, data reduction procedures, achieved sensitivities to date, and the complete data set for future reference. We show that the observed infrared backgrounds in the S-COSMOS field are within 10% of the predicted background levels. The fluctuations in the background at 24 \u03bcm have been measured and do not show any significant contribution from cirrus, as expected. In addition, we report on the number of asteroid detections in the low Galactic latitude COSMOS field. We use the Cycle 2 S-COSMOS data to determine preliminary number counts, and compare our results with those from previous Spitzer Legacy surveys (e.g., SWIRE, GOODS). The results from this \"first analysis\" confirm that the S-COSMOS survey will have sufficient sensitivity with IRAC to detect ~L^* disks and spheroids out to z \u2273 3, and with MIPS to detect ultraluminous starbursts and AGNs out to z ~ 3 at 24 \u03bcm and out to z ~ 1.5-2 at 70 and 160 \u03bcm.", "date": "2007-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "172", "number": "1", "publisher": "American Astronomical Society", "pagerange": "86-98", "id_number": "CaltechAUTHORS:20100310-103340276", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100310-103340276", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL", "grant_number": "1278386" }, { "agency": "NASA/JPL/Caltech", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/517885", "primary_object": { "basename": "SANapjss07.pdf", "url": "https://authors.library.caltech.edu/records/rzhjp-de478/files/SANapjss07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Sanders, D. B.; Salvato, M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vjtba-xaf16", "eprint_id": 16720, "eprint_status": "archive", "datestamp": "2023-08-22 09:41:31", "lastmod": "2023-10-19 22:30:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "Philip" } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Spoon-H-W-W", "name": { "family": "Spoon", "given": "Henrik" }, "orcid": "0000-0002-8712-369X" } ] }, "title": "Spitzer Mid-Infrared Spectroscopy of Infrared Luminous Galaxies at z~2. II. Diagnostics", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : active; galaxies : high-redshift; infrared : galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 January 26; accepted 2007 April 12.\nWe would like to thank Vassilis Charmandaris, Guilaine\nLagache, and Daniel Stern for useful discussions. Many thanks\nto Kalliopi Dasyra for help with PG QSO data and useful discussions.\nWe would like to thank the anonymous referee for\nhelpful suggestions that have improved the presentation of this\npaper. This work is based on observations made with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under contract with\nNASA. Support for this work was provided by NASA through\nan award issued by JPL/Caltech. A. S. acknowledges support\nby NASA through grant 09865 from the Space Telescope Science\nInstitute, which is operated by the Association of Universities\nfor Research in Astronomy, Inc., under NASA contract\nBAS5-26555.\n\nPublished - SAJapj07.pdf
Submitted - 0704.1765v1.pdf
Erratum - Sajina2010p10227Astrophys_J.pdf
", "abstract": "We present mid-IR spectral decomposition of a sample of 48 Spitzer-selected ULIRGs spanning z ~ 1-3 and likely L_(IR) ~ 10^(12)-10^(13) L_\u2299. Our study aims at quantifying the star formation and active galactic nucleus (AGN) processes in these sources that recent results suggest have evolved strongly between the observed epoch and today. To do this, we study the mid-IR contribution of PAH emission, continuum, and extinction. About 3/4 of our sample are continuum (i.e., AGN) dominated sources, but ~60% of these show PAH emission, suggesting the presence of star formation activity. These sources have redder mid-IR colors than typical optically selected quasars. About 25% of our sample have strong PAH emission, but none are likely to be pure starbursts as reflected in their relatively high 5 \u03bcm hot dust continua. However, their steep 30-14 \u03bcm slopes suggest that star formation might dominate the total infrared luminosity. Six of our z ~ 2 sources have EW_(6.2) \u2273 0.3 \u03bcm and L_(14 \u03bcm) \u2273 10^(12) L_\u2299 (implying L_(IR) \u2273 10^(13) L_\u2299). At these luminosities, such high EW_(6.2) ULIRGs do not exist in the local universe. We find a median optical depth at 9.7 \u03bcm of <\u03c4_(9.7 \u03bcm)> = 1.4. This is consistent with local IRAS-selected ULIRGs but differs from early results on SCUBA-selected z ~ 2 ULIRGs. Similar to local ULIRGs, about 25% of our sample shows extreme obscuration (\u03c4_(9.7 \u03bcm) \u2273 3), suggesting buried nuclei. In general, we find that our sources are similar to local ULIRGs but are an order of magnitude more luminous. It is not clear whether our z ~ 2 ULIRGs are simply scaled-up versions of local ULIRGs or subject to fundamentally different physical processes.", "date": "2007-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "664", "number": "2", "publisher": "American Astronomical Society", "pagerange": "713-737", "id_number": "CaltechAUTHORS:20091117-080409038", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-080409038", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "09865" }, { "agency": "NASA", "grant_number": "BAS5-26555" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/519446", "primary_object": { "basename": "0704.1765v1.pdf", "url": "https://authors.library.caltech.edu/records/vjtba-xaf16/files/0704.1765v1.pdf" }, "related_objects": [ { "basename": "SAJapj07.pdf", "url": "https://authors.library.caltech.edu/records/vjtba-xaf16/files/SAJapj07.pdf" }, { "basename": "Sajina2010p10227Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/vjtba-xaf16/files/Sajina2010p10227Astrophys_J.pdf" } ], "resource_type": "article", "pub_year": "2007", "author_list": "Sajina, Anna; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/w61cp-5jk72", "eprint_id": 17523, "eprint_status": "archive", "datestamp": "2023-08-22 09:30:31", "lastmod": "2023-10-19 23:58:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "A." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Bot-C", "name": { "family": "Bot", "given": "C." } }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" } ] }, "title": "Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample", "ispublished": "pub", "full_text_status": "public", "keywords": "dust; extinction; galaxies : abundances; galaxies : general; galaxies : ISM; infrared : galaxies; ISM : general", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 January 16; accepted 2007 March 5.\nWe thank S. Madden and the anonymous referee for helpful\ncomments. Support for this work, part of the Spitzer Space Telescope\nLegacy Science Program, was provided by NASA through\nthe Jet Propulsion Laboratory under NASA contract 1407. B. T. D.\nwas supported in part by NSF grant AST 04-06883.\nB. T. D. is grateful to R. H. Lupton for availability of the SM\ngraphics program.\n\nPublished - DRAapj07.pdf
", "abstract": "Physical dust models are presented for 65 galaxies in SINGS that are strongly detected in the four IRAC bands and three MIPS bands. For each galaxy we estimate (1) the total dust mass, (2) the fraction of the dust mass contributed by PAHs, and (3) the intensity of the starlight heating the dust grains. We find that spiral galaxies have dust properties resembling the dust in the local region of the Milky Way, with similar dust-to-gas ratio and similar PAH abundance. The observed SEDs, including galaxies with SCUBA photometry, can be reproduced by dust models that do not require \"cold\" (T \u227e 10 K) dust. The dust-to-gas ratio is observed to be dependent on metallicity. In the interstellar media of galaxies with A_O \u2261 12 + log_(10)(O/H) > 8.1, grains contain a substantial fraction of interstellar Mg, Si, and Fe. Galaxies with A_O < 8.1 and extended H I envelopes in some cases appear to have global dust-to-gas ratios that are low for their measured oxygen abundance, but the dust-to-gas ratio in the regions where infrared emission is detected generally appears to be consistent with a substantial fraction of interstellar Mg, Si, and Fe being contained in dust. The PAH index q_(PAH), the fraction of the dust mass in the form of PAHs, correlates with metallicity. The nine galaxies in our sample with A_O < 8.1 have a median q_(PAH) = 1.0%, whereas galaxies with A_O > 8.1 have a median q_(PAH) = 3.55%. The derived dust masses favor a value X_(CO) \u2248 4 \u00d7 10^(20) cm^(-2) (K km s^(-1))^(-1) for the CO-to-H_2 conversion factor. Except for some starbursting systems (Mrk 33, Tol 89, NGC 3049), dust in the diffuse ISM dominates the IR power.", "date": "2007-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "663", "number": "2", "publisher": "American Astronomical Society", "pagerange": "866-894", "id_number": "CaltechAUTHORS:20100218-131653499", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100218-131653499", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NSF", "grant_number": "AST 04-06883" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/518306", "primary_object": { "basename": "DRAapj07.pdf", "url": "https://authors.library.caltech.edu/records/w61cp-5jk72/files/DRAapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Draine, B. T.; Dale, D. A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bqmq4-aws28", "eprint_id": 16711, "eprint_status": "archive", "datestamp": "2023-08-22 09:30:21", "lastmod": "2023-10-19 22:30:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rahman-N", "name": { "family": "Rahman", "given": "Nurur" } }, { "id": "Howell-J-H", "name": { "family": "Howell", "given": "Justin H." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Mazzarella-J-M", "name": { "family": "Mazzarella", "given": "Joseph M." }, "orcid": "0000-0002-8204-8619" }, { "id": "Buckalew-B", "name": { "family": "Buckalew", "given": "Brent" } } ] }, "title": "Exploring Infrared Properties of Giant Low Surface Brightness Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : individual (Malin 1, UGC 6614, UGC 6879; UGC 9024); galaxies : ISM galaxies : spiral; galaxies : structure", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2007 January 10; accepted 2007 March 30.\nThe anonymous referee is thanked for constructive comments\nand suggestions. We happily thank D. Dale for his model fits. We\nalso thank Y. Wu, B. R. Brandl, and J. R. Houck for helpful communications.\nWe acknowledge useful discussions from A. Blain,\nG. D. Bothun, and S. S. McGaugh on LSB galaxy populations.\nOne of us (N. R.) gratefully acknowledges the support of a Research\nAssociateship administered by Oak Ridge Associated Universities\n(ORAU) during this research. This research has made\nuse of the NASA/ IPAC Extragalactic Database (NED), which is\noperated by the Jet Propulsion Laboratory, California Institute of\nTechnology, under contract with the National Aeronautics and\nSpace Administration, and the LEDA database in France. This study\nis based on observations made with the Spitzer Space Telescope,\nwhich is operated by the Jet Propulsion Laboratory, California Institute\nof Technology, under NASA contract 1407. This study has\nmade use of data products from the Two Micron All Sky Survey,\nwhich is a joint project of the University of Massachusetts and IPAC/\nCaltech, funded by NASA and the National Science Foundation.\nThis study also acknowledges the use of data products from the\nSloan Digital Sky Survey.\n\nPublished - RAHapj07.pdf
", "abstract": "We present an analysis of Spitzer Space Telescope observations of the three low surface brightness (LSB) optical giant galaxies Malin 1, UGC 6614, and UGC 9024. Mid- and far-infrared morphology, spectral energy distributions, and integrated colors are used to derive the dust mass, dust-to-gas mass ratio, total infrared luminosity, and star formation rate (SFR). We also investigate UGC 6879, which is intermediate between high surface brightness (HSB) and LSB galaxies. The 8 \u03bcm images indicate that polycyclic aromatic hydrocarbon (PAH) molecules are present in the central regions of all three metal-poor LSB galaxies. The diffuse optical disks of Malin 1 and UGC 9024 remain undetected at mid- and far-infrared wavelengths. The dustiest of the three LSB galaxies, UGC 6614, has infrared morphology that varies significantly with wavelength; 160 \u03bcm (cool) dust emission is concentrated in two clumps on the northeast and northwest sides of a distinct ring seen in the 24 and 8 \u03bcm images (and a broken ring at 70 \u03bcm) at a radius of ~40\" (18 kpc) from the galaxy center. The 8 and 24 \u03bcm emission is cospatial with H\u03b1 emission previously observed in the outer ring of UGC 6614. The estimated dust-to-gas ratios, from less than 10^(-3) to 10^(-2), support previous indications that the LSB galaxies are relatively dust-poor compared to the HSB galaxies. The total infrared luminosities are approximately 1/3 to 1/2 the blue-band luminosities, suggesting that old stellar populations are the primary source of dust heating in these LSB objects. The SFR estimated from the infrared data ranges ~0.01-0.88 M_\u2299 yr^(-1), consistent with results from optical studies.", "date": "2007-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "663", "number": "2", "publisher": "American Astronomical Society", "pagerange": "908-923", "id_number": "CaltechAUTHORS:20091116-091302719", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091116-091302719", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Oak Ridge Associated Universities (ORAU)" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "NSF" } ] }, "doi": "10.1086/518554", "primary_object": { "basename": "RAHapj07.pdf", "url": "https://authors.library.caltech.edu/records/bqmq4-aws28/files/RAHapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Rahman, Nurur; Howell, Justin H.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/t05aw-wq036", "eprint_id": 105639, "eprint_status": "archive", "datestamp": "2023-08-19 20:14:03", "lastmod": "2024-01-15 17:05:04", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Braun-R", "name": { "family": "Braun", "given": "R." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Kenney-J-D-P", "name": { "family": "Kenney", "given": "J. D. P." } } ] }, "title": "Van der Kruit to Spitzer: a New Look at the Far\u2013Infrared\u2013Radio Correlation", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "infrared: galaxies - radio continuum: galaxies - cosmic rays: galaxies", "note": "\u00a9 2007 Springer.", "abstract": "We present an initial look at the far-infrared\u2013radio correlation within the starforming disks of four nearby, nearly face\u2013on galaxies (NGC 2403, NGC3031, NGC5194, and NGC6946). Using Spitzer MIPS imaging and WSRT radio continuum data, we are able to probe variations in the logarithmic 70 \u03bcm/22 cm (q70) flux density ratios across each disk at sub\u2013kpc scales.", "date": "2007-05-24", "date_type": "published", "publisher": "Springer", "place_of_pub": "Dordrecht", "pagerange": "409-415", "id_number": "CaltechAUTHORS:20200929-130809231", "isbn": "978-1-4020-5572-0", "book_title": "Island Universes: Structure and Evolution of Disk Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200929-130809231", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "De-Jong-R-S", "name": { "family": "De Jong", "given": "R. S." } } ] }, "corp_creators": { "items": [ "SINGS Team" ] }, "doi": "10.1007/978-1-4020-5573-7_71", "resource_type": "book_section", "pub_year": "2007", "author_list": "Murphy, E. J.; Braun, R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jey6d-04084", "eprint_id": 16755, "eprint_status": "archive", "datestamp": "2023-08-22 09:05:45", "lastmod": "2023-10-19 22:32:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Cannon-J-M", "name": { "family": "Cannon", "given": "John M." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H\u00e9l\u00e8ne" } }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "George J." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "John" } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "George H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl" } }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David J." } }, { "id": "Lee-Janice-C", "name": { "family": "Lee", "given": "Janice" }, "orcid": "0000-0002-2278-9407" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "Aigen" } }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "Martin J." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael W." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Brinks-E", "name": { "family": "Brinks", "given": "Elias" }, "orcid": "0000-0002-7758-9699" }, { "id": "de-Blok-W-J-G", "name": { "family": "de Blok", "given": "W. J. G." } }, { "id": "Bigiel-F", "name": { "family": "Bigiel", "given": "Frank" } }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "Michele D." } } ] }, "title": "Dust and Atomic Gas in Dwarf Irregular Galaxies of the M81 Group: The SINGS and THINGS View", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; galaxies: individual (DDO 53, DDO 165, Holmberg I, Holmberg II, IC 2574, M81 dwA, M81 dwB); galaxies: irregular; galaxies: ISM; infrared: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 1 (2007 May 20); received 2006 September 26; accepted for publication 2007 February 12.\n\nSome of the data presented here are part of the Spitzer Space\nTelescope Legacy Science Program The Spitzer Nearby Galaxies\nSurvey (SINGS), which was made possible by NASA through\ncontract 1224769 issued by JPL/Caltech under NASA contract\n1407. This work was also supported in part by NSF grant AST\n04-06883.\n\nPublished - WALapj07.pdf
", "abstract": "We present observations of the dust and atomic gas phase in seven dwarf irregular galaxies of the M81 group from the Spitzer SINGS and VLA THINGS surveys. The Spitzer observations provide a first glimpse of the nature of the nonatomic ISM in these metal-poor (Z ~ 0.1 Z_\u2609), quiescent (SFR ~ 0.001-0.1 M_\u2609 yr^(-1)) dwarf galaxies. Most detected dust emission is restricted to H I column densities >1 \u00d7 10^(21) cm^(-2), and almost all regions of high H I column density (>2.5 \u00d7 10^(21) cm^(-2)) have associated dust emission. Spitzer spectroscopy of two regions in the brightest galaxies (IC 2574 and Holmberg II) show distinctly different spectral shapes and aromatic features, although the galaxies have comparable gas-phase metallicities. This result emphasizes that the strength of the aromatic features is not a simple linear function of metallicity. We estimate dust masses of ~10^(4)-10^(6) M_\u2609 for the M81 dwarf galaxies, resulting in an average dust-to-gas ratio (M_(dust)/M_(H I)) of ~3 \u00d7 10^(-4) (1.5 \u00d7 10^(-3) if only the H I that is associated with dust emission is considered); this is an order of magnitude lower than the typical value derived for the SINGS spirals. The dwarf galaxies are underluminous per unit star formation rate at 70 \u03bcm as compared to the more massive galaxies in SINGS by a factor of ~2. However, the average 70/160 \u03bcm ratio in the sample dwarf galaxies is higher than what is found in the other galaxies of the SINGS sample. This can be explained by a combination of a lower dust content in conjunction with a higher dust temperature in the dwarfs.", "date": "2007-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "661", "number": "1", "publisher": "American Astronomical Society", "pagerange": "102-114", "id_number": "CaltechAUTHORS:20091119-084804447", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091119-084804447", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 04-06883" }, { "agency": "NASA", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/514807", "primary_object": { "basename": "WALapj07.pdf", "url": "https://authors.library.caltech.edu/records/jey6d-04084/files/WALapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Walter, Fabian; Cannon, John M.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zkvej-5gc68", "eprint_id": 16502, "eprint_status": "archive", "datestamp": "2023-08-22 09:00:59", "lastmod": "2023-10-19 22:18:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Caputi-K-I", "name": { "family": "Caputi", "given": "K. I." }, "orcid": "0000-0001-8183-1460" }, { "id": "Lagache-Guilaine", "name": { "family": "Lagache", "given": "G." }, "orcid": "0000-0003-1492-2519" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Dole-H", "name": { "family": "Dole", "given": "H." } }, { "id": "Bavouzet-N", "name": { "family": "Bavouzet", "given": "N." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Reddy-N-A", "name": { "family": "Reddy", "given": "N." }, "orcid": "0000-0001-9687-4973" } ] }, "title": "The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function; infrared: galaxies", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 October 11; accepted 2007 January 8.\n\nThis paper is based on observations made with the Spitzer Observatory, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Also based on observations made with the Advanced Camera for Surveys on board the Hubble Space Telescope operated by NASA/ ESA and with the Infrared Spectrometer and Array Camera on the ''Antu'' Very Large Telescope operated by the European Southern Observatory in Cerro Paranal, Chile, and which form part of the publicly available GOODS data sets. We thank the GOODS teams for providing reduced data products. We are grateful to He\u00b4ctor Flores and Francois Hammer, for providing us additional spectroscopic redshifts for the GOODS/ CDF-S; Jiasheng Huang, for sending us the results of his 8 m LF at z 0 before publication; and Dieter Lutz and Pablo Perez-Gonzalez, for providing us with some of their published results in electronic format.We thank the anonymous referee for helpful comments and suggestions. K. I. C. and G. L. thank the Infrared Processing and Analysis Center (IPAC) at Caltech for hospitality while part of this work was being done. K. I. C. acknowledges CNES and CNRS funding.\n\nPublished - CAPapj07.pdf
", "abstract": "We present the rest-frame 8 \u00b5m LF at redshifts z = 1 and ~ 2, computed from Spitzer 24 \u00b5m\u2013selected galaxies in the GOODS fields over an area of 291 arcmin^2. Using classification criteria based on X-ray data and IRAC colors, we identify the AGNs in our sample. The rest-frame 8 \u00b5m LFs for star-forming galaxies at redshifts z = 1 and ~ 2 have the same shape as at z ~ 0, but with a strong positive luminosity evolution. The number density of star-forming galaxies with log_(10)(vL^8_v^(\u00b5m)) > 11 increases by a factor >250 from redshift z ~ 0 to 1 and is basically the same at z = 1 and ~ 2. The resulting rest-frame 8 \u00b5m luminosity densities associated with star formation at z = 1 and ~ 2 are more than 4 and 2 times larger than at z ~ 0, respectively. We also compute the total rest-frame 8 \u00b5m LF for star-forming galaxies and AGNs at z ~ 2 and show that AGNs dominate its bright end, which is well described by a power law. Using a new calibration based on Spitzer star-forming galaxies at 0 < z < 0.6 and validated at higher redshifts through stacking analysis, we compute the bolometric IR LF for star-forming galaxies at z = 1 and ~ 2. We find that the respective bolometric IR luminosity densities are (1.2 \u00b1 0.2) \u00d7 10^9 and (6.6^(+1.2)_(-1.0)) \u00d7 10^8 L_\u2299 Mpc^(-3), in agreement with previous studies within the error bars. At z ~ 2, around 90% of the IR luminosity density associated with star formation is produced by luminous and ultraluminous IR galaxies, with the two populations contributing in roughly similar amounts. Finally, we discuss the consistency of our findings with other existing observational results on galaxy evolution.", "date": "2007-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "660", "number": "1", "publisher": "American Astronomical Society", "pagerange": "97-116", "id_number": "CaltechAUTHORS:20091027-144736801", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091027-144736801", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/512667", "primary_object": { "basename": "CAPapj07.pdf", "url": "https://authors.library.caltech.edu/records/zkvej-5gc68/files/CAPapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Caputi, K. I.; Lagache, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/svwjs-8ey12", "eprint_id": 16482, "eprint_status": "archive", "datestamp": "2023-08-22 08:54:42", "lastmod": "2023-10-19 22:17:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Conselice-C-J", "name": { "family": "Conselice", "given": "C. J." }, "orcid": "0000-0003-1949-7638" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "S." }, "orcid": "0000-0003-1250-8314" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "R. G." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "The Role of Galaxy Interactions and Mergers in Star Formation at z \u2264 1.3: Mid-Infrared Properties in the Spitzer First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : evolution; galaxies : formation; galaxies : interactions; galaxies : starburst", "note": "\u00a9 2007 The American Astronomical Society.\nReceived 2006 August 20; accepted 2006 December 21.\nWe would like to thank H. Shim, M. Im, R. Chary, and C. Borys\nfor their contributions to this work, V. Charmandaris for useful\nsuggestions, and the anonymous referee for valuable comments\nthat improved the clarity of the paper. This work is based on observations\nmade with the Spitzer Observatory, which is operated\nby the Jet Propulsion Laboratory, California Institute of Technology,\nunder NASA contract 107. Support for this work was provided\nin part by the Spitzer Graduate Student Fellowship program\nand an Ontario Graduate Scholarship in Science and Technology.\nThe authors wish to recognize and acknowledge the very significant\ncultural role and reverence that the summit of Mauna Kea\nhas always had within the indigenous Hawaiian community. We\nare most fortunate to have the opportunity to conduct observations\nfrom this mountain.\n\nPublished - BRIapj07a.pdf
", "abstract": "By combining the 0.12 deg2 F814W Hubble Space Telescope (HST) and Spitzer MIPS 24 \u03bcm imaging in the First Look Survey (FLS), we investigate the properties of interacting and merging mid-infrared bright and faint sources at 0.2 \u2264 z \u2264 1.3. We find a marginally significant increase in the pair fraction for MIPS 24 \u03bcm detected, optically selected close pairs, with a pair fraction of 0.25 \u00b1 0.10 at z ~ 1, in contrast to 0.11 \u00b1 0.08 at z ~ 0.4, while galaxies below our 24 \u03bcm MIPS detection limit show a pair fraction consistent with zero at all redshifts. In addition, 24 \u03bcm detected galaxies with fluxes \u2265 0.1 mJy are on average 5 times more likely to be in a close galaxy pair in the range 0.2 \u2264 z \u2264 1.3 than galaxies below this flux limit. Using the 24 \u03bcm flux to derive the total far-IR luminosity, we find that paired galaxies (early-stage mergers) are responsible for 27% \u00b1 9% of the IR luminosity density resulting from star formation at z ~ 1, while morphologically classified (late stage) mergers make up 34% \u00b1 11%. This implies that 61% \u00b1 14% of the infrared luminosity density and, in turn, ~40% of the star formation rate density at z ~ 1 can be attributed to galaxies at some stage of a major merger or interaction. We argue that close pairs/mergers in a LIRG/ULIRG phase become increasingly important contributors to the IR luminosity and star formation rate density of the universe at z > 0.7.", "date": "2007-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "659", "number": "2", "publisher": "American Astronomical Society", "pagerange": "931-940", "id_number": "CaltechAUTHORS:20091026-143517879", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091026-143517879", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "107" }, { "agency": "Spitzer Graduate Student Fellowship" }, { "agency": "Ontario Graduate Scholarship in Science and Technology" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/512029", "primary_object": { "basename": "BRIapj07a.pdf", "url": "https://authors.library.caltech.edu/records/svwjs-8ey12/files/BRIapj07a.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Bridge, C. R.; Appleton, P. N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/bchz0-eaj94", "eprint_id": 16725, "eprint_status": "archive", "datestamp": "2023-08-22 08:50:25", "lastmod": "2023-10-19 22:30:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "Anna" }, "orcid": "0000-0002-1917-1200" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "Phil" } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "Harry" }, "orcid": "0000-0002-7064-5424" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David" }, "orcid": "0000-0003-1924-1122" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Spitzer Mid-Infrared Spectroscopy of Infrared Luminous Galaxies at z ~ 2. I. The Spectra", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 April 1); received 2006 October 13; accepted for publication 2006 December 4.\n\nWe would like to thank many helpful discussions with Henrik\nSpoon, Tom Soifer, and Guilaine Lagache. Support for this work\nwas provided by NASA through an award issued by JPL/Caltech.\nA. Sajina acknowledges support through NASA grant 09865 from\nthe Space Telescope Science Institute, which is operated by the\nAssociation of Universities for Research in Astronomy, Inc.,\nunder NASA contract BAS5-26555.\n\nPublished - YANapj07a.pdf
", "abstract": "We present the mid-infrared spectra obtained with the Spitzer IRS for 52 sources, selected as infrared luminous, z \u2273 1 candidates in the Extragalactic First Look Survey. The sample selection criteria are f_(24 \u03bcm) \u2273 0.9 mJy, \u03bdf_\u03bd(24 \u03bcm)/\u03bdf_\u03bd(8 \u03bcm) \u2273 3.16, and \u03bdf_\u03bd(24 \u03bcm)/\u03bdf_\u03bd(0.7 \u03bcm) \u2273 10. Of the 52 spectra, 47 (90%) produced measurable redshifts based solely on the mid-IR spectral features, with 35/47 (74%) at 1.5 \u2272 z \u2272 3.2. Keck spectroscopy of a subsample (17/47) agrees with the mid-IR redshift measurements. The observed spectra fall into three categories: (1) 33% (17/52) have strong PAH emission and are probably powered by star formation with total IR luminosity roughly a factor of 5 higher than the local starburst ULIRGs; (2) 33% (17/52) have only deep silicate absorption at 9.8 \u03bcm, indicatiing deeply embedded dusty systems\u2014these data alone cannot determine the energetic nature of the heating sources in these systems; and (3) the remaining 34% are mid-IR continuum-dominated systems with weak PAH emission and/or silicate absorption. This subsample is probably AGNs. We derived monochromatic, rest-frame 5.8 \u03bcm, continuum luminosities (\u03bdL_\u03bd), ranging from 10^(10.3) to 10^(12.6) L_\u2609. Our spectra have mid-IR slope \u03b1_(5-15 \u03bcm) \u2273 2.1, much redder than the median value of 1.3 for the optically selected PG quasars. From the silicate absorption feature, we estimate that roughly two-thirds of the sample have optical depth \u03c4_(9.8 \u03bcm) > 1. Their L_(1600 \u00c5) and L_(IR) suggest that our sample is among the most luminous and most dust-enshrouded systems of its epoch. Our study has revealed a significant population of dust-enshrouded galaxies at z ~ 2, whose enormous energy output, comparable to that of quasars, is generated by AGNs, as well as starbursts. This IR-luminous population has very little overlap with submillimeter and UV-selected populations.", "date": "2007-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "658", "number": "2", "publisher": "American Astronomical Society", "pagerange": "778-793", "id_number": "CaltechAUTHORS:20091117-094832114", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-094832114", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL/Caltech" }, { "agency": "NASA", "grant_number": "09865" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/511516", "primary_object": { "basename": "YANapj07a.pdf", "url": "https://authors.library.caltech.edu/records/bchz0-eaj94/files/YANapj07a.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Yan, Lin; Sajina, Anna; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/gc4qe-dyd17", "eprint_id": 17453, "eprint_status": "archive", "datestamp": "2023-08-22 08:35:05", "lastmod": "2023-10-19 23:54:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "A." } }, { "id": "Malhorta-S", "name": { "family": "Malhorta", "given": "S." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" } ] }, "title": "The Mid-Infrared Spectrum of Star-forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: ISM; infrared: galaxies; techniques: spectroscopic", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 February 20); received 2006 May 5; accepted for publication 2006 October 29.\n\nThe authors thank H. Spoon for assistance with spline-based\ntechniques, K. Masters for early access to her updated local flow\nmodel, C. Markwardt for his indispensable IDL L-M fitting\npackage, J. Chiar, E. Peeters, C. Papovich,D. Elbaz, and R. Chary\nfor helpful discussions, and an anonymous referee for many\nuseful suggestions. This work made use of the NASA/ IPAC\nExtragalactic Database (NED), operated by JPL/Caltech, under\ncontract with NASA. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through contract 1224769 issued by JPL/Caltech under contract 1407. B. T. D. has been partially supported by NSF grant AST 04-06883.\n\nPublished - SMIapj07.pdf
", "abstract": "We present a sample of low-resolution 5-38 \u03bcm Spitzer IRS spectra of the inner few square kiloparsecs of 59 nearby galaxies spanning a large range of star formation properties. A robust method for decomposing mid-infrared galaxy spectra is described and used to explore the behavior of PAH emission and the prevalence of silicate dust extinction. Evidence for silicate extinction is found in ~1/8 of the sample, at strengths that indicate that most normal galaxies undergo A_V \u2272 3 mag averaged over their centers. The contribution of PAH emission to the total infrared power is found to peak near 10% and extend up to ~20% and is suppressed at metallicities Z \u2272 Z_\u2609/4, as well as in low-luminosity AGN environments. Strong interband PAH feature strength variations (2-5 times) are observed, with the presence of a weak AGN and, to a lesser degree, increasing metallicity shifting power to the longer wavelength bands. A peculiar PAH emission spectrum with markedly diminished 5-8 \u03bcm features arises among the sample solely in systems with relatively hard radiation fields harboring low-luminosity AGNs. The AGNs may modify the emitting grain distribution and provide the direct excitation source of the unusual PAH emission, which cautions against using absolute PAH strength to estimate star formation rates in systems harboring active nuclei. Alternatively, the low star formation intensity often associated with weak AGNs may affect the spectrum. The effect of variations in the mid-infrared spectrum on broadband infrared surveys is modeled and points to more than a factor of 2 uncertainty in results that assume a fixed PAH emission spectrum, for redshifts z = 0-2.5.", "date": "2007-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "656", "number": "2", "publisher": "American Astronomical Society", "pagerange": "770-791", "id_number": "CaltechAUTHORS:20100211-104124267", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100211-104124267", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "JPL/Caltech", "grant_number": "1407" }, { "agency": "NSF", "grant_number": "AST 04-06883" } ] }, "doi": "10.1086/510549", "primary_object": { "basename": "SMIapj07.pdf", "url": "https://authors.library.caltech.edu/records/gc4qe-dyd17/files/SMIapj07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "Smith, J. D. T.; Draine, B. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://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" } ], "resource_type": "article", "pub_year": "2007", "author_list": "Dale, D. A.; Gil de Paz, A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7kqd3-prm55", "eprint_id": 106070, "eprint_status": "archive", "datestamp": "2023-08-19 19:24:07", "lastmod": "2024-01-15 18:13:30", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael" } }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "Michele D." } }, { "id": "Vogel-S-N", "name": { "family": "Vogel", "given": "Stuart N." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David J." } }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "Martin" } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "Claus" }, "orcid": "0000-0003-2685-4488" }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "Sangeeta" }, "orcid": "0000-0002-9226-5350" }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "George H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Rieke-M-J", "name": { "family": "Rieke", "given": "Marcia J." }, "orcid": "0000-0002-7893-6170" } ] }, "title": "Sings observations of spiral galaxies - Evidence for secular evolution", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "galaxies: structure - galaxies: ISM - dust, extinction - infrared: gala", "note": "\u00a9 2007 Springer.", "abstract": "One process in the secular evolution of galaxies is the formation of pseudo-bulges. The formation of these pseudo-bulges requires the inflow of gas to smaller radii. If the inflow rate is faster than the rate of star formation, a central concentration of gas will form. In this paper we present radial profiles of stellar and 8 micron emission from Polycyclic Aromatic Hydrocarbons (PAHs) for 11 spiral galaxies to investigate whether the interstellar medium in these galaxies contains a central concentration above that expected from the exponential disk. We find that in five of the 11 galaxies there is a central excess in the 8 micron and CO emission above the inner extrapolation of an exponential disk. In particular, all four barred galaxies in the sample have strong central excesses in both 8 micron and CO emission. This correlation suggests that the excess seen in the CO profiles is, in general, not simply due to a radial increase in the CO emissivity.", "date": "2007", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "341-346", "id_number": "CaltechAUTHORS:20201014-145552562", "isbn": "978-1-4020-5572-0", "book_title": "Island Universes: Structure and Evolution of Disk Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201014-145552562", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "contributors": { "items": [ { "id": "de-Jong-R-S", "name": { "family": "de Jong", "given": "R. S." } } ] }, "doi": "10.1007/978-1-4020-5573-7_58", "resource_type": "book_section", "pub_year": "2007", "author_list": "Regan, Michael; Thornley, Michele D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/cad73-3y326", "eprint_id": 24269, "eprint_status": "archive", "datestamp": "2023-08-22 07:45:53", "lastmod": "2023-10-23 20:26:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rahman-N", "name": { "family": "Rahman", "given": "Nurur" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Mazzarella-J-M", "name": { "family": "Mazzarella", "given": "Joseph M." }, "orcid": "0000-0002-8204-8619" } ] }, "title": "Probing Cool and Warm Infrared Galaxies Using Photometric and Structural Measures", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: general; galaxies: spiral; galaxies: starburst; galaxies: structure", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2006 July 10; accepted 2006 August 16.\n\nWe thank the referee Jim Houck for insightful comments, and\nThomas Jarrett for many useful communications. N. R. thanks\nRanga Ram Chary, Roc Cutri, Justin Howell, Guilain Lagache,\nSeppo Laine, Naveen Reddy, Kevin Xu, Min Su Yun, and Zang\nWang for discussions. N. R. gratefully acknowledges the support of a research associateship administered by the National Research Council (up to 2005 December) and the Oak Ridge Associated Universities (currently) during this research. This study 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, and the LEDA database in France.\n\nPublished - RAHapj06.pdf
", "abstract": "We have analyzed a sample of nearby cool and warm infrared (IR) galaxies using photometric and structural parameters. The set of measures include far-infrared color [C = log(S_(60 \u03bcm)/S_(100 \u03bcm))], total IR luminosity (L_TIR), radio surface brightness, and radio, near-infrared, and optical sizes. In a given luminosity range cool and warm galaxies are considered as those sources that are found approximately 1 \u03c3 below and above the mean color in the far-infrared C-L_TIR diagram. We find that galaxy radio surface brightness is well correlated with color whereas size is less well correlated with color. Our analysis indicates that IR galaxies that are dominated by cool dust are large, massive spirals that are not strongly interacting or merging and presumably the ones with the least active star formation. Dust in these cool objects is less centrally concentrated than in the more typical luminous and ultraluminous IR galaxies that are dominated by warm dust. Our study also shows that low-luminosity early-type unbarred and transitional spirals are responsible for the large scatter in the C-LTIR diagram. Among highly luminous galaxies, late-type unbarred spirals are predominately warm, and early-type unbarred and barred spirals are systematically cooler. We highlight the significance of the C-L_TIR diagram in terms of local and high-redshift submillimeter galaxies.", "date": "2006-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "652", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1068-1076", "id_number": "CaltechAUTHORS:20110630-105626479", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110630-105626479", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Research Council" } ] }, "doi": "10.1086/508566", "primary_object": { "basename": "RAHapj06.pdf", "url": "https://authors.library.caltech.edu/records/cad73-3y326/files/RAHapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Rahman, Nurur; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/67syz-41t65", "eprint_id": 24578, "eprint_status": "archive", "datestamp": "2023-08-22 07:45:58", "lastmod": "2023-10-23 23:28:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael W." } }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "Michele D." } }, { "id": "Vogel-S-N", "name": { "family": "Vogel", "given": "Stuart N." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David J." } }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "Martin" } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "Brent" } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "Claus" }, "orcid": "0000-0003-2685-4488" }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "Sangeeta" }, "orcid": "0000-0002-9226-5350" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric" }, "orcid": "0000-0001-7089-7325" }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "George H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Rieke-M-J", "name": { "family": "Rieke", "given": "Marcia J." }, "orcid": "0000-0002-7893-6170" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" } ] }, "title": "The Radial Distribution of the Interstellar Medium in Disk Galaxies: Evidence for Secular Evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (NGC 628, NGC 3351, NGC 3521, NGC 3627, NGC 4321, NGC 4736, NGC 4826, NGC 5055, NGC 5194, NGC 6946, NGC 7331); galaxies: ISM; galaxies: structure; infrared: galaxies", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2005 December 21; accepted 2006 April 24.\n\nIt is a pleasure to acknowledge our SSC liaison scientist, Nancy Silbermann, for her capable assistance throughout the planning and early science phases of the SINGS project. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through contract [1224769] issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407.\n\nPublished - REGapj06.pdf
", "abstract": "One possible way for spiral galaxies to internally evolve would be for gas to flow to the center and form stars in a central disk (pseudo-bulge). If the inflow rate is faster than the rate of star formation, a central concentration of gas will form. In this paper we present radial profiles of stellar and 8 \u03bcm emission from polycyclic aromatic hydrocarbons (PAHs) for 11 spiral galaxies to investigate whether the interstellar medium in these galaxies contains a central concentration above that expected from the exponential disk. In general, we find that the two-dimensional CO and PAH emission morphologies are similar, and that they exhibit similar radial profiles. We find that in 6 of the 11 galaxies there is a central excess in the 8 \u03bcm and CO emission above the inward extrapolation of an exponential disk. In particular, all four barred galaxies in the sample have strong central excesses in both 8 \u03bcm and CO emission. These correlations suggest that the excess seen in the CO profiles is, in general, not simply due to a radial increase in the CO emissivity. In the inner disk, the ratio of the stellar to the 8 \u03bcm radial surface brightness is similar for 9 of the 11 galaxies, suggesting a physical connection between the average stellar surface brightness and the average gas surface brightness at a given radius. We also find that the ratio of the CO to 8 \u03bcm PAH surface brightness is consistent over the sample, implying that the 8 \u03bcm PAH surface brightness can be used as an approximate tracer of the interstellar medium.", "date": "2006-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "652", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1112-1121", "id_number": "CaltechAUTHORS:20110728-093151102", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110728-093151102", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/505382", "primary_object": { "basename": "REGapj06.pdf", "url": "https://authors.library.caltech.edu/records/67syz-41t65/files/REGapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Regan, Michael W.; Thornley, Michele D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/87cw6-xr319", "eprint_id": 22269, "eprint_status": "archive", "datestamp": "2023-08-22 07:37:10", "lastmod": "2023-10-23 15:51:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "George J." } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David" } }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "Aigen" } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Prescott-M-K-M", "name": { "family": "Prescott", "given": "Moire K. M." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David T." }, "orcid": "0000-0003-1545-5078" } ] }, "title": "The Spectral Energy Distribution of Dust Emission in the Edge-on spiral galaxy NGC 4631 as seen with Spitzer and the James Clerk Maxwell telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 4631); galaxies: ISM; infrared: galaxies", "note": "\u00a9 2006 The American Astronomical Society. Received 2006 May 19; accepted 2006 July 27. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through contract 1224769 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. B.T.D. was supported in part by NSF grant AST 04-06833. A.L. is supported by the University of Missouri Summer Research Fellowship, the University of Missouri Research Board, and NASA/Spitzer Theory Programs.\nFacilities: Spitzer (IRAC,MIPS), JCMT(SCUBA)\n\nPublished - BENapj06b.pdf
", "abstract": "We explore variations in dust emission within the edge-on Sd spiral galaxy NGC 4631 using 3.6-160 \u03bcm Spitzer Space Telescope data and 450-850 \u03bcm JCMT data with the goals of understanding the relation between PAHs and dust emission, studying the variations in the colors of the dust emission, and searching for possible excess submillimeter emission compared to what is expected from dust models extrapolated from far-infrared wavelengths. The 8 \u03bcm PAH emission correlates best with 24 \u03bcm hot dust emission on 1.7 kpc scales, but the relation breaks down on 650 pc scales, possibly because of differences in the mean free paths between photons that excite the PAHs and photons that heat the dust and possibly because the PAHs are destroyed by the hard radiation fields within some star formation regions. The ratio of 8 \u03bcm PAH emission to 160 \u03bcm cool dust emission appears to vary as a function of radius. The 70 \u03bcm/160 \u03bcm and 160 \u03bcm/450 \u03bcm flux density ratios are remarkably constant even though the surface brightnesses vary by factors of 25, which suggests that the emission is from dust heated by a nearly uniform radiation field. Globally, we find an excess of 850-1230 \u03bcm emission relative to what would be predicted by dust models. The 850 \u03bcm excess is highest in regions with low 160 \u03bcm surface brightnesses, although the magnitude depends on the model fit to the data. We rule out variable emissivity functions or ~4 K dust as the possible origins of this 850 \u03bcm emission, but we do discuss the other possible mechanisms that could produce the emission.", "date": "2006-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "652", "number": "1", "publisher": "American Astronomical Society", "pagerange": "283-305", "id_number": "CaltechAUTHORS:20110217-072843228", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110217-072843228", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1244769" }, { "agency": "NASA/JPL", "grant_number": "1407" }, { "agency": "NSF", "grant_number": "AST 04-06833" }, { "agency": "University of Missouri" }, { "agency": "NASA/Spitzer Theory Programs" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/508057", "primary_object": { "basename": "BENapj06b.pdf", "url": "https://authors.library.caltech.edu/records/87cw6-xr319/files/BENapj06b.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Bendo, George J.; Dale, Daniel A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/71f4c-4tg32", "eprint_id": 18847, "eprint_status": "archive", "datestamp": "2023-08-22 06:18:52", "lastmod": "2023-10-20 19:07:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cannon-J-M", "name": { "family": "Cannon", "given": "John M." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "George J." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "Claus" }, "orcid": "0000-0003-2685-4488" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "Brent A." } }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David J." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "Thomas H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "Aigen" } }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "Martin J." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael W." } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "George H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Rieke-M-J", "name": { "family": "Rieke", "given": "Marcia J." }, "orcid": "0000-0002-7893-6170" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H\u00e9l\u00e8ne" } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "Michele D." } } ] }, "title": "Warm Dust and Spatially Variable Polycyclic Aromatic Hydrocarbon Emission in the Dwarf Starburst Galaxy NGC 1705", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; galaxies: individual (NGC 1705); galaxies: irregular; galaxies: ISM; infrared: galaxies", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2005 October 12; accepted 2006 April 24.\n\nThe Spitzer Space Telescope Legacy Science Program ''The\nSpitzer Nearby Galaxies Survey'' was made possible by NASA\nthrough contract 1224769 issued by JPL/Caltech under NASA\ncontract 1407. The authors thank Henry Lee for helpful discussions,\nGerhardt Meurer for providing the H i image used in our\nanalysis, and the anonymous referee for an exceptionally detailed\nreport that helped to improve the manuscript. This research has\nmade use of the NASA/IPAC Extragalactic Database (NED),\nwhich is operated by the Jet Propulsion Laboratory, California\nInstitute of Technology, under contract with the National Aeronautics\nand Space Administration, and NASA's Astrophysics\nData System.\n\nPublished - CANapj06.pdf
", "abstract": "We present Spitzer observations of the nearby dwarf starburst galaxy NGC 1705 obtained as part of the Spitzer Infrared Nearby Galaxies Survey. The galaxy morphology is very different shortward and longward of ~5 \u03bcm: optical and short-wavelength IRAC imaging shows an underlying red stellar population, with the central super star cluster (SSC) dominating the luminosity; longer wavelength IRAC and MIPS imaging reveals warm dust emission arising from two off-nuclear regions that are offset by ~250 pc from the SSC and that dominate the far-IR flux of the system. These regions show little extinction at optical wavelengths. The galaxy has a relatively low global dust mass (~2 \u00d7 10^5 M_\u2609, implying a global dust-to-gas mass ratio ~2-4 times lower than the Milky Way average, roughly consistent with the metallicity decrease). The off-nuclear dust emission appears to be powered by photons from the same stellar population responsible for the excitation of the observed H\u03b1 emission; these photons are unassociated with the SSC (although a contribution from embedded sources to the IR luminosity of the off-nuclear regions cannot be ruled out). Low-resolution IRS spectroscopy shows moderate-strength PAH emission in the 11.3 \u03bcm band in the more luminous eastern peak; no PAH emission is detected in the SSC or the western dust emission complex. There is significant diffuse emission in the IRAC 8 \u03bcm band after starlight has been removed by scaling shorter wavelength data; the fact that IRS spectroscopy shows spatially variable PAH emission strengths compared to the local continuum within this diffuse gas suggests caution in the interpretation of IRAC diffuse 8 \u03bcm emission as arising from PAH carriers alone. The nebular metallicity of NGC 1705 falls at the transition level of ~0.35 Z_\u2609 found by Engelbracht and collaborators, below which PAH emission is difficult to detect; the fact that a system at this metallicity shows spatially variable PAH emission demonstrates the complexity of interpreting diffuse 8 \u03bcm emission in galaxies. NGC 1705 deviates significantly from the canonical far-infrared versus radio correlation, having significant far-infrared emission but no detected radio continuum.", "date": "2006-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "647", "number": "1", "publisher": "American Astronomical Society", "pagerange": "293-302", "id_number": "CaltechAUTHORS:20100629-095228088", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100629-095228088", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/505339", "primary_object": { "basename": "CANapj06.pdf", "url": "https://authors.library.caltech.edu/records/71f4c-4tg32/files/CANapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Cannon, John M.; Smith, John-David T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1fm7x-k0d96", "eprint_id": 5941, "eprint_status": "archive", "datestamp": "2023-08-22 06:15:46", "lastmod": "2023-10-23 17:18:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D." }, "orcid": "0000-0003-1545-5078" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D. J." } }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } }, { "id": "Spoon-H-W-W", "name": { "family": "Spoon", "given": "H. W." }, "orcid": "0000-0002-8712-369X" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Meyer-M-J", "name": { "family": "Meyer", "given": "M. J." } }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "M. W." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" } ] }, "title": "The opaque nascent starburst in NGC 1377: Spitzer SINGS observations", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction\u2014galaxies: evolution\u2014galaxies: individual (NGC 1377)\u2014galaxies: ISM\u2014galaxies: starburst\u2014infrared: galaxies", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2006 March 5; accepted 2006 April 11. \n\nWe wish to thank Marc Sauvage for fruitful discussions, Mark Wolfire for tirelessly running photodissociation region models to help interpret the data, and Nancy Silbermann for the timely scheduling of the Spitzer IRS observations. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through an award issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407.\n\nPublished - ROUapj06.pdf
Submitted - 0604267.pdf
", "abstract": "We analyze extensive data on NGC 1377 from the Spitzer Infrared Nearby Galaxies Survey (SINGS). Within the category of nascent starbursts that we previously selected as having infrared-to-radio continuum ratios in large excess of the average and containing hot dust, NGC 1377 has the largest infrared excess yet measured. Optical imaging reveals a morphological distortion suggestive of a recent accretion event. Infrared spectroscopy reveals a compact and opaque source dominated by a hot, self-absorbed continuum (\u03c4~ 20 in the 10\u03bcm silicate band). We provide physical evidence against nonstellar activity being the heating source. H II regions are detected through the single [Ne II] line, probing <1% of the ionizing radiation. Not only is the optical depth in different gas and dust phases very high, but >85% of ionizing photons are suppressed by dust. The only other detected emission features are molecular hydrogen lines, arguably excited mainly by shocks, besides photodissociation regions, and weak aromatic bands. The new observations support our interpretation in terms of an extremely young starburst (<1 Myr). More generally, galaxies deficient in radio synchrotron emission are likely observed within a few Myr of the onset of a starburst and after a long quiescence, prior to the replenishment of the interstellar medium with cosmic rays. The similar infrared-radio properties of NGC 1377 and some infrared-luminous galaxies suggest that NGC 1377 constitutes an archetype that will be useful to better understand starburst evolution. Although rare locally because observed in a brief evolutionary stage, nascent starbursts may represent a nonnegligible fraction of merger-induced starbursts that dominate deep infrared counts. Since they differ dramatically from usual starburst templates, they have important consequences for the interpretation of deep surveys.", "date": "2006-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "646", "number": "2", "publisher": "American Astronomical Society", "pagerange": "841-857", "id_number": "CaltechAUTHORS:ROUapj06", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:ROUapj06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/505038", "primary_object": { "basename": "0604267.pdf", "url": "https://authors.library.caltech.edu/records/1fm7x-k0d96/files/0604267.pdf" }, "related_objects": [ { "basename": "ROUapj06.pdf", "url": "https://authors.library.caltech.edu/records/1fm7x-k0d96/files/ROUapj06.pdf" } ], "resource_type": "article", "pub_year": "2006", "author_list": "Roussel, H.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/6zxct-bn417", "eprint_id": 18848, "eprint_status": "archive", "datestamp": "2023-08-22 06:06:17", "lastmod": "2023-10-20 19:07:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J. D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Moustakas-J", "name": { "family": "Moustakas", "given": "J." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "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": "Kewley-L-J", "name": { "family": "Kewley", "given": "L. J." }, "orcid": "0000-0001-8152-3943" }, { "id": "Leitherer-C", "name": { "family": "Leitherer", "given": "C." }, "orcid": "0000-0003-2685-4488" }, { "id": "Li-Aigen", "name": { "family": "Li", "given": "A." } }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "S." }, "orcid": "0000-0002-9226-5350" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" } ] }, "title": "Mid-Infrared Spectral Diagnostics of Nuclear and Extranuclear Regions in Nearby Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "active; galaxies: nuclei; H ii regions; infrared: galaxies; infrared: ISM", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2006 February 24; accepted 2006 March 31.\n\nMike Brotherton provided helpful comments. Support for this\nwork, part of the Spitzer Space Telescope Legacy Science Program,\nwas provided by NASA through contract 1224769 issued\nby the Jet Propulsion Laboratory, California Institute of Technology\nunder NASA contract 1407. This research has made use\nof the NASA/IPAC Extragalactic Database, which is operated\nby JPL/Caltech, under contract with NASA. This publication\nmakes use of data products from the Two Micron All Sky Survey,\nwhich is a joint project of the University of Massachusetts and\nthe Infrared Processing and Analysis Center/California Institute\nof Technology, funded by the National Aeronautics and Space\nAdministration and the National Science Foundation.\n\nPublished - DALapj06.pdf
", "abstract": "Mid-infrared diagnostics are presented for a large portion of the Spitzer Infrared Nearby Galaxies Survey (SINGS) sample plus archival data from ISO and Spitzer. The SINGS data set includes low- and high-resolution spectral maps and broadband imaging in the infrared for over 160 nuclear and extranuclear regions within 75 nearby galaxies spanning a wide range of morphologies, metallicities, luminosities, and star formation rates. Our main result is that these mid-infrared diagnostics effectively constrain a target's dominant power source. The combination of a high-ionization line index and PAH strength serves as an efficient discriminant between AGNs and star-forming nuclei, confirming progress made with ISO spectroscopy on starbursting and ultraluminous infrared galaxies. The sensitivity of Spitzer allows us to probe fainter nuclear and star-forming regions within galaxy disks. We find that both star-forming nuclei and extranuclear regions stand apart from nuclei that are powered by Seyfert or LINER activity. In fact, we identify areas within four diagnostic diagrams containing >90% Seyfert/LINER nuclei or >90% H II regions/H II nuclei. We also find that, compared to starbursting nuclei, extranuclear regions typically separate even further from AGNs, especially for low-metallicity extranuclear environments. In addition, instead of the traditional mid-infrared approach to differentiating between AGNs and star-forming sources that utilizes relatively weak high-ionization lines, we show that strong low-ionization cooling lines of X-ray-dominated regions like [Si II] 34.82 \u03bcm can alternatively be used as excellent discriminants. Finally, the typical target in this sample shows relatively modest interstellar electron density (~400 cm^(-3)) and obscuration (A_V ~ 1.0 mag for a foreground screen), consistent with a lack of dense clumps of highly obscured gas and dust residing in the emitting regions.", "date": "2006-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "646", "number": "1", "publisher": "American Astronomical Society", "pagerange": "161-173", "id_number": "CaltechAUTHORS:20100629-095238210", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100629-095238210", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/504835", "primary_object": { "basename": "DALapj06.pdf", "url": "https://authors.library.caltech.edu/records/6zxct-bn417/files/DALapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Dale, D. A.; Smith, J. D. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/14pfe-ap113", "eprint_id": 7751, "eprint_status": "archive", "datestamp": "2023-08-22 06:02:09", "lastmod": "2023-10-23 17:19:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "George J." } }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "Brent A." } }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "Bruce T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Joseph-R-D", "name": { "family": "Joseph", "given": "Robert D." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "Kartik" }, "orcid": "0000-0002-5496-4118" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "John-David T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Walter-F", "name": { "family": "Walter", "given": "Fabian" }, "orcid": "0000-0003-4793-7880" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Cannon-J-M", "name": { "family": "Cannon", "given": "John M." } }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "Charles W." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "Karl D." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "David" } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H\u00e9l\u00e8ne" } } ] }, "title": "Spitzer and JCMT observations of the active galactic nucleus in the Sombrero Galaxy (NGC 4594)", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active\u2014 galaxies: individual (NGC 4594)\u2014 galaxies: ISM\u2014galaxies: nuclei\u2014infrared: galaxies", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2006 January 5; accepted 2006 March 7. \n\nSupport for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through contract 1224769, issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. B.T.D. was supported in part by NSF grant AST 04-06833.\n\nPublished - BENapj06a.pdf
Submitted - 0603160.pdf
", "abstract": "We present Spitzer 3.6\u2013160 \u03bcm images, Spitzer mid-infrared spectra, and JCMT SCUBA 850 \u03bcm images of the Sombrero Galaxy (NGC 4594), an Sa galaxy with a 10^9 M\u2299 ; low-luminosity active galactic nucleus (AGN). The brightest infrared sources in the galaxy are the nucleus and the dust ring. The spectral energy distribution of the AGN demonstrates that, while the environment around the AGN is a prominent source of mid-infrared emission, it is a relatively weak source of far-infrared emission, as had been inferred for AGNs in previous research. The weak nuclear 160 \u03bcm emission and the negligible polycyclic aromatic hydrocarbon emission from the nucleus also implies that the nucleus is a site of only weak star formation activity and the nucleus contains relatively little cool interstellar gas needed to fuel such activity. We propose that this galaxy may be representative of a subset of low-ionization nuclear emission region galaxies that are in a quiescent AGN phase because of the lack of gas needed to fuel circumnuclear star formation and Seyfert-like AGN activity. Surprisingly, the AGN is the predominant source of 850 \u03bcm emission. We examine the possible emission mechanisms that could give rise to the 850 \u03bcm emission and find that neither thermal dust emission, CO line emission, bremsstrahlung emission, nor the synchrotron emission observed at radio wavelengths can adequately explain the measured 850 \u03bcm flux density by themselves. The remaining possibilities for the source of the 850 \u03bcm emission include a combination of known emission mechanisms, synchrotron emission that is self-absorbed at wavelengths longer than 850 \u03bcm, or unidentified spectral lines in the 850 \u03bcm band.", "date": "2006-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "645", "number": "1", "publisher": "American Astronomical Society", "pagerange": "134-147", "id_number": "CaltechAUTHORS:BENapj06a", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BENapj06a", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1407" }, { "agency": "NSF", "grant_number": "AST 04-06833" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/504033", "primary_object": { "basename": "0603160.pdf", "url": "https://authors.library.caltech.edu/records/14pfe-ap113/files/0603160.pdf" }, "related_objects": [ { "basename": "BENapj06a.pdf", "url": "https://authors.library.caltech.edu/records/14pfe-ap113/files/BENapj06a.pdf" } ], "resource_type": "article", "pub_year": "2006", "author_list": "Bendo, George J.; Buckalew, Brent A.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/j75qe-rvn36", "eprint_id": 75461, "eprint_status": "archive", "datestamp": "2023-08-19 17:57:18", "lastmod": "2023-10-25 15:04:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shim-Hyunjin", "name": { "family": "Shim", "given": "Hyunjin" } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "Myungshin" }, "orcid": "0000-0002-8537-6714" }, { "id": "Pak-Soojong", "name": { "family": "Pak", "given": "Soojong" } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "Philip" } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "Lisa" }, "orcid": "0000-0002-5987-5210" } ] }, "title": "Deep u*- and g-Band Imaging of the Spitzer Space Telescope First Look Survey Field: Observations and Source Catalogs", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2014 galaxies: photometry \u2014 surveys", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2006 January 31; accepted 2006 February 24. \n\nWe acknowledge the FLS members for their support on this program, and Luc Simard and Tom Soifer for helping us to prepare the CFHT proposal. This work was supported by the University-Institute Cooperative Research Fund from the Korea Astronomy and Space Science Institute, and grant R01-2005-000-10610-0 from the Basic Research Program of the Korea Science and Engineering Foundation. We also acknowledge the hospitality of the Korean Institute of Advanced Study during the final stage of this work, and the support from the School of Earth and Environmental Sciences Brain Korea 21 program at Seoul National University. \n\nFacilities: CFHT(MegaCam).\n\nPublished - Shim_2006_ApJS_164_435.pdf
Submitted - 0708.0886.pdf
", "abstract": "We present deep u*- and g-band images taken with the MegaCam on the 3.6 m Canada-France-Hawai'i Telescope to support the extragalactic component of the Spitzer First Look Survey (FLS). In this paper we outline the observations, present source catalogs, and characterize the completeness, reliability, astrometric accuracy, and number counts of this data set. In the central 1 deg^2 region of the FLS, we reach depths of g ~ 26.5 mag and u* ~ 26.2 mag (AB magnitude, 5 \u03c3 detection over a 3'' aperture) with ~4 hr of exposure time for each filter. For the entire FLS region (~5 deg^2 coverage), we obtained u*-band images to the shallower depth of u* = 25.0-25.4 mag (5 \u03c3, 3'' aperture). The average seeing of the observations is 0.\"85 for the central field and ~1.\"00 for the other fields. Astrometric calibration of the fields yields an absolute astrometric accuracy of 0.\"15 when matched with the SDSS point sources between 18 < g < 22. Source catalogs have been created using SExtractor. The catalogs are 50% complete and >99.3% reliable down to g \u2243 26.5 mag and u* \u224326.2 mag for the central 1 deg^2 field. In the shallower u*-band images, the catalogs are 50% complete and 98.2% reliable down to 24.8-25.4 mag. These images and source catalogs will serve as a useful resource for studying the galaxy evolution using the FLS data.", "date": "2006-06", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "164", "number": "2", "publisher": "American Astronomical Society", "pagerange": "435-449", "id_number": "CaltechAUTHORS:20170328-081530065", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170328-081530065", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2005-000-10610-0" }, { "agency": "Seoul National University" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/503709", "primary_object": { "basename": "0708.0886.pdf", "url": "https://authors.library.caltech.edu/records/j75qe-rvn36/files/0708.0886.pdf" }, "related_objects": [ { "basename": "Shim_2006_ApJS_164_435.pdf", "url": "https://authors.library.caltech.edu/records/j75qe-rvn36/files/Shim_2006_ApJS_164_435.pdf" } ], "resource_type": "article", "pub_year": "2006", "author_list": "Shim, Hyunjin; Im, Myungshin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zhdxa-rgy34", "eprint_id": 13007, "eprint_status": "archive", "datestamp": "2023-08-22 05:47:43", "lastmod": "2023-10-17 21:42:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "Dario" }, "orcid": "0000-0002-3698-7076" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "Francine R." } }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "Lisa J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Makozov-D", "name": { "family": "Makozov", "given": "David" } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G. K." }, "orcid": "0000-0002-1977-5717" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Wilson-G", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" }, { "id": "Yang-L", "name": { "family": "Yang", "given": "L." } } ] }, "title": "The Spitzer Space Telescope Extragalactic First Look Survey: 24 \u03bcm Data Reduction, Catalog, and Source Identification", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; infrared: galaxies; surveys; techniques: photometric", "note": "\u00a9 2006. The American Astronomical Society. \n\nReceived 2005 December 30; accepted 2006 March 6. Print publication: Issue 6 (2006 June). \n\nD.F. is grateful to Alberto Noriega-Crespo for enlightening discussions about MIPS data processing issues. We acknowledge also the anonymous referee for useful comments and suggestions.\n\nPublished - FADaj06.pdf
", "abstract": "We present the reduction of the 24 \u03bcm data obtained during the first cosmological survey performed by the Spitzer Space Telescope. Images of a region of sky at moderately high Galactic latitude (l = 88.3\u00b0, b = +34.9\u00b0) were obtained on 2003 December 9-11. The survey consists of a shallow observation of 2.5\u00b0 \u00d7 2\u00b0 centered at 17h18m, +59\u00b030' (main survey) and a deeper observation of 1\u00b0 \u00d7 0.5\u00b0 centered at 17h17m, +59\u00b045' (verification survey). Issues with the reduction of the 24 \u03bcm MIPS data are discussed and solutions to attenuate instrumental effects are proposed and applied to the data. Approximately 17,000 sources are extracted with a signal-to-noise ratio (S/N) greater than 5. The photometry of the point sources is evaluated through point-spread function (PSF) fitting using an empirical PSF derived from the data. Aperture corrections and the absolute calibration have been checked using stars in the field. Astrometric and photometric errors depend on the S/N of the source varying between 0farcs35^-1\" and 5%-15%, respectively, for sources detected at 20-5 \u03c3. The fluxes of the 123 extended sources have been estimated through aperture photometry. The extended sources cover less than 0.3% of the total area of the survey. Based on simulations, the main and verification surveys are 50% complete at 0.3 and 0.15 mJy, respectively. Counterparts have been searched for in optical and radio catalogs. More than 80% of the 24 \u03bcm sources have a reliable optical counterpart down to R = 25.5; 16% of the sources have a 20 cm counterpart down to 0.1 mJy and ~80% of the radio-IR associations have a reliable optical counterpart. A residual map is obtained by subtracting point sources detected at the 3 \u03c3 level and interpolating the regions occupied by extended sources. Several Galactic clouds with low and intermediate velocities are identified by comparison with neutral hydrogen data from this field.", "date": "2006-06", "date_type": "published", "publication": "Astronomical Journal", "volume": "131", "number": "6", "publisher": "American Astronomical Society", "pagerange": "2859-2876", "id_number": "CaltechAUTHORS:FADaj06", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:FADaj06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/504034", "primary_object": { "basename": "FADaj06.pdf", "url": "https://authors.library.caltech.edu/records/zhdxa-rgy34/files/FADaj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Fadda, Dario; Marleau, Francine R.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/4hcbj-c3h20", "eprint_id": 22346, "eprint_status": "archive", "datestamp": "2023-08-22 05:42:02", "lastmod": "2023-10-23 15:52:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Kundurthy-P", "name": { "family": "Kundurthy", "given": "P." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C." }, "orcid": "0000-0001-5448-1821" }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J.-D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "M. W." } }, { "id": "Makovoz-D", "name": { "family": "Makovoz", "given": "D." } }, { "id": "Sosey-M-L", "name": { "family": "Sosey", "given": "M." } }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Meyer-M-R", "name": { "family": "Meyer", "given": "M." }, "orcid": "0000-0003-1227-3084" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Hollenbach-D-J", "name": { "family": "Hollenbach", "given": "D." } }, { "id": "Cannon-J-M", "name": { "family": "Cannon", "given": "J. M." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Buckalew-B-A", "name": { "family": "Buckalew", "given": "B. A." } }, { "id": "Sheth-K", "name": { "family": "Sheth", "given": "K." }, "orcid": "0000-0002-5496-4118" } ] }, "title": "Extended Mid-Infrared Aromatic Feature Emission in M82", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (M82); galaxies: ISM; galaxies: peculiar; galaxies: starburst", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2006 February 2; accepted 2006 March 27; published 2006 April 17.\n\nWe thank the anonymous referee for a constructive report\nthat improved this Letter. This work is based in part on observations made with the Spitzer Space Telescope, which is\noperated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through contracts 1224769 and 1255094 issued by JPL/Caltech.\n\nPublished - ENGapjl06.pdf
", "abstract": "We present new images (ground-based optical and mid-infrared [MIR] from the Spitzer Space Telescope) and spectra (from Spitzer) of the archetypal starburst galaxy M82. The Spitzer data show that the MIR emission extends at least 6 kpc along the minor axis of the galaxy. We use the optical and infrared data to demonstrate that the extended emission is dominated by emission from dust. The colors of the MIR emission and the spectra indicate that there is a strong component of aromatic feature emission (the MIR features commonly attributed to polycyclic aromatic hydrocarbons). The dust continuum and aromatic feature emission are both strong in the well-known superwind region of this galaxy; clearly, the carrier of the aromatic features can survive in close proximity to the wind, far from the plane of the galaxy. We also see significant emission by dust well outside the superwind region, providing the clearest picture to date of the dust distribution in the halo of this galaxy.", "date": "2006-05-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "642", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L127-L132", "id_number": "CaltechAUTHORS:20110217-092654489", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110217-092654489", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1224769" }, { "agency": "NASA", "grant_number": "1255094" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/504590", "primary_object": { "basename": "ENGapjl06.pdf", "url": "https://authors.library.caltech.edu/records/4hcbj-c3h20/files/ENGapjl06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Engelbracht, C. W.; Kundurthy, P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/9pm3p-50c80", "eprint_id": 75466, "eprint_status": "archive", "datestamp": "2023-08-22 05:00:00", "lastmod": "2023-10-25 15:04:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Star Formation Rates and Extinction Properties of IR-luminous Galaxies in the Spitzer First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: bulges; galaxies: evolution; galaxies: high-redshift; galaxies: spiral; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2006. The American Astronomical Society. \n\nReceived 2005 June 19; accepted 2005 September 27. \n\nWe thank the anonymous referee for insightful comments that have significantly improved this paper. We thank Dave Thomson for his contribution to the observation and reduction of the WIRC data. We would also like to thank Carol Lonsdale, Robert Kennicutt, and Rolf Jansen for early discussions that helped shape this project. 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 an award issued by JPL, Caltech. M. I. was supported by grant R01-2005-000-10610-0 from the Basic Research Program of the Korea Science and Engineering Foundation. We are indebted to Grant Hill, Greg Wirth, and the rest of the Keck observatory staff for their phenomenal observation support. The analysis pipeline used to reduce the DEIMOS data was developed by the DEEP2 group at UC Berkeley with support from NSF grant AST 00-71048. Finally, we wish to recognize and acknowledge the significant cultural role and reverence that the summit of Mauna Kea has within the indigenous Hawaiian community. We are grateful for the opportunity to conduct observations from this mountain.\n\nPublished - Choi_2006_ApJ_637_227.pdf
Submitted - 0509894.pdf
", "abstract": "We investigate the instantaneous star formation rates (SFRs) and extinction properties for a large (N = 274), near-infrared (NIR: 2.2 \u03bcm) + mid-infrared (MIR: 24 \u03bcm)-selected sample of normal to ultraluminous infrared galaxies (ULIRGs; 10^9 < L_(IR)/L_\u2609 < 10^(12.5)) with\u3008 z\u3009~ 0.8 in the Spitzer Extragalactic First Look Survey (FLS). We combine 24 \u03bcm observations with high-resolution Keck DEIMOS spectroscopy to derive optical emission-line (H\u03b1, H\u03b2, and [O II]) and infrared star formation rates (SFR_(opt) and SFR_(IR), respectively). Comparison of SFR diagnostics reveals a wide extinction range (1.0 < A_V < 4.0 mag) for this sample, even after removing spectroscopic and IRAC color-selected AGN candidates (\u224812% of the sample). Objects with SFRs of a few M_\u2609 yr^(-1) have extinction values consistent with normal spirals (A_V \u2248 1.0 mag). By contrast, LIRGs at z \u2273 1, which comprise a fraction of our sample, have SFR \u2248 100 M_\u2609 yr^(-1) and a mean A_V \u2248 2.5 mag. This translates to a 97% mean [O II] \u03bb\u03bb3727 attentuation and in extreme cases is as high as 99.7%. We derive an IR-luminosity-dependent A^(IR)_V function [A^(IR)_V = 0.75 log(L_(IR)/L_\u2609) - 6.35 mag] that we use to extinction correct our line luminosities. The resulting correlation between SFR_(IR) and SFR_(opt) has a dispersion of ~0.2 dex (semi-interquartile range). Comparison of the A_V dependence on redshift and LIR reveals that for a fixed L_(IR), there is no significant AV evolution. Comparison to previous studies reveals a mean attenuation that is intermediate between that of local optical/UV- and radio-selected samples with a marginally stronger L_(IR) dependence.", "date": "2006-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "637", "number": "1", "publisher": "American Astronomical Society", "pagerange": "227-241", "id_number": "CaltechAUTHORS:20170328-093303002", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170328-093303002", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2005-000-10610-0" }, { "agency": "NSF", "grant_number": "AST 00-71048" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/498388", "primary_object": { "basename": "0509894.pdf", "url": "https://authors.library.caltech.edu/records/9pm3p-50c80/files/0509894.pdf" }, "related_objects": [ { "basename": "Choi_2006_ApJ_637_227.pdf", "url": "https://authors.library.caltech.edu/records/9pm3p-50c80/files/Choi_2006_ApJ_637_227.pdf" } ], "resource_type": "article", "pub_year": "2006", "author_list": "Choi, P. I.; Yan, L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/h8awm-wkr85", "eprint_id": 75460, "eprint_status": "archive", "datestamp": "2023-08-22 04:54:12", "lastmod": "2023-10-25 15:04:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Beck-R", "name": { "family": "Beck", "given": "R." } }, { "id": "Dole-H", "name": { "family": "Dole", "given": "H." } }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Henderson-D", "name": { "family": "Henderson", "given": "D." } }, { "id": "Hesselroth-T-D", "name": { "family": "Hesselroth", "given": "T." } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Kelly-D-M", "name": { "family": "Kelly", "given": "D. M." } }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "S." }, "orcid": "0000-0003-1250-8314" }, { "id": "Latter-W-B", "name": { "family": "Latter", "given": "W. B." } }, { "id": "Mahoney-W-A", "name": { "family": "Mahoney", "given": "W." } }, { "id": "Makovoz-D", "name": { "family": "Makovoz", "given": "D." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Morrison-J-E", "name": { "family": "Morrison", "given": "J. E." } }, { "id": "Moshir-M", "name": { "family": "Moshir", "given": "M." } }, { "id": "Noriega-Crespo-A", "name": { "family": "Noriega-Crespo", "given": "A." }, "orcid": "0000-0002-6296-8960" }, { "id": "Padgett-D-L", "name": { "family": "Padgett", "given": "D. L." }, "orcid": "0000-0001-5334-5107" }, { "id": "Pesenson-M-Z", "name": { "family": "Pesenson", "given": "M." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G. K." }, "orcid": "0000-0002-1977-5717" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." } } ] }, "title": "Spitzer 70 and 160 \u03bcm Observations of the Extragalactic First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2006 The American Astronomical Society. \n\nReceived 2005 August 1; accepted 2005 September 21. \n\nWe thank all of our colleagues associated with the Spitzer mission who have made these observations possible. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407.\n\nPublished - Frayer_2006_AJ_131_250.pdf
Submitted - 0509649.pdf
", "abstract": "We present 70 and 160 \u03bcm observations from the Spitzer extragalactic First Look Survey (xFLS). The data reduction techniques and the methods for producing co-added mosaics and source catalogs are discussed. Currently, 26% of the 70 \u03bcm sample and 49% of the 160 \u03bcm\u2013selected sources have redshifts. The majority of sources with redshifts are star-forming galaxies at z < 0.5, while about 5% have infrared colors consistent with active galactic nuclei. The observed infrared colors agree with the spectral energy distributions (SEDs) of local galaxies previously determined from IRAS and Infrared Space Observatory data. The average 160 \u03bcm/70 \u03bcm color temperature for the dust is T_d \u2243 30 \u00b1 5 K, and the average 70 \u03bcm/24 \u03bcm spectral index is \u03b1 \u2243 2.4 \u00b1 0.4. The observed infrared-to-radio correlation varies with redshift as expected out to z ~ 1 based on the SEDs of local galaxies. The xFLS number counts at 70 and 160 \u03bcm are consistent within uncertainties with the models of galaxy evolution, but there are indications that the current models may require slight modifications. Deeper 70 \u03bcm observations are needed to constrain the models, and redshifts for the faint sources are required to measure the evolution of the infrared luminosity function.", "date": "2006-01", "date_type": "published", "publication": "Astronomical Journal", "volume": "131", "number": "1", "publisher": "American Astronomical Society", "pagerange": "250-260", "id_number": "CaltechAUTHORS:20170328-075452484", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170328-075452484", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/498690", "primary_object": { "basename": "0509649.pdf", "url": "https://authors.library.caltech.edu/records/h8awm-wkr85/files/0509649.pdf" }, "related_objects": [ { "basename": "Frayer_2006_AJ_131_250.pdf", "url": "https://authors.library.caltech.edu/records/h8awm-wkr85/files/Frayer_2006_AJ_131_250.pdf" } ], "resource_type": "article", "pub_year": "2006", "author_list": "Frayer, D. T.; Fadda, D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/m5yj4-vqn92", "eprint_id": 75315, "eprint_status": "archive", "datestamp": "2023-08-19 16:35:29", "lastmod": "2023-10-25 14:56:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Laine-S-J", "name": { "family": "Laine", "given": "S." }, "orcid": "0000-0003-1250-8314" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G. K." }, "orcid": "0000-0002-1977-5717" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "The Infrared Array Camera Component of the Spitzer Space Telescope Extragalactic First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2014 infrared: galaxies \u2014 surveys", "note": "\u00a9 2005 The American Astronomical Society. \n\nReceived 2004 December 30; accepted 2005 June 8. \n\nWe thank the other members of the IRAC instrument/instrument support team, in particular Sean Carey, for helpful discussions, and Dan Stern and Lexi Moustakas for making their software available. We also thank I. Drozdovsky for supplying the mosaics of the ACS data in the XFLS field, and the anonymous referee for helpful comments. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. The Two Micron All Sky Survey (2MASS) 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 (NASA) and the National Science Foundation (NSF).\n\nPublished - Lacy_2005_ApJS_161_41.pdf
Submitted - 0507143.pdf
", "abstract": "We present Infrared Array Camera (IRAC) data and source catalogs from the Spitzer Space Telescope Extragalactic First Look Survey. The data were taken in four broad bands centered at nominal wavelengths of 3.6, 4.5, 5.8, and 8.0 \u03bcm. A set of mosaics and catalogs have been produced that are \u224880% complete and \u224899% reliable to their chosen flux density limits. The main field survey covers 3.8 deg^2 and has flux density limits of 20, 25, 100, and 100 \u03bcJy at wavelengths of 3.6, 4.5, 5.8, and 8.0 \u03bcm, respectively. The deeper \"verification\" survey covers 0.25 deg^2 with limits of 10, 10, 30, and 30 \u03bcJy, respectively. We also include deep data in the ELAIS-N1 field, which covers 0.041 deg2 with limits of 4, 3, 10, and 10 \u03bcJy, respectively, but with only two wavelength coverages at a given sky position. The final bandmerged catalogs contain 103,193 objects in the main field, 12,224 in the verification field, and 5239 in ELAIS-N1. Flux densities of high signal-to-noise objects are accurate to about 10%, and the residual systematic error in the absolute flux density scale is ~2%-3%. We have successfully extracted sources at source densities as high as 100,000 deg-2 in our deepest 3.6 and 4.5 \u03bcm data. The mosaics and source catalogs will be made available through the Spitzer Science Center archive and the Infrared Science Archive.", "date": "2005-11", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "161", "number": "1", "publisher": "American Astronomical Society", "pagerange": "41-52", "id_number": "CaltechAUTHORS:20170322-105720718", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-105720718", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "1407" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/432894", "primary_object": { "basename": "0507143.pdf", "url": "https://authors.library.caltech.edu/records/m5yj4-vqn92/files/0507143.pdf" }, "related_objects": [ { "basename": "Lacy_2005_ApJS_161_41.pdf", "url": "https://authors.library.caltech.edu/records/m5yj4-vqn92/files/Lacy_2005_ApJS_161_41.pdf" } ], "resource_type": "article", "pub_year": "2005", "author_list": "Lacy, M.; Wilson, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/evsgx-fxe73", "eprint_id": 106071, "eprint_status": "archive", "datestamp": "2023-08-22 02:58:05", "lastmod": "2024-01-15 18:13:32", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H\u00e9l\u00e8ne" } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "James" }, "orcid": "0000-0003-4724-1939" }, { "id": "Beck-R", "name": { "family": "Beck", "given": "Rainer" } } ] }, "title": "Nascent Starbursts in Synchrotron-Deficient Galaxies", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Dust Temperature; Rare Category; Young Stellar Population; Star Burst; Cent Imeter Wave", "note": "\u00a9 2005 Springer.", "abstract": "We have identified a rare category of galaxies deviating from the universal infrared-radio correlation of star-forming galaxies in being significantly deficient in synchrotron radiation at 20 cm. The selected objects also have high dust temperatures, indicating intense radiation fields. From a detailed study of the prototype of this class, NGC 1377, the most likely scenario accounting for their properties is a starburst just breaking out in a host previously quiescent for at least 100 Myr. We have selected a statistical sample of candidate nascent starbursts from the cross-correlation of the IRAS Faint Source Catalog with the NVSS and FIRST VLA radio surveys, and discuss the first results obtained from a recent multi-wavelength VLA campaign.", "date": "2005", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "223-226", "id_number": "CaltechAUTHORS:20201014-150720595", "isbn": "978-1-4020-3538-8", "book_title": "Starbursts: From 30 Doradus to Lyman Break Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201014-150720595", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "de-Grijs-R", "name": { "family": "de Grijs", "given": "Richard" } }, { "id": "Gonz\u00e1lez-Delgado-R-M", "name": { "family": "Gonz\u00e1lez Delgado", "given": "Rosa M." } } ] }, "doi": "10.1007/1-4020-3539-x_39", "resource_type": "book_section", "pub_year": "2005", "author_list": "Roussel, H\u00e9l\u00e8ne; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/0f45r-y6k73", "eprint_id": 60274, "eprint_status": "archive", "datestamp": "2023-08-22 02:54:52", "lastmod": "2023-10-24 16:22:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burgdorf-M-J", "name": { "family": "Burgdorf", "given": "Martin J." } }, { "id": "Cohen-Martin", "name": { "family": "Cohen", "given": "Martin" } }, { "id": "Ingalls-J-G", "name": { "family": "Ingalls", "given": "James G." }, "orcid": "0000-0003-4714-1364" }, { "id": "Ramirez-S-V", "name": { "family": "Ramirez", "given": "S." } }, { "id": "Rho-Jeonghee", "name": { "family": "Rho", "given": "Jeonghee" }, "orcid": "0000-0003-3643-839X" }, { "id": "Stolovy-S-R", "name": { "family": "Stolovy", "given": "S. R." } }, { "id": "Carey-S-J", "name": { "family": "Carey", "given": "Sean J." }, "orcid": "0000-0002-0221-6871" }, { "id": "Fajardo-Acosta-S-B", "name": { "family": "Fajardo-Acosta", "given": "S. B." }, "orcid": "0000-0001-9309-0102" }, { "id": "Glaccum-W-J", "name": { "family": "Glaccum", "given": "W. J." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hoard-D-W", "name": { "family": "Hoard", "given": "D. W." }, "orcid": "0000-0002-6800-6519" }, { "id": "Karr-J", "name": { "family": "Karr", "given": "J." } }, { "id": "Lowrance-P-J", "name": { "family": "Lowrance", "given": "P. J." }, "orcid": "0000-0001-8014-0270" }, { "id": "O'Linger-J-C", "name": { "family": "O'Linger", "given": "J." } }, { "id": "Padgett-D-L", "name": { "family": "Padgett", "given": "Deborah L." }, "orcid": "0000-0001-5334-5107" }, { "id": "Reach-W-T", "name": { "family": "Reach", "given": "W. T." }, "orcid": "0000-0001-8362-4094" }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "L. M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "John R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Wachter-S", "name": { "family": "Wachter", "given": "S." } } ] }, "title": "The galactic first-look survey with the Spitzer space telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "Milky Way; IR; Spitzer; Surveys", "note": "\u00a9 2005 COSPAR Published by Elsevier Ltd. Received 1 October 2004; received in revised form 11 May 2005; accepted 18 May 2005. Available online 6 July 2005.\n\nWe thank A. Noriega-Crespo for useful conversations.\n\nPublished - 1-s2.0-S0273117705006800-main.pdf
", "abstract": "The galactic first look survey (GFLS) of the Spitzer space telescope was executed during 1\u201311 December 2003 as one of the first science observations during nominal operations. The aim of the FLS is to provide a characteristic \"first-look\" at the mid-and far-infrared sky at sensitivities that allow the detection of point sources \u2248100 times fainter than those in previous systematic large-area surveys. The whole program took 35.5 h to complete and consisted of the following elements:\n\u2022Galactic longitudinal strips of size 15\u2032 \u00d7 1\u00b0 with IRAC and MIPS at l = 105.6\u00b0 and 254.4\u00b0 and various galactic latitudes.\n\u202210\u2032 \u00d7 10\u2032 IRAC maps at l = 97.5\u00b0 and b = 0\u00b0, \u00b14\u00b0, and +16\u00b0.\n\u2022Coverage of L1228 with 2\u00b0 scan maps.\nEven at these large distances from the galactic center, confusion sets a limit to the detection of point sources in the galactic plane for IRAC channel 1 (3.6 \u03bcm) at 100 \u03bcJy \u2248 16.1^m. As positive galactic latitudes were mainly sampled at l = 97.5\u00b0 and 105.6\u00b0 and negative latitudes at 254.4\u00b0 galactic longitude, the observations are well suited to derive information on the warp of the galactic disk. In order to reproduce the source counts from the GFLS we had to assume an amplitude of the warp within 20% of that derived from 2MASS. The whole survey is included in the Spitzer science archive which opened in April 2004.", "date": "2005", "date_type": "published", "publication": "Advances in Space Research", "volume": "36", "number": "6", "publisher": "Elsevier", "pagerange": "1050-1056", "id_number": "CaltechAUTHORS:20150916-094156500", "issn": "0273-1177", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-094156500", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1016/j.asr.2005.05.064", "primary_object": { "basename": "1-s2.0-S0273117705006800-main.pdf", "url": "https://authors.library.caltech.edu/records/0f45r-y6k73/files/1-s2.0-S0273117705006800-main.pdf" }, "resource_type": "article", "pub_year": "2005", "author_list": "Burgdorf, Martin J.; Cohen, Martin; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1mada-kxn61", "eprint_id": 75443, "eprint_status": "archive", "datestamp": "2023-08-19 14:11:33", "lastmod": "2023-10-25 15:03:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "Francine R." } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Makovoz-D", "name": { "family": "Makovoz", "given": "D." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S." } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G." }, "orcid": "0000-0002-1977-5717" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." } } ] }, "title": "Extragalactic Source Counts at 24 Microns in the Spitzer First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: statistics \u2014 infrared: galaxies", "note": "\u00a9 2004 The American Astronomical Society. \n\nReceived 2004 March 29; accepted 2004 May 13. \n\nWe thank A. Noriega-Crespo for useful discussions and the\nreferee M. Malkan for insightful comments. We are grateful to H. Dole and A. Franceschini for providing us with their model predictions. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - Marleau_2004_ApJS_154_66.pdf
Submitted - 0405635.pdf
", "abstract": "We present the Spitzer Multiband Imaging Photometer 24 \u03bcm source counts in the Extragalactic First Look Survey (FLS) main, verification, and European Large Area ISO Survey N1 fields. Spitzer's increased sensitivity and efficiency in large areal coverage over previous infrared telescopes, coupled with the enhanced sensitivity of the 24 \u03bcm band to sources at intermediate redshift, dramatically improve the quality and statistics of number counts in the mid-infrared. The FLS observations cover areas of 4.4, 0.26, and 0.015 deg^2, respectively, and reach 3 \u03c3 depths of 0.11, 0.08, and 0.03 mJy. The extragalactic counts derived for each survey agree remarkably well. The counts can be fitted by a super-Euclidean power law of index \u03b1 = -2.9 from 0.2 to 0.9 mJy, with a flattening of the counts at fluxes fainter than 0.2 mJy. Comparison with infrared galaxy evolution models reveals a peak's displacement in the 24 \u03bcm counts. This is probably due to the detection of a new population of galaxies with redshift between 1 and 2, previously unseen in the 15 \u03bcm deep counts.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "66-69", "id_number": "CaltechAUTHORS:20170327-153742897", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170327-153742897", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422584", "primary_object": { "basename": "0405635.pdf", "url": "https://authors.library.caltech.edu/records/1mada-kxn61/files/0405635.pdf" }, "related_objects": [ { "basename": "Marleau_2004_ApJS_154_66.pdf", "url": "https://authors.library.caltech.edu/records/1mada-kxn61/files/Marleau_2004_ApJS_154_66.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Marleau, Francine R.; Fadda, D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7b982-c4810", "eprint_id": 75357, "eprint_status": "archive", "datestamp": "2023-08-22 02:23:21", "lastmod": "2023-10-25 14:58:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Willner-S-P", "name": { "family": "Willner", "given": "S. P." }, "orcid": "0000-0002-9895-5758" }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Barmby-P", "name": { "family": "Barmby", "given": "P." }, "orcid": "0000-0003-2767-0090" }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Pahre-M-A", "name": { "family": "Pahre", "given": "M." } }, { "id": "Smith-H-A", "name": { "family": "Smith", "given": "H. A." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "Robert C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "Daniela" }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael W." } }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "S." }, "orcid": "0000-0002-9226-5350" }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "Michele D." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Stolovy-S-R", "name": { "family": "Stolovy", "given": "S." } }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L." }, "orcid": "0000-0002-5987-5210" } ] }, "title": "Infrared Array Camera (IRAC) Observations of M81", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (M81); galaxies: ISM; galaxies: spiral; galaxies: stellar content; infrared: galaxies", "note": "\u00a9 2004 American Astronomical Society. \n\nReceived 2004 March 26. Accepted 2004 May 27. \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA through contract 1256790 issued by JPL/Caltech. Support for the IRAC instrument was provided by NASA through contract 960541 issued by JPL. M. A. P. acknowledges NASA/LTSA grant NAG5-10777. \n\nIRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. \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\nPublished - Willner_2004_ApJS_154_222.pdf
", "abstract": "Infrared Array Camera (IRAC) images of M81 show three distinct morphological constituents: a smooth distribution of evolved stars with bulge, disk, and spiral arm components; a clumpy distribution of dust emission tracing the spiral arms; and a pointlike nuclear source. The bulge stellar colors are consistent with M-type giants, and the disk colors are consistent with a slightly younger population. The dust emission generally follows the blue and ultraviolet emission, but there are large areas that have dust emission without ultraviolet and smaller areas with ultraviolet but little dust emission. The former are presumably caused by extinction, and the latter may be due to cavities in the gas and dust created by supernova explosions. The nucleus appears fainter at 8 \u03bcm than expected from ground-based 10 \u03bcm observations made 4 years ago.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "222-228", "id_number": "CaltechAUTHORS:20170323-131933186", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170323-131933186", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech", "grant_number": "1256790" }, { "agency": "JPL", "grant_number": "960541" }, { "agency": "NASA", "grant_number": "NAG5-10777" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422913", "primary_object": { "basename": "Willner_2004_ApJS_154_222.pdf", "url": "https://authors.library.caltech.edu/records/7b982-c4810/files/Willner_2004_ApJS_154_222.pdf" }, "resource_type": "article", "pub_year": "2004", "author_list": "Willner, S. P.; Ashby, M. L. N.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y0sge-rcx71", "eprint_id": 75308, "eprint_status": "archive", "datestamp": "2023-08-19 14:11:19", "lastmod": "2023-10-25 14:56:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Morganti-R", "name": { "family": "Morganti", "given": "R." } }, { "id": "Garrett-M-A", "name": { "family": "Garrett", "given": "M. A." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G. K." }, "orcid": "0000-0002-1977-5717" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." } } ] }, "title": "Infrared Properties of Radio\u2010selected Submillimeter Galaxies in the Spitzer First Look Survey Verification Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2014 galaxies: evolution \u2014 galaxies: formation \u2014 galaxies: starburst \u2014 infrared: galaxies", "note": "\u00a9 2004 The American Astronomical Society. \n\nReceived 2004 March 27; accepted 2004 June 7. \n\nWe thank the staff at the JCMT and the Spitzer Science Center for their support of these observations. 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 NASA contract 1407.\n\nPublished - Frayer_2004_ApJS_154_137.pdf
Submitted - 0406351.pdf
", "abstract": "We report on submillimeter and infrared observations of 28 radio-selected galaxies in the Spitzer First Look Survey verification field. All of the radio-selected galaxies that show evidence for emission at 850 \u03bcm with SCUBA have Spitzer counterparts at 24 \u03bcm, while only half of the radio-selected galaxies without 850 \u03bcm emission have detectable counterparts at 24 \u03bcm. The data show a wide range of infrared colors (S_(70 \u03bcm)/S_(24 \u03bcm) < 5-30, S_(8 \u03bcm)/S_(3.6 \u03bcm) < 0.3-4), indicative of a mixture of infrared-warm AGN-dominated and cooler starburst-dominated sources. The galaxies showing 850 \u03bcm emission have Spitzer flux densities and flux density ratios consistent with the range of values expected for high-redshift (z = 1-4) ultraluminous infrared galaxies.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "137-141", "id_number": "CaltechAUTHORS:20170322-094800747", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-094800747", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/423250", "primary_object": { "basename": "0406351.pdf", "url": "https://authors.library.caltech.edu/records/y0sge-rcx71/files/0406351.pdf" }, "related_objects": [ { "basename": "Frayer_2004_ApJS_154_137.pdf", "url": "https://authors.library.caltech.edu/records/y0sge-rcx71/files/Frayer_2004_ApJS_154_137.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Frayer, D. T.; Chapman, S. C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/19yvq-pmb91", "eprint_id": 75445, "eprint_status": "archive", "datestamp": "2023-08-22 02:23:33", "lastmod": "2023-10-25 15:03:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Sajina-Anna", "name": { "family": "Sajina", "given": "A." }, "orcid": "0000-0002-1917-1200" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Obscured and Unobscured Active Galactic Nuclei in the Spitzer Space Telescope First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: Seyfert; infrared: galaxies; quasars: general", "note": "\u00a9 2004 The American Astronomical Society. \n\nReceived 2004 March 26; accepted 2004 April 28. \n\nWe thank Michael Gregg for assistance with the Lick observations, Susan Ridgway for advice and comments, B. Januzzi and A. Ford for the R-band survey, and J. Condon for the Very Large Array survey. We thank the SDSS team for targeting the FLS region in the DR1. This work is based on observations made with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology, under NASA contract 1407. Support was provided by NASA through JPL. The SDSS Archive is funded by the Alfred P. Sloan Foundation, the Participating Institutions, NASA, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.\n\nPublished - Lacy_2004_ApJS_154_166.pdf
Submitted - 0405604.pdf
", "abstract": "Selection of active galactic nuclei (AGNs) in the infrared facilitates the discovery of AGNs whose optical emission is extinguished by dust. In this paper, we use the Spitzer Space Telescope First Look Survey (FLS) to assess the fraction of AGNs with mid-infrared (MIR) luminosities that are comparable to quasars and that are missed in optical quasar surveys because of dust obscuration. We begin by using the Sloan Digital Sky Survey (SDSS) database to identify 54 quasars within the 4 deg^2 extragalactic FLS. These quasars occupy a distinct region in MIR color space by virtue of their strong, red continua. This has allowed us to define an MIR color criterion for selecting AGN candidates. About 2000 FLS objects have colors that are consistent with them being AGNs, but most are much fainter in the MIR than the SDSS quasars, which typically have 8 \u03bcm flux densities S_(8.0) ~ 1 mJy. We have investigated the properties of 43 objects with S_(8.0) \u2265 1 mJy that satisfy our AGN color selection. This sample should contain both unobscured quasars as well as AGNs that are absent from the SDSS survey because of extinction in the optical. After removing 16 known quasars, three probable normal quasars, and eight spurious or confused objects from the initial sample of 43, we are left with 16 objects that are likely to be obscured quasars or luminous Seyfert 2 galaxies. This suggests that the numbers of obscured and unobscured AGNs are similar in samples selected in the MIR at S_(8.0) ~ 1 mJy.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "166-169", "id_number": "CaltechAUTHORS:20170327-155242177", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170327-155242177", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422816", "primary_object": { "basename": "0405604.pdf", "url": "https://authors.library.caltech.edu/records/19yvq-pmb91/files/0405604.pdf" }, "related_objects": [ { "basename": "Lacy_2004_ApJS_154_166.pdf", "url": "https://authors.library.caltech.edu/records/19yvq-pmb91/files/Lacy_2004_ApJS_154_166.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Lacy, M.; Storrie-Lombardi, L. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dc73a-4b491", "eprint_id": 75314, "eprint_status": "archive", "datestamp": "2023-08-19 14:11:25", "lastmod": "2023-10-25 14:56:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "P\u00e9rez\u2010Gonz\u00e1lez-P-G", "name": { "family": "P\u00e9rez\u2010Gonz\u00e1lez", "given": "P. G." } }, { "id": "Misselt-K-A", "name": { "family": "Misselt", "given": "K. A." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Walter-F", "name": { "family": "Walter", "given": "F." }, "orcid": "0000-0003-4793-7880" }, { "id": "Thornley-M-D", "name": { "family": "Thornley", "given": "M. D." } }, { "id": "Kennicutt-R-C", "name": { "family": "Kennicutt", "given": "R. C., Jr." }, "orcid": "0000-0001-5448-1821" }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G. H." }, "orcid": "0000-0003-2303-6519" }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Smith-J-D-T", "name": { "family": "Smith", "given": "J.\u2010D. T." }, "orcid": "0000-0003-1545-5078" }, { "id": "Alonso-Herrero-A", "name": { "family": "Alonso-Herrero", "given": "A." }, "orcid": "0000-0001-6794-2519" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Calzetti-D", "name": { "family": "Calzetti", "given": "D." }, "orcid": "0000-0002-5189-8004" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Draine-B-T", "name": { "family": "Draine", "given": "B. T." }, "orcid": "0000-0002-0846-936X" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hinz-J-L", "name": { "family": "Hinz", "given": "J. L." } }, { "id": "Hines-D-C", "name": { "family": "Hines", "given": "D. C." }, "orcid": "0000-0003-4653-6161" }, { "id": "Kelly-D-M", "name": { "family": "Kelly", "given": "D. M." } }, { "id": "Morrison-J-E", "name": { "family": "Morrison", "given": "J. E." } }, { "id": "Muzerolle-J-C", "name": { "family": "Muzerolle", "given": "J." }, "orcid": "0000-0002-5943-1222" }, { "id": "Regan-M-W", "name": { "family": "Regan", "given": "M. W." } }, { "id": "Stansberry-J-A", "name": { "family": "Stansberry", "given": "J. A." } }, { "id": "Stolovy-S-R", "name": { "family": "Stolovy", "given": "S. R." } }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Su-Katherine-Y-L", "name": { "family": "Su", "given": "K. Y. L." }, "orcid": "0000-0002-3532-5580" }, { "id": "Young-E-T", "name": { "family": "Young", "given": "E. T." } } ] }, "title": "Spatially Resolved Ultraviolet, H\u03b1, Infrared, and Radio Star Formation in M81", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction \u2014 galaxies: individual (M81) \u2014 galaxies: ISM \u2014 galaxies: spiral \u2014\ninfrared: galaxies", "note": "\u00a9 2004 The American Astronomical Society.\n\nReceived 2004 March 26; accepted 2004 May 20.\n\nThe SINGS team is warmly thanked for allowing M81 to be part of the ERO program. We thank Rene Waterbos for providing us with the H\u03b1 and R-band images. The radio image used in this paper was taken with the VLA, which is operated by the National Radio Astronomy Observatory. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA through contract 960785 issued by JPL/Caltech.\n\nPublished - Gordon_2004_ApJS_154_215.pdf
Submitted - 0406064.pdf
", "abstract": "We present Multiband Imaging Photometer for Spitzer (MIPS) observations of M81 at 24, 70, and 160 \u03bcm. The grand design nature of M81 is clearly seen, showing two well-resolved spiral arms containing numerous bright star-forming regions. The MIPS images reveal a significant amount of cold dust associated with the spiral arms. We investigate the variation of the ultraviolet (UV), H\u03b1, and infrared (IR) luminosities and star formation rate (SFR) indicators across the face of M81 using the MIPS images and archival UV and H\u03b1 images. For regions in M81, we find that UV and H\u03b1 SFRs (uncorrected for dust attenuation) are always lower than the IR SFR. The cause of this behavior is dust attenuation and/or using SFR calibrations appropriate for entire galaxies, not regions in galaxies. The characteristics of the dust attenuation for the regions indicate the dust grains and/or geometry are different from those in starburst galaxies. The behavior of the infrared-radio correlation in M81 is seen to vary from the global average, with variations correlated with the morphology of M81.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "215-221", "id_number": "CaltechAUTHORS:20170322-103931321", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-103931321", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA", "grant_number": "960785" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422714", "primary_object": { "basename": "Gordon_2004_ApJS_154_215.pdf", "url": "https://authors.library.caltech.edu/records/dc73a-4b491/files/Gordon_2004_ApJS_154_215.pdf" }, "related_objects": [ { "basename": "0406064.pdf", "url": "https://authors.library.caltech.edu/records/dc73a-4b491/files/0406064.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Gordon, K. D.; P\u00e9rez\u2010Gonz\u00e1lez, P. G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/yx7ef-2n066", "eprint_id": 75374, "eprint_status": "archive", "datestamp": "2023-08-22 02:23:26", "lastmod": "2023-10-25 14:59:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "Philip I." } }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Storrie\u2010Lombardi-L-J", "name": { "family": "Storrie\u2010Lombardi", "given": "L. J." } }, { "id": "Thompson-D-J", "name": { "family": "Thompson", "given": "D. J." } }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Chapman-S", "name": { "family": "Chapman", "given": "S." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Heinrichsen-I", "name": { "family": "Heinrichsen", "given": "I." } }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G. K." }, "orcid": "0000-0002-1977-5717" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Wilson-G", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" } ] }, "title": "Spitzer 24 Micron Observations of Optical/Near\u2010Infrared\u2013Selected Extremely Red Galaxies: Evidence for Assembly of Massive Galaxies at z \u223c 1\u20132?", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: bulges; galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2004 American Astronomical Society. \n\nReceived 2004 April 5. Accepted 2004 May 25. \n\nThis work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA. The spectroscopic 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. We also 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.\n\nPublished - Yan_2004_ApJS_154_75.pdf
", "abstract": "We carried out direct measurement of the fraction of dusty sources in a sample of extremely red galaxies with (R - K_s) \u2265 5.3 mag and K_s < 20.2 mag, using 24 \u03bcm data from the Spitzer Space Telescope. Combining deep 24 \u03bcm Ks- and R-band data over an area of ~64 arcmin^2 in ELAIS N1 of the Spitzer First Look Survey (FLS), we find that 50% \u00b1 6% of our extremely red object (ERO) sample have measurable 24 \u03bcm flux above the 3 \u03c3 flux limit of 40 \u03bcJy. This flux limit corresponds to a star formation rate (SFR) of 12 M_\u2299 yr^(-1) at z ~ 1, much more sensitive than any previous long-wavelength measurement. The 24 \u03bcm-detected EROs have 24 \u03bcm/2.2 \u03bcm and 24 \u03bcm/0.7 \u03bcm flux ratios consistent with infrared luminous, dusty sources at z \u2265 1, and are an order of magnitude too red to be explained by an infrared quiescent spiral or a pure old stellar population at any redshift. Some of these 24 \u03bcm-detected EROs could be active galactic nuclei; however, the fraction among the whole ERO sample is probably small, 10%-20%, as suggested by deep X-ray observations as well as optical spectroscopy. Keck optical spectroscopy of a sample of similarly selected EROs in the FLS field suggests that most of the EROs in ELAIS N1 are probably at z ~ 1. The mean 24 \u03bcm flux (167 \u03bcJy) of the 24 \u03bcm-detected ERO sample roughly corresponds to the rest-frame 12 \u03bcm luminosity, \u03bdL_\u03bd(12 \u03bcm), of 3 \u00d7 10^(10) L_\u2299 at z ~ 1. Using the correlation between IRAS \u03bdL_\u03bd(12 \u03bcm) and infrared luminosity LIR(8-1000 \u03bcm), we infer that the \u3008L_(IR)\u3009 of the 24 \u03bcm-detected EROs is 3 \u00d7 10^(11) and 1 \u00d7 10^(12) L_\u2299 at z = 1.0 and 1.5, respectively, similar to that of local luminous infrared galaxies (LIRGs) and ultraluminous infrared galaxies (ULIRGs). The corresponding SFR would be roughly 50-170 M_\u2299 yr^(-1). If the timescale of this starbursting phase is on the order of 10^8 yr as inferred for the local LIRGs and ULIRGs, the lower limit on the masses of these 24 \u03bcm-detected EROs is 5 \u00d7 10^9 to 2 \u00d7 10^(10) M_\u2299. It is plausible that some of the starburst EROs are in the midst of a violent transformation to become massive early type galaxies at the epoch of z ~ 1-2.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "75-79", "id_number": "CaltechAUTHORS:20170324-082411883", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170324-082411883", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech", "grant_number": "1407" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422917", "primary_object": { "basename": "Yan_2004_ApJS_154_75.pdf", "url": "https://authors.library.caltech.edu/records/yx7ef-2n066/files/Yan_2004_ApJS_154_75.pdf" }, "resource_type": "article", "pub_year": "2004", "author_list": "Yan, Lin; Choi, Philip I.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/zyx7t-k5f74", "eprint_id": 75291, "eprint_status": "archive", "datestamp": "2023-08-22 02:23:16", "lastmod": "2023-10-25 14:55:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P." }, "orcid": "0000-0002-7607-8766" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Stolovy-S-R", "name": { "family": "Stolovy", "given": "S." } }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L." }, "orcid": "0000-0002-5987-5210" }, { "id": "Hurt-R-L", "name": { "family": "Hurt", "given": "R." } }, { "id": "Lowrance-P-J", "name": { "family": "Lowrance", "given": "P." }, "orcid": "0000-0001-8014-0270" }, { "id": "Makovoz-D", "name": { "family": "Makovoz", "given": "D." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Gordon-K-D", "name": { "family": "Gordon", "given": "K. D." } }, { "id": "Alonso\u2010Herrero-A", "name": { "family": "Alonso\u2010Herrero", "given": "A." } }, { "id": "Engelbracht-C-W", "name": { "family": "Engelbracht", "given": "C. W." } }, { "id": "Misselt-K-A", "name": { "family": "Misselt", "given": "K." } }, { "id": "Rieke-G-H", "name": { "family": "Rieke", "given": "G." }, "orcid": "0000-0003-2303-6519" }, { "id": "Rieke-M-J", "name": { "family": "Rieke", "given": "M." }, "orcid": "0000-0002-7893-6170" }, { "id": "Willner-S-P", "name": { "family": "Willner", "given": "S. P." }, "orcid": "0000-0002-9895-5758" }, { "id": "Pahre-M-A", "name": { "family": "Pahre", "given": "M." } }, { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Smith-H-A", "name": { "family": "Smith", "given": "H. A." } } ] }, "title": "The Anatomy of Star Formation in NGC 300", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 300); galaxies: ISM; infrared: galaxies; stars: formation", "note": "\u00a9 2004. The American Astronomical Society. \n\nReceived 2004 March 30; accepted 2004 May 5. \n\nThe Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Extragalactic Database, which is operated by JPL/Caltech, under contract with NASA.\n\nPublished - Helou_2004_ApJS_154_253.pdf
Submitted - 0408248.pdf
", "abstract": "The Spitzer Space Telescope was used to study the mid- to far-infrared properties of NGC 300 and to compare dust emission to H\u03b1 to elucidate the heating of the interstellar medium (ISM) and the star formation cycle at scales smaller than 100 pc. The new data allow us to discern clear differences in the spatial distribution of 8 \u03bcm dust emission with respect to 24 \u03bcm dust and to H II regions traced by H\u03b1 light. The 8 \u03bcm emission highlights the rims of H II regions, and the 24 \u03bcm emission is more strongly peaked in star-forming regions than 8 \u03bcm. We confirm the existence and approximate amplitude of interstellar dust emission at 4.5 \u03bcm, detected statistically in Infrared Space Observatory (ISO) data, and conclude it arises in star-forming regions. When averaging over regions larger than ~1 kpc, the ratio of H\u03b1 to aromatic feature emission in NGC 300 is consistent with the values observed in disks of spiral galaxies. The mid- to far-infrared spectral energy distribution of dust emission is generally consistent with pre-Spitzer models.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "253-258", "id_number": "CaltechAUTHORS:20170321-154553869", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170321-154553869", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422640", "primary_object": { "basename": "0408248.pdf", "url": "https://authors.library.caltech.edu/records/zyx7t-k5f74/files/0408248.pdf" }, "related_objects": [ { "basename": "Helou_2004_ApJS_154_253.pdf", "url": "https://authors.library.caltech.edu/records/zyx7t-k5f74/files/Helou_2004_ApJS_154_253.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Helou, G.; Roussel, H.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rqdn8-mj470", "eprint_id": 75305, "eprint_status": "archive", "datestamp": "2023-08-19 14:11:13", "lastmod": "2023-10-25 14:55:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Fadda-Dario", "name": { "family": "Fadda", "given": "D. T." }, "orcid": "0000-0002-3698-7076" }, { "id": "Marleau-F-R", "name": { "family": "Marleau", "given": "F. R." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "J. J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Choi-Philip-I", "name": { "family": "Choi", "given": "P. I." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Lacy-M", "name": { "family": "Lacy", "given": "M." }, "orcid": "0000-0002-3032-1783" }, { "id": "Wilson-G", "name": { "family": "Wilson", "given": "G." }, "orcid": "0000-0002-6572-7089" }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Fang-Fan", "name": { "family": "Fang", "given": "F." } }, { "id": "Heinrichson-I", "name": { "family": "Heinrichson", "given": "I." } }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Jannuzi-B-T", "name": { "family": "Jannuzi", "given": "B. T." }, "orcid": "0000-0002-1578-6582" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D." }, "orcid": "0000-0003-4401-0430" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Squires-G-K", "name": { "family": "Squires", "given": "G." }, "orcid": "0000-0002-1977-5717" }, { "id": "Teplitz-H-I", "name": { "family": "Teplitz", "given": "H. I." }, "orcid": "0000-0002-7064-5424" } ] }, "title": "The Far- and Mid-Infrared/Radio Correlations in the Spitzer Extragalactic First Look Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2014 galaxies: evolution \u2014 galaxies: high-redshift \u2014 infrared: galaxies", "note": "\u00a9 2004 The American Astronomical Society. \n\nReceived 2004 March 27; accepted 2004 May 5. \n\nThis work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. \n\nThe authors wish to thank V. Charmandaris (Cornell University), D. Dale (University of Wyoming), and an anonymous referee for helpful contributions to this work.\n\nPublished - Appleton_2004_ApJS_154_147.pdf
Submitted - 0406030.pdf
Erratum - Appleton_2005_ApJS_156_111.pdf
", "abstract": "Using the Spitzer Space Telescope and the Very Large Array (VLA), we present the first direct evidence that the well-known far-infrared/radio correlation is valid to cosmologically significant redshift. We also confirm, with improved statistics compared with previous surveys, a similar result for the mid-IR/radio correlation. We explore the dependence of monochromatic q_(24) and q_(70) on z. The results were obtained by matching Spitzer sources at 24 and 70 \u03bcm with VLA 1.4 GHz microjansky radio sources obtained for the Spitzer First Look Survey (FLS). Spectroscopic redshifts have been obtained for over 500 matched IR/radio sources using observations at WIYN and Keck, and archival Sloan Digital Sky Survey (SDSS) data extending out to z > 2. We find that q_(24) shows significantly more dispersion than q_(70). By comparing the observed fluxes at 70, 24, and 4.5 \u03bcm with a library of SED templates, we find that the larger dispersion in q_(24) is predictable in terms of systematic variations in spectral energy distribution (SED) shape throughout the population. Although the models are not able to encompass the full range of observed behavior (both the presence of either extremely flat or extremely steep IR SEDs), the fitting parameters were used to \"k-correct\" the higher z galaxies, which resulted in a reduced scatter in q. For comparison, we also corrected these data using the SED for M82. The results for 24 and 70 \u03bcm provide strong consistent evidence for the universality of the mid- and far-IR/radio correlations out to redshifts of at least z = 1.", "date": "2004-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "154", "number": "1", "publisher": "American Astronomical Society", "pagerange": "147-150", "id_number": "CaltechAUTHORS:20170322-091729060", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-091729060", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1407" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/422425", "primary_object": { "basename": "Appleton_2005_ApJS_156_111.pdf", "url": "https://authors.library.caltech.edu/records/rqdn8-mj470/files/Appleton_2005_ApJS_156_111.pdf" }, "related_objects": [ { "basename": "0406030.pdf", "url": "https://authors.library.caltech.edu/records/rqdn8-mj470/files/0406030.pdf" }, { "basename": "Appleton_2004_ApJS_154_147.pdf", "url": "https://authors.library.caltech.edu/records/rqdn8-mj470/files/Appleton_2004_ApJS_154_147.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Appleton, P. N.; Fadda, D. T.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/na4za-gte12", "eprint_id": 60272, "eprint_status": "archive", "datestamp": "2023-08-22 01:20:11", "lastmod": "2023-10-24 16:22:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Infrared astronomy archived data: overview and prospects", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Infrared processing and analysis center; Astronomy surveys; Infrared astronomy archived data", "note": "\u00a9 2004 COSPAR. Published by Elsevier Ltd.\n\nIPAC and IRSA are funded by the US National Aeronautics and Space Administration under contract with Jet Propulsion Laboratory, California Institute of Technology.", "abstract": "Taken collectively, the data sets from the various past infrared missions form a remarkable base of knowledge about the sky. These data support archival research, motivate and inform planning for new missions. In today's information technology environment, the scientific potential of such a collection is enhanced by the integrated access and analysis tools coming online in efforts generally described as \"Virtual Observatory\" projects. The Infrared Processing and Analysis Center (IPAC) is a major hub of the archived infrared sky, having been designated by NASA as the infrared Science Archive Center. This talk surveys the infrared data sets available today on-line, the prospects for future additions, and the astrophysics enabled both within the infrared domain and by connection to other wavelength domains.", "date": "2004", "date_type": "published", "publication": "Advances in Space Research", "volume": "34", "number": "3", "publisher": "Elsevier", "pagerange": "666-669", "id_number": "CaltechAUTHORS:20150916-080550904", "issn": "0273-1177", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-080550904", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1016/j.asr.2003.04.033", "resource_type": "article", "pub_year": "2004", "author_list": "Helou, G." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/wvxm9-5rz98", "eprint_id": 101228, "eprint_status": "archive", "datestamp": "2023-08-22 01:22:26", "lastmod": "2024-01-14 22:06:59", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Regan-M-W", "name": { "family": "Regan", "given": "Michael W." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "orcid": "0000-0003-3498-2973" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H\u00e9l\u00e8ne" } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "Thomas H." }, "orcid": "0000-0002-4939-734X" } ] }, "title": "The Sings View of Barred Galaxies", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Star Formation; Spiral Galaxy; Wavelength Channel; Galaxy Evolution; MIPS Image", "note": "\u00a9 2004 Springer Science+Business Media New York.", "abstract": "Well-resolved infrared observations of nearby galaxies are of fundamental importance to the study of the processes that affect galactic evolution. Here, we report on the first imaging results from the Spitzer Infrared Nearby Galaxies Survey (SINGS) using observations of the Sb galaxy NGC 7331. We present images of NGC 7331 over a large range of wavelengths that allow us to compare the distributions of gas, stars, and dust in unprecedented detail.", "date": "2004", "date_type": "published", "publisher": "Springer", "place_of_pub": "Dordrecht", "pagerange": "661-665", "id_number": "CaltechAUTHORS:20200211-143303314", "isbn": "978-94-015-7085-5", "book_title": "Penetrating Bars through Masks of Cosmic Dust: The Hubble Tuning Fork strikes a New Note", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200211-143303314", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Block-D-L", "name": { "family": "Block", "given": "David L." } }, { "id": "Puerari-I", "name": { "family": "Puerari", "given": "Iv\u00e2nio" } }, { "id": "Freeman-K-C", "name": { "family": "Freeman", "given": "Kenneth C." } }, { "id": "Groess-R", "name": { "family": "Groess", "given": "Robert" } }, { "id": "Block-E-K", "name": { "family": "Block", "given": "Elizabeth K." } } ] }, "doi": "10.1007/978-1-4020-2862-5_55", "resource_type": "book_section", "pub_year": "2004", "author_list": "Regan, Michael W.; Armus, Lee; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7gct5-1pm68", "eprint_id": 106122, "eprint_status": "archive", "datestamp": "2023-08-22 00:50:18", "lastmod": "2023-10-23 16:04:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." }, "orcid": "0000-0001-5617-7129" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Beck-R", "name": { "family": "Beck", "given": "R." } }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "J. J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Bosma-A", "name": { "family": "Bosma", "given": "A." } }, { "id": "Matthews-Keith-Astronomy", "name": { "family": "Matthews", "given": "K." } }, { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" } ] }, "title": "Nascent Starbursts in Synchrotron-deficient Galaxies with Hot Dust", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: starburst; galaxies: individual (IC 1953 NGC 1377 NGC 4418 NGC 4491); infrared: galaxies; radio continuum: galaxies; supernova remnants", "note": "\u00a9 2003. The American Astronomical Society. \n\nReceived 2002 December 17; accepted 2003 May 2. \n\nWe are grateful to Antonio Garc\u00eda-Barreto for providing us his H_\u03b1+[N II] and I-band maps of IC 1953, to Sangeeta Malhotra for mentioning the peculiar infrared properties of NGC 4418, thereby arousing our curiosity, to the persons who assisted us in the observations at Effelsberg, Palomar, and La Silla, and to James Brauher for communicating us some fluxes in advance of publication. 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 IPAC/Caltech, funded by NASA and the National Science Foundation. The ISOCAM data presented in this paper were analyzed using and adapting the CIA package, a joint development by the ESA Astrophysics Division and the ISOCAM Consortium. This research also benefited from the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory of Caltech.\n\nH. Roussel et al 2004 ApJ 601 1160\n\nPublished - Roussel_2003_ApJ_593_733.pdf
Accepted Version - 0305046.pdf
Erratum - pdf
", "abstract": "Three nearby galaxies that have abnormally high infrared-to-radio continuum ratios, NGC 1377, IC 1953, and NGC 4491, are investigated with a view to understanding the physical origin of their peculiarity. We review the existing data and present new radio continuum measurements along with near-infrared integral-field spectroscopy and molecular gas observations. The three galaxies have low luminosities but starburst-like infrared colors; in NGC 1377, no synchrotron emission is detected at any wavelength; in IC 1953, the observed synchrotron component is attributable to the spiral disk alone and is lacking in the central regions; and the radio spectrum of NGC 4491 is unusually flat. We also compare and contrast them with NGC 4418, a heavily extinguished galaxy that shares some attributes with them. After examining various scenarios, we conclude that these galaxies are most likely observed within a few megayears of the onset of an intense star formation episode after being quiescent for at least \u2248100 Myr. This starburst, while heating the dust, has not produced optical signatures or a normal amount of cosmic rays yet. We briefly discuss the statistics of such galaxies and what they imply for star formation surveys.", "date": "2003-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "593", "number": "2", "publisher": "American Astronomical Society", "pagerange": "733-759", "id_number": "CaltechAUTHORS:20201016-145652458", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201016-145652458", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/376691", "primary_object": { "basename": "0305046.pdf", "url": "https://authors.library.caltech.edu/records/7gct5-1pm68/files/0305046.pdf" }, "related_objects": [ { "basename": "Roussel_2003_ApJ_593_733.pdf", "url": "https://authors.library.caltech.edu/records/7gct5-1pm68/files/Roussel_2003_ApJ_593_733.pdf" }, { "basename": "pdf", "url": "https://authors.library.caltech.edu/records/7gct5-1pm68/files/pdf" } ], "resource_type": "article", "pub_year": "2003", "author_list": "Roussel, H.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/ftsf2-c5v61", "eprint_id": 75300, "eprint_status": "archive", "datestamp": "2023-08-19 11:23:51", "lastmod": "2023-10-25 14:55:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Condon-J-J", "name": { "family": "Condon", "given": "J. J." }, "orcid": "0000-0003-4724-1939" }, { "id": "Cotton-W-D", "name": { "family": "Cotton", "given": "W. D." } }, { "id": "Yin-Q-F", "name": { "family": "Yin", "given": "Q.-F." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Storrie-Lombardi-L-J", "name": { "family": "Storrie-Lombardi", "given": "L. J." }, "orcid": "0000-0002-5987-5210" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Werner-M-W", "name": { "family": "Werner", "given": "M. W." } } ] }, "title": "The SIRTF First-Look Survey. I. VLA Image and Source Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2014 galaxies: active \u2014 galaxies: starburst \u2014 infrared radiation \u2014 radio continuum \u2014 surveys", "note": "\u00a9 2003 The American Astronomical Society. \n\nReceived 2003 January 27; accepted 2003 February 5. \n\nQ. F. Yin was supported in part by Jet Propulsion Laboratory contract number 1234549.\n\nPublished - Condon_2003_AJ_125_2411.pdf
", "abstract": "The First-Look Survey (FLS) of the Space Infrared Telescope Facility (SIRTF) will cover about 5 deg^2 centered on J2000.0 \u03b1 = 17^h18^m, \u03b4 = +59\u00b030' in order to characterize the extragalactic infrared sky 2 orders of magnitude deeper than the IRAS survey. We expect that most of the FLS far-infrared (\u03bb = 160, 70, and 24 \u03bcm) sources will be star-forming galaxies obeying the very tight far-infrared/radio correlation and will be continuum radio sources with flux densities S \u2273100 \u03bcJy at \u03bd = 1.4 GHz. Conversely, radio sources stronger than 100 \u03bcJy are usually powered by star-forming galaxies, plus some active galactic nuclei, and most should be detectable by the SIRTF FLS. Thus, a sensitive radio survey can be used to select and identify most of the SIRTF FLS source population before launch. We used the B configuration of the VLA to make an image of the FLS area at \u03bd = 1.4 GHz with \u03c3 \u2248 23 \u03bcJy beam^(-1) rms fluctuations, \u03b8 = 5.\"0 resolution, and \u03c3_\u03b1 \u2248 \u03c3\u03b4 \u227e0.\"5 rms uncertainties in right ascension and declination. The resulting radio image and catalog of 3565 radio components with peak flux densities S_p \u2265 5 \u03c3 = 115 \u03bcJy beam^(-1) have been released via the Web to expedite follow-up optical identification and spectroscopy.", "date": "2003-05", "date_type": "published", "publication": "Astronomical Journal", "volume": "125", "number": "5", "publisher": "American Astronomical Society", "pagerange": "2411-2426", "id_number": "CaltechAUTHORS:20170322-085802408", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-085802408", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL", "grant_number": "1234549" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/374633", "primary_object": { "basename": "Condon_2003_AJ_125_2411.pdf", "url": "https://authors.library.caltech.edu/records/ftsf2-c5v61/files/Condon_2003_AJ_125_2411.pdf" }, "resource_type": "article", "pub_year": "2003", "author_list": "Condon, J. J.; Cotton, W. D.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/s6gv2-ykh05", "eprint_id": 92273, "eprint_status": "archive", "datestamp": "2023-08-19 11:10:29", "lastmod": "2024-01-14 21:26:04", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "P." } }, { "id": "Emming-J-G", "name": { "family": "Emming", "given": "J." } }, { "id": "Finley-P-T", "name": { "family": "Finley", "given": "P. T." } }, { "id": "Gautier-T-N-III", "name": { "family": "Gautier", "given": "T. N." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hopkins-R-A", "name": { "family": "Hopkins", "given": "R. A." } }, { "id": "Johnson-G-B", "name": { "family": "Johnson", "given": "G. B." } }, { "id": "Keene-Jocelyn", "name": { "family": "Keene", "given": "J." } }, { "id": "Kwok-J-H", "name": { "family": "Kwok", "given": "J. H." } }, { "id": "Lee-Jeff-H", "name": { "family": "Lee", "given": "J. H." } }, { "id": "Nieczkoski-S-J", "name": { "family": "Nieczkoski", "given": "S. J." } }, { "id": "Roellig-T-L", "name": { "family": "Roellig", "given": "T. L." } }, { "id": "Schweickart-R-B", "name": { "family": "Schweickart", "given": "R." } } ] }, "title": "Operating SIRTF for maximum lifetime", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cryogenics, infrared telescopes", "note": "\u00a9 2003 Society of Photo-optical Instrumentation Engineers (SPIE).\n\nPublished - 153.pdf
", "abstract": "The instruments of the Space Infrared Telescope Facility (SIRTF) are cooled directly by liquid helium, while the optical system is cooled by helium vapor. The greater the power dissipation into the liquid helium, the more vapor is produced, and the colder the telescope. Observations at shorter wavelengths do not require telescope temperatures as low as those required at shorter wavelengths. By taking advantage of this, it may be possible to extend the helium and mission lifetime by 10% or even 20%.", "date": "2003-03-05", "date_type": "published", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_pub": "Bellingham, WA", "pagerange": "153-161", "id_number": "CaltechAUTHORS:20190115-084104903", "isbn": "9780819446299", "book_title": "IR Space Telescopes and Instruments", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190115-084104903", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Mather-J-C", "name": { "family": "Mather", "given": "John C." } } ] }, "doi": "10.1117/12.461953", "primary_object": { "basename": "153.pdf", "url": "https://authors.library.caltech.edu/records/s6gv2-ykh05/files/153.pdf" }, "resource_type": "book_section", "pub_year": "2003", "author_list": "Lawrence, C. R.; Eisenhardt, P.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/mzdpp-4dr83", "eprint_id": 85003, "eprint_status": "archive", "datestamp": "2023-08-19 10:11:05", "lastmod": "2023-10-18 17:03:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunt-L-K", "name": { "family": "Hunt", "given": "L. K." }, "orcid": "0000-0001-9162-2371" }, { "id": "Giovanardi-C", "name": { "family": "Giovanardi", "given": "C." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Hot dust in normal star-forming galaxies: J H K L^' photometry of the ISO Key Project sample", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: spiral - galaxies: starbursts - galaxies: ISM - ISM: dust", "note": "\u00a9 2002 ESO. \n\nReceived: 13 August 2002. Accepted: 12 September 2002. \n\nThe TIRGO staff was instrumental in the success of these observations. We are grateful to Giovanni Moriondo who valiantly attempted to observe for this project, and to the TIRGO Time Allocation Committee for generous time allocations. We gladly acknowledge enlightening discussions with Marc Sauvage, and would like to thank an anonymous referee for several insightful comments.\n\nPublished - aa3010.pdf
Submitted - 0209471.pdf
", "abstract": "We present JHK and 3.8 \u03bcm\u2002(L^') photometry of 26 galaxies in the Infrared Space Observatory (ISO) Normal Galaxy Key Project (KP) sample and of seven normal ellipticals with the aim of investigating the origin of the 4 \u03bcm\u2002emission. The majority of the KP galaxies, and all the ellipticals, have K - L \u227e 1.0, consistent with stellar photospheres plus moderate dust extinction. Ten of the 26 KP galaxies have K - L \u2273 1.0, corresponding to a flat or rising 4 \u03bcm\u2002continuum, consistent with significant emission from hot dust at 600\u20131000\u2009K. K -L is anticorrelated with ISO flux ratio F_(6.75)/F15, weakly correlated with line ratio [O\u2009i]/[C\u2009ii], but not with [C\u2009ii]/FIR or IRAS ratio F_(60)/F_(100). Photodissociation-region models for these galaxies show that the hot dust responsible for red K - L resides in regions of high pressure and intense far-ultraviolet radiation field. Taken together, these results suggest that star formation in normal star-forming galaxies can assume two basic forms: an \"active\", relatively rare, mode characterized by hot dust, suppressed Aromatic Features in Emission (AFEs), high pressure, and intense radiation field; and the more common \"passive\" mode that occurs under more quiescent physical conditions, with AFEs, and without hot dust. The occurrence of these modes appears to only weakly depend on the star-formation rate per unit area. Passive star formation over large scales makes up the bulk of star-forming activity locally, while the \"active\" regime may dominate at high redshifts.", "date": "2002-10-21", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "394", "number": "3", "publisher": "EDP Sciences", "pagerange": "873-882", "id_number": "CaltechAUTHORS:20180228-100722335", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180228-100722335", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1051/0004-6361:20021335", "primary_object": { "basename": "0209471.pdf", "url": "https://authors.library.caltech.edu/records/mzdpp-4dr83/files/0209471.pdf" }, "related_objects": [ { "basename": "aa3010.pdf", "url": "https://authors.library.caltech.edu/records/mzdpp-4dr83/files/aa3010.pdf" } ], "resource_type": "article", "pub_year": "2002", "author_list": "Hunt, L. K.; Giovanardi, C.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/965nh-x2a10", "eprint_id": 74478, "eprint_status": "archive", "datestamp": "2023-08-21 22:36:10", "lastmod": "2023-10-24 22:41:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dale-D-A", "name": { "family": "Dale", "given": "Daniel A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "David T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Condon-J-J", "name": { "family": "Condon", "given": "James J." }, "orcid": "0000-0003-4724-1939" } ] }, "title": "Multiwavelength Observations of the Low-Metallicity Blue Compact Dwarf Galaxy SBS 0335\u2212052", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (SBS 0335-052); galaxies: ISM", "note": "\u00a9 2001 American Astronomical Society. \n\nReceived 2001 June 3. Accepted 2001 July 9. \n\nWe are happy to acknowledge M. Sauvage for the generous donation of unpublished ISO results. We are also grateful T. Murphy helped with the LWS observations and the PIFS data reduction, and for the assistance E. Egami provided with the PIFS observing run. The comments from an anonymous referee helped to improve the text. The W. M. Keck Observatory is operated as a scientific partnership between the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. It was made possible by the generous financial support of the W. M. Keck Foundation. ISO is an ESA project with instruments funded by ESA member states (especially the PI countries: France, Germany, The Netherlands and the United Kingdom) and with the participation of ISAS and NASA. This research has made use of the NASA/IPAC Extragalactic Database, which is operated by JPL/Caltech, under contract with NASA. B. T. S. is supported by grants from the NSF and NASA. D. T. F. acknowledges support from NSF grant AST 96-13717 made to the Owens Valley Millimeter Array.\n\nPublished - Dale_2001_AJ_122_1736.pdf
Accepted Version - 0107108.pdf
", "abstract": "New infrared and millimeter observations from Keck, Palomar, ISO, and OVRO and archival data from the NRAO^(**) VLA and IRAS are presented for the low-metallicity blue compact dwarf galaxy SBS 0335-052. Mid-infrared imaging shows this young star-forming system is compact (0farcs31; 80 pc) at 12.5 \u03bcm. The large Br\u03b3 equivalent width (235 \u00c5) measured from integral field spectroscopy is indicative of a ~5 Myr starburst. The central source appears to be optically thin in emission, containing both a warm (~80 K) and a hot (~210 K) dust component, and the overall interstellar radiation field is quite intense, about 10,000 times the intensity in the solar neighborhood. CO emission is not detected, though the galaxy shows an extremely high global H I gas-to-dust mass ratio, high even for blue compact dwarfs. Finally, the galaxy's ratio of mid-infrared-to-optical and mid-to-near-infrared luminosities are quite high, whereas its far-infrared-to-radio and far-infrared-to-optical flux ratios are surprisingly similar to what is seen in normal star-forming galaxies. The relatively high bolometric infrared-to-radio ratio is more easily understood in the context of such a young system with negligible nonthermal radio continuum emission. These new lines of evidence may outline features common to primordial galaxies found at high redshift.", "date": "2001-10", "date_type": "published", "publication": "Astronomical Journal", "volume": "122", "number": "4", "publisher": "American Astronomical Society", "pagerange": "1736-1746", "id_number": "CaltechAUTHORS:20170222-162910356", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-162910356", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "ESA Member States" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST 96-13717" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/323308", "primary_object": { "basename": "0107108.pdf", "url": "https://authors.library.caltech.edu/records/965nh-x2a10/files/0107108.pdf" }, "related_objects": [ { "basename": "Dale_2001_AJ_122_1736.pdf", "url": "https://authors.library.caltech.edu/records/965nh-x2a10/files/Dale_2001_AJ_122_1736.pdf" } ], "resource_type": "article", "pub_year": "2001", "author_list": "Dale, Daniel A.; Helou, George; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/e2xc3-7hk84", "eprint_id": 99355, "eprint_status": "archive", "datestamp": "2023-08-19 07:40:54", "lastmod": "2023-10-18 18:14:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Contursi-A", "name": { "family": "Contursi", "given": "A." } }, { "id": "Brauher-J", "name": { "family": "Brauher", "given": "J." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "The [CII] and [OI] emission lines in NGC6946 and NGC1313", "ispublished": "pub", "full_text_status": "restricted", "keywords": "ISO, Far infrared structure lines, galaxies, galaxies, ISMdust, gas, ISM, heating, cooling", "note": "\u00a9 2001 Kluwer Academic Publishers.", "abstract": "The [CII (158 \u03bcm)] fine structure line, which is the principal cooling line of the atomic gas, in two nearby galaxies observed with LWS on board ISO is compared to dust and HI gas emission and heating intensity. The relation between photoelectric effect on different grains populations, dust and gas heating found for a sample of 60 normal galaxies for which global [CII] measurements are available, still holds on scale of \u223c1.5 kpc. We also succeed in detecting cooling from a low density diffuse atomic gas associated with the diffuse optical disk in both galaxies, accounting typically for \u223c 30\u201340% of the total [CII] emission.", "date": "2001-05", "date_type": "published", "publication": "Astrophysics and Space Science", "volume": "277", "number": "S1", "publisher": "Springer", "pagerange": "59-62", "id_number": "CaltechAUTHORS:20191018-094103570", "issn": "0004-640X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191018-094103570", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1023/a:1012771409683", "resource_type": "article", "pub_year": "2001", "author_list": "Contursi, A.; Brauher, J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/vwwsg-qka09", "eprint_id": 101534, "eprint_status": "archive", "datestamp": "2023-08-21 20:47:25", "lastmod": "2024-01-14 22:08:07", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lonsdale-Carol-J", "name": { "family": "Lonsdale", "given": "Carol J." }, "orcid": "0000-0003-0898-406X" }, { "id": "Hurt-R-L", "name": { "family": "Hurt", "given": "Robert" } }, { "id": "Smith-H-E", "name": { "family": "Smith", "given": "Harding E." } }, { "id": "Levine-D-A", "name": { "family": "Levine", "given": "Deborah" } }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Chas" }, "orcid": "0000-0002-5627-5471" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Cesarsky-C-J", "name": { "family": "Cesarsky", "given": "Catherine J." } }, { "id": "Lemke-D", "name": { "family": "Lemke", "given": "Dietrich" } }, { "id": "Klaas-U", "name": { "family": "Klaas", "given": "Ulrich" } }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "David" }, "orcid": "0000-0002-7631-647X" } ] }, "title": "ISO-IRAS Faint Galaxy Survey: ISOCAM Imaging and Optical Spectroscopy", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Background Source; Color Selection; Infrared Galaxy; Narrow Slice; Emission Line Galaxy", "note": "\u00a9 2000 Springer-Verlag Berlin Heidelberg.\n\nThis research has been supported in part by grants from NASA to IPAC\nand UCSD and by the US NSF to UCSD.", "abstract": "The goal of the ISO-IRAS Faint Galaxy Survey was to obtain a sample of the most distant, highest luminosity infrared galaxies from the 0.75 million sources in the IRAS Faint Source Survey. The strategy involved providing a large sample of sources, selected to be faint, high-luminosity (hence highredshift) infrared galaxies, that ISO could select from to fill short (\u223c 12 mins) schedule gaps. The initial observing program involved CAM LW10 imaging at 12\u03bcm plus PHT 90\u03bcm photometry (PHT22) in order to obtain SED information and to provide good positions and reliable identifications for optical spectroscopy and other follow-up observations.", "date": "2000", "date_type": "published", "publisher": "Springer", "place_of_pub": "Berlin", "pagerange": "267-274", "id_number": "CaltechAUTHORS:20200225-110915168", "isbn": "978-3-540-67479-5", "book_title": "ISO Surveys of a Dusty Universe", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200225-110915168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "University of California, San Diego" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Lemke-D", "name": { "family": "Lemke", "given": "D." } }, { "id": "Stickel-M", "name": { "family": "Stickel", "given": "M." } }, { "id": "Wilke-K", "name": { "family": "Wilke", "given": "K." } } ] }, "doi": "10.1007/3-540-45553-1_34", "resource_type": "book_section", "pub_year": "2000", "author_list": "Lonsdale, Carol J.; Hurt, Robert; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/s07jn-2ae61", "eprint_id": 103934, "eprint_status": "archive", "datestamp": "2023-08-21 20:47:53", "lastmod": "2024-01-15 04:31:57", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Normal Galaxies in the Infrared", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Optical Depth; Star Formation; Star Formation Rate; Spectral Energy Distribution; Infrared Emission", "note": "\u00a9 2000 EDP Sciences, Springer-Verlag.\n\nFirst Online: 31 July 2002.\n\nI would like to thank the organizers of the Summer School for the invitation\nto participate in this exciting encounter, and for their patience when\nit came to submitting the manuscript. James Lequeux in addition provided\nhelp and comments on the manuscript. Danny Dale and Alessandra\nContursi helped with customized plots, and a careful reading of the manuscript. This work was carried out at the California Institute of\nTechnology, under funding by the National Aeronautics and Space\nAdministration. It was supported in part by the ISO Data Analysis\nFunding Program, administered for NASA by the Jet Propulsion\nLaboratory, California Institute of Technology.", "abstract": "A normal galaxy is one that derives its luminosity primarily from nuclear burning in stars, and is at neither the high nor the low extreme of the luminosity distribution. In such galaxies, the visible and ultraviolet is the only direct window onto the photospheres of stars, whereas the rest of the spectrum reflects reprocessed light from stars (Fig. 1). Dust in the interstellar medium reprocesses part of the stellar luminosity into infrared emission from a few \u03bcm to 1 mm or longer wavelengths. The radio emission at millimeter wavelengths derives from thermal emission from ionized plasmas in HII regions, whereas the synchrotron emission from cosmic ray electrons (CR e\u207b) trapped in the magnetic field of the galaxy fill in the cm-wavelength spectrum. In the X-rays, the luminosity is dominated by very hot plasmas at T \u2273 10 K\u2076 created by shocks from supernova explosions. The global spectrum of normal galaxies has some very stable signatures, and other quite variable aspects. Much of this article is an attempt to understand what makes for stability in the spectrum, and what significance to attach to the variable parameters.", "date": "2000", "date_type": "published", "publisher": "Springer", "place_of_pub": "Berlin", "pagerange": "337-380", "id_number": "CaltechAUTHORS:20200615-163436555", "isbn": "978-3-540-67386-6", "book_title": "Astronomie spatiale infrarouge, aujourd'hui et demain: Infrared space astronomy, today and tomorrow", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200615-163436555", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "contributors": { "items": [ { "id": "Casoli-F", "name": { "family": "Casoli", "given": "F." } }, { "id": "Lequeux-J", "name": { "family": "Lequeux", "given": "J." } }, { "id": "David-F", "name": { "family": "David", "given": "F." } } ] }, "doi": "10.1007/3-540-45573-6_8", "resource_type": "book_section", "pub_year": "2000", "author_list": "Helou, G." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/jdv3k-37157", "eprint_id": 74495, "eprint_status": "archive", "datestamp": "2023-08-22 13:07:01", "lastmod": "2023-10-24 22:41:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levine-D-A", "name": { "family": "Levine", "given": "Deborah A." } }, { "id": "Lonsdale-C-J", "name": { "family": "Lonsdale", "given": "Carol J." }, "orcid": "0000-0003-0898-406X" }, { "id": "Hurt-R-L", "name": { "family": "Hurt", "given": "Robert L." } }, { "id": "Smith-H-E", "name": { "family": "Smith", "given": "Harding E." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles" }, "orcid": "0000-0002-5627-5471" }, { "id": "Cesarsky-C", "name": { "family": "Cesarsky", "given": "Catherine" } }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "David" }, "orcid": "0000-0002-7631-647X" }, { "id": "Klaas-U", "name": { "family": "Klaas", "given": "Ulrich" } }, { "id": "Laureijs-R", "name": { "family": "Laureijs", "given": "Rene" } }, { "id": "Lemke-D", "name": { "family": "Lemke", "given": "Detrich" } }, { "id": "Lord-S-D", "name": { "family": "Lord", "given": "Steven" } }, { "id": "McMahon-R-G", "name": { "family": "McMahon", "given": "Richard" } }, { "id": "Moshir-M", "name": { "family": "Moshir", "given": "Mehrdad" } }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Van-Buren-D", "name": { "family": "Van Buren", "given": "Dave" } }, { "id": "Wehrle-A-E", "name": { "family": "Wehrle", "given": "Ann" } }, { "id": "Wolstencroft-R", "name": { "family": "Wolstencroft", "given": "Ray" } } ] }, "title": "First Results from the ISO\u2010IRAS Faint Galaxy Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: photometry; infrared: galaxies; surveys", "note": "\u00a9 1998 American Astronomical Society. \n\nReceived 1997 November 24. Accepted 1998 April 3. \n\nWe wish to thank the staff of Lick Observatory for supporting the optical observations reported here, especially Rem Stone for measuring the filter curves and also K. H. Smith for tireless assistance with the observations. The ISOCAM data presented in this paper were reduced using components of CIA, a joint development by the ESA Astrophysics Division and the ISOCAM Consortium led by the ISOCAM PI, C. Cesarsky, Direction des Sciences de la Matiere, CEA-Saclay, France. The ISOPHOT data were reduced using PIA, which is a joint development by the ESA Astrophysics Division and the ISOPHOT consortium. This project has benefited from the use of the NASA Extragalactic Database, supported at IPAC by NASA, and the STScI Digitized Sky Survey images of the Palomar Observatory Sky Survey. H. E. S. thanks IPAC for providing continuing support as a home away from home. IPAC/JPL is supported by NASA. Additional support of this project has been provided by NASA ISO grants to IPAC and to UCSD.\n\nPublished - Levine_1998_ApJ_504_64.pdf
", "abstract": "We present the first results from the ISO-IRAS Faint Galaxy Survey (IIFGS), a program designed to obtain ISO observations of the most distant and luminous galaxies in the IRAS Faint Source Survey by filling short gaps in the ISO observing schedule with pairs of 12 \u03bcm ISOCAM and 90 \u03bcm ISOPHOT observations. As of 1997 October, over 500 sources have been observed, with an ISOCAM detection rate over 80%, covering over 1.25 deg^2 of sky to an 11.5 \u03bcm point-source completeness limit of approximately 1.0 mJy (corresponding to a ~10 \u03c3 detection sensitivity). Observations are presented for nine sources detected by ISOPHOT and ISOCAM early in the survey for which we have ground-based G- and I-band images and optical spectroscopy. The ground-based data confirm that the IIFGS strategy efficiently detects moderate-redshift (z = 0.11-0.38 for this small sample) strong emission line galaxies with L_(60 \u03bcm) \u2273 10^(11) L_\u2609; one of our sample has L_(60 \u03bcm) > 10^(12) L_\u2609 (H_0 = 75 km s^(-1) Mpc^(-1), \u03a9 = 1). The infrared-optical spectral energy distributions are comparable to those of nearby luminous infrared galaxies, which span the range from pure starburst (e.g., Arp 220) to infrared QSO (Mrk 231). Two of the systems show signs of strong interaction, and four show active galactic nucleus (AGN)-like excitation; one of the AGNs, F15390+6038, which shows a high excitation Seyfert 2 spectrum, has an unusually warm far- to mid-infrared color and may be an obscured QSO. The IIFGS sample is one of the largest and deepest samples of infrared-luminous galaxies available, promising to be a rich sample for studying infrared-luminous galaxies up to z ~ 1 and for understanding the evolution of infrared galaxies and the star formation rate in the universe.", "date": "1998-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "504", "number": "1", "publisher": "American Astronomical Society", "pagerange": "64-76", "id_number": "CaltechAUTHORS:20170223-104256512", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170223-104256512", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Lick Observatory" }, { "agency": "NASA/JPL" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/306065", "primary_object": { "basename": "Levine_1998_ApJ_504_64.pdf", "url": "https://authors.library.caltech.edu/records/jdv3k-37157/files/Levine_1998_ApJ_504_64.pdf" }, "resource_type": "article", "pub_year": "1998", "author_list": "Levine, Deborah A.; Lonsdale, Carol J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rzqtz-vfd05", "eprint_id": 96172, "eprint_status": "archive", "datestamp": "2023-08-22 12:27:52", "lastmod": "2024-01-14 21:46:48", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" } ] }, "title": "The ISO Perspective on Normal Galaxies", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Star Formation; Spiral Galaxy; Star Formation Rate; Starburst Galaxy; Normal Galaxy", "note": "\u00a9 1998 Springer Science+Business Media Dordrecht. \n\nISO is an ESA project with instruments funded by ESA member states, with participation by ISAS and NASA. This work was supported by ISO data analysis funding from the National Aeronautics and Space Administration, and was carried out at the Infrared Processing and Analysis Center and the Jet Propulsion Laboratory of the California Institute of Technology.", "abstract": "Based on results from the first half of its mission, ISO (Kessler et al. 1996) is contributing to our understanding of normal galaxies by offering effective gauges of the physical conditions within the interstellar medium (ISM) of galaxies. ISO data permit a more precise and detailed characterization of the radiation, dust and gas deep within many more galaxies than had been previously possible. This in turn yields new insight into the regulation mechanisms of star formation and galaxy evolution. Apart from these ISM diagnostics, ISO also contributes a vastly improved empirical description of galaxies at all infrared wavelengths, which will be critical in guiding the search for the origins and early life of galaxies.", "date": "1998", "date_type": "published", "publisher": "Springer", "place_of_pub": "Dordrecht", "pagerange": "1134-1136", "id_number": "CaltechAUTHORS:20190605-154512650", "isbn": "978-0-7923-5556-4", "book_title": "Highlights of Astronomy", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190605-154512650", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ESA Member States" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Andersen-J", "name": { "family": "Andersen", "given": "J." } } ] }, "doi": "10.1007/978-94-011-4778-1_155", "resource_type": "book_section", "pub_year": "1998", "author_list": "Helou, G." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/e3v3a-cps78", "eprint_id": 74532, "eprint_status": "archive", "datestamp": "2023-08-19 02:15:13", "lastmod": "2024-01-13 20:25:20", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-H-E", "name": { "family": "Smith", "given": "Harding E." } }, { "id": "Hurt-R-L", "name": { "family": "Hurt", "given": "Robert L." } }, { "id": "Lonsdale-C-J", "name": { "family": "Lonsdale", "given": "Carol J." }, "orcid": "0000-0003-0898-406X" }, { "id": "Levine-D-A", "name": { "family": "Levine", "given": "Deborah A." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles" }, "orcid": "0000-0002-5627-5471" }, { "id": "Cesarsky-C", "name": { "family": "Cesarsky", "given": "Catherine" } }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "David" }, "orcid": "0000-0002-7631-647X" }, { "id": "Klaas-U", "name": { "family": "Klaas", "given": "Ulrich" } }, { "id": "Laureijs-R", "name": { "family": "Laureijs", "given": "Rene" } }, { "id": "Lemke-D", "name": { "family": "Lemke", "given": "Detrich" } }, { "id": "Lord-S-D", "name": { "family": "Lord", "given": "Steven" } }, { "id": "McMahon-R-G", "name": { "family": "McMahon", "given": "Richard" } }, { "id": "Moshir-M", "name": { "family": "Moshir", "given": "Mehrdad" } }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Van-Buren-D", "name": { "family": "Van Buren", "given": "Dave" } }, { "id": "Wehrle-A-E", "name": { "family": "Wehrle", "given": "Ann" } }, { "id": "Wolstencroft-R", "name": { "family": "Wolstencroft", "given": "Ray" } } ] }, "title": "The ISO-IRAS Faint Galaxy Survey", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 1998 Astronomical Society of the Pacific.\n\nPublished - 1998ASPC__146__220S.pdf
", "abstract": "The ISO-IRAS Faint Galaxy Survey will obtain comprehensive\nspace- and ground-based observations of the most distant and luminous galaxies in the IRAS Faint Source Survey. ISO observations are obtained by filling short gaps in the ISO observing schedule with pairs of 11.5\u03bcm ISOCAM and 90\u03bcm ISOPHOT observations. As of the October 1997 date of this Conference, over 500 sources have been observed by ISO with an ISOCAM detection rate exceeding 803. Ground-based\nspectrophotometry confirms that the IIFGS efficiently detects moderateredshift, strong emission line Luminous Infrared Galaxies. Spectrophotometry is currently available for 67 galaxies with 0.07 < z < 0. 7 and\nL_(fir) > 10^(11) L_\u2609. The galaxies are comparable to nearby LIGs, showing HII/Liner excitation; about 10% exhibit strong AGN characteristics. As a part of this survey we will cover over 1.25 square degrees of\nsky to an 11.5\u03bcm limit of approximately l.0mJy, allowing a sensitive estimate of the 11.5\u03bcm logN-logS Relationship. Preliminary ll.5\u03bcm source counts suggest substantial evolution in the mid-infrared galaxy population.", "date": "1998", "date_type": "published", "publisher": "Astronomical Society of the Pacific", "place_of_pub": "San Francisco, CA", "pagerange": "220-224", "id_number": "CaltechAUTHORS:20170227-074348896", "isbn": "1-886733-66-X", "book_title": "The Young Universe", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170227-074348896", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "D'Odorico-S", "name": { "family": "D'Odorico", "given": "S." } }, { "id": "Fontana-A", "name": { "family": "Fontana", "given": "A." } }, { "id": "Giallongo-E", "name": { "family": "Giallongo", "given": "E." } } ] }, "primary_object": { "basename": "1998ASPC__146__220S.pdf", "url": "https://authors.library.caltech.edu/records/e3v3a-cps78/files/1998ASPC__146__220S.pdf" }, "resource_type": "book_section", "pub_year": "1998", "author_list": "Smith, Harding E.; Hurt, Robert L.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/1g9y4-qcf47", "eprint_id": 60271, "eprint_status": "archive", "datestamp": "2023-08-19 01:03:32", "lastmod": "2024-01-13 16:24:58", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hurt-R-L", "name": { "family": "Hurt", "given": "R. L." } }, { "id": "Lonsdale-C-J", "name": { "family": "Lonsdale", "given": "C. J." }, "orcid": "0000-0003-0898-406X" }, { "id": "Levine-D-A", "name": { "family": "Levine", "given": "D. A." } }, { "id": "Smith-H-E", "name": { "family": "Smith", "given": "H. E." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Van-Buren-D", "name": { "family": "Van Buren", "given": "D." } }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C. A." }, "orcid": "0000-0002-5627-5471" }, { "id": "Lord-S-D", "name": { "family": "Lord", "given": "S. D." } }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Moshir-M", "name": { "family": "Moshir", "given": "M." } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Wehrle-A-E", "name": { "family": "Wehrle", "given": "A." } }, { "id": "Cesarsky-C", "name": { "family": "Cesarsky", "given": "C." } }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "id": "Klaas-U", "name": { "family": "Klaas", "given": "U." } }, { "id": "Laureijs-R", "name": { "family": "Laureijs", "given": "R." } }, { "id": "Lemke-D", "name": { "family": "Lemke", "given": "D." } }, { "id": "McMahon-R-G", "name": { "family": "McMahon", "given": "R. G." } }, { "id": "Wolstencroft-R-D", "name": { "family": "Wolstencroft", "given": "R. D." } } ] }, "title": "The ISO-IRAS Faint Galaxy Survey: Early results", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 1997 American Institute of Physics. Published online 10 February 1997.\n\nPublished - 1.52822.pdf
", "abstract": "We present preliminary results for AGNs and starburst galaxies the ISO-IRAS Faint Galaxy Survey (IIFGS). The goal of the survey is to produce a database of infrared-luminous galaxies at redshifts of about 0.1\u20131 to help explore the AGN-starburst relationship, study the cosmological evolution of luminous infrared galaxies, and identify possible protogalaxy candidates. The candidate list of \u223c3700 sources has been extracted from the IRAS Faint Source Survey using criteria selecting for faint, infrared-bright galaxies. The ISO observations will confirm the IRAS detections, yield sensitive 12 & 90 \u03bcm fluxes, and provide positions to \u223c6\" accuracy which will allow unambiguous optical identifications. Confirmed sources are being followed up with ground-based observations to determine optical magnitudes and accurate redshifts. In this preliminary phase we have in hand \u223c100 observed fields and are developing techniques to maximize the sensitivity of the observations. Early results for the ISOCAM 12 \u03bcm images indicate we can reliably detect sources as faint as \u223c0.5\u2009mJy; \u223c80% of the fields contain at least one source.", "date": "1997-02-10", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Melville, NY", "pagerange": "506-509", "id_number": "CaltechAUTHORS:20150916-073006781", "isbn": "1-56396-678-6", "book_title": "The seventh astrophysical conference: Star formation, near and far", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-073006781", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Holt-S-S", "name": { "family": "Holt", "given": "S. S." } }, { "id": "Mundy-L-G", "name": { "family": "Mundy", "given": "L. G." } } ] }, "doi": "10.1063/1.52822", "primary_object": { "basename": "1.52822.pdf", "url": "https://authors.library.caltech.edu/records/1g9y4-qcf47/files/1.52822.pdf" }, "resource_type": "book_section", "pub_year": "1997", "author_list": "Hurt, R. L.; Lonsdale, C. J.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/rag6s-4xb04", "eprint_id": 60265, "eprint_status": "archive", "datestamp": "2023-08-20 07:08:26", "lastmod": "2024-01-13 16:24:56", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bernard-J-P", "name": { "family": "Bernard", "given": "J. P." } }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "F." } }, { "id": "D\u00e9sert-F-X", "name": { "family": "D\u00e9sert", "given": "F. X." } }, { "id": "Puget-J-L", "name": { "family": "Puget", "given": "J. L." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Langer-W", "name": { "family": "Langer", "given": "W." } } ] }, "title": "Dust in the diffuse ISM as revealed by DIRBE observations", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 1996 American Institute of Physics. Published online 01 January 1996. \n\nWe are grateful to the Goddard Space Flight center team for their help in reducing the DIRBE data. This work was conducted in part at the Jet Propulsion Laboratory, California Institute of Technology under contract to NASA and\nsupported in part under the LTSA program and a post-doctoral fellowship from the European Space Agency.\n\nPublished - 1.49251.pdf
", "abstract": "The weekly averaged DIRBE full sky images have been processed to separate the various components contributing to the total brightness in the various bands. The zodiacal emission, which dominates at 12 and 25 \u03bcm and the zodiacal dust scattering at \u03bb<5 \u03bcm are both accounted for using an empirical fit to the data. The diffuse stellar emission which dominates at \u03bb<5 \u03bcm is determined using the shortest DIRBE photometric bands at 1.25 and 2.2 \u03bcm and a standard NIR extinction law. Preliminary results based on the first release of the DIRBE data have been presented in Bernard et al. 1994. When the zodiacal light and stellar emission are subtracted, significant emission remains above 2.2 \u03bcm, which follows the general distribution of the dust emission as seen in the IRAS bands. The DIRBE images therefore allow to extend our knowledge of the dust emission spectrum below 12 \u03bcm and above 100 \u03bcm. In the L(3.5 \u03bcm) and M(4.9 \u03bcm) bands, the dust emission can be seen not only toward the galactic plane but also in diffuse regions above the plane as well as toward closeby molecular complexes (\u03c1\u2010Ophiuchi, Orion, Taurus,...). The existence of NIR dust emission in cold and diffuse regions strongly suggests transiently heated small dust particles as the carrier. The dust NIR spectrum is generally consistent with the dust model of D\u00e9sert et al. 1990. In particular, the dust emission increases from 4.9 to 3.5 \u03bcm, which can be attributed to the contribution of the 3.3 \u03bcm emission feature of Polycyclic Aromatic Hydrocarbons (PAH). Significant continuum emission, or other feature emission, is also required to explain the observed brightness in the L band and the AROME ballon experiment results at low galactic latitude.", "date": "1996-01-01", "date_type": "published", "publisher": "American Institute of Physics", "place_of_pub": "Woodbury, NY", "pagerange": "105-111", "id_number": "CaltechAUTHORS:20150915-152124243", "isbn": "9781563965081", "book_title": "The COBE workshop", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150915-152124243", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "LTSA" }, { "agency": "European Space Agency (ESA)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Dwek-E", "name": { "family": "Dwek", "given": "E." } } ] }, "doi": "10.1063/1.49251", "primary_object": { "basename": "1.49251.pdf", "url": "https://authors.library.caltech.edu/records/rag6s-4xb04/files/1.49251.pdf" }, "resource_type": "book_section", "pub_year": "1996", "author_list": "Bernard, J. P.; Boulanger, F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/33k5t-d7c66", "eprint_id": 56580, "eprint_status": "archive", "datestamp": "2023-08-20 06:00:23", "lastmod": "2023-10-23 15:34:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Radio and optical connected", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 1995 Nature Publishing Group.", "abstract": "With instruments of striking diversity and\nprecision, observational cosmologists\ntranslate the whispers of distant galaxies\ninto clues to cosmic history. But the same\ncorner of Universe is not often probed\nwith more than one instrument, so we are\nleft to piece together that history like the\nproverbial blind men examining an\nelephant. When two probes do intersect,\nthe result is something akin to a Rosetta\nStone, where observations at various\nwavelengths can be woven together to\nyield a hitherto unseen picture.", "date": "1995-06-08", "date_type": "published", "publication": "Nature", "volume": "375", "number": "6531", "publisher": "Nature Publishing Group", "pagerange": "448-449", "id_number": "CaltechAUTHORS:20150410-155623063", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150410-155623063", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/375448a0", "resource_type": "article", "pub_year": "1995", "author_list": "Helou, George" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/q3625-g3g36", "eprint_id": 106936, "eprint_status": "archive", "datestamp": "2023-08-20 05:12:54", "lastmod": "2024-01-15 18:15:43", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ebert-R", "name": { "family": "Ebert", "given": "R." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Mazzarella-Joseph-M", "name": { "family": "Mazzarella", "given": "J." }, "orcid": "0000-0002-8204-8619" } ] }, "title": "IPAC datasets and on-line services", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "European Space Agency, Infrared Space Observatory, IRAS Source, Infrared Astronomical Satellite, IRAS Point Source Catalog", "note": "\u00a9 Springer Science+Business Media Dordrecht 1995. \n\nAll members of the IPAC Tools Group are contributing to the software and systems discussed here. They are J. Bennett, B. Hartley, L. Hermans, I. Khan, M. Kong, G. Laughlin, S. Lord, R. Narron, and D. Van Buren. IPAC is operated by the Jet Propulsion Laboratory, California Institute of Technology for the Astrophysics division of NASA.", "abstract": "The Infrared Processing and Analysis Center (IPAC) was created by NASA to process and analyze data from the Infrared Astronomical Satellite (IRAS) in 1983. Now that the IRAS work is completed, IPAC exists to perform data processing and science support activities that are critical to other NASA infrared astronomy missions. But the IRAS archive lives on, and continues to be used extensively, both for ongoing research and to prepare for future missions.", "date": "1995", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "147-152", "id_number": "CaltechAUTHORS:20201205-161423801", "isbn": "9789401041782", "book_title": "Information & On-Line Data in Astronomy", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201205-161423801", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Egret-Daniel", "name": { "family": "Egret", "given": "Daniel" } }, { "id": "Albrecht-Miguel-A", "name": { "family": "Albrecht", "given": "Miguel A." } } ] }, "corp_creators": { "items": [ "IPAC Tools Group" ] }, "doi": "10.1007/978-94-011-0397-8_14", "resource_type": "book_section", "pub_year": "1995", "author_list": "Ebert, R.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/y0rys-j6005", "eprint_id": 106709, "eprint_status": "archive", "datestamp": "2023-08-20 05:12:38", "lastmod": "2024-01-15 18:14:50", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schmitz-M", "name": { "family": "Schmitz", "given": "M." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Dubois-P", "name": { "family": "Dubois", "given": "P." } }, { "id": "LaGue-C", "name": { "family": "LaGue", "given": "C." } }, { "id": "Madore-B", "name": { "family": "Madore", "given": "B." } }, { "id": "Corwin-H-G", "name": { "family": "Corwin", "given": "H. G." } }, { "id": "Lesteven-S", "name": { "family": "Lesteven", "given": "S." } } ] }, "title": "NED and SIMBAD conventions for bibliographic reference coding", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Physical Review, Astronomy Report, Astronomy Letter, Volume Number, Page Number", "note": "\u00a9 Springer Science+Business Media Dordrecht 1995. \n\nWe thank Helmut Abt and the rest of the NED and SIMBAD groups for their help in defining the reference codes. Table 24-2 has been prepared with the kind help of Suzanne Lalo\u00eb at the Institut d' Astrophysique de Paris. NED is a research support program operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (Astrophysics Division, Science Operations Branch). SIMBAD is maintained by the Centre de Donnees astronomiques de Strasbourg, France.", "abstract": "The uniform 19\u2014digit code used for bibliographic references within NED and SIMBAD was developed by both teams in consultation with Dr. H. Abt, editor of the Astrophysical Journal. The primary purpose of the \"REF_CODE\" is to provide a unique and traceable representation of a bibliographic reference within the structure of each database. However, in many cases, the code has sufficient information to be quickly deciphered by eye, and it is used frequently in the interfaces as a succinct abbreviation of a full bibliographic reference. Since its inception, it has become a standard code not only for NED and SIMBAD, but \u2014 with minor variations \u2014 for ADS and other bibliographic services. In addition, the acronyms for journals used as part of the code have become standards for some of the main astronomical journals in their own bibliographies.", "date": "1995", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "259-270", "id_number": "CaltechAUTHORS:20201117-175540451", "isbn": "9789401041782", "book_title": "Information & On-Line Data in Astronomy", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201117-175540451", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Egret-D", "name": { "family": "Egret", "given": "Daniel" } }, { "id": "Albrecht-M-A", "name": { "family": "Albrecht", "given": "Miguel A." } } ] }, "doi": "10.1007/978-94-011-0397-8_24", "resource_type": "book_section", "pub_year": "1995", "author_list": "Schmitz, M.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/v633w-xx694", "eprint_id": 105679, "eprint_status": "archive", "datestamp": "2023-08-22 10:14:28", "lastmod": "2024-01-15 17:05:32", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Schmitz-M", "name": { "family": "Schmitz", "given": "M." } }, { "id": "Wu-X", "name": { "family": "Wu", "given": "X." } }, { "id": "Corwin-H-G-Jr", "name": { "family": "Corwin", "given": "H. G., Jr." } }, { "id": "LaGue-C", "name": { "family": "LaGue", "given": "C." } }, { "id": "Bennett-J", "name": { "family": "Bennett", "given": "J." } }, { "id": "Sun-H", "name": { "family": "Sun", "given": "H." } } ] }, "title": "The NASA/IPAC Extragalactic Database", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Radio Source; Object Type; Bibliographic Reference; Extragalactic Source; Infrared Source", "note": "\u00a9 Springer Science+Business Media Dordrecht 1995. \n\nMany people have contributed to NED, and continue to do so; we would like to thank Rick Ebert and Maneesh Sahani for their help in the software arena; we also recognize IPAC's support, especially through the computer systems group. We especially acknowledge the friendly collaboration of the SIMBAD project, Centre des Donn\u00e9es astronomiques de Strasbourg. Last but not least, we thank all the authors and the National Space Science Data Center, who send us computer-readable versions of their data or catalogs. \n\nNED is funded by the Science Operations Branch of the Astrophysics Division, Office of Space Science and Applications, NASA. This work is carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.", "abstract": "The NASA/IPAC Extragalactic Database (NED) is an electronic research tool which provides uniquely powerful access to published multi-wavelength data on extragalactic objects. It consists of a computer database with a broad range of published information, and a user interface which allows fast and flexible retrieval of the information via the Internet. It is accessible anonymously and free of charge to any account on the networks, and used primarily by researchers, students and librarians. NED is physically located at the Infrared Processing and Analysis Center (IPAC) on the Caltech campus in Pasadena, California (USA).", "date": "1995", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "95-113", "id_number": "CaltechAUTHORS:20200930-113054788", "isbn": "9789401041782", "book_title": "Information & On-Line Data in Astronomy", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200930-113054788", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Egret-D", "name": { "family": "Egret", "given": "Daniel" } }, { "id": "Albrecht-M-A", "name": { "family": "Albrecht", "given": "Miguel A." } } ] }, "doi": "10.1007/978-94-011-0397-8_10", "resource_type": "book_section", "pub_year": "1995", "author_list": "Helou, G.; Madore, B. F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8japf-p5q82", "eprint_id": 95936, "eprint_status": "archive", "datestamp": "2023-08-20 03:39:28", "lastmod": "2024-01-14 21:45:27", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jarrett-T-H", "name": { "family": "Jarrett", "given": "T. H." }, "orcid": "0000-0002-4939-734X" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C. A." }, "orcid": "0000-0002-5627-5471" } ] }, "title": "Brackett-\u03b3 Line Emission Maps of Four Galaxies", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Galaxies: Massive Star Formation - H II Regions", "note": "\u00a9 Springer Science+Business Media Dordrecht 1994.", "abstract": "Observations of the Br-\u03b3 hydrogen recombination line have been made in a sample of four galaxies. The data were acquired with the new Palomar Prime-Focus Infrared Camera (PFIRCAM) mounted at the prime focus (f/3.3) of the Hale 5-m telescope. The galaxies were imaged with narrow band filters centered on the Br-\u03b3 (2.166 \u03bcm) line and nearby K-band continuum. This project was undertaken with two goals in mind. First, to demonstrate the feasibility of extragalactic narrow-band imaging with near-infrared arrays, and second, to measure the Br-\u03b3 to H\u03b1 flux ratio corresponding to regions undergoing massive star formation. The galaxies are all at low redshift, but of a variety of morphologies: late-type galaxies, NGC 3683 (Sbc, 1656 km/s) and NGC 4713 (Sbd, 653 km/s), early-type galaxy, NGC 5866 (S0-f , 770 km/s), and irregular-type galaxy, NGC 2537 (IRR, 447 km/s). In three of the galaxies, NGC 2537, NGC 3683 and NGC 4713, we detect Br-\u03b3 emission at the \u22653\u03c3 level, and in NGC 5866 we obtain an upper limit. The spatial resolution of the raw 2.2\u03bcm data was about 1\u2033, with the final maps smoothed to a resolution of 1 \u2013 1.5\u2033. Our Br-\u03b3 detections resolve individual H II region complexes in the galaxies. By comparing the Br-\u03b3 emission with H\u03b1 emission, we may derive an effective extinction measure, and infer a Lyman continuum flux from massive stars. This Lyman luminosity can then be converted into a total mass estimate for young stars, assuming an initial mass function and an upper mass cut-off. To date we have acquired Ha images of NGC 3683, NGC 4713, and NGC 5866. The preliminary results of NGC 4713 are presented in this paper.", "date": "1994", "date_type": "published", "publisher": "Springer", "place_of_pub": "Dordrecht", "pagerange": "177-178", "id_number": "CaltechAUTHORS:20190529-162854210", "isbn": "9789401044660", "book_title": "Infrared Astronomy with Arrays: the Next Generation", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-162854210", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "McLean-I-S", "name": { "family": "McLean", "given": "Ian S." } } ] }, "doi": "10.1007/978-94-011-1070-9_61", "resource_type": "book_section", "pub_year": "1994", "author_list": "Jarrett, T. H.; Helou, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8dkhf-ptp66", "eprint_id": 105678, "eprint_status": "archive", "datestamp": "2023-08-22 07:55:05", "lastmod": "2024-01-15 17:05:30", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Schmitz-M", "name": { "family": "Schmitz", "given": "M." } }, { "id": "Bicay-M-D", "name": { "family": "Bicay", "given": "M. D." } }, { "id": "Wu-X", "name": { "family": "Wu", "given": "X." } }, { "id": "Bennett-J", "name": { "family": "Bennett", "given": "J." } } ] }, "title": "The NASA/IPAC Extragalactic Database", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Line Source; Bibliographic Reference; Virgo Cluster; Extragalactic Source; Infrared Space Observatory", "note": "\u00a9 Springer Science+Business Media Dordrecht 1991. \n\nMany people have contributed to NED, and continue to do so; we would like to thank Nian Chiu, Rick Ebert, Alan Mazer, and Maneesh Sahani for their help in the software arena; April Michel, Walter Rice and Carol Lonsdale for help with populating the database; and especially Rosanne Hernandez and Eve Scholey for their dedication to digitizing the abstracts, and John Good for his advice and suggestions. We especially acknowledge the friendly collaboration of the SIMBAD project, Centre de Donnees astronomiques de Strasbourg. We would also like to thank all the authors who send us computer-legible versions of their data or catalogs. NED is funded by the Science Operations Branch of the Astrophysics Division, Office of Space Science and Applications, NASA. This work was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.", "abstract": "The NASA/IPAC Extragalactic Database (NED) is a research tool in the form of a central archive which accumulates published data, is organized for fast, flexible retrieval, and is accessible to all astronomers. This service was designed in response to an increasing need driven by ever larger data sets collected in surveys, by the exponential growth in the volume of the technical literature, and by a greater tendency among astronomers to take a multi-spectral approach to the study of astrophysical problems.", "date": "1991", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "89-106", "id_number": "CaltechAUTHORS:20200930-113054696", "isbn": "9789401054331", "book_title": "Databases & On-line Data in Astronomy", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200930-113054696", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Albrecht-M-A", "name": { "family": "Albrecht", "given": "Miguel A." } }, { "id": "Egret-D", "name": { "family": "Egret", "given": "Daniel" } } ] }, "doi": "10.1007/978-94-011-3250-3_10", "resource_type": "book_section", "pub_year": "1991", "author_list": "Helou, G.; Madore, B. F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/30jhf-bjd73", "eprint_id": 105922, "eprint_status": "archive", "datestamp": "2023-08-19 22:18:24", "lastmod": "2024-01-15 18:12:35", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Madore-B-F", "name": { "family": "Madore", "given": "B. F." }, "orcid": "0000-0002-1576-1676" }, { "id": "Bicay-M-D", "name": { "family": "Bicay", "given": "M. D." } }, { "id": "Schmitz-M", "name": { "family": "Schmitz", "given": "M." } }, { "id": "Liang-J", "name": { "family": "Liang", "given": "J." } } ] }, "title": "The NASA/IPAC Extragalactic Database", "ispublished": "unpub", "full_text_status": "restricted", "note": "\u00a9 Kluwer Academic Publishers 1990. \n\nThis research was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.D.B. gratefully acknowledges the support of a National Research Council Research Associateship.", "abstract": "The NASA/IPAC Extragalactic Database (NED) is a computer-based service under development which will be made available in 1990 to the international astronomical community. This service will consist of a compendium of published data on extragalactic objects, and the software required to allow effective access to the data.", "date": "1990", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "109-113", "id_number": "CaltechAUTHORS:20201008-112317073", "isbn": "9789401067317", "book_title": "Windows on Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201008-112317073", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "National Research Council" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Fabbiano-G", "name": { "family": "Fabbiano", "given": "Giuseppina" } }, { "id": "Gallagher-J-S-III", "name": { "family": "Gallagher", "given": "John S." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "Alvio" } } ] }, "doi": "10.1007/978-94-009-0543-6_15", "resource_type": "book_section", "pub_year": "1990", "author_list": "Helou, G.; Madore, B. F.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/x30f8-h1592", "eprint_id": 105924, "eprint_status": "archive", "datestamp": "2023-08-22 07:04:34", "lastmod": "2024-01-15 18:12:39", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Bicay-M-D", "name": { "family": "Bicay", "given": "Michael D." } } ] }, "title": "The Radio-Infrared Correlation within Galaxies", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Star Formation; Spiral Galaxy; Tight Coupling; Disk Galaxy; Star Formation Activity", "note": "\u00a9 Kluwer Academic Publishers 1990. \n\nThis research was supported through the IRAS Extended Mission Program by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.D.B. gratefully acknowledges the support of a National Research Council Research Associateship.", "abstract": "A comparison of the distributions of 60\u03bcm infrared and 20cm radio continuum emission within spiral galaxies reveals a broad correlation between the two, which is modulated by a slow decrease in the 60\u03bcm-to-20cm ratio with increasing radius. Using these results, we propose a physical model for understanding the tight correlation between far-infrared and non-thermal radio luminosities in star-forming galaxies. This approach suggests that the basic constraint implied by the correlation is a tight coupling between the sources of the dust-heating photons and those of cosmic-ray electrons. Among spiral galaxies, we require in addition a universal relation whereby magnetic field strength scales with gas density to a power l/3 \u2264 \u03b2 \u2264 2/3.", "date": "1990", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "115-119", "id_number": "CaltechAUTHORS:20201008-112317285", "isbn": "9789401067317", "book_title": "Windows on Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201008-112317285", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "National Research Council" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Fabbiano-G", "name": { "family": "Fabbiano", "given": "Giuseppina" } }, { "id": "Gallagher-J-S-III", "name": { "family": "Gallagher", "given": "John S." } }, { "id": "Renzini-A", "name": { "family": "Renzini", "given": "Alvio" } } ] }, "doi": "10.1007/978-94-009-0543-6_16", "resource_type": "book_section", "pub_year": "1990", "author_list": "Helou, George and Bicay, Michael D." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/v0wvw-43z87", "eprint_id": 105677, "eprint_status": "archive", "datestamp": "2023-08-22 06:11:19", "lastmod": "2023-10-20 22:17:14", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Hoffman-G-L", "name": { "family": "Hoffman", "given": "G. Lyle" } }, { "id": "Salpeter-E-E", "name": { "family": "Salpeter", "given": "E. E." } } ] }, "title": "Blue Compact Dwarf Galaxies in the W Cloud of Virgo", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Dwarf Galaxy; Cluster Core; Present Epoch; Virgo Cluster; Bright Galaxy", "note": "\u00a9 Springer-Verlag New York, Inc. 1989. \n\nThis work was supported in part by NASA through the IRAS Extended Mission at the Infrared Processing and Analysis Center, JPL, Caltech.", "abstract": "As part of our study of Blue Compact Dwarf (BCD) galaxies in the Virgo Cluster (Hoffman et al. 1988), we have examined how location in the Cluster affects the properties of these objects. For a source list, we used the Virgo Cluster Catalog by Binggeli, Sandage, and Tammann (1987), which contains 64 objects classified as \"BCD\" with varying degrees of uncertainty. A neutral hydrogen survey at Arecibo and a subsequent spectroscopic survey with the Palomar 5-meter reflector (in addition to other sources), have yielded 35 detections at heliocentric redshift V_\u2299 < 3000 km s\u207b\u00b9, and 26 in the background (Hoffman et al. 1987, Helou and Schombert 1988, Schulte-Ladbeck and Cardelli 1987), leaving only three objects with unknown redshifts.", "date": "1989", "date_type": "published", "publisher": "Springer", "place_of_pub": "New York, NY", "pagerange": "496-498", "id_number": "CaltechAUTHORS:20200930-113054593", "isbn": "9781461393580", "book_title": "The World of Galaxies", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200930-113054593", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Corwin-H-G-Jr", "name": { "family": "Corwin", "given": "Harold G., Jr." } }, { "id": "Bottinelli-L", "name": { "family": "Bottinelli", "given": "Lucette" } } ] }, "doi": "10.1007/978-1-4613-9356-6_77", "resource_type": "book_section", "pub_year": "1989", "author_list": "Helou, George; Hoffman, G. Lyle; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/dbhfj-a1757", "eprint_id": 105939, "eprint_status": "archive", "datestamp": "2023-08-22 06:12:06", "lastmod": "2024-01-15 18:12:55", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Far Infrared Emission from Galactic and Extragalactic Dust", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Interstellar Medium; Molecular Cloud; Spiral Galaxy; Radio Galaxy; Large Magellanic Cloud", "note": "\u00a9 IAU 1989. \n\nI would like to thank Helen Knudsen, Rosanne Hernandez and the IPAC Library for help with the literature search and collection of references, Mary Ellen Barba for help with the manuscript, and Fran\u00e7ois Boulanger, Chas Beichman and Tom Soifer for helpful comments on the manuscript. This work was supported as part of the IRAS Extended Mission by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.", "abstract": "This review examines the question of how similar far infrared and submillimeter dust properties are among galaxies including the Milky Way, and within the Milky Way. The IRAS data are examined, and no evidence is found for variations in the broad-band dust properties between 10 and 100 \u00b5m. Submillimeter data are examined in a search for a power-law index describing the emissivity of dust at \u03bb > 100 \u00b5m. The data are consistent with a universal value of the index between 1 and 2. The evidence for large amounts of cold dust (10 to 15 K) in galaxies is reviewed and found quite soft in light of conflicting data. In most spiral galaxies, the dust-to-gas ratios are comparable to their values in the Milky Way, with a few well-documented exceptions such as the Magellanic Clouds and Blue Compact Dwarf galaxies, which have a lower ratio. No compelling evidence is found for gradients in the dust-to-gas ratio within disks of galaxies. Very small grains with fluctuating temperatures appear to be present in all galaxies examined, and to behave just like those observed in the Milky Way.", "date": "1989", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "285-301", "id_number": "CaltechAUTHORS:20201008-131242705", "isbn": "9780792304494", "book_title": "Interstellar Dust", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201008-131242705", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Allamandola-L-J", "name": { "family": "Allamandola", "given": "L. J." } }, { "id": "Tielens-A-G-G-M", "name": { "family": "Tielens", "given": "A. G. G. M." } } ] }, "doi": "10.1007/978-94-009-2462-8_25", "resource_type": "book_section", "pub_year": "1989", "author_list": "Helou, George" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/8txa7-d8427", "eprint_id": 105675, "eprint_status": "archive", "datestamp": "2023-08-22 04:38:04", "lastmod": "2024-01-15 17:05:26", "type": "book_section", "metadata_visibility": "show", "creators": { "items": [ { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" } ] }, "title": "Statistical Properties of IRAS Galaxies", "ispublished": "unpub", "full_text_status": "restricted", "keywords": "Extragalactic Source; Bright Galaxy; Small Magellanic Cloud; Normal Galaxy; IRAS Source", "note": "\u00a9 D. Reidel Publishing Company 1986. \n\nI would like to thank B. T. Soifer for interesting and enlightening discussions. This work was supported through the Jet Propulsion Laboratory (JPL), California Institute of Technology, under contract with the National Aeronautics and\nSpace Administration.", "abstract": "Statistical approaches to the study of galaxies seen by IRAS are reviewed, stressing the contrast between infrared complete and optically complete samples. A statistical overview is given of the Cataloged Galaxies and Quasars Observed in the IRAS Survey. The bi-variate distribution of ESO/U galaxies as a function of 60 \u00b5m flux and optical size is used to predict the size of an infrared complete sample from the optically complete sample. To within the uncertainties, both samples are found to belong to the same population, leaving little room for a fundamentally new class of extragalactic objects, besides infrared bright galaxies like Arp220.", "date": "1986", "date_type": "published", "publisher": "Springer Netherlands", "place_of_pub": "Dordrecht", "pagerange": "405-414", "id_number": "CaltechAUTHORS:20200930-113054378", "isbn": "9789401085779", "book_title": "Light on Dark Matter", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200930-113054378", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "contributors": { "items": [ { "id": "Israel-F-P", "name": { "family": "Israel", "given": "Frank P." } } ] }, "doi": "10.1007/978-94-009-4672-9_87", "resource_type": "book_section", "pub_year": "1986", "author_list": "Helou, George" }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/szx6a-4ye31", "eprint_id": 74842, "eprint_status": "archive", "datestamp": "2023-08-19 17:52:40", "lastmod": "2023-10-24 23:21:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hacking-P-B", "name": { "family": "Hacking", "given": "P." } }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Emerson-J", "name": { "family": "Emerson", "given": "J." } }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C." }, "orcid": "0000-0002-5627-5471" }, { "id": "Chester-T-J", "name": { "family": "Chester", "given": "T." } }, { "id": "Gillett-F-C", "name": { "family": "Gillett", "given": "F." } }, { "id": "Habing-H-J", "name": { "family": "Habing", "given": "H." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Houck-J", "name": { "family": "Houck", "given": "J." } }, { "id": "Olnon-F", "name": { "family": "Olnon", "given": "F." } }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Walker-D", "name": { "family": "Walker", "given": "D." } } ] }, "title": "The brightest high-latitude 12-micron IRAS sources", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared sources\u2014late-type stars\u2014circumstellar matter", "note": "\u00a9 1985 Astronomical Society of the Pacific. \n\nReceived 1985 January 2, revised 1985 April 11. \n\nThe Infrared Astronomical Satellite was developed and is operated by the U.S. National Aeronautics and Space Administration (NASA), the Netherlands Agency for Aerospace Programs (NIVR), and the U.K. Science and Engineering Research Council (SERC). \n\nWe thank H.H. Aumann for useful discussions, Sharon Conrad and Rosanne Hernandez for their help and patience with the text and tables, and Judy Bennett, Joe Chillemi, and Ted Sesplaukis for helping the data flow smoothly.\n\nPublished - 1985PASP___97__616H.pdf
", "abstract": "The Infrared Astronomical Satellite (IRAS) Point Source catalog was searched for sources brighter than 28 Jy (0 mag) at 12 \u03bcm with absolute galactic latitude greater than 30\u00b0 excluding the Large Magellanic Cloud. The search resulted in 269 sources, two of which are the galaxies NGC 1068 and M82. The remaining 267 sources are identified with, or have infrared color indices consistent with late-type stars some of which show evidence of circumstellar dust shells. Seven sources are previously uncataloged stars. K and M stars without circumstellar dust shells, M stars with circumstellar dust shells, and carbon stars occupy well-defined regions of infrared color-color diagrams.", "date": "1985-07", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "97", "number": "593", "publisher": "Astronomical Society of the Pacific", "pagerange": "616-633", "id_number": "CaltechAUTHORS:20170307-102025070", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170307-102025070", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1086/131576", "primary_object": { "basename": "1985PASP___97__616H.pdf", "url": "https://authors.library.caltech.edu/records/szx6a-4ye31/files/1985PASP___97__616H.pdf" }, "resource_type": "article", "pub_year": "1985", "author_list": "Hacking, P.; Neugebauer, G.; et el." }, { "id": "https://authors.library.caltech.eduhttps://authors.library.caltech.edu/records/7dhxb-gce86", "eprint_id": 74760, "eprint_status": "archive", "datestamp": "2023-08-19 17:06:26", "lastmod": "2023-10-24 22:54:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Lonsdale-C-J", "name": { "family": "Lonsdale", "given": "C. J." }, "orcid": "0000-0003-0898-406X" }, { "id": "Hacking-P-B", "name": { "family": "Hacking", "given": "P." } }, { "id": "Rice-W-K-M", "name": { "family": "Rice", "given": "W." } }, { "id": "Houck-J-R", "name": { "family": "Houck", "given": "J. R." } }, { "id": "Low-F-J", "name": { "family": "Low", "given": "F. J." } }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } } ] }, "title": "The remarkable infrared galaxy ARP 220 = IC 4553", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: sources galaxies: photometry galaxies: Seyfert", "note": "\u00a9 1984 American Astronomical Society. \n\nReceived 1984 March 12; accepted 1984 May 15. \n\nIt is a pleasure to thank our many colleagues in the IRAS project Science Data Analysis System for assisting in the reduction of the data used here. We thank Harm Rahing and George Miley for a careful reading of the manuscript. The work described here was supported in part through the Jet Propulsion Laboratory; California Institute of Technology, under contract with NASA.\n\nPublished - 1984ApJ___283L___1S.pdf
", "abstract": "IRAS observations of the peculiar galaxy Arp 220 = IC 4553 show that it is extremely luminous in the far-infrared with a total luminosity of - 2 X 10^(12) L_\u2609. The infrared-to-blue luminosity ratio of this galaxy is - 80, which is the largest value of the ratio for galaxies in the UGC catalog, and places it in the range of the\n\"unidentified\" infrared sources recently reported by Houck et al. in the IRAS all-sky survey. Other observations of Arp 220, combined with the luminosity in the infrared, allow either a Seyfert-like or starburst origin for this luminosity.", "date": "1984-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "283", "publisher": "American Astronomical Society", "pagerange": "L1-L4", "id_number": "CaltechAUTHORS:20170306-091617017", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170306-091617017", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1086/184319", "primary_object": { "basename": "1984ApJ___283L___1S.pdf", "url": "https://authors.library.caltech.edu/records/7dhxb-gce86/files/1984ApJ___283L___1S.pdf" }, "resource_type": "article", "pub_year": "1984", "author_list": "Soifer, B. T.; Neugebauer, G.; et el." } ]