[ { "id": "https://authors.library.caltech.edu/records/ag24s-eja85", "eprint_id": 115787, "eprint_status": "archive", "datestamp": "2023-08-22 16:49:22", "lastmod": "2023-10-24 16:43:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Green-Paul-J", "name": { "family": "Green", "given": "Paul J." }, "orcid": "0000-0002-8179-9445" }, { "id": "Pulgarin-Duque-Lina", "name": { "family": "Pulgarin-Duque", "given": "Lina" } }, { "id": "Anderson-Scott-F", "name": { "family": "Anderson", "given": "Scott F." } }, { "id": "MacLeod-Chelsea-L", "name": { "family": "MacLeod", "given": "Chelsea L." }, "orcid": "0000-0003-3422-2202" }, { "id": "Eracleous-Michael", "name": { "family": "Eracleous", "given": "Michael" }, "orcid": "0000-0002-3719-940X" }, { "id": "Ruan-John-J", "name": { "family": "Ruan", "given": "John J." }, "orcid": "0000-0001-8665-5523" }, { "id": "Runnoe-Jessie", "name": { "family": "Runnoe", "given": "Jessie" }, "orcid": "0000-0001-8557-2822" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew" }, "orcid": "0000-0002-3168-0139" }, { "id": "Roulston-Benjamin-R", "name": { "family": "Roulston", "given": "Benjamin R." }, "orcid": "0000-0002-9453-7735" }, { "id": "Schneider-Donald-P", "name": { "family": "Schneider", "given": "Donald P." }, "orcid": "0000-0001-7240-7449" }, { "id": "Ahlf-Austin", "name": { "family": "Ahlf", "given": "Austin" } }, { "id": "Bizyaev-Dmitry", "name": { "family": "Bizyaev", "given": "Dmitry" }, "orcid": "0000-0002-3601-133X" }, { "id": "Brownstein-Joel-R", "name": { "family": "Brownstein", "given": "Joel R." }, "orcid": "0000-0002-8725-1069" }, { "id": "del-Casal-Sonia-Joesephine", "name": { "family": "del Casal", "given": "Sonia Joesephine" } }, { "id": "Dodd-Sierra-A", "name": { "family": "Dodd", "given": "Sierra A." }, "orcid": "0000-0002-3696-8035" }, { "id": "Hoover-Daniel", "name": { "family": "Hoover", "given": "Daniel" } }, { "id": "Matt-Cayenne", "name": { "family": "Matt", "given": "Cayenne" } }, { "id": "Merloni-Andrea", "name": { "family": "Merloni", "given": "Andrea" } }, { "id": "Pan-Kaike", "name": { "family": "Pan", "given": "Kaike" }, "orcid": "0000-0002-2835-2556" }, { "id": "Ramirez-Arnulfo", "name": { "family": "Ramirez", "given": "Arnulfo" } }, { "id": "Ridder-Margaret", "name": { "family": "Ridder", "given": "Margaret" } } ] }, "title": "The Time Domain Spectroscopic Survey: Changing-look Quasar Candidates from Multi-epoch Spectroscopy in SDSS-IV", "ispublished": "pub", "full_text_status": "public", "keywords": "Accretion; Quasars; Active galactic nuclei; Variable radiation sources; Catalogs; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2022 January 13; revised 2022 April 25; accepted 2022 May 23; published 2022 July 13. \n\nMany thanks to Qian Yang for comments and suggestions. \n\nS.F.A., P.J.G., C.L.M, B.R., and J.J.R. are supported by the National Science Foundation under grant Nos. AST- 1715121, and AST-1715763. C.L.M. and Q.Y. were partially supported for spectroscopic observations and analysis by the National Aeronautics and Space Administration through Chandra Award Nos. GO8-19089X and GO9-20086X, issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract No. NAS8-03060. \n\nPhotometric light curves used herein 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 the Lawrence Berkeley National Laboratory. Operations are conducted by COO, IPAC, and UW. \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 website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics \u2223 Harvard & Smithsonian, the Chilean Participation Group, the French Participation Group, 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\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\nThe authors acknowledge the use of the Catalog Archive Server Jobs System (CasJobs) service at http://casjobs.sdss.org/CasJobs, developed by the JHU/SDSS team. \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. The Zwicky Transient Facility 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 COO, IPAC, and UW. \n\nThe Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). \n\nThis work made use of data products from the Catalina Sky Survey. The CSS survey is funded by the National Aeronautics and Space Administration under grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grant Nos. AST-0909182 and AST-1313422. \n\nFacilities: Sloan - Sloan Digital Sky Survey Telescope, ING:Herschel - , Magellan:Baade (LDSS2 imaging spectrograph - , Boller & Chivens spectrograph) - , MMT (Blue Channel spectrograph - , BinoSpec) - , PS1 - , PO:1.2 m - , SO:Schmidt - , SO:1.5 m - , SO:1m - . \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), TOPCAT (Taylor 2005).\n\n
Published - Green_2022_ApJ_933_180.pdf
Accepted Version - 2201.09123.pdf
", "abstract": "Active galactic nuclei (AGN) can vary significantly in their rest-frame optical/UV continuum emission, and with strong associated changes in broad line emission, on much shorter timescales than predicted by standard models of accretion disks around supermassive black holes. Most such changing-look or changing-state AGN\u2014and at higher luminosities, changing-look quasars (CLQs)\u2014have been found via spectroscopic follow-up of known quasars showing strong photometric variability. The Time Domain Spectroscopic Survey of the Sloan Digital Sky Survey IV (SDSS-IV) includes repeat spectroscopy of large numbers of previously known quasars, many selected irrespective of photometric variability, and with spectral epochs separated by months to decades. Our visual examination of these repeat spectra for strong broad line variability yielded 61 newly discovered CLQ candidates. We quantitatively compare spectral epochs to measure changes in continuum and H\u03b2 broad line emission, finding 19 CLQs, of which 15 are newly recognized. The parent sample includes only broad line quasars, so our study tends to find objects that have dimmed, i.e., turn-off CLQs. However, we nevertheless find four turn-on CLQs that meet our criteria, albeit with broad lines in both dim and bright states. We study the response of H\u03b2 and Mg ii emission lines to continuum changes. The Eddington ratios of CLQs are low, and/or their H\u03b2 broad line width is large relative to the overall quasar population. Repeat quasar spectroscopy in the upcoming SDSS-V black hole Mapper program will reveal significant numbers of CLQs, enhancing our understanding of the frequency and duty cycle of such strong variability, and the physics and dynamics of the phenomenon.", "date": "2022-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "933", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 180", "id_number": "CaltechAUTHORS:20220722-769194000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220722-769194000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1715121" }, { "agency": "NSF", "grant_number": "AST-1715763" }, { "agency": "NASA", "grant_number": "GO8-19089X" }, { "agency": "NASA", "grant_number": "GO9-20086X" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" }, { "agency": "Pan-STARRS Project Office" }, { "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" }, { "agency": "NSF", "grant_number": "AST-1313422" } ] }, "local_group": { "items": [ { "id": "Zwicky-Transient-Facility" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/1538-4357/ac743f", "primary_object": { "basename": "2201.09123.pdf", "url": "https://authors.library.caltech.edu/records/ag24s-eja85/files/2201.09123.pdf" }, "related_objects": [ { "basename": "Green_2022_ApJ_933_180.pdf", "url": "https://authors.library.caltech.edu/records/ag24s-eja85/files/Green_2022_ApJ_933_180.pdf" } ], "pub_year": "2022", "author_list": "Green, Paul J.; Pulgarin-Duque, Lina; et el." }, { "id": "https://authors.library.caltech.edu/records/72050-nf728", "eprint_id": 112873, "eprint_status": "archive", "datestamp": "2023-08-22 13:49:40", "lastmod": "2023-10-23 22:49:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Bauer-Evan-B", "name": { "family": "Bauer", "given": "Evan B." }, "orcid": "0000-0002-4791-6724" }, { "id": "van-Roestel-Joannes", "name": { "family": "van Roestel", "given": "Jan" }, "orcid": "0000-0002-2626-2872" }, { "id": "Bellm-Eric-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Bildsten-Lars", "name": { "family": "Bildsten", "given": "Lars" }, "orcid": "0000-0001-8038-6836" }, { "id": "Fuller-J", "name": { "family": "Fuller", "given": "Jim" }, "orcid": "0000-0002-4544-0750" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Heber-Ulrich", "name": { "family": "Heber", "given": "Ulrich" }, "orcid": "0000-0001-7798-6769" }, { "id": "Geier-Stephan", "name": { "family": "Geier", "given": "Stephan" }, "orcid": "0000-0002-3948-9339" }, { "id": "Green-Matthew-J", "name": { "family": "Green", "given": "Matthew J." }, "orcid": "0000-0002-0948-4801" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Bloemen-Steven", "name": { "family": "Bloemen", "given": "Steven" }, "orcid": "0000-0002-6636-921X" }, { "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": "Schneider-David", "name": { "family": "Schneider", "given": "David" } } ] }, "title": "Discovery of a Double-detonation Thermonuclear Supernova Progenitor", "ispublished": "pub", "full_text_status": "public", "keywords": "B subdwarf stars; Close binary stars; White dwarf stars; Eclipsing binary stars", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 October 23; revised 2022 January 4; accepted 2022 January 5; published 2022 January 27. \n\nThis research benefited from interactions that were funded by the Gordon and Betty Moore Foundation through grant GBMF5076. This work was supported by the National Science Foundation through grants PHY-1748958 and ACI-1663688. T.K. would like to thank Ylva G\u00f6tberg for providing the template for Figure 4. T.K. acknowledges support from the National Science Foundation through grant AST #2107982. D.S. was supported by the Deutsche Forschungsgemeinschaft (DFG) under grants HE 1356/70-1 and IR 190/1-1. \n\nObservations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the PTF 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. \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\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\nSome results presented in this paper are based on observations made with the WHT operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Institutio de Astrofisica de Canarias. \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: PO:1.2 m (PTF) - , PO:1.2 m (ZTF) - , Hale (DBSP) - , ING:Herschel (ISIS) - , Keck:I (HIRES) - , Keck:II (ESI) - , Hale (Chimera) - . \n\nSoftware: Gatspy (Vanderplas 2015; VanderPlas & Ivezi\u0107 2015), FITSB2 (Napiwotzki et al. 2004), LCURVE (Copperwheat et al. 2010), emcee (Foreman-Mackey et al. 2013), MESA (Paxton et al. 2011, 2013, 2015, 2018, 2019), Matplotlib (Hunter 2007), Astropy (Astropy Collaboration et al. 2013, 2018), Numpy (Oliphant 2015), ISIS (Houck & Denicola 2000), MAKEE (https://sites.astro.caltech.edu/~tb/makee/).\n\nPublished - Kupfer_2022_ApJL_925_L12.pdf
Accepted Version - 2110.11974.pdf
", "abstract": "We present the discovery of a new double-detonation progenitor system consisting of a hot subdwarf B (sdB) binary with a white dwarf companion with a P_(orb) = 76.34179(2) minutes orbital period. Spectroscopic observations are consistent with an sdB star during helium core burning residing on the extreme horizontal branch. Chimera light curves are dominated by ellipsoidal deformation of the sdB star and a weak eclipse of the companion white dwarf. Combining spectroscopic and light curve fits, we find a low-mass sdB star, M_(sdB) = 0.383 \u00b1 0.028 M_\u2299 with a massive white dwarf companion, M_(WD) = 0.725 \u00b1 0.026 M_\u2299. From the eclipses we find a blackbody temperature for the white dwarf of 26,800 K resulting in a cooling age of \u224825 Myr whereas our MESA model predicts an sdB age of \u2248170 Myr. We conclude that the sdB formed first through stable mass transfer followed by a common envelope which led to the formation of the white dwarf companion \u224825 Myr ago. Using the MESA stellar evolutionary code we find that the sdB star will start mass transfer in \u22486 Myr and in \u224860 Myr the white dwarf will reach a total mass of 0.92 M_\u2299 with a thick helium layer of 0.17 M\u2299. This will lead to a detonation that will likely destroy the white dwarf in a peculiar thermonuclear supernova. PTF1 J2238+7430 is only the second confirmed candidate for a double-detonation thermonuclear supernova. Using both systems we estimate that at least \u22481% of white dwarf thermonuclear supernovae originate from sdB+WD binaries with thick helium layers, consistent with the small number of observed peculiar thermonuclear explosions.", "date": "2022-02-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "925", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L12", "id_number": "CaltechAUTHORS:20220113-182226341", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220113-182226341", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NSF", "grant_number": "PHY-1748958" }, { "agency": "NSF", "grant_number": "ACI-1663688" }, { "agency": "NSF", "grant_number": "AST-2107982" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "HE 1356/70-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "IR 190/1-1" }, { "agency": "NSF", "grant_number": "AST-1440341" }, { "agency": "ZTF partner institutions" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Gaia Multilateral Agreement" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Zwicky-Transient-Facility" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/2041-8213/ac48f1", "primary_object": { "basename": "2110.11974.pdf", "url": "https://authors.library.caltech.edu/records/72050-nf728/files/2110.11974.pdf" }, "related_objects": [ { "basename": "Kupfer_2022_ApJL_925_L12.pdf", "url": "https://authors.library.caltech.edu/records/72050-nf728/files/Kupfer_2022_ApJL_925_L12.pdf" } ], "pub_year": "2022", "author_list": "Kupfer, Thomas; Bauer, Evan B.; et el." }, { "id": "https://authors.library.caltech.edu/records/bbp0n-fb256", "eprint_id": 109215, "eprint_status": "archive", "datestamp": "2023-08-22 12:51:24", "lastmod": "2023-10-23 17:44:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johansson-Joel", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Cenko-S-Bradley", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Fox-Ori-D", "name": { "family": "Fox", "given": "O. D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Dhawan-Suhail", "name": { "family": "Dhawan", "given": "S." }, "orcid": "0000-0002-2376-6979" }, { "id": "Goobar-Ariel", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Stanishev-Vallery", "name": { "family": "Stanishev", "given": "V." }, "orcid": "0000-0002-7626-1181" }, { "id": "Butler-Nathaniel-R", "name": { "family": "Butler", "given": "N." }, "orcid": "0000-0002-9110-6673" }, { "id": "Lee-William-H-K", "name": { "family": "Lee", "given": "W. H." } }, { "id": "Watson-Alan-M", "name": { "family": "Watson", "given": "A. M." } }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "U. C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Nugent-Peter-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Petrushevska-Tanja", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" }, { "id": "Sollerman-Jesper", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Burke-Jamison", "name": { "family": "Burke", "given": "J." }, "orcid": "0000-0003-0035-6659" }, { "id": "Hosseinzadeh-Griffin", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Howell-D-Andrew", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "McCully-Curtis", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Valenti-Stefano", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" } ] }, "title": "Near-infrared Supernova Ia Distances: Host Galaxy Extinction and Mass-step Corrections Revisited", "ispublished": "pub", "full_text_status": "public", "keywords": "Type Ia supernovae; Cosmology; Interstellar dust extinction", "note": "\u00a9 2021. 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 May 24; revised 2021 October 11; accepted 2021 October 12; published 2021 December 24. \n\nWe are grateful for valuable comments from Jakob Nordin and feedback from the CSP team (Chris Burns, Eric Hsiao, Mark Phillips, and Shuvo Uddin). We thank Melissa L. Graham for helping to obtain follow-up observations with Las Cumbres Observatory in 2013. \n\nA.G. acknowledges support from the Swedish Research Council under Dnr VR 2016-03274 and 2020-03444. T.P. acknowledges the financial support from the Slovenian Research Agency (grants I0-0033, P1-0031, J1-8136 and Z1-1853). Research by S.V. is supported by NSF grants AST-1813176 and AST-2008108. \n\nThis work makes use of observations from the Las Cumbres Observatory network. The LCO team was supported by NSF grants AST-1313484 and AST-1911225. The intermediate Palomar Transient Factory project is 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. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. \n\nSoftware: FPipe (Fremling et al. 2016), QUBA pipeline (Valenti et al. 2011), lcogtsnpipe (Valenti et al. 2016), IRAF (Tody 1993), astrometry.net (Lang et al. 2010), swarp (Bertin 2010), (Becker 2015), SNooPy (Burns et al. 2011).\n\nPublished - Johansson_2021_ApJ_923_237.pdf
Submitted - 2105.06236.pdf
", "abstract": "We present optical and near-infrared (NIR, Y-, J-, H-band) observations of 42 Type Ia supernovae (SNe Ia) discovered by the untargeted intermediate Palomar Transient Factory survey. This new data set covers a broad range of redshifts and host galaxy stellar masses, compared to previous SN Ia efforts in the NIR. We construct a sample, using also literature data at optical and NIR wavelengths, to examine claimed correlations between the host stellar masses and the Hubble diagram residuals. The SN magnitudes are corrected for host galaxy extinction using either a global total-to-selective extinction ratio, R_V = 2.0, for all SNe, or a best-fit R_V for each SN individually. Unlike previous studies that were based on a narrower range in host stellar mass, we do not find evidence for a \"mass step,\" between the color- and stretch-corrected peak J and H magnitudes for galaxies below and above log(M\u2217/M\u2299) = 10. However, the mass step remains significant (3\u03c3) at optical wavelengths (g, r, i) when using a global R_V, but vanishes when each SN is corrected using their individual best-fit R_V. Our study confirms the benefits of the NIR SN Ia distance estimates, as these are largely exempted from the empirical corrections dominating the systematic uncertainties in the optical.", "date": "2021-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "923", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 237", "id_number": "CaltechAUTHORS:20210520-145954019", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-145954019", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council", "grant_number": "2016-03274" }, { "agency": "Swedish Research Council", "grant_number": "2020-03444" }, { "agency": "Slovenian Research Agency", "grant_number": "I0-0033" }, { "agency": "Slovenian Research Agency", "grant_number": "P1-0031" }, { "agency": "Slovenian Research Agency", "grant_number": "J1-8136" }, { "agency": "Slovenian Research Agency", "grant_number": "Z1-1853" }, { "agency": "NSF", "grant_number": "AST-1813176" }, { "agency": "NSF", "grant_number": "AST-2008108" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "NSF", "grant_number": "AST-1911225" }, { "agency": "Los Alamos National Laboratory" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/1538-4357/ac2f9e", "primary_object": { "basename": "2105.06236.pdf", "url": "https://authors.library.caltech.edu/records/bbp0n-fb256/files/2105.06236.pdf" }, "related_objects": [ { "basename": "Johansson_2021_ApJ_923_237.pdf", "url": "https://authors.library.caltech.edu/records/bbp0n-fb256/files/Johansson_2021_ApJ_923_237.pdf" } ], "pub_year": "2021", "author_list": "Johansson, J.; Cenko, S. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/xrrdr-s4e65", "eprint_id": 105411, "eprint_status": "archive", "datestamp": "2023-08-22 10:36:40", "lastmod": "2023-10-20 21:58:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schulze-Steve", "name": { "family": "Schulze", "given": "Steve" }, "orcid": "0000-0001-6797-1889" }, { "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "name": { "family": "Leloudas", "given": "Giorgos" }, "orcid": "0000-0002-8597-0756" }, { "name": { "family": "Gal", "given": "Amit" } }, { "name": { "family": "Wright", "given": "Angus H." }, "orcid": "0000-0001-7363-7932" }, { "name": { "family": "Lunnan", "given": "Ragnhild" }, "orcid": "0000-0001-9454-4639" }, { "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "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": "Neill-James-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "name": { "family": "Strothjohann", "given": "Nora Linn" }, "orcid": "0000-0002-4667-6730" }, { "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "name": { "family": "Bianco", "given": "Federica" }, "orcid": "0000-0003-1953-8727" }, { "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "De-Kishalay", "name": { "family": "De", "given": "Kishalay" }, "orcid": "0000-0002-8989-0542" }, { "name": { "family": "Fraser", "given": "Morgan" }, "orcid": "0000-0003-2191-1674" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "Christoffer U." }, "orcid": "0000-0002-4223-103X" }, { "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "name": { "family": "Johansson", "given": "Joel" }, "orcid": "0000-0001-5975-290X" }, { "name": { "family": "Kelly", "given": "Patrick L." }, "orcid": "0000-0003-3142-997X" }, { "name": { "family": "Kne\u017eevi\u0107", "given": "Nikola" } }, { "name": { "family": "Kne\u017eevi\u0107", "given": "Sladjana" }, "orcid": "0000-0003-1416-8069" }, { "name": { "family": "Maguire", "given": "Kate" }, "orcid": "0000-0002-9770-3508" }, { "name": { "family": "Nyholm", "given": "Anders" } }, { "name": { "family": "Papadogiannakis", "given": "Semeli" }, "orcid": "0000-0003-0783-3323" }, { "name": { "family": "Petrushevska", "given": "Tanja" }, "orcid": "0000-0003-4743-1679" }, { "name": { "family": "Rubin", "given": "Adam" }, "orcid": "0000-0003-4557-0632" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "name": { "family": "Yang", "given": "Yi" }, "orcid": "0000-0002-9024-4150" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott M." }, "orcid": "0000-0001-5855-5939" }, { "name": { "family": "Bufano", "given": "Filomena" }, "orcid": "0000-0002-3429-2481" }, { "name": { "family": "Clubb", "given": "Kelsey I." } }, { "name": { "family": "Foley", "given": "Ryan J." }, "orcid": "0000-0002-2445-5275" }, { "name": { "family": "Green", "given": "Yoav" }, "orcid": "0000-0002-0809-6575" }, { "name": { "family": "Harmanen", "given": "Jussi" }, "orcid": "0000-0001-8242-4090" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "Anna Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "name": { "family": "Hook", "given": "Isobel M." }, "orcid": "0000-0002-2960-978X" }, { "name": { "family": "Hosseinzadeh", "given": "Griffin" }, "orcid": "0000-0002-0832-2974" }, { "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "name": { "family": "Kong", "given": "Albert K. H." }, "orcid": "0000-0002-5105-344X" }, { "name": { "family": "Kotak", "given": "Rubina" }, "orcid": "0000-0001-5455-3653" }, { "name": { "family": "Matheson", "given": "Thomas" }, "orcid": "0000-0001-6685-0479" }, { "name": { "family": "McCully", "given": "Curtis" }, "orcid": "0000-0001-5807-7893" }, { "name": { "family": "Milisavljevic", "given": "Dan" }, "orcid": "0000-0002-0763-3885" }, { "name": { "family": "Pan", "given": "Yen-Chen" }, "orcid": "0000-0001-8415-6720" }, { "name": { "family": "Poznanski", "given": "Dovi" }, "orcid": "0000-0003-1470-7173" }, { "name": { "family": "Shivvers", "given": "Isaac" }, "orcid": "0000-0003-3373-8047" }, { "name": { "family": "van Velzen", "given": "Sjoert" }, "orcid": "0000-0002-3859-8074" }, { "name": { "family": "Verbeek", "given": "Kars K." } } ] }, "title": "The Palomar Transient Factory Core-collapse Supernova Host-galaxy Sample. I. Host-galaxy Distribution Functions and Environment Dependence of Core-collapse Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "Supernovae; Core-collapse supernovae; Galaxies; Galactic and extragalactic astronomy", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 August 13; revised 2021 April 15; accepted 2021 April 21; published 2021 August 10. \n\nWe thank the referee for a careful reading of the manuscript and for helpful comments that improved this paper. We thank Nino Cucchiara, Thomas de Jaeger, Harald Ebeling, David Levitan, Bruce Margon, Jon Mauerhan, Jacob Rex, David Sand, Jeffrey M. Silverman, Vicky Toy, and Brad Tucker for performing some of the observations, and Ido Irani and Maryam Modjaz for valuable discussions. I.A. is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe Program and acknowledges support from that program, from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement 852097), from the Israel Science Foundation (grants 2108/18 and 2752/19), from the United States\u2014Israel Binational Science Foundation (BSF), and from the Israeli Council for Higher Education Alon Fellowship. J.S.B. was partially supported by a Gordon and Betty Moore Foundation Data-Driven Discovery grant. The UCSC team is supported in part by National Aeronautics and Space Administration (NASA) grant NNG17PX03C, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by a fellowship from the David and Lucile Packard Foundation to R. J. Foley. A.V.F. acknowledges support from the US National Science Foundation (NSF), the Christopher R. Redlich Fund, the TABASGO Foundation, and the U.C. Berkeley Miller Institute for Basic Research in Science (in which he is a Miller Senior Fellow). M.F. is supported by a Royal Society\u2014Science Foundation Ireland University Research Fellowship. A.G.-Y.'s research is supported by the EU via ERC grant 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-CIT joint research grant; A.G.-Y. is the recipient of the Helen and Martin Kimmel Award for Innovative Investigation. A.Y.Q.H. was supported by an NSF Graduate Research Fellowship under grant DGE1144469 and by the GROWTH project funded by the NSF under PIRE grant 1545949. D.A.H., G.H., and C.M. were supported by NSF grant AST-1313484. M.M.K. acknowledges support by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the NSF under PIRE Grant No. 1545949. S.K. was supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia through contract 451-03-68/2020/14/20002 made with the Astronomical Observatory of Belgrade. G.L. is supported by a research grant (19054) from VILLUM FONDEN. R.L. is supported by 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). K.M. acknowledges funding from EU H2020 ERC grant 758638. T.P. acknowledges the financial support from the Slovenian Research Agency (grants I0-0033, P1-0031, J1-8136, and Z1-1853). S.S. gratefully acknowledges support provided by the Feinberg Graduate School at the Weizmann Institute, Israel. A.H.W. is supported by a European Research Council Consolidator Grant (770935). The Palomar Transient Factory project is 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. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. This work makes use of data from the Las Cumbres Observatory network. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. The data presented herein were obtained in part with ALFOSC, which is provided by the Instituto de Astrof\u00edsica de Andaluc\u00eda (IAA) under a joint agreement with the University of Copenhagen and NOTSA. The Cerro Tololo Inter-American Observatory and the National Optical Astronomy Observatory are operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the NSF. We thank the staff of the various observatories at which data were obtained for their excellent assistance. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the US Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, the 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. The 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, NASA under grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the NSF under grant AST-1238877, the University of Maryland, and E\u00f6tv\u00f6s Lor\u00e1nd University (ELTE). 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 NASA and the NSF. This publication also 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 NASA. The LBNL Physics Division is supported by the US Department of Energy Office of Science High Energy Physics. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. The Computational HEP program in the Department of Energy's Science Office of High Energy Physics provided resources through the \"Cosmology Data Repository\" project (grant #KA2401022). \n\nSoftware: Astropy v3.2.3 (Astropy Collaboration et al. 2013; 2018), Flexible Stellar Population Synthesis (FSPS; Conroy et al. 2009), High Order Transform of Psf ANd Template Subtraction v5.1.11 (Hotpants; Becker 2015), IRAF (Tody 1986), LAMBDAR (Wright et al. 2016), Prospector v0.3 (Leja et al. 2017), python-fsps (Foreman-Mackey et al. 2014) scikit-learn v0.21.2 (Pedregosa et al. 2011), Software for Calibrating AstroMetry and Photometry (SCAMP; Bertin 2006) v2.0.4, Source Extractor v2.19.5 (Bertin & Arnouts 1996), Supernova Identification v5.0 (Blondin & Tonry 2007), Superfit v3.5 (Howell et al. 2005).\n\nPublished - Schulze_2021_ApJS_255_29.pdf
Submitted - 2008.05988.pdf
", "abstract": "Several thousand core-collapse supernovae (CCSNe) of different flavors have been discovered so far. However, identifying their progenitors has remained an outstanding open question in astrophysics. Studies of SN host galaxies have proven to be powerful in providing constraints on the progenitor populations. In this paper, we present all CCSNe detected between 2009 and 2017 by the Palomar Transient Factory. This sample includes 888 SNe of 12 distinct classes out to redshift z \u2248 1. We present the photometric properties of their host galaxies from the far-ultraviolet to the mid-infrared and model the host-galaxy spectral energy distributions to derive physical properties. The galaxy mass function of Type Ic, Ib, IIb, II, and IIn SNe ranges from 10\u2075 to 10^(11.5) M_\u2299, probing the entire mass range of star-forming galaxies down to the least-massive star-forming galaxies known. Moreover, the galaxy mass distributions are consistent with models of star-formation-weighted mass functions. Regular CCSNe are hence direct tracers of star formation. Small but notable differences exist between some of the SN classes. Type Ib/c SNe prefer galaxies with slightly higher masses (i.e., higher metallicities) and star formation rates than Type IIb and II SNe. These differences are less pronounced than previously thought. H-poor superluminous supernovae (SLSNe) and SNe Ic-BL are scarce in galaxies above 10\u00b9\u2070 M_\u2299. Their progenitors require environments with metallicities of < 0.4 and < 1 solar, respectively. In addition, the hosts of H-poor SLSNe are dominated by a younger stellar population than all other classes of CCSNe. Our findings corroborate the notion that low metallicity and young age play an important role in the formation of SLSN progenitors.", "date": "2021-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "255", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 29", "id_number": "CaltechAUTHORS:20200916-112847454", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112847454", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "European Research Council (ERC)", "grant_number": "852097" }, { "agency": "Israel Science Foundation", "grant_number": "2108/18" }, { "agency": "Israel Science Foundation", "grant_number": "2752/19" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Council for Higher Education (Israel)" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "NASA", "grant_number": "NNG17PX03C" }, { "agency": "Heising-Simons Foundation" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "Royal Society" }, { "agency": "Science Foundation, Ireland" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Ministry of Science (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": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "Ministry of Education, Science and Technological Development (Serbia)", "grant_number": "51-03-68/2020/14/20002" }, { "agency": "VILLUM FONDEN", "grant_number": "19054" }, { "agency": "Marie Curie Fellowship", "grant_number": "794467" }, { "agency": "European Research Council (ERC)", "grant_number": "758638" }, { "agency": "Slovenian Research Agency", "grant_number": "I0-0033" }, { "agency": "Slovenian Research Agency", "grant_number": "P1-0031" }, { "agency": "Slovenian Research Agency", "grant_number": "J1-8136" }, { "agency": "Slovenian Research Agency", "grant_number": "Z1-1853" }, { "agency": "European Research Council (ERC)", "grant_number": "770935" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Google" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Participating Institutions" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Lawrence Berkeley National Laboratory" }, { "agency": "Department of Energy (DOE)", "grant_number": "KA2401022" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4365/abff5e", "primary_object": { "basename": "2008.05988.pdf", "url": "https://authors.library.caltech.edu/records/xrrdr-s4e65/files/2008.05988.pdf" }, "related_objects": [ { "basename": "Schulze_2021_ApJS_255_29.pdf", "url": "https://authors.library.caltech.edu/records/xrrdr-s4e65/files/Schulze_2021_ApJS_255_29.pdf" } ], "pub_year": "2021", "author_list": "Schulze, Steve; Yaron, Ofer; et el." }, { "id": "https://authors.library.caltech.edu/records/45mnp-m7a21", "eprint_id": 107855, "eprint_status": "archive", "datestamp": "2023-08-20 03:55:31", "lastmod": "2023-10-23 16:17:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Barbarino-Cristina", "name": { "family": "Barbarino", "given": "C." }, "orcid": "0000-0002-3821-6144" }, { "id": "Sollerman-Jesper", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-Francesco", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Karamehmetoglu-Emir", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Arcavi-Iair", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Gal-Yam-Avishay", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Schulze-Steve", "name": { "family": "Schulze", "given": "S." }, "orcid": "0000-0001-6797-1889" }, { "id": "Wo\u017aniak-Przemyslaw-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Type Ic supernovae from the (intermediate) Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 ESO 2021. Article published by EDP Sciences. \n\nReceived 10 July 2020; Accepted 10 November 2020; Published online 20 July 2021. \n\nThe Oskar Klein Centre was funded by the Swedish Research Council. C.B. gratefully acknowledges support from the Knut and Alice Wallenberg Foundation, and from the Wennergren Foundation (PI JS). The intermediate Palomar Transient Factory project is 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. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. The data presented herein 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. IA is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe Program and acknowledges support from that program, from the Israel Science Foundation (grant numbers 2108/18 and 2752/19), from the United States \u2013 Israel Binational Science Foundation (BSF), and from the Israeli Council for Higher Education Alon Fellowship. AGY'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, Paul and Tina Gardner, Yeda-Sela and the WIS-CIT joint research grant; AGY is the recipient of the Helen and Martin Kimmel Award for Innovative Investigation.\n\nPublished - aa38890-20.pdf
Submitted - 2010.08392.pdf
", "abstract": "Context. Type Ic supernovae represent the explosions of the most stripped massive stars, but their progenitors and explosion mechanisms remain unclear. Larger samples of observed supernovae can help characterize the population of these transients. \n\nAims. We present an analysis of 44 spectroscopically normal Type Ic supernovae, with focus on the light curves. The photometric data were obtained over 7 years with the Palomar Transient Factory and its continuation, the intermediate Palomar Transient Factory. This is the first homogeneous and large sample of SNe Ic from an untargeted survey, and we aim to estimate explosion parameters for the sample. \n\nMethods. We present K-corrected Bgriz light curves of these SNe, obtained through photometry on template-subtracted images. We performed an analysis on the shape of the r-band light curves and confirmed the correlation between the rise parameter \u0394m\u208b\u2081\u2080 and the decline parameter \u0394m\u2081\u2085. Peak r-band absolute magnitudes have an average of \u221217.71 \u00b1 0.85 mag. To derive the explosion epochs, we fit the r-band lightcurves to a template derived from a well-sampled light curve. We computed the bolometric light curves using r and g band data, g \u2212 r colors and bolometric corrections. Bolometric light curves and Fe\u202fII \u03bb5169 velocities at peak were used to fit to the Arnett semianalytic model in order to estimate the ejecta mass M_(ej), the explosion energy E_K and the mass of radioactive nickel M(\u2075\u2076Ni) for each SN. \n\nResults. Including 41 SNe, we find average values of \u27e8M_(ej)\u27e9 = 4.50 \u00b1 0.79\u2006M\u2299, \u27e8E_K\u27e9 = 1.79 \u00b1 0.29 \u00d7 10\u2075\u00b9 erg, and \u27e8M\u2075\u2076Ni\u27e9 = 0.19 \u00b1 0.03\u2006M\u2299. The explosion-parameter distributions are comparable to those available in the literature, but our large sample also includes some transients with narrow and very broad light curves leading to more extreme ejecta masses values.", "date": "2021-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "651", "publisher": "EDP Sciences", "pagerange": "Art. No. A81", "id_number": "CaltechAUTHORS:20210202-095227669", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210202-095227669", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Wenner-Gren Foundation" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Israel Science Foundation", "grant_number": "2108/18" }, { "agency": "Israel Science Foundation", "grant_number": "2752/19" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Council for Higher Education (Israel)" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Benoziyo Center for Astrophysics" }, { "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" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/202038890", "primary_object": { "basename": "2010.08392.pdf", "url": "https://authors.library.caltech.edu/records/45mnp-m7a21/files/2010.08392.pdf" }, "related_objects": [ { "basename": "aa38890-20.pdf", "url": "https://authors.library.caltech.edu/records/45mnp-m7a21/files/aa38890-20.pdf" } ], "pub_year": "2021", "author_list": "Barbarino, C.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/hkjpg-3xc25", "eprint_id": 103707, "eprint_status": "archive", "datestamp": "2023-08-20 02:00:21", "lastmod": "2023-10-20 16:37:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johansson-Joel", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Goobar-Ariel", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Price-Sedona-H", "name": { "family": "Price", "given": "S.H." }, "orcid": "0000-0002-0108-4176" }, { "id": "Sagu\u00e9s-Carracedo-Ana", "name": { "family": "Sagu\u00e9s Carracedo", "given": "A." }, "orcid": "0000-0002-3498-2167" }, { "id": "Della-Bruna-L", "name": { "family": "Della Bruna", "given": "L." } }, { "id": "Nugent-Peter-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Dhawan-Suhail", "name": { "family": "Dhawan", "given": "S." }, "orcid": "0000-0002-2376-6979" }, { "id": "M\u00f6rtsell-Edvard", "name": { "family": "M\u00f6rtsell", "given": "E." }, "orcid": "0000-0002-8380-6143" }, { "id": "Papadogiannakis-Sem\u00e9li", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Amanullah-Rahman", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Goldstein-Daniel-A", "name": { "family": "Goldstein", "given": "D." }, "orcid": "0000-0003-3461-8661" }, { "id": "Cenko-S-Bradley", "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": "Dugas-Alison-M", "name": { "family": "Dugas", "given": "A." }, "orcid": "0000-0001-7344-0208" }, { "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" }, { "id": "Lunnan-Ragnhild", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" } ] }, "title": "Spectroscopy of the first resolved strongly lensed Type Ia supernova iPTF16geu", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: strong \u2013 supernovae: general \u2013 supernova: individual (iPTF16geu)", "note": "\u00a9 2020 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2020 December 8. Received 2020 November 24; in original form 2020 April 23. Published: 16 December 2020. \n\nWe thank E. Zackrisson and A. Adamo for helpful discussions. We thank T. Brink, R. Bruch, Cooper, S. Goldwasser, A. Ho, I. Irani, B. Jain, Y. Sharma, A. Tzanidakis, Q. Ye, and W. Zheng for performing observations. \n\nAG acknowledges support from the Swedish National Space Agency and the Swedish Research Council. RL is supported by 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). ASC acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsr\u00e5det, the Swedish Research Council. \n\nThe Intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee (USA), the Oskar Klein Center at Stockholm University (Sweden), 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\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 Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nThese results made use of the Lowell Discovery Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale and by a grant from the Mt. Cuba Astronomical Foundation. \n\nData Availability: All our spectra are available from the WISeREP archive (Yaron & Gal-Yam 2012).\n\nPublished - staa3829.pdf
Submitted - 2004.10164.pdf
", "abstract": "We report the results from spectroscopic observations of the multiple images of the strongly lensed Type Ia supernova (SN Ia), iPTF16geu, obtained with ground-based telescopes and the Hubble Space Telescope (HST). From a single epoch of slitless spectroscopy with HST, we resolve spectra of individual lensed supernova images for the first time. This allows us to perform an independent measurement of the time-delay between the two brightest images, \u0394t = 1.4 \u00b1 5.0 d, which is consistent with the time-delay measured from the light curves. We also present measurements of narrow emission and absorption lines characterizing the interstellar medium in the SN Ia host galaxy at z = 0.4087, as well as in the foreground lensing galaxy at z = 0.2163. We detect strong Na\u2009ID absorption in the host galaxy, indicating that iPTF16geu belongs to a subclass of SNe Ia displaying 'anomalously' large Na\u2009ID column densities compared to dust extinction derived from light curves. For the lens galaxy, we refine the measurement of the velocity dispersion, \u03c3 = 129 \u00b1 4 km\u2009s\u207b\u00b9, which significantly constrains the lens model. We use ground-based spectroscopy, boosted by a factor \u223c70 from lensing magnification, to study the properties of a high-z SN Ia with unprecedented signal-to-noise ratio. The spectral properties of the supernova, such as pseudo-Equivalent widths of several absorption features and velocities of the Si\u2009II-line, indicate that iPTF16geu is a normal SN Ia. We do not detect any significant deviations of the SN spectral energy distribution from microlensing of the SN photosphere by stars and compact objects in the lensing galaxy.", "date": "2021-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "502", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "510-520", "id_number": "CaltechAUTHORS:20200604-151427243", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151427243", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish National Space Agency" }, { "agency": "Swedish Research Council" }, { "agency": "Marie Curie Fellowship", "grant_number": "H2020-MSCA-IF-2017-794467" }, { "agency": "G.R.E.A.T. Research Environment" }, { "agency": "W. M. Keck Foundation" }, { "agency": "John and Ginger Giovale" }, { "agency": "Mt. Cuba Astronomical Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/staa3829", "primary_object": { "basename": "2004.10164.pdf", "url": "https://authors.library.caltech.edu/records/hkjpg-3xc25/files/2004.10164.pdf" }, "related_objects": [ { "basename": "staa3829.pdf", "url": "https://authors.library.caltech.edu/records/hkjpg-3xc25/files/staa3829.pdf" } ], "pub_year": "2021", "author_list": "Johansson, J.; Goobar, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/swmhf-anr14", "eprint_id": 104815, "eprint_status": "archive", "datestamp": "2023-08-22 05:54:40", "lastmod": "2023-10-20 20:52:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yang-Fan", "name": { "family": "Yang", "given": "Fan" }, "orcid": "0000-0002-6039-8212" }, { "id": "Long-R-J", "name": { "family": "Long", "given": "Richard J." }, "orcid": "0000-0002-8559-0067" }, { "id": "Shan-Su-Su", "name": { "family": "Shan", "given": "Su-Su" }, "orcid": "0000-0002-5744-2016" }, { "id": "Zhang-Bo", "name": { "family": "Zhang", "given": "Bo" }, "orcid": "0000-0002-6434-7201" }, { "id": "Guo-Rui", "name": { "family": "Guo", "given": "Rui" } }, { "id": "Bai-Yu", "name": { "family": "Bai", "given": "Yu" }, "orcid": "0000-0002-4740-3857" }, { "id": "Bai-Zhongrui", "name": { "family": "Bai", "given": "Zhongrui" }, "orcid": "0000-0003-3884-5693" }, { "id": "Cui-Kai-Ming", "name": { "family": "Cui", "given": "Kai-Ming" } }, { "id": "Wang-Song", "name": { "family": "Wang", "given": "Song" }, "orcid": "0000-0003-3116-5038" }, { "id": "Liu-Ji-Feng", "name": { "family": "Liu", "given": "Ji-Feng" } } ] }, "title": "A Catalog of Short Period Spectroscopic and Eclipsing Binaries Identified from the LAMOST and PTF Surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "Eclipsing binary stars; Close binary stars; Spectroscopic binary stars; Binary stars; Detached binary stars; Contact binary stars", "note": "\u00a9 2020. The American Astronomical Society. \n\nReceived 2019 September 9; revised 2020 June 1; accepted 2020 June 4; published 2020 August 7. \n\nWe wish to thank the referee for their most useful comments that have greatly improved the paper. This work made use of astroML8 and IPAC database for PTF.9 We acknowledge the use of LAMOST data and the catalog. We would like to thank Lin He and Chang-Qing Luo for the useful discussion. We also thank Weiming Gu for the feedback on the work. F.Y. and J.F.L. acknowledge funding from National Natural Science Foundation of China (NSFC.11988101), National Science Fund for Distinguished Young Scholars (No. 11425313), and National Key Research and Development Program of China (No. 2016YFA0400800).\n\nPublished - Yang_2020_ApJS_249_31.pdf
Accepted Version - 2006.04430.pdf
", "abstract": "Binaries play key roles in determining stellar parameters and exploring stellar evolution models. We build a catalog of 88 eclipsing binaries with spectroscopic information, taking advantage of observations from both the Large Sky Area Multi-Object fiber Spectroscopic Telescope and the Palomar Transient Factory surveys. A software pipeline is constructed to identify binary candidates by examining their light curves. The orbital periods of binaries are derived from the Lomb\u2013Scargle method. The key distinguishing features of eclipsing binaries are recognized by a new filter, Flat Test. We classify the eclipsing binaries by applying a Fourier analysis on the light curves. Among all the binary stars, 13 binaries are identified as eclipsing binaries for the first time. The catalog contains the following information: the position, primary eclipsing magnitude and time, eclipsing depth, the number of photometry and radial velocity observations, largest radial velocity difference, binary type, the effective temperature of the observable star T eff, and surface gravity of the observable star log g. The false-positive probability is calculated by using both a Monte Carlo simulation and real data from the Sloan Digital Sky Survey Stripe 82 Standard Catalog. The binaries in the catalog are mostly with a period of less than one day. The period distribution shows a 0.22 day cutoff, which is consistent with the low probability of an eclipsing binary rotating with such a period.", "date": "2020-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "249", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20200807-090348710", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200807-090348710", "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": "11988101" }, { "agency": "National Science Fund for Distinguished Young Scholars", "grant_number": "11425313" }, { "agency": "National Key Research and Development Program of China", "grant_number": "2016YFA0400800" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/1538-4365/ab9b77", "primary_object": { "basename": "2006.04430.pdf", "url": "https://authors.library.caltech.edu/records/swmhf-anr14/files/2006.04430.pdf" }, "related_objects": [ { "basename": "Yang_2020_ApJS_249_31.pdf", "url": "https://authors.library.caltech.edu/records/swmhf-anr14/files/Yang_2020_ApJS_249_31.pdf" } ], "pub_year": "2020", "author_list": "Yang, Fan; Long, Richard J.; et el." }, { "id": "https://authors.library.caltech.edu/records/8r5z8-qw012", "eprint_id": 96618, "eprint_status": "archive", "datestamp": "2023-08-19 21:08:12", "lastmod": "2023-10-20 21:21:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "A." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Tartaglia-L", "name": { "family": "Tartaglia", "given": "L." }, "orcid": "0000-0003-3433-1492" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Mor\u00e5-K", "name": { "family": "Mor\u00e5", "given": "K." } }, { "id": "Moriya-T-J", "name": { "family": "Moriya", "given": "T. J." }, "orcid": "0000-0003-1169-1954" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Papadogiannakis-S", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "U." }, "orcid": "0000-0002-2560-3495" }, { "id": "Schulze-S", "name": { "family": "Schulze", "given": "S." }, "orcid": "0000-0001-6797-1889" } ] }, "title": "Type IIn supernova light-curve properties measured from an untargeted survey sample", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 13 June 2019; Accepted 30 September 2019; Published online 19 May 2020. \n\nBased on observations made with the Palomar Transient Factory\nand intermediate Palomar Transient Factory surveys. \n\nA.N. gratefully acknowledges a grant from Stiftelsen Gustaf och Ellen Kobbs stipendiefond, and wishes to thank Ashley Villar for providing MOSFiT contours in table format for Fig. 13, Axel Runnholm for help with Python, Ofer Yaron for help with WISeREP, Timothy E. Holy for making the distinguishable_colors function, Maayane Soumagnac and Peter Lundqvist for discussions, and opponent Philip James for questions and comments at the PhD thesis defence in Stockholm 2019 September 23. We gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. The intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin (Milwaukee), the Oskar Klein Centre, 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. This work was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. A.V.F. is grateful for financial assistance from National Science Foundation (NSF) grant AST-1211916, the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U. C. Berkeley). E.O.O. is grateful for support by grants from the Israeli Ministry of Science, ISF, Minerva, BSF, BSF transformative program, Weizmann-UK, and the I-CORE Program of the Planning and Budgeting Committee and the Israel Science Foundation (grant No. 1829/12). G.L. was supported by research grant 19054 from VILLUM FONDEN. 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 (NASA). SED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171. Based in part on observations obtained at the Gemini Observatory, under programs: GN-2010B-Q13 and GN-2010A-Q20 (PI: Howell), 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 NSF (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). Partly based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognise 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. Partly based on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the NSF. The authors are honoured to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. 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. Partly based on observations made with the University of Hawaii's 2.2 m telescope, at Maunakea Observatory, Hawaii, USA. Partly based on observations made with the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. Partly based on observations made with the 5 m Hale Telescope (P200), at Palomar Observatory, California, USA. Partly based on observations made with the Kast spectrograph on the Shane 3 m telescope at Lick Observatory, Mount Hamilton, California, USA. Research at Lick Observatory is partially supported by a generous gift from Google. We thank S. Bradley Cenko, Kelsey I. Clubb, Melissa L. Graham, Michael T. Kandrashoff, Patrick L. Kelly, Alekzandir Morton, Peter E. Nugent, and Jeffrey M. Silverman for help with some of the observations and reductions. This research used the Latest Supernovae web page (maintained by D. Bishop) and the Open Supernova Catalog (maintained by J. Guillochon and J. Parrent). This research used the SIMBAD and VizieR databases operated at CDS, Strasbourg, France, as well as the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and NASA's Astrophysics Data System. STSDAS and PYRAF are products of the Space Telescope Science Institute, which is operated by AURA for NASA. We acknowledge the whole PTF and iPTF collaborations for finding and following the SNe IIn studied in this sample.\n\nSubmitted - 1906.05812.pdf
Updated - aa36097-19.pdf
", "abstract": "The evolution of a Type IIn supernova (SN IIn) is governed by the interaction between the SN ejecta and a hydrogen-rich circumstellar medium. The SNe IIn thus allow us to probe the late-time mass-loss history of their progenitor stars. We present a sample of SNe IIn from the untargeted, magnitude-limited surveys of the Palomar Transient Factory (PTF) and its successor, the intermediate PTF (iPTF). To date, statistics on SN IIn optical light-curve properties have generally been based on small (\u227210 SNe) samples from targeted SN surveys. The SNe IIn found and followed by the PTF/iPTF were used to select a sample of 42 events with useful constraints on the rise times as well as with available post-peak photometry. The sample SNe were discovered in 2009\u22122016 and have at least one low-resolution classification spectrum, as well as photometry from the P48 and P60 telescopes at Palomar Observatory. We study the light-curve properties of these SNe IIn using spline fits (for the peak and the declining portion) and template matching (for the rising portion). We study the peak-magnitude distribution, rise times, decline rates, colour evolution, host galaxies, and K-corrections of the SNe in our sample. We find that the typical rise times are divided into fast and slow risers at 20 \u00b1 6 d and 50 \u00b1 11 d, respectively. The decline rates are possibly divided into two clusters (with slopes 0.013 \u00b1 0.006 mag d\u22121 and 0.040 \u00b1 0.010 mag d\u22121), but this division has weak statistical significance. We find no significant correlation between the peak luminosity of SNe IIn and their rise times, but the more luminous SNe IIn are generally found to be more long-lasting. Slowly rising SNe IIn are generally found to decline slowly. The SNe in our sample were hosted by galaxies of absolute magnitude \u221222\u2004\u2272\u2004M_g\u2004\u2272\u2004\u221213 mag. The K-corrections at light-curve peak of the SNe IIn in our sample are found to be within 0.2 mag for the observer's frame r-band, for SNe at redshifts z\u2004< \u20040.25. By applying K-corrections and also including ostensibly \"superluminous\" SNe IIn, we find that the peak magnitudes are M^r_(peak) = \u221219.18 \u00b1 1.32 mag. We conclude that the occurrence of conspicuous light-curve bumps in SNe IIn, such as in iPTF13z, are limited to 1.4^(+14.6)_(\u22121.0) % of the SNe IIn. We also investigate a possible sub-type of SNe IIn with a fast rise to a \u227350 d plateau followed by a slow, linear decline.", "date": "2020-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "637", "publisher": "EDP Sciences", "pagerange": "Art. No. A73", "id_number": "CaltechAUTHORS:20190621-083724261", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190621-083724261", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Stiftelsen Gustaf och Ellen Kobbs" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "MINERVA (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Weizmann Institute of Science" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "VILLUM FONDEN", "grant_number": "19054" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1106171" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Google" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1051/0004-6361/201936097", "primary_object": { "basename": "1906.05812.pdf", "url": "https://authors.library.caltech.edu/records/8r5z8-qw012/files/1906.05812.pdf" }, "related_objects": [ { "basename": "aa36097-19.pdf", "url": "https://authors.library.caltech.edu/records/8r5z8-qw012/files/aa36097-19.pdf" } ], "pub_year": "2020", "author_list": "Nyholm, A.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/wp3q4-ra897", "eprint_id": 99125, "eprint_status": "archive", "datestamp": "2023-08-22 04:38:45", "lastmod": "2023-10-18 17:53:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soraisam-M-D", "name": { "family": "Soraisam", "given": "Monika D." } }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Drout-M-R", "name": { "family": "Drout", "given": "Maria R." }, "orcid": "0000-0001-7081-0082" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Variability of massive stars in M31 from the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "Andromeda galaxy; Massive stars; Supergiant stars; Catalogs; Surveys", "note": "\u00a9 2020 The American Astronomical Society.\n\nReceived 2019 August 6; revised 2020 February 21; accepted 2020 February 26; published 2020 April 8. \n\nM.D.S. is supported by the Illinois Survey Science Fellowship of the Center for Astrophysical Surveys at the University of Illinois at Urbana-Champaign. This research was supported in part by the National Science Foundation through grant PHY-1748958 at the KITP and benefited from interactions that were funded by the Gordon and Betty Moore Foundation through grant GBMF5076. M.D.S. thanks Chien-Hsiu Lee for helpful discussions on observational studies of stellar variability, as well as Niels Oppermann for insights regarding proper applications of signal analysis tools. We also thank Charlie Conroy and Yan-Fei Jiang for discussions, and the latter for providing his simulation data. M.R.D. acknowledges support from the Dunlap Institute at the University of Toronto and the Canadian Institute for Advanced Research (CIFAR). This work was based on observations obtained with the 48 inch Samuel Oschin Telescope at the Palomar Observatory as part of the Palomar Transient Factory project. Operations were conducted by Caltech Optical Observatories and data processing by IPAC. We thank Xiaodian Chen for helpful comments on the period\u2013luminosity relation of contact binaries. \n\nSoftware: numpy (van der Walt et al. 2011), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration et al. 2013), pyfits, pandas (McKinney 2010), mpi4py (Dalc\u00edn et al. 2005), matplotlib (Hunter 2007), DAOPHOT (Stetson 1987), DAOGROW (Stetson 1990), NIFTy (Selig et al. 2013).\n\nPublished - Soraisam_2020_ApJ_893_11.pdf
Submitted - 1908.02439.pdf
", "abstract": "Using data from the (intermediate) Palomar Transient Factory (iPTF), we characterize the time variability of \u2248500 massive stars in M31. Our sample is those stars that are spectrally typed by Massey and collaborators, including Luminous Blue Variables, Wolf\u2013Rayets, and warm and cool supergiants. We use the high-cadence, long-baseline (\u22485 yr) data from the iPTF survey, coupled with data-processing tools that model complex features in the light curves. We find widespread photometric (R-band) variability in the upper Hertzsprung Russell diagram (or CMD) with an increasing prevalence of variability with later spectral types. Red stars (V \u2212 I > 1.5) exhibit larger amplitude fluctuations than their bluer counterparts. We extract a characteristic variability timescale, t_(ch), via wavelet transformations that are sensitive to both continuous and localized fluctuations. Cool supergiants are characterized by longer timescales (>100 days) than the hotter stars. The latter have typical timescales of tens of days but cover a wider range, from our resolution limit of a few days to longer than 100 days. Using a 60 night block of data straddling two nights with a cadence of around 2 minutes, we extracted t_(ch) in the range 0.1\u201310 days with amplitudes of a few percent for 13 stars. Though there is broad agreement between the observed variability characteristics in the different parts of the upper CMD with theoretical predictions, detailed comparison requires models with a more comprehensive treatment of the various physical processes operating in these stars, such as pulsation, subsurface convection, and the effect of binary companions.", "date": "2020-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "893", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 11", "id_number": "CaltechAUTHORS:20191007-150028591", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191007-150028591", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Illinois Urbana-Champaign" }, { "agency": "NSF", "grant_number": "PHY-1748958" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "Dunlap Institute for Astronomy and Astrophysics" }, { "agency": "University of Toronto" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/ab7b7b", "primary_object": { "basename": "1908.02439.pdf", "url": "https://authors.library.caltech.edu/records/wp3q4-ra897/files/1908.02439.pdf" }, "related_objects": [ { "basename": "Soraisam_2020_ApJ_893_11.pdf", "url": "https://authors.library.caltech.edu/records/wp3q4-ra897/files/Soraisam_2020_ApJ_893_11.pdf" } ], "pub_year": "2020", "author_list": "Soraisam, Monika D.; Bildsten, Lars; et el." }, { "id": "https://authors.library.caltech.edu/records/8yk17-spp77", "eprint_id": 96449, "eprint_status": "archive", "datestamp": "2023-08-19 16:21:51", "lastmod": "2023-10-20 21:11:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Frohmaier-C", "name": { "family": "Frohmaier", "given": "C." }, "orcid": "0000-0001-9553-4723" }, { "id": "Sullivan-M", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Smith-M", "name": { "family": "Smith", "given": "M." }, "orcid": "0000-0002-3321-1432" }, { "id": "Dimitriadis-G", "name": { "family": "Dimitriadis", "given": "G." } }, { "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": "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" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "The volumetric rate of normal type Ia supernovae in the local Universe discovered by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis, surveys, supernovae: general", "note": "\u00a9 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) \n\nAccepted 2019 March 13. Received 2019 March 13; in original form 2018 December 7. \n\nWe thank the anonymous referee for their useful comments. \n\nWe acknowledge support from EU/FP7 ERC grant number 615929. We acknowledge the use of the IRIDIS High Performance Computing Facility, and associated support services, at the University of Southampton. 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. Observations were obtained with the Samuel Oschin Telescope and the 60-inch Telescope at the Palomar Observatory 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.\n\nPublished - stz807.pdf
Accepted Version - 1903.08580.pdf
", "abstract": "We present the volumetric rate of normal type Ia supernovae (SNe Ia) discovered by the Palomar Transient Factory (PTF). Using strict data-quality cuts, and considering only periods when the PTF maintained a regular cadence, PTF discovered 90 SNe Ia at z \u2264 0.09 in a well-controlled sample over three years of operation (2010\u20132012). We use this to calculate the volumetric rate of SN Ia events by comparing this sample to simulations of hundreds of millions of SN Ia light curves produced in statistically representative realizations of the PTF survey. This quantifies the recovery efficiency of each PTF SN Ia event, and thus the relative weighting of each event. From this, the volumetric SN Ia rate was found to be r_v = 2.43 \u00b1 0.29(stat)^(+0.33)_(\u22120.19)(sys) \u00d7 10^(\u22125) SNe yr^(\u22121) Mpc^(\u22123) h^3_(70)\u2060. This represents the most precise local measurement of the SN Ia rate. We fit a simple SN Ia delay-time distribution model, \u221d t^(\u2212\u03b2), to our PTF rate measurement combined with a literature sample of rate measurements from surveys at higher redshifts. We find \u03b2 \u223c 1, consistent with a progenitor channel governed by the gravitational inspiral of binary white dwarfs.", "date": "2019-06-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "486", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2308-2320", "id_number": "CaltechAUTHORS:20190614-134340278", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190614-134340278", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stz807", "primary_object": { "basename": "stz807.pdf", "url": "https://authors.library.caltech.edu/records/8yk17-spp77/files/stz807.pdf" }, "related_objects": [ { "basename": "1903.08580.pdf", "url": "https://authors.library.caltech.edu/records/8yk17-spp77/files/1903.08580.pdf" } ], "pub_year": "2019", "author_list": "Frohmaier, C.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/xpst1-qq633", "eprint_id": 94687, "eprint_status": "archive", "datestamp": "2023-08-19 15:35:36", "lastmod": "2023-10-20 18:10:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Zackay-B", "name": { "family": "Zackay", "given": "B." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "A Six-year Image-subtraction Light Curve of SN 2010jl", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical \u2013 stars: mass-loss \u2013 (stars:) supernovae: general \u2013 (stars:) supernovae: individual", "note": "\u00a9 2019 The Astronomical Society of the Pacific. \n\nReceived 2018 October 10; accepted 2019 February 25; published 2019 April 12. \n\nThis paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, Oskar Klein Centre, 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 grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation, Minerva, BSF, BSF-transformative, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). B.Z. is grateful for receiving the support of the Infosys membership fund.\n\nSubmitted - 1903.02016.pdf
", "abstract": "SN 2010jl was a luminous Type IIn supernova (SN), detected in radio, optical, X-ray and hard X-rays. Here we report on its six-year R- and g-band light curves obtained using the Palomar Transient Factory. The light curve was generated using a pipeline based on the proper image-subtraction method and we discuss the algorithm performances. As noted before, the R-band light curve, up to about 300 days after maximum light is well described by a power-law decline with a power-law index of \u03b1 \u2248 \u22120.5. Between day 300 and day 2300 after maximum light, it is consistent with a power-law decline, with a power-law index of about \u03b1 \u2248 \u22123.4. The longevity of the light curve suggests that the massive circumstellar material around the progenitor was ejected on timescales of at least tens of years prior to the progenitor explosion.", "date": "2019-05", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "131", "number": "999", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 054204", "id_number": "CaltechAUTHORS:20190412-095510961", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190412-095510961", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Infosys" } ] }, "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/ab0a19", "primary_object": { "basename": "1903.02016.pdf", "url": "https://authors.library.caltech.edu/records/xpst1-qq633/files/1903.02016.pdf" }, "pub_year": "2019", "author_list": "Ofek, E. O.; Zackay, B.; et el." }, { "id": "https://authors.library.caltech.edu/records/jjaf7-3kn03", "eprint_id": 94138, "eprint_status": "archive", "datestamp": "2023-08-19 14:59:32", "lastmod": "2023-10-20 17:43:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Isaacson-H-T", "name": { "family": "Isaacson", "given": "Howard" }, "orcid": "0000-0002-0531-1073" }, { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" }, { "id": "Joshi-V", "name": { "family": "Joshi", "given": "Vishal" } }, { "id": "Banerjee-D-P-K", "name": { "family": "Banerjee", "given": "D. P. K." } }, { "id": "Cutri-R-M", "name": { "family": "Cutri", "given": "Roc M." }, "orcid": "0000-0002-0077-2305" } ] }, "title": "PTF14jg: The Remarkable Outburst and Post-burst Evolution of a Previously Anonymous Galactic Star", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter \u2013 infrared: stars \u2013 stars: activity \u2013 stars: pre-main sequence \u2013 stars: variables:\ngeneral \u2013 stars: winds, outflows", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 July 27; revised 2019 January 27; accepted 2019 January 28; published 2019 March 26. \n\nWe have made extensive use of SIMBAD and ADS online resources in sleuthing for possible analogs of PTF 14jg. We also spent a considerable amount of quality time with the NIST atomic database in attemping line identification in the HIRES data, and we consulted the MILES population synthesis spectral database when searching for spectral templates. We are grateful to Cathie Clarke and Giuseppe Lodato for locating electronic copies of photometric data on the \"classical\" FU Ori outbursts that were published in their 2005 paper and to Ariel Langer, who contributed to our analysis of these light curves. We thank Mark Heyer for locating CO channel maps from his 1998 paper. We benefited from allocations by Tom Soifer as director of the Spitzer Space Telescope and Lee Mundy as director of CARMA of small amounts of DDT to obtain the observations reported here. We thank the spectroscopic observers listed in Table 6 who are not otherwise acknowledged with authorship, especially Yi Cao, Sumin Tang, Jacob Jencson, and Anna Ho. D.P.K.B. thanks N. M. Ashok and V. Venkataraman for help with some of the Mount Abu observations. The research at PRL is supported by the Department of Space, Government of India. We thank the staff members at the various observational facilities used and the numerous instrument builders. The Intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin\u2013Milwaukee, 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. Finally, L.A.H. is grateful for the tolerance of the many young star and nova pundits on whom various versions of this story have been tried out over the past several years. And we thank the referee for comments that provided a valuable opportunity for us to reexamine our presentation. \n\nFacilities: PO:1.2m:PTF - , PO:1.5m:GRBcam - , MIRO:1.2m - , Hale:DBSP - , Hale:TSPEC - , Keck:I:HIRES - , Keck:I:LRIS - , Keck:I:DEIMOS - , Keck:I:MOSFIRE - , APO:DIS - , APO:TSPEC - , 2MASS - , Spitzer, WISE(NEOWISE) - , Swift:UVOT - , Swift:XRT - , CARMA - Combined Array for Research in Millimeter-Wave Astronomy, IRSA. -\n\nPublished - Hillenbrand_2019_ApJ_874_82.pdf
Accepted Version - 1901.10693.pdf
", "abstract": "We report the outbursting source PTF 14jg, which, prior to the onset of its late 2013 eruption, was a faint, unstudied, and virtually uncataloged star. The salient features of the PTF 14jg outburst are (i) projected location near the W4 H II region and radial velocity consistent with physical association; (ii) a light curve that underwent an ~6\u20137 mag optical (R-band) through mid-infrared (L-band) brightening on a timescale of a few months, peaked and then faded by ~3 mag, but plateaued still >3.5 mag above quiescence by ~8 months post-peak, lasting to at least 4 yr after eruption; (iii) strong outflow signatures with velocities reaching \u2212530 km s^(-1); (iv) a low-gravity and broad (~100\u2013150 km s^(-1) FWHM) optical absorption-line spectrum that systematically changes its spectral type with wavelength; (v) lithium; and (vi) ultraviolet and infrared excess. We tentatively identify the outburst as exhibiting characteristics of a young star FU Ori event. However, the burst would be unusually hot, with an absorption spectrum exhibiting high-excitation (~11,000\u201315,000 K) lines in the optical and no evidence of CO in the near-infrared, in addition to exhibiting an unusual light curve. We thus also consider alternative scenarios\u2014including various forms of novae, nuclear-burning instabilities, massive star events, and mergers\u2014finding them all inferior to the atypically hot FU Ori star classification. The source eventually may be interpreted as a new category of young star outburst with a larger amplitude and shorter rise time than most FU Ori\u2013like events.", "date": "2019-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "874", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 82", "id_number": "CaltechAUTHORS:20190326-084628949", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190326-084628949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Space (India)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab06c8", "primary_object": { "basename": "1901.10693.pdf", "url": "https://authors.library.caltech.edu/records/jjaf7-3kn03/files/1901.10693.pdf" }, "related_objects": [ { "basename": "Hillenbrand_2019_ApJ_874_82.pdf", "url": "https://authors.library.caltech.edu/records/jjaf7-3kn03/files/Hillenbrand_2019_ApJ_874_82.pdf" } ], "pub_year": "2019", "author_list": "Hillenbrand, Lynne A.; Miller, Adam A.; et el." }, { "id": "https://authors.library.caltech.edu/records/94pn3-vdp47", "eprint_id": 93621, "eprint_status": "archive", "datestamp": "2023-08-22 01:04:12", "lastmod": "2023-10-20 17:17:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Duggan-G-E", "name": { "family": "Duggan", "given": "G." }, "orcid": "0000-0002-9256-6735" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Levan-A", "name": { "family": "Levan", "given": "A." }, "orcid": "0000-0001-7821-9369" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Pasham-D-R", "name": { "family": "Pasham", "given": "D. R." } }, { "id": "Veilleux-S", "name": { "family": "Veilleux", "given": "S." }, "orcid": "0000-0002-3158-6820" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Zheng-Wei", "name": { "family": "Zheng", "given": "W." } } ] }, "title": "The Broad Absorption Line Tidal Disruption Event iPTF15af: Optical and Ultraviolet Evolution", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: nuclei; stars: individual (iPTF15af)", "note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2018 September 19; revised 2019 January 23; accepted 2019 February 1; published 2019 March 7. \n\nWe thank the anonymous referee, whose comments and suggestions helped to improve the paper. We are grateful to Peter Maksym, Sterl Phinney, Eliot Quataert, Cl\u00e9ment Bonnerot, Tiara Hung, and Sjoert Van Velzen for valuable discussions and comments on this work. We are grateful to Eric Bellm, Melissa Graham, Anna Ho, and Daniel Perley for carrying out some of the spectroscopic observations and/or reductions, and Linda Strubbe for her support with the HST proposal. We thank the HST staff for the prompt scheduling of these ToO observations, as well as the PI Neil Gehrels and the Swift ToO team for the timely execution of our observations.\n\nThis work was supported by the GROWTH project funded by the National Science Foundation (NSF) under grant AST-1545949. 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). Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. \n\nA.H. acknowledges support by the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation. This research was supported by a Grant from the GIF, the German-Israeli Foundation for Scientific Research and Development. A.V.F.'s group at UC Berkeley is grateful for financial assistance from the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (UC Berkeley). \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 (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work makes use of observations from Las Cumbres Observatory. 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 NASA and the NSF. 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 NASA. Based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. \n\nFacilities: HST (STIS) - , Karl G. Jansky Very Large Array - , Keck:I (LRIS) - , PO:1.2 m - , PO:1.5 m - , Swift - , WISE. - \n\nSoftware: Astropy (The Astropy Collaboration et al. 2018), emcee (Foreman-Mackey et al. 2013), FPipe (Fremling et al. 2016), lcogtsnpipe (Valenti et al. 2016), lmfit (Newville et al. 2014), lpipe http://www.astro.caltech.edu/~dperley/programs/lpipe.html, MOSFIT (Guillochon et al. 2018), NumPy (van der Walt et al. 2011), PTFIDE (Masci et al. 2017), SciPy (Jones et al. 2001).\n\nPublished - Blagorodnova_2019_ApJ_873_92.pdf
Submitted - 1809.07446.pdf
", "abstract": "We present multiwavelength observations of the tidal disruption event (TDE) iPTF15af, discovered by the intermediate Palomar Transient Factory survey at redshift z = 0.07897. The optical and ultraviolet (UV) light curves of the transient show a slow decay over 5 months, in agreement with previous optically discovered TDEs. It also has a comparable blackbody peak luminosity of L_(peak) \u2248 1.2 \u00d7 10^(44) erg s^(-1). The inferred temperature from the optical and UV data shows a value of (3\u20135) \u00d7 10^4 K. The transient is not detected in X-rays up to L_X < 3 \u00d7 10^(42) erg s^(-1) within the first 5 months after discovery. The optical spectra exhibit two distinct broad emission lines in the He ii region, and at later times also H\u03b1 emission. Additionally, emission from [N iii] and [O iii] is detected, likely produced by the Bowen fluorescence effect. UV spectra reveal broad emission and absorption lines associated with high-ionization states of N v, C iv, Si iv, and possibly P v. These features, analogous to those of broad absorption line quasars (BAL QSOs), require an absorber with column densities N_H > 10^(23) cm^(\u22122). This optically thick gas would also explain the nondetection in soft X-rays. The profile of the absorption lines with the highest column density material at the largest velocity is opposite that of BAL QSOs. We suggest that radiation pressure generated by the TDE flare at early times could have provided the initial acceleration mechanism for this gas. Spectral UV line monitoring of future TDEs could test this proposal.", "date": "2019-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "873", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 92", "id_number": "CaltechAUTHORS:20190307-092619351", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190307-092619351", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "016.192.277" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NAS5-98034" } ] }, "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": "10.3847/1538-4357/ab04b0", "primary_object": { "basename": "Blagorodnova_2019_ApJ_873_92.pdf", "url": "https://authors.library.caltech.edu/records/94pn3-vdp47/files/Blagorodnova_2019_ApJ_873_92.pdf" }, "related_objects": [ { "basename": "1809.07446.pdf", "url": "https://authors.library.caltech.edu/records/94pn3-vdp47/files/1809.07446.pdf" } ], "pub_year": "2019", "author_list": "Blagorodnova, N.; Cenko, S. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/bg15y-rvm81", "eprint_id": 94663, "eprint_status": "archive", "datestamp": "2023-08-19 14:35:17", "lastmod": "2023-10-20 18:09:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Papadogiannakis-S", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Bulla-M", "name": { "family": "Bulla", "given": "M." }, "orcid": "0000-0002-8255-5127" }, { "id": "Dhawan-S", "name": { "family": "Dhawan", "given": "S." } }, { "id": "Doran-G-B", "name": { "family": "Doran", "given": "G." } }, { "id": "Feindt-U", "name": { "family": "Feindt", "given": "U." }, "orcid": "0000-0002-9435-2167" }, { "id": "Ferretti-R", "name": { "family": "Ferretti", "given": "R." }, "orcid": "0000-0001-7814-5814" }, { "id": "Hangard-L", "name": { "family": "Hangard", "given": "L." } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "A." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" } ] }, "title": "R-band light-curve properties of Type Ia supernovae from the (intermediate) Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 cosmology: observations", "note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model(https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). \n\nAccepted 2018 November 30. Received 2018 November 29; in original form 2018 June 13. Published: 06 December 2018. \n\nSP would like to thank D. Men\u00e9ndez Hurtado, K. Muroe, D. Mortlock, and T. Calv\u00e9n for helpful discussions. The authors thank the anonymous referee for comments and suggestions which improved the paper. \n\nThe Intermediate Palomar Transient Factory project is 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 (Taiwan Next Generation OIR via UST-Caltech Collaboration) of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. The iPTF Swedish collaboration is funded through a grant from the Knut and Alice Wallenberg foundation and individual grants from the Swedish National Science Council as well as the Swedish National Space Agency. DAH is supported by NSF grant AST-1313484. This work was supported by the GROWTH project (Global Relay of Observatories Watching Transients Happen) funded by the National Science Foundation under Grant No 1545949. GROWTH is a collaborative project between California Institute of Technology (USA), Pomona College (USA), San Diego State University (USA), Los Alamos National Laboratory (USA), University of Maryland College Park (USA), University of Wisconsin Milwaukee (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). The Weizmann interactive supernova data repository - http://wiserep.weizmann.ac.il was used to make the data public. This research was conducted using the resources of High Performance Computing Center North (HPC2N) under the proposal SNIC 2017/3-64. 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\nPublished - sty3301.pdf
Accepted Version - 1812.01439.pdf
Supplemental Material - sty3301_supplemental_figures.zip
", "abstract": "We present the best 265 sampled R-band light curves of spectroscopically identified Type Ia supernovae (SNe) from the Palomar Transient Factory (PTF; 2009-2012) survey and the intermediate Palomar Transient Factory (iPTF; 2013-2017). A model-independent light-curve template is built from our data-set with the purpose to investigate average properties and diversity in our sample. We searched for multiple populations in the light-curve properties using machine learning tools. We also utilized the long history of our light curves, up to 4000 days, to exclude any significant pre- or post- supernova flares. From the shapes of light curves we found the average rise time in the R band to be 16.8^(+0.5)_(\u22120.6) days. Although PTF/iPTF were single-band surveys, by modelling the residuals of the SNe in the Hubble\u2013Lema\u00eetre diagram, we estimate the average colour excess of our sample to be \u3008E(B \u2212 V)\u3009 \u2248 0.05(2) mag and thus the mean corrected peak brightness to be M_R = \u221219.02 \u00b1 0.02 +5log(H_0[kms^(\u22121)Mpc^(\u22121)]/70) mag with only weak dependennce on light\u2013curve shape. The intrinsic scatter is found to be \u03c3R = 0.186 \u00b1 0.033 mag for the redshift range 0.05 < z < 0.1, without colour corrections of individual SNe. Our analysis shows that Malmquist bias becomes very significant at z = 0.13. A similar limitation is expected for the ongoing Zwicky Transient Facility (ZTF) survey using the same telescope, but new camera expressly designed for ZTF.", "date": "2019-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "483", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "5045-5076", "id_number": "CaltechAUTHORS:20190411-131634820", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190411-131634820", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish National Science Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/sty3301", "primary_object": { "basename": "1812.01439.pdf", "url": "https://authors.library.caltech.edu/records/bg15y-rvm81/files/1812.01439.pdf" }, "related_objects": [ { "basename": "sty3301.pdf", "url": "https://authors.library.caltech.edu/records/bg15y-rvm81/files/sty3301.pdf" }, { "basename": "sty3301_supplemental_figures.zip", "url": "https://authors.library.caltech.edu/records/bg15y-rvm81/files/sty3301_supplemental_figures.zip" } ], "pub_year": "2019", "author_list": "Papadogiannakis, S.; Goobar, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/21tvb-0p157", "eprint_id": 92454, "eprint_status": "archive", "datestamp": "2023-08-19 13:40:13", "lastmod": "2023-10-20 15:43:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Barbarino-C", "name": { "family": "Barbarino", "given": "C." }, "orcid": "0000-0002-3821-6144" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Hiramatsu-Daichi", "name": { "family": "Hiramatsu", "given": "D." } }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "A." } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" } ] }, "title": "Analysis of broad-lined Type Ic supernovae from the (intermediate) Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2019 ESO. Article published by EDP Sciences. \n\nReceived 15 October 2018; Accepted 12 November 2018; Published online 10 January 2019. \n\nThe Oskar Klein Centre is funded by the Swedish Research Council. F.T. and J.S. gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. D.A.H. and G.H. are supported by National Science Foundation (NSF) grant AST-1313484. A.V.F. is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). A.G.-Y. 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. The intermediate Palomar Transient Factory project is 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. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. We acknowledge contributions from the full PTF and iPTF collaborations that made it possible to discover and monitor the SE SNe analyzed in this work. This work was supported by the GROWTH project funded by NSF under grant AST-1545949. We thank the staff at the various observatories at which data were collected. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias. The data presented herein 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. Our results made use of the Discovery Channel Telescope (DCT) at Lowell Observatory. Lowell is a private, nonprofit institution dedicated to astrophysical research and public appreciation of astronomy, and it operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale. This work makes use of the Las Cumbres Observatory network and the LCO Supernova Key Project. Research at Lick Observatory is partially supported by a generous gift from Google. 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 (NASA). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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. We thank Mark Sullivan for contributing spectral data obtained under his observing programs. We acknowledge the large number of observers and those responsible for data reduction who helped acquire the spectroscopic database over the years. Among others, these include S. Adams, C. Badenes, S. Ben-Ami, N. Blagorodnova, J. S. Bloom, J. Botyanszki, K. Burdge, Y. Cao, J. Choi, N. Chotard, K. I. Clubb, D. Cook, N. Cucchiara, A. De Cia, A. Drake, G. Duggan, M. Fraser, M. L. Graham, T. Hashimoto, A. Ho, I. Hook, A. Horesh, E. Hsiao, T. Hung, M. Kandrashoff, M. Kasliwal, E. Kirby, I. Kleiser, S. Knezevic, T. Kupfer, K. Maguire, T. Matheson, A. A. Miller, K. P. Mooley, E. Ofek, Y.-C. Pan, D. Polishook, D. Poznanski, V. Ravi, J. Rex, A. Rubin, B. Sesar, I. Shivvers, A. Sternberg, N. Suzuki, D. Tal, C. Theissen, J. van Roestel. P. Vreeswijk, E. Walker, A. Waszczak, D. Xu, O. Yaron, and B. Zackay. We also thank the staff at the observatories where data were obtained. We acknowledge Umaa Rebbapragada and her group for the work with the machine-learning algorithm that allowed iPTF to discover transients. We thank Maryam Modjaz for the productive discussion on the SN classification.\n\nPublished - aa34429-18.pdf
Accepted Version - 1811.09544.pdf
", "abstract": "We study 34 Type Ic supernovae that have broad spectral features (SNe Ic-BL). This is the only SN type found in association with long-duration gamma-ray bursts (GRBs). We obtained our photometric data with the Palomar Transient Factory (PTF) and its continuation, the intermediate PTF (iPTF). This is the first large, homogeneous sample of SNe Ic-BL from an untargeted survey. Furthermore, given the high observational cadence of iPTF, most of these SNe Ic-BL were discovered soon after explosion. We present K-corrected Bgriz light curves of these SNe, obtained through photometry on template-subtracted images. We analyzed the shape of the r-band light curves, finding a correlation between the decline parameter \u0394m_(15) and the rise parameter \u0394m_(\u221210). We studied the SN colors and, based on g \u2212 r, we estimated the host-galaxy extinction for each event. Peak r-band absolute magnitudes have an average of \u221218.6 \u00b1 0.5 mag. We fit each r-band light curve with that of SN 1998bw (scaled and stretched) to derive the explosion epochs. We computed the bolometric light curves using bolometric corrections, r-band data, and g \u2212 r colors. Expansion velocities from Fe\u202fII were obtained by fitting spectral templates of SNe Ic. Bolometric light curves and velocities at peak were fitted using the semianalytic Arnett model to estimate ejecta mass M_(ej), explosion energy E_K and ^(56)Ni mass M(^(56)Ni) for each SN. We find average values of M_(ej)\u2004=\u20044 \u00b1 3\u2006M\u2299, EK\u2004=\u2004(7 \u00b1 6)\u00d710^(51) erg, and M(^(56)Ni)=0.31\u2006 \u00b1 \u20060.16\u2006M\u2299. The parameter distributions were compared to those presented in the literature and are overall in agreement with them. We also estimated the degree of ^(56)Ni mixing using scaling relations derived from hydrodynamical models and we find that all the SNe are strongly mixed. The derived explosion parameters imply that at least 21% of the progenitors of SNe Ic-BL are compatible with massive (> 28\u2006M\u2299), possibly single stars, whereas at least 64% might come from less massive stars in close binary systems.", "date": "2019-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "621", "publisher": "EDP Sciences", "pagerange": "Art. No. A71", "id_number": "CaltechAUTHORS:20190124-114218177", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190124-114218177", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Quantum Universe I-Core Program" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Kimmel Award" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Google" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "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": "10.1051/0004-6361/201834429", "primary_object": { "basename": "1811.09544.pdf", "url": "https://authors.library.caltech.edu/records/21tvb-0p157/files/1811.09544.pdf" }, "related_objects": [ { "basename": "aa34429-18.pdf", "url": "https://authors.library.caltech.edu/records/21tvb-0p157/files/aa34429-18.pdf" } ], "pub_year": "2019", "author_list": "Taddia, F.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/9r6wp-71807", "eprint_id": 92341, "eprint_status": "archive", "datestamp": "2023-08-19 13:39:21", "lastmod": "2023-10-20 00:12:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Burke-J-P", "name": { "family": "Burke", "given": "J." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Andersen-O", "name": { "family": "Andersen", "given": "O." } }, { "id": "Andreoni-I", "name": { "family": "Andreoni", "given": "I." }, "orcid": "0000-0002-8977-1498" }, { "id": "Barbarino-C", "name": { "family": "Barbarino", "given": "C." }, "orcid": "0000-0002-3821-6144" }, { "id": "Blagorodova-N", "name": { "family": "Blagorodova", "given": "N." } }, { "id": "Brink-T-G", "name": { "family": "Brink", "given": "T. G." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Hiramatsu-Daichi", "name": { "family": "Hiramatsu", "given": "D." } }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "de-Jaeger-T", "name": { "family": "de Jaeger", "given": "T." }, "orcid": "0000-0001-6069-1139" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "McCully-C", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Tartaglia-L", "name": { "family": "Tartaglia", "given": "L." }, "orcid": "0000-0003-3433-1492" }, { "id": "Terreran-G", "name": { "family": "Terreran", "given": "G." } }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Wang-X", "name": { "family": "Wang", "given": "X." } } ] }, "title": "Late-time observations of the extraordinary Type II supernova iPTF14hls", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual: iPTF14hls", "note": "\u00a9 2019 ESO. Article published by EDP Sciences. \n\nReceived 21 June 2018; Accepted 23 October 2018; Published online 03 January 2019. \n\nWe gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. Based on observations obtained with the Samuel Oschin 48-inch telescope and the 60-inch telescope at the Palomar Observatory as part of the intermediate Palomar Transient Factory (iPTF) 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. The Oskar Klein Centre is funded by the Swedish Research Council. This work is partly based on observations made with DOLoRes at TNG, and on observations made with the Nordic Optical Telescope, operated by NOTSA at IAC using ALFOSC, which is provided by the IAA. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W.M. Keck Foundation. Some of the Keck observations were partially supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). Support for I. Arcavi was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. R.L. acknowledge GROWTH. Research funding to I. Andreoni is provided by the Australian Astronomical Observatory. A.V.F. has been supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and the Miller Institute for Basic Research in Science (U.C. Berkeley) where he is a Miller Senior Fellow. His work was conducted in part at the Aspen Center for Physics, which is supported by US National Science Foundation grant PHY-1607611; he thanks the Center for its hospitality during the supermassive black holes workshop in June and July 2018. X. W. is supported by the National Natural Science Foundation of China (NSFC grants 11325313 and 11633002). Special thanks to A. Bostroem and W. Zheng for help with Keck observations.\n\nPublished - aa33689-18.pdf
Accepted Version - 1806.10001.pdf
", "abstract": "Aims. We study iPTF14hls, a luminous and extraordinary long-lived Type II supernova, which lately has attracted much attention and disparate interpretation. \n\nMethods. We have presented new optical photometry that extends the light curves up to more than three years past discovery. We also obtained optical spectroscopy over this period, and furthermore present additional space-based observations using Swift and HST. \n\nResults. After an almost constant luminosity for hundreds of days, the later light curve of iPTF14hls finally fades and then displays a dramatic drop after about 1000 d, but the supernova is still visible at the latest epochs presented. The spectra have finally turned nebular, and our very last optical spectrum likely displays signatures from the deep and dense interior of the explosion. A high-resolution HST image highlights the complex environment of the explosion in this low-luminosity galaxy. \n\nConclusions. We provide a large number of additional late-time observations of iPTF14hls, which are (and will continue to be) used to assess the many different interpretations for this intriguing object. In particular, the very late (+1000 d) steep decline of the optical light curve is difficult to reconcile with the proposed central engine models. The lack of very strong X-ray emission, and the emergence of intermediate-width emission lines including [S II] that we propose originate from dense, processed material in the core of the supernova ejecta, are also key observational tests for both existing and future models.", "date": "2019-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "621", "publisher": "EDP Sciences", "pagerange": "Art. No. A30", "id_number": "CaltechAUTHORS:20190117-095029584", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190117-095029584", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Northwestern University" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "GROWTH" }, { "agency": "Australian Astronomical Observatory (AAO)" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "NSF", "grant_number": "PHY-1607611" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11325313" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11633002" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201833689", "primary_object": { "basename": "1806.10001.pdf", "url": "https://authors.library.caltech.edu/records/9r6wp-71807/files/1806.10001.pdf" }, "related_objects": [ { "basename": "aa33689-18.pdf", "url": "https://authors.library.caltech.edu/records/9r6wp-71807/files/aa33689-18.pdf" } ], "pub_year": "2019", "author_list": "Sollerman, J.; Taddia, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/7ftc8-g0s41", "eprint_id": 92447, "eprint_status": "archive", "datestamp": "2023-08-19 13:40:04", "lastmod": "2023-10-20 15:42:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Barbarino-C", "name": { "family": "Barbarino", "given": "C." }, "orcid": "0000-0002-3821-6144" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "West-S-S", "name": { "family": "West", "given": "S." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" } ] }, "title": "The luminous late-time emission of the type-Ic supernova iPTF15dtg \u2013 evidence for powering from a magnetar?", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual: SN 2011bm \u2013 supernovae: individual: iPTF15dtg \u2013 supernovae: individual: SN 2010mb \u2013 supernovae: general", "note": "\u00a9 2019 ESO. Article published by EDP Sciences. \n\nReceived 21 June 2018; Accepted 4 November 2018; Published online 09 January 2019. \n\nFT and JS gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. JS acknowledges the support of Vetenskapsr\u00e5det through VR grants 2012-2265 and 2017-03699. This 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. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the intermediate Palomar Transient Factory (iPTF) 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\nPublished - aa33688-18.pdf
Accepted Version - 1806.10000.pdf
", "abstract": "Context. The transient iPTF15dtg is a type-Ic supernova (SN) showing a broad light curve around maximum light, consistent with massive ejecta if we assume a radioactive-powering scenario.\nAims. We aim to study the late-time light curve of iPTF15dtg, which turned out to be extraordinarily luminous for a stripped-envelope (SE) SN, and investigate possible powering mechanisms.\nMethods. We compare the observed light curves to those of other SE SNe and also to models for the ^(56)Co decay. We analyze and compare the spectra to nebular spectra of other SE SNe. We build a bolometric light curve and fit it with different models, including powering by radioactivity, magnetar powering, and a combination of the two.\nResults. Between 150 and 750 d post-explosion, the luminosity of iPTF15dtg declined by merely two magnitudes instead of the six magnitudes expected from ^(56)Co decay. This is the first spectroscopically regular SE SN found to show this behavior. The model with both radioactivity and magnetar powering provides the best fit to the light curve and appears to be the most realistic powering mechanism. An alternative mechanism might be circumstellar-medium (CSM) interaction. However, the spectra of iPTF15dtg are very similar to those of other SE SNe, and do not show signs of strong CSM interaction.\nConclusions. The object iPTF15dtg is the first spectroscopically regular SE SN whose light curve displays such clear signs of a magnetar contributing to its late-time powering. Given this result, the mass of the ejecta needs to be revised to a lower value, and therefore the progenitor mass could be significantly lower than the previously estimated > 35 M\u2299.", "date": "2019-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "621", "publisher": "EDP Sciences", "pagerange": "Art. No. A64", "id_number": "CaltechAUTHORS:20190124-082804593", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190124-082804593", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Vetenskapsr\u00e5det", "grant_number": "2012-2265" }, { "agency": "Vetenskapsr\u00e5det", "grant_number": "2017-03699" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201833688", "primary_object": { "basename": "1806.10000.pdf", "url": "https://authors.library.caltech.edu/records/7ftc8-g0s41/files/1806.10000.pdf" }, "related_objects": [ { "basename": "aa33688-18.pdf", "url": "https://authors.library.caltech.edu/records/7ftc8-g0s41/files/aa33688-18.pdf" } ], "pub_year": "2019", "author_list": "Taddia, F.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/xh063-2en23", "eprint_id": 89484, "eprint_status": "archive", "datestamp": "2023-09-22 22:48:43", "lastmod": "2023-10-23 23:29:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Woosley-S-E", "name": { "family": "Woosley", "given": "S. E." } }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "B. D." }, "orcid": "0000-0002-7856-3570" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "A." }, "orcid": "0000-0003-2082-1626" }, { "id": "Cook-D-O", "name": { "family": "Cook", "given": "D. O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C. U." }, "orcid": "0000-0002-4223-103X" }, { "id": "Gatkine-P", "name": { "family": "Gatkine", "given": "P." }, "orcid": "0000-0002-1955-2230" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "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" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "A." } }, { "id": "Rubin-A-E", "name": { "family": "Rubin", "given": "A." } }, { "id": "Suzuki-Naoyuki", "name": { "family": "Suzuki", "given": "N." } }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "A UV resonance line echo from a shell around a hydrogen-poor superluminous supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "Stellar evolution; Time-domain astronomy; Transient astrophysical phenomena", "note": "\u00a9 2018 Springer Nature Limited. \n\nReceived 07 March 2018; Accepted 02 August 2018; Published\n10 September 2018. \n\nWe are grateful for discussions with C.-I. Bj\u00f6rnsson, S. Blinnikov, E. Sorokina, E. Ramirez-Ruiz and J. Fuller. The iPTF project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Centre, 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. This work was supported by the GROWTH project funded by the National Science Foundation (NSF grant no. 1545949). This research was supported by the Swedish Research Council, the Swedish National Space Board, and the Knut and Alice Wallenberg Foundation. 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 (NASA). A.G.-Y. is supported by the European Union through ERC grant no. 725161, the Quantum Universe I-Core programme, the Israel Science Foundation, the BSF Transformative programme and a Kimmel award. P.E.N. acknowledges support from the US Department of Energy (DOE) through DE-FOA-0001088, Analytical Modeling for Extreme-Scale Computing Environments. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the US DOE under contract no. DE-AC02-05CH11231. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the NSF. Some of the data 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 financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are fortunate to have the opportunity to conduct observations from this mountain. \n\nAuthor Contributions: R.L. coordinated the observational campaign, was PI of the Keck programme under which the late-time spectra were obtained, analysed the data and wrote the manuscript. C.F. wrote the resonance scattering code, ran the simulations, performed model comparisons, and contributed to manuscript writing. P.M.V. contributed to the interpretation and resonance line calculations and to the manuscript preparation. S.E.W. contributed to the comparison with PPI models and manuscript preparation. G.L., D.A.P., R.M.Q., L.Y., A.D.C. and A.G.-Y. contributed to the discovery, analysis, interpretation and manuscript preparation. M.M.K. contributed to manuscript preparation. S.R.K. is the PI of iPTF and of the P200/Keck programmes under which the early spectra were taken, and contributed to manuscript preparation. A.N. contributed to finding the supernova and to manuscript preparation. N.B., D.O.C. and A.R. reduced spectra. S.B.C. and P.G. obtained and reduced DCT photometry. C.U.F. reduced the P60 photometry. N.S. obtained and reduced the Subaru spectrum. F.J.M. and P.E.N. contributed to the photometric pipelines applied by iPTF. B.D.B. and P.W. contributed to the iPTF machine learning codes for transient search. \n\nThe authors declare no competing interests. \n\nCode availability: The light echo modelling code is available from C.F. (claes@astro.su.se) upon request. \n\nData availability: The photometry of iPTF16eh is available in Supplementary Table 1, and the spectra are available from WISeREP35 (http://wiserep.weizmann.ac.il/). In general, the data that support the plots within this paper and other findings of this study are available from the corresponding author upon reasonable request.\n\nAccepted Version - 1808.04887.pdf
Supplemental Material - 41550_2018_568_MOESM1_ESM.pdf
Supplemental Material - 41550_2018_568_MOESM2_ESM.txt
Supplemental Material - 41550_2018_568_MOESM3_ESM.txt
Supplemental Material - 41550_2018_568_MOESM4_ESM.txt
", "abstract": "Hydrogen-poor superluminous supernovae (SLSN-I) are a class of rare and energetic explosions that have been discovered in untargeted transient surveys in the past decade. The progenitor stars and the physical mechanism behind their large radiated energies (about 10^(51)\u2009erg or 10^(44)\u2009J) are both debated, with one class of models primarily requiring a large rotational energy and the other requiring very massive progenitors that either convert kinetic energy into radiation through interaction with circumstellar material (CSM) or engender an explosion caused by pair-instability (loss of photon pressure due to particle\u2013antiparticle production). Observing the structure of the CSM around SLSN-I offers a powerful test of some scenarios, although direct observations are scarce. Here, we present a series of spectroscopic observations of the SLSN-I iPTF16eh, which reveal both absorption and time- and frequency-variable emission in the Mg IIresonance doublet. We show that these observations are naturally explained as a resonance scattering light echo from a circumstellar shell. Modelling the evolution of the emission, we infer a shell radius of 0.1\u2009pc and velocity of 3,300\u2009km\u2009s\u22121, implying that the shell was ejected three decades before the supernova explosion. These properties match theoretical predictions of shell ejections occurring because of pulsational pair-instability and imply that the progenitor had a helium core mass of about 50\u201355 M_\u2299, corresponding to an initial mass of about 115 M_\u2299.", "date": "2018-11", "date_type": "published", "publication": "Nature Astronomy", "volume": "2", "number": "11", "publisher": "Nature Publishing Group", "pagerange": "887-895", "id_number": "CaltechAUTHORS:20180910-104151114", "issn": "2397-3366", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180910-104151114", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Quantum Universe I-Core Programme" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Kimmel Award" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FOA-0001088" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "W. M. Keck Foundation" } ] }, "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": "10.1038/s41550-018-0568-z", "primary_object": { "basename": "41550_2018_568_MOESM1_ESM.pdf", "url": "https://authors.library.caltech.edu/records/xh063-2en23/files/41550_2018_568_MOESM1_ESM.pdf" }, "related_objects": [ { "basename": "41550_2018_568_MOESM2_ESM.txt", "url": "https://authors.library.caltech.edu/records/xh063-2en23/files/41550_2018_568_MOESM2_ESM.txt" }, { "basename": "41550_2018_568_MOESM3_ESM.txt", "url": "https://authors.library.caltech.edu/records/xh063-2en23/files/41550_2018_568_MOESM3_ESM.txt" }, { "basename": "41550_2018_568_MOESM4_ESM.txt", "url": "https://authors.library.caltech.edu/records/xh063-2en23/files/41550_2018_568_MOESM4_ESM.txt" }, { "basename": "1808.04887.pdf", "url": "https://authors.library.caltech.edu/records/xh063-2en23/files/1808.04887.pdf" } ], "pub_year": "2018", "author_list": "Lunnan, R.; Fransson, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/rry12-hd505", "eprint_id": 91527, "eprint_status": "archive", "datestamp": "2023-08-19 12:04:12", "lastmod": "2023-10-19 23:10:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dhawan-S", "name": { "family": "Dhawan", "given": "S." } }, { "id": "Bulla-M", "name": { "family": "Bulla", "given": "M." }, "orcid": "0000-0002-8255-5127" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C" }, "orcid": "0000-0001-8532-3594" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Papadogiannakis-S", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" } ] }, "title": "iPTF16abc and the population of Type Ia supernovae: comparing the photospheric, transitional, and nebular phases", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general, supernova: individual (iPTF16abc)", "note": "\u00a9 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices) \n\nAccepted 2018 July 9. Received 2018 June 11; in original form 2018 February 2.\n\nWe would like to thank Peter Nugent for pointing us to the DECaLS photometry of iPTF16abc. We acknowledge fruitful comments from Jesper Sollerman. Funding from the Swedish Research Council, the Swedish Space Board, and the Knut & Alice (K&A) Wallenberg foundation made this research possible. A.A.M. is funded by the Large Synoptic Survey Telescope Corporation in support of the Data Science Fellowship Program. This work made use of the Heidelberg Supernova Model Archive (HESMA), https://hesma.h-its.org.\n\nPublished - sty1908.pdf
Accepted Version - 1808.02330.pdf
", "abstract": "Key information about the progenitor system and the explosion mechanism of Type Ia supernovae (SNe Ia) can be obtained from early observations, within a few days from explosion. iPTF16abc was discovered as a young SN Ia with excellent early time data. Here, we present photometry and spectroscopy of the SN in the nebular phase. A comparison of the early time data with a sample of SNe Ia shows distinct features, differing from normal SNe Ia at early phases but similar to normal SNe Ia at a few weeks after maximum light (i.e. the transitional phase) and well into the nebular phase. The transparency time-scales (t_0) for this sample of SNe Ia range between \u223c25 and 41 d indicating a diversity in the ejecta masses. t_0 also weakly correlates with the peak bolometric luminosity, consistent with the interpretation that SNe with higher ejecta masses would produce more ^(56)Ni\u2009. Comparing the t_0 and the maximum luminosity, L_(max)\u2009distribution of a sample of SNe Ia to predictions from a wide range of explosion models we find an indication that the sub-Chandrasekhar mass models span the range of observed values. However, the bright end of the distribution can be better explained by Chandrasekhar mass delayed detonation models, hinting at multiple progenitor channels to explain the observed bolometric properties of SNe Ia. iPTF16abc appears to be consistent with the predictions from the M_(ch)\u2009models.", "date": "2018-10-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "480", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1445-1456", "id_number": "CaltechAUTHORS:20181205-163501667", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181205-163501667", "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": "Knut and Alice Wallenberg Foundation" }, { "agency": "Large Synoptic Survey Telescope Corporation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/sty1908", "primary_object": { "basename": "1808.02330.pdf", "url": "https://authors.library.caltech.edu/records/rry12-hd505/files/1808.02330.pdf" }, "related_objects": [ { "basename": "sty1908.pdf", "url": "https://authors.library.caltech.edu/records/rry12-hd505/files/sty1908.pdf" } ], "pub_year": "2018", "author_list": "Dhawan, S.; Bulla, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/wmzdz-15220", "eprint_id": 90266, "eprint_status": "archive", "datestamp": "2023-08-19 11:57:35", "lastmod": "2023-10-18 23:19:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "De-Kishalay", "name": { "family": "De", "given": "K." }, "orcid": "0000-0002-8989-0542" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Duggan-G-E", "name": { "family": "Duggan", "given": "G. E." }, "orcid": "0000-0002-9256-6735" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" } ] }, "title": "A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Association for the Advancement of Science. \n\nReceived 31 December 2017; accepted 26 July 2018. \n\nWe thank the anonymous referees for a careful reading of the manuscript, which helped improve the quality of the paper. We thank C. Steidel, N. Stone, D. Stern, P. Hopkins, S. de Mink, Y. Suwa, A. Heger, and T. M. Tauris for valuable discussions. M.M.K. thanks J. Fuller, E. S. Phinney, L. Bildsten, and E. Quataert for stimulating discussions at the Skyhouse during a PTF-TN meeting. We also thank T. Staley and G. Anderson for help with scheduling of the AMI observations. Additional facility acknowledgments are provided in the supplementary materials. \n\nThe Intermediate Palomar Transient Factory project is 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. This work was supported by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation under PIRE Grant 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); Indian Institute of Technology Bombay (India); Weizmann Institute of Science (Israel); The Oskar Klein Centre at Stockholm University (Sweden); Humboldt University (Germany); and Liverpool John Moores University (UK). A.H. acknowledges support by the I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation. A.G.-Y. is supported by the EU via ERC grant 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program, and a Kimmel award. E.O.O. is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), Israel Science Foundation, Minerva, BSF, BSF-transformative, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). F.T. and J.S. gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. 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 DE-AC02-05CH11231. M.S. acknowledges support from EU/FP7 ERC grant 615929. P.E.N. acknowledges support from the DOE through DE-FOA-0001088, Analytical Modeling for Extreme-Scale Computing Environments. T.J.M. is supported by Grants-in-Aid for Scientific Research of the Japan Society for the Promotion of Science (16H07413 and 17H02864). Numerical computations were, in part, carried out on the PC cluster at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. 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. Author contributions: K.D. and M.M.K. initiated the study, conducted analysis, and wrote the manuscript. I.M. initiated the follow-up of the young transient. D.A.P., G.E.D., and Y.C. conducted Keck and Palomar observations and contributed to data reduction and manuscript preparation. S.B.C. conducted Keck and Swift observations and contributed to data reduction and manuscript preparation. M.S. conducted the WHT observations and data reduction. F.T. and J.S. conducted NOT observations and data analysis and contributed to manuscript preparation. J.B. conducted the LCO observations and data reduction. T.P. conducted Gemini observations and data analysis. C.R. and R.P.F. conducted the AMI observations and data reduction. A.H. conducted the VLA observations and data reduction. S.R.K. is iPTF PI and contributed to manuscript preparation. T.J.M. and P.A.M. prepared the ultra-stripped SN models presented in the paper. E.O.O., C.F., A.G.-Y., R.L., P.E.N., and A.L.P. contributed to manuscript preparation. G.B.D., R.R.L., and F.M. contributed to the machine learning codes used to search for young transients. \n\nThe authors declare no competing interests. \n\nData and materials availability: All photometric data used in this paper are provided in the supplementary materials (tables S1 and S2), and all observed spectra are available via the WISeREP repository at https://wiserep.weizmann.ac.il/ (under source name iPTF 14gqr). The software used for the ultra-stripped SN modeling is presented in (50), and the synthetic model spectra are available in data S1.\n\nAccepted Version - 1810.05181.pdf
Supplemental Material - aas8693_Data_S1.zip
Supplemental Material - aas8693_De_SM.pdf
", "abstract": "Compact neutron star binary systems are produced from binary massive stars through stellar evolution involving up to two supernova explosions. The final stages in the formation of these systems have not been directly observed. We report the discovery of iPTF 14gqr (SN 2014ft), a type Ic supernova with a fast-evolving light curve indicating an extremely low ejecta mass (\u22480.2 solar masses) and low kinetic energy (\u22482 \u00d7 10^(50) ergs). Early photometry and spectroscopy reveal evidence of shock cooling of an extended helium-rich envelope, likely ejected in an intense pre-explosion mass-loss episode of the progenitor. Taken together, we interpret iPTF 14gqr as evidence for ultra-stripped supernovae that form neutron stars in compact binary systems.", "date": "2018-10-12", "date_type": "published", "publication": "Science", "volume": "362", "number": "6411", "publisher": "American Association for the Advancement of Science", "pagerange": "201-206", "id_number": "CaltechAUTHORS:20181012-132958254", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181012-132958254", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Quantum Universe I-Core Program" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Kimmel Award" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "MINERVA (Israel)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FOA-0001088" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16H07413" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "17H02864" }, { "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": "10.1126/science.aas8693", "primary_object": { "basename": "1810.05181.pdf", "url": "https://authors.library.caltech.edu/records/wmzdz-15220/files/1810.05181.pdf" }, "related_objects": [ { "basename": "aas8693_Data_S1.zip", "url": "https://authors.library.caltech.edu/records/wmzdz-15220/files/aas8693_Data_S1.zip" }, { "basename": "aas8693_De_SM.pdf", "url": "https://authors.library.caltech.edu/records/wmzdz-15220/files/aas8693_De_SM.pdf" } ], "pub_year": "2018", "author_list": "De, K.; Kasliwal, M. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/r569z-q1a31", "eprint_id": 90278, "eprint_status": "archive", "datestamp": "2023-08-22 00:11:41", "lastmod": "2023-10-18 23:20:13", "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": "Cantwell-Therese", "name": { "family": "Cantwell", "given": "Therese" }, "orcid": "0000-0001-9159-6599" }, { "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": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "Joel" }, "orcid": "0000-0001-5975-290X" }, { "id": "Kong-Albert-K-H", "name": { "family": "Kong", "given": "Albert" }, "orcid": "0000-0002-5105-344X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "Ragnhild" }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Matuszewski-M", "name": { "family": "Matuszewski", "given": "Matt" } }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "Kunal P." }, "orcid": "0000-0002-2557-5180" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "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": "Perrott-Y", "name": { "family": "Perrott", "given": "Yvette" }, "orcid": "0000-0002-6255-8240" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "Umaa D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Rubin-A", "name": { "family": "Rubin", "given": "Adam" }, "orcid": "0000-0003-4557-0632" }, { "id": "O'Sullivan-Donal", "name": { "family": "O'Sullivan", "given": "Donal" }, "orcid": "0000-0002-4959-9179" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" } ] }, "title": "iPTF 16hgs: A Double-peaked Ca-rich Gap Transient in a Metal-poor, Star-forming Dwarf Galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (iPTF 16hgs); surveys", "note": "\u00a9 2018. The American Astronomical Society. \n\nReceived 2018 June 26; revised 2018 September 2; accepted 2018 September 4; published 2018 October 15. \n\nWe thank the referee Hagai Perets for a careful reading of the manuscript and providing valuable feedback that has improved its content. We thank C. Steidel, E. Kirby, K. Shen, T. Moriya, L. Bildsten, D. Kasen, A. Horesh, and N. Stone for valuable discussions. We thank Ken Shen, Takashi Moriya, and Stuart Sim for providing the comparison models presented in this paper. We thank Q. Ye, N. Blagorodnova, V. Ravi, S. Adams, and R. Lau for assisting with the observations presented in the paper. \n\nThe Intermediate Palomar Transient Factory project is 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. 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), 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). \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. These results made use of the Discovery Channel Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale. We thank the staff of the Mullard Radio Astronomy Observatory for their invaluable assistance in the commissioning and operation of AMI, which is supported by Cambridge University and the European Research Council under grant ERC-2012-StG-307215 LODESTONE. 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. The GMRT is run by the National Center for Radio Astrophysics of the Tata Institute of Fundamental Research. 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. Y.C.P. is supported by a Trinity College JRF. \n\nFacilities: PO 1.2 m - , PO 1.5 m - , DCT - , Hale (DBSP - , CWI) - , Keck-I (LRIS) - , Swift (XRT - , UVOT) - , AMI - , VLA - , uGMRT - . \n\nSoftware: HEAsoft (Arnaud 1996), BOXFIT code (van Eerten et al. 2010), pyMCZ code (Bianco et al. 2016), FAST code (Kriek et al. 2009), STARLIGHT code (Cid Fernandes et al. 2005), AMI-REDUCE (Davies et al. 2009), CASA (McMullin et al. 2007), Astropy (The Astropy Collaboration et al. 2018).\n\nPublished - De_2018_ApJ_866_72.pdf
Submitted - 1806.10623
", "abstract": "Calcium-rich gap transients represent an intriguing new class of faint and fast-evolving supernovae that exhibit strong [Ca ii] emission in their nebular phase spectra. In this paper, we present the discovery and follow-up observations of a faint and fast-evolving transient, iPTF 16hgs, that exhibited a double-peaked light curve. Exhibiting a Type Ib spectrum in the photospheric phase and an early transition to a [Ca ii] dominated nebular phase, iPTF 16hgs shows properties consistent with the class of Ca-rich gap transients, with two important exceptions. First, while the second peak of the light curve is similar to other Ca-rich gap transients, the first blue and fast-fading peak (declining over \u22482 days) is unique to this source. Second, we find that iPTF 16hgs occurred in the outskirts (projected offset of \u22486 kpc \u2248 1.9 R_(eff)) of a low-metallicity (\u22480.4 Z_\u2299), star-forming, dwarf spiral galaxy. Deep limits from late-time radio observations suggest a low-density environment for the source. If iPTF 16hgs shares explosion physics with the class of Ca-rich gap transients, the first peak can be explained by the presence of 0.01 M_\u2299 of ^(56)Ni in the outer layers the ejecta, reminiscent of some models of He-shell detonations on WDs. However, if iPTF 16hgs is physically unrelated to the class, the first peak is consistent with shock cooling emission (of an envelope with a mass of \u22480.08 M_\u2299 and radius of \u224813 R_\u2299) in a core-collapse explosion of a highly stripped massive star in a close binary system.", "date": "2018-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "866", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 72", "id_number": "CaltechAUTHORS:20181016-134539015", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181016-134539015", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "W. M. Keck Foundation" }, { "agency": "John and Ginger Giovale" }, { "agency": "European Research Council (ERC)", "grant_number": "307215" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Trinity College" } ] }, "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": "10.3847/1538-4357/aadf8e", "primary_object": { "basename": "1806.10623", "url": "https://authors.library.caltech.edu/records/r569z-q1a31/files/1806.10623" }, "related_objects": [ { "basename": "De_2018_ApJ_866_72.pdf", "url": "https://authors.library.caltech.edu/records/r569z-q1a31/files/De_2018_ApJ_866_72.pdf" } ], "pub_year": "2018", "author_list": "De, Kishalay; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/acvcx-vkf38", "eprint_id": 90042, "eprint_status": "archive", "datestamp": "2023-08-19 11:42:23", "lastmod": "2023-10-18 23:09:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hung-Tiara", "name": { "family": "Hung", "given": "T." }, "orcid": "0000-0002-9878-7889" }, { "id": "Gezari-Suvi", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Cenko-S-Bradley", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "van-Velzen-Sjoert", "name": { "family": "van Velzen", "given": "S." }, "orcid": "0000-0002-3859-8074" }, { "id": "Blagorodnova-Nadejda", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Lunnan-Ragnhild", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Kupfer-Thomas", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "Kong-Albert-K-H", "name": { "family": "Kong", "given": "A. K. H." }, "orcid": "0000-0002-5105-344X" }, { "id": "Nugent-Peter-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-Frank-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Roy-R", "name": { "family": "Roy", "given": "R." } }, { "id": "Petrushevska-Tanja", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" } ] }, "title": "Sifting for Sapphires: Systematic Selection of Tidal Disruption Events in iPTF", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: nuclei \u2013 surveys \u2013 ultraviolet: general", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 December 8; revised 2018 July 20; accepted 2018 August 4; published 2018 September 27. \n\nWe thank the anonymous referee for helpful comments that improved the manuscript. T.H. thanks Jesper Sollerman for his feedback on the manuscript. S.G. is supported in part by NASA Swift Cycle 12 grant NNX16AN85G and NSF CAREER grant 1454816. These results made use of the Discovery Channel Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DEAC02-05CH11231.\n\nPublished - Hung_2018_ApJS_238_15.pdf
Accepted Version - 1712.04936.pdf
Accepted Version - nihms-1527449.pdf
", "abstract": "We present results from a systematic selection of tidal disruption events (TDEs) in a wide-area (4800 deg^2), g+R band, Intermediate Palomar Transient Factory experiment. Our selection targets typical optically selected TDEs: bright (>60% flux increase) and blue transients residing in the centers of red galaxies. Using photometric selection criteria to down-select from a total of 493 nuclear transients to a sample of 26 sources, we then use follow-up UV imaging with the Neil Gehrels Swift Telescope, ground-based optical spectroscopy, and light curve fitting to classify them as 14 Type Ia supernovae (SNe Ia), 9 highly variable active galactic nuclei (AGNs), 2 confirmed TDEs, and 1 potential core-collapse supernova. We find it possible to filter AGNs by employing a more stringent transient color cut (g \u2212 r < \u22120.2 mag); further, UV imaging is the best discriminator for filtering SNe, since SNe Ia can appear as blue, optically, as TDEs in their early phases. However, when UV-optical color is unavailable, higher-precision astrometry can also effectively reduce SNe contamination in the optical. Our most stringent optical photometric selection criteria yields a 4.5:1 contamination rate, allowing for a manageable number of TDE candidates for complete spectroscopic follow-up and real-time classification in the Zwicky Transient Facility era. We measure a TDE per galaxy rate of 1.7^(+2.9)_(-1.3) x 10^(-4) gal^(-1) yr^(-1) (90% CL in Poisson statistics). This does not account for TDEs outside our selection criteria, and thus may not reflect the total TDE population, which is yet to be fully mapped.", "date": "2018-10", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "238", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20180927-161113513", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180927-161113513", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX16AN85G" }, { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "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": "10.3847/1538-4365/aad8b1", "pmcid": "PMC6544052", "primary_object": { "basename": "nihms-1527449.pdf", "url": "https://authors.library.caltech.edu/records/acvcx-vkf38/files/nihms-1527449.pdf" }, "related_objects": [ { "basename": "1712.04936.pdf", "url": "https://authors.library.caltech.edu/records/acvcx-vkf38/files/1712.04936.pdf" }, { "basename": "Hung_2018_ApJS_238_15.pdf", "url": "https://authors.library.caltech.edu/records/acvcx-vkf38/files/Hung_2018_ApJS_238_15.pdf" } ], "pub_year": "2018", "author_list": "Hung, T.; Gezari, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/50d7z-dk675", "eprint_id": 87150, "eprint_status": "archive", "datestamp": "2023-08-19 09:50:38", "lastmod": "2023-10-18 20:54:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "Annalisa" }, "orcid": "0000-0003-2082-1626" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 August 4; revised 2018 March 22; accepted 2018 March 23; published 2018 June 15. \n\nWe thank the referee for a useful and constructive report, which helped make the paper more robust. We thank L. Dessart, A. Jerkstrand, A. Kozyreva, and the SLSN MIAPP 2017 workshop participants for insightful discussions. A.D.C. acknowledges support by the Weizmann Institute of Science Koshland Center for Basic Research. Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. M.S. acknowledges support from EU/FP7-ERC grant No. [615929]. K.M. acknowledges support from the STFC through an Ernest Rutherford Fellowship. E.O.O. is grateful for 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 Committee and The Israel Science Foundation. A.C. acknowledges support from the NSF CAREER award 1455090. M.M.K. acknowledges support from the GROWTH project funded by the National Science Foundation under grant No. 1545949. The intermediate Palomar Transient Factory project is 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. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration. 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. This research has made use of NASA's Astrophysics Data System. This paper made use of Lowell Observatory's Discovery Channel Telescope (DCT). Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. Large Monolithic Imager (LMI) on DCT was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). This work makes use of observations taken with the LCO network. 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. 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\nSoftware: MS pipeline (Sullivan et al. 2006; Ofek et al. 2014a; Firth et al. 2015; Dimitriadis et al. 2017), LPIPE (http://www.astro.caltech.edu/~dperley/programs/lpipe.html), LCOGT pipeline (Valenti et al. 2016), HOTPANTS (http://www.astro.washington.edu/users/becker/v2.0/hotpants.html), IRAF (Tody 1986, 1993), SWarp (Bertin et al. 2002), DrizzlePac 2.0 (http://drizzlepac.stsci.edu).\n\nPublished - De_Cia_2018_ApJ_860_100.pdf
Submitted - 1708.01623.pdf
", "abstract": "We investigate the light-curve properties of a sample of 26 spectroscopically confirmed hydrogen-poor superluminous supernovae (SLSNe-I) in the Palomar Transient Factory survey. These events are brighter than SNe Ib/c and SNe Ic-BL, on average, by about 4 and 2 mag, respectively. The peak absolute magnitudes of SLSNe-I in rest-frame g band span \u221222 \u227e M g \u227e \u221220 mag, and these peaks are not powered by radioactive ^(56)Ni, unless strong asymmetries are at play. The rise timescales are longer for SLSNe than for normal SNe Ib/c, by roughly 10 days, for events with similar decay times. Thus, SLSNe-I can be considered as a separate population based on photometric properties. After peak, SLSNe-I decay with a wide range of slopes, with no obvious gap between rapidly declining and slowly declining events. The latter events show more irregularities (bumps) in the light curves at all times. At late times, the SLSN-I light curves slow down and cluster around the ^(56)Co radioactive decay rate. Powering the late-time light curves with radioactive decay would require between 1 and 10 M\u2299 of Ni masses. Alternatively, a simple magnetar model can reasonably fit the majority of SLSNe-I light curves, with four exceptions, and can mimic the radioactive decay of ^(56)Co, up to ~400 days from explosion. The resulting spin values do not correlate with the host-galaxy metallicities. Finally, the analysis of our sample cannot strengthen the case for using SLSNe-I for cosmology.", "date": "2018-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "860", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 100", "id_number": "CaltechAUTHORS:20180615-092514599", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180615-092514599", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Weizmann Institute of Science" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "NSF", "grant_number": "AST-1455090" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1005313" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aab9b6", "primary_object": { "basename": "De_Cia_2018_ApJ_860_100.pdf", "url": "https://authors.library.caltech.edu/records/50d7z-dk675/files/De_Cia_2018_ApJ_860_100.pdf" }, "related_objects": [ { "basename": "1708.01623.pdf", "url": "https://authors.library.caltech.edu/records/50d7z-dk675/files/1708.01623.pdf" } ], "pub_year": "2018", "author_list": "De Cia, Annalisa; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.edu/records/96khp-xea60", "eprint_id": 86590, "eprint_status": "archive", "datestamp": "2023-08-19 09:19:14", "lastmod": "2023-10-18 19:45:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soraisam-M-D", "name": { "family": "Soraisam", "given": "Monika D." } }, { "id": "Bilsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Drout-M-R", "name": { "family": "Drout", "given": "Maria R." }, "orcid": "0000-0001-7081-0082" }, { "id": "Bauer-E-B", "name": { "family": "Bauer", "given": "Evan B." }, "orcid": "0000-0002-4791-6724" }, { "id": "Gilfanov-M", "name": { "family": "Gilfanov", "given": "Marat" } }, { "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" }, "orcid": "0000-0002-8532-9395" }, { "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": "Matheson-T", "name": { "family": "Matheson", "given": "Thomas" }, "orcid": "0000-0001-6685-0479" }, { "id": "Saha-Abhijit", "name": { "family": "Saha", "given": "Abhijit" }, "orcid": "0000-0002-6839-4881" } ] }, "title": "Variability of Red Supergiants in M31 from the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: groups: individual (M31) \u2013 stars: massive \u2013 stars: oscillations \u2013 supergiants \u2013 surveys", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 January 15; revised 2018 March 27; accepted 2018 April 2; published 2018 May 24. \n\nThis work was supported by the National Science Foundation through grants PHY 11-25915, PHY 17-148958, and ACI 16-63688, and funded in part by the Gordon and Betty Moore Foundation through Grant GBMF5076. M.S. is grateful to Niels Oppermann for the detailed discussions on statistical approaches and methods of proper signal reconstruction. M.S. also thanks Mathew Graham and Ashish Mahabal for helpful discussions on the period-finding algorithms, and Matteo Cantiello for the helpful suggestions and comments on the manuscript. E.B. thanks Sang-Hyun Chun for providing MESA inlists necessary to reproduce their RSG models, and Matteo Cantiello for discussion of RSG evolution in MESA. PyFITS is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. Support for this work was provided to M.R.D. by NASA through Hubble Fellowship grant NSG-HF2-51373 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. M.R.D. acknowledges support from the Dunlap Institute at the University of Toronto. M.G. acknowledges the hospitality of the Kazan Federal University (KFU) and support by the Russian Government Program of Competitive Growth of KFU. \n\nSoftware: numpy (van der Walt et al. 2011), scipy (Jones et al. 2001), astropy (Astropy Collaboration et al. 2013), pyfits, pandas (McKinney 2010), mpi4py (Dalc\u00edn et al. 2005), matplotlib (Hunter 2007), DAOPHOT (Stetson 1987), DAOGROW (Stetson 1990), NIFTy (Selig et al. 2013).\n\nPublished - Soraisam_2018_ApJ_859_73.pdf
Submitted - 1803.09934.pdf
", "abstract": "Most massive stars end their lives as red supergiants (RSGs), a short-lived evolutionary phase when they are known to pulsate with varying amplitudes. The RSG period\u2013luminosity (PL) relation has been measured in the Milky Way, the Magellanic Clouds and M33 for about 120 stars in total. Using over 1500 epochs of R-band monitoring from the Palomar Transient Factory survey over a five-year period, we study the variability of 255 spectroscopically cataloged RSGs in M31. We find that all RGSs brighter than M_K \u2248 \u221210 mag (log(L/L\u2299) > 4.8) are variable at \u0394m_R > 0.05 mag. Our period analysis finds 63 with significant pulsation periods. Using the periods found and the known values of M K for these stars, we derive the RSG PL relation in M31 and show that it is consistent with those derived earlier in other galaxies of different metallicities. We also detect, for the first time, a sequence of likely first-overtone pulsations. Comparison to stellar evolution models from MESA confirms the first-overtone hypothesis and indicates that the variable stars in this sample have 12 M\u2299 < M < 24 M\u2299. As these RSGs are the immediate progenitors to Type II-P core-collapse supernovae (SNe), we also explore the implication of their variability in the initial-mass estimates for SN progenitors based on archival images of the progenitors. We find that this effect is small compared to the present measurement errors.", "date": "2018-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "859", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 73", "id_number": "CaltechAUTHORS:20180524-105736998", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180524-105736998", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 11-25915" }, { "agency": "NSF", "grant_number": "PHY 17-148958" }, { "agency": "NSF", "grant_number": "ACI 16-63688" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NASA Hubble Fellowship", "grant_number": "NSG-HF2-51373" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Dunlap Institute" }, { "agency": "Russian Government Program of Competitive Growth" }, { "agency": "Kazan Federal University" } ] }, "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": "10.3847/1538-4357/aabc59", "primary_object": { "basename": "Soraisam_2018_ApJ_859_73.pdf", "url": "https://authors.library.caltech.edu/records/96khp-xea60/files/Soraisam_2018_ApJ_859_73.pdf" }, "related_objects": [ { "basename": "1803.09934.pdf", "url": "https://authors.library.caltech.edu/records/96khp-xea60/files/1803.09934.pdf" } ], "pub_year": "2018", "author_list": "Soraisam, Monika D.; Bildsten, Lars; et el." }, { "id": "https://authors.library.caltech.edu/records/pekdb-25660", "eprint_id": 85501, "eprint_status": "archive", "datestamp": "2023-08-19 08:39:16", "lastmod": "2023-10-18 18:16:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "van-Roestel-J", "name": { "family": "van Roestel", "given": "J." }, "orcid": "0000-0002-2626-2872" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Ruiz-Carmona-R", "name": { "family": "Ruiz-Carmona", "given": "R." } }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "P. J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Burdge-K-B", "name": { "family": "Burdge", "given": "K." }, "orcid": "0000-0002-7226-836X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E." }, "orcid": "0000-0001-8018-5348" } ] }, "title": "Discovery of 36 eclipsing EL CVn binaries found by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close \u2013 binaries: eclipsing \u2013 stars: individual: EL CVn \u2013white dwarfs", "note": "\u00a9 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 December 18. Received 2017 December 18; in original form 2017 July 20. Published: 31 January 2018. \n\nWe thank the referee, Simon Jeffery, for a thorough reading of the manuscript and for providing us with useful comments and suggestions. We thank Adam Miller, Fabian Gieseke and Tom Heskes for many useful discussions about machine learning classification. We thank Tom Marsh for the use of LCURVE. We thank Luc Hendriks for suggesting the use of XGBOOST. JvR acknowledges support from the Netherlands Research School of Astronomy (NOVA) and the Foundation for Fundamental Research on Matter (FOM), and also the California Institute of Technology where a large part of this work was conducted. JvR and PJG thank the University of Cape Town (UCT) for their hospitality; this work was finalized while visiting UCT, supported by the NWO-NRF Bilateral Agreement in Astronomy. This research was supported in part by the National Science Foundation under Grant No. NSF PHY-1125915 and PJG thanks the Kavli Institute for Theoretical Physics at the University of California, Santa Barbara for a productive stay. \n\nThe Intermediate Palomar Transient Factory project is a scientific collaboration between 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. Funding for the SDSS-IV has been provided by the Alfred P. Sloan Foundation, the US 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\nThe 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, 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 Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. \n\nThis publication made use of data products from the 2MASS, 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\nBased on observations made with the NASA Galaxy Evolution Explorer, which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. \n\nThis publication made use of data products from the 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. \n\nThis research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS 143, 23. \n\nThis research has made use of the SVO Filter Profile Service (http://svo2.cab.inta-csic.es/theory/fps/) supported from the Spanish MINECO through grant AyA2014-55216. \n\nThis research made use of Scikit-learn (Pedregosa et al. 2011). \n\nThis research made use of ASTROPY, a community-developed core PYTHON package for Astronomy (Robitaille et al. 2013). \n\nIRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation (Tody 1993).\n\nPublished - stx3291.pdf
Submitted - 1712.06507.pdf
", "abstract": "We report on the discovery and analysis of 36 new eclipsing EL CVn-type binaries, consisting of a core helium-composition pre-white dwarf (pre-He-WD) and an early-type main-sequence companion. This more than doubles the known population of these systems. We have used supervised machine learning methods to search 0.8 million light curves from the Palomar Transient Factory (PTF), combined with Sloan Digital Sky Survey (SDSS), Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) and Two-Micron All-Sky Survey (2MASS) colours. The new systems range in orbital periods from 0.46 to 3.8\u2009d and in apparent brightness from \u223c14 to 16\u2009mag in the PTF R or g\u0384 filters. For 12 of the systems, we obtained radial velocity curves with the Intermediate Dispersion Spectrograph at the Isaac Newton Telescope. We modelled the light curves, radial velocity curves and spectral energy distributions to determine the system parameters. The radii (0.3\u20130.7\u2009R\u2299) and effective temperatures (8000\u201317\u2009000\u2009K) of the pre-He-WDs are consistent with stellar evolution models, but the masses (0.12\u20130.28 M\u2299) show more variance than models have predicted. This study shows that using machine learning techniques on large synoptic survey data is a powerful way to discover substantial samples of binary systems in short-lived evolutionary stages.", "date": "2018-04-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "475", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2560-2590", "id_number": "CaltechAUTHORS:20180329-132609534", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180329-132609534", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Onderzoekschool Voor Astronomie (NOVA)" }, { "agency": "Foundation for Fundamental Research on Matter (FOM)" }, { "agency": "Caltech" }, { "agency": "NSF", "grant_number": "PHY-1125915" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" }, { "agency": "Eotvos Lorand University (ELTE)" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "NASA", "grant_number": "NAS5-98034" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)", "grant_number": "AyA2014-55216" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stx3291", "primary_object": { "basename": "1712.06507.pdf", "url": "https://authors.library.caltech.edu/records/pekdb-25660/files/1712.06507.pdf" }, "related_objects": [ { "basename": "stx3291.pdf", "url": "https://authors.library.caltech.edu/records/pekdb-25660/files/stx3291.pdf" } ], "pub_year": "2018", "author_list": "van Roestel, J.; Kupfer, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/ytfx3-acn65", "eprint_id": 84973, "eprint_status": "archive", "datestamp": "2023-08-19 08:12:09", "lastmod": "2023-10-18 17:01:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "Annalisa" }, "orcid": "0000-0003-2082-1626" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "Giorgos" }, "orcid": "0000-0002-8597-0756" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "Ragnhild" }, "orcid": "0000-0001-9454-4639" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "Paul M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "Jeff" }, "orcid": "0000-0001-5703-2108" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard" }, "orcid": "0000-0001-7782-7071" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Keliser-I-K-W", "name": { "family": "Kleiser", "given": "Io K. W." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Matheson-T", "name": { "family": "Matheson", "given": "Thomas" }, "orcid": "0000-0001-6685-0479" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Pan-Yen-Chen", "name": { "family": "Pan", "given": "Yen-Chen" } }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "Assaf" } }, { "id": "Sullivan-M", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" } ] }, "title": "Spectra of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 September 13. Accepted 2018 January 25. Published 2018 February 27. \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 (NASA). The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank the following for assistance with some of the Lick and Keck observations and reductions: Kelsey Clubb, Ryan Foley, Christopher Griffith, Pat Kelly, Michael Kandrashoff, and Isaac Shivvers. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. Research at Lick Observatory is supported in part by a generous gift from Google. Support for HST programs GO-12223 and GO-12524 was provided by NASA through a grant from STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. \n\nM.S. acknowledges support from EU/FP7-ERC grant no [615929]. A.D.C. acknowledges support by the Weizmann Institute of Science Koshland Center for Basic Research. A.V.F.'s supernova research group at U.C. Berkeley is grateful for generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant AST-1211916, and the Miller Institute for Basic Research in Science (U.C. Berkeley). M.M.K. acknowledges support by the GROWTH project funded by NSF grant AST-1545949. J.C. acknowledges support from the Australian Research Council Future Fellowship, grant FT130101219. A.G.-Y. 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. We thank Melissa Graham for providing spectra of PTF12dam, PTF12gty, and PTF12hni.\n\nPublished - Quimby_2018_ApJ_855_2.pdf
", "abstract": "Most Type I superluminous supernovae (SLSNe-I) reported to date have been identified by their high peak luminosities and spectra lacking obvious signs of hydrogen. We demonstrate that these events can be distinguished from normal-luminosity SNe (including Type Ic events) solely from their spectra over a wide range of light-curve phases. We use this distinction to select 19 SLSNe-I and four possible SLSNe-I from the Palomar Transient Factory archive (including seven previously published objects). We present 127 new spectra of these objects and combine these with 39 previously published spectra, and we use these to discuss the average spectral properties of SLSNe-I at different spectral phases. We find that Mn ii most probably contributes to the ultraviolet spectral features after maximum light, and we give a detailed study of the O ii features that often characterize the early-time optical spectra of SLSNe-I. We discuss the velocity distribution of O ii, finding that for some SLSNe-I this can be confined to a narrow range compared to relatively large systematic velocity shifts. Mg ii and Fe ii favor higher velocities than O ii and C ii, and we briefly discuss how this may constrain power-source models. We tentatively group objects by how well they match either SN 2011ke or PTF12dam and discuss the possibility that physically distinct events may have been previously grouped together under the SLSN-I label.", "date": "2018-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "855", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 2", "id_number": "CaltechAUTHORS:20180227-110439240", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180227-110439240", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Google" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Weizmann Institute of Science" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Miller Institute for Basic Research in Science" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Australian Research Council", "grant_number": "FT130101219" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/aaac2f", "primary_object": { "basename": "Quimby_2018_ApJ_855_2.pdf", "url": "https://authors.library.caltech.edu/records/ytfx3-acn65/files/Quimby_2018_ApJ_855_2.pdf" }, "pub_year": "2018", "author_list": "Quimby, Robert M.; De Cia, Annalisa; et el." }, { "id": "https://authors.library.caltech.edu/records/f75cs-3r893", "eprint_id": 84762, "eprint_status": "archive", "datestamp": "2023-08-21 22:46:15", "lastmod": "2023-10-18 16:40:32", "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Zhao-Weijie", "name": { "family": "Zhao", "given": "Weijie" } }, { "id": "Rusu-F", "name": { "family": "Rusu", "given": "Florin" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Ravi-Vikram", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "Scott M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Brady-P-R", "name": { "family": "Brady", "given": "Patrick R." }, "orcid": "0000-0002-4611-9387" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Kann-D-A", "name": { "family": "Kann", "given": "David Alexander" }, "orcid": "0000-0003-2902-3583" }, { "id": "Kaplan-D", "name": { "family": "Kaplan", "given": "David" }, "orcid": "0000-0001-6295-2881" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "id": "Urban-A-L", "name": { "family": "Urban", "given": "Alex" } } ] }, "title": "iPTF Archival Search for Fast Optical Transients", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; gamma-ray burst: general; stars: activity; stars: flare; stars: jets; surveys", "note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 December 5. Accepted 2018 January 24.\nPublished 2018 February 9. \n\nIt is a pleasure to thank Yi Cao, Jim Davenport, Adam Miller, Yuguang Chen, Harish Vendantham, Lynne Hillenbrand, and Trevor David for helpful discussions and assistance. We are grateful to the anonymous referee for constructive feedback that improved the quality of the paper. A.Y.Q.H. was supported by a National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. D.A.K. acknowledges support from from the Spanish research project AYA 2014-58381-P and the Juan de la Cierva Incorporac\u00edon fellowship IJCI-2015-261. This work was supported by the GROWTH project funded by the National Science Foundation under PIRE grant No. 1545949. The Intermediate Palomar Transient Factory project is 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. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013).\n\nPublished - Ho_2018_ApJL_854_L13.pdf
Submitted - 1712.00949.pdf
", "abstract": "There has been speculation about a class of relativistic explosions with an initial Lorentz factor \u0393_(init) smaller than that of classical gamma-ray bursts (GRBs). These \"dirty fireballs\" would lack prompt GRB emission but could be pursued via their optical afterglow, appearing as transients that fade overnight. Here we report a search for such transients (that fade by 5-\u03c3 in magnitude overnight) in four years of archival photometric data from the intermediate Palomar Transient Factory (iPTF). Our search criteria yielded 50 candidates. Of these, two were afterglows to GRBs that had been found in dedicated follow-up observations to triggers from the Fermi GRB Monitor. Another (iPTF14yb) was a GRB afterglow discovered serendipitously. Eight were spurious artifacts of reference image subtraction, and one was an asteroid. The remaining 38 candidates have red stellar counterparts in external catalogs. The photometric and spectroscopic properties of the counterparts identify these transients as strong flares from M dwarfs of spectral type M3\u2013M7 at distances of d \u2248 0.15\u20132.1 kpc; three counterparts were already spectroscopically classified as late-type M stars. With iPTF14yb as the only confirmed relativistic outflow discovered independently of a high-energy trigger, we constrain the all-sky rate of transients that peak at m = 18 and fade by \u0394m = 2 mag in \u0394t = 3 hr to be 680 yr^(-1), with a 68% confidence interval of 119-2236, yr^(-1). This implies that the rate of visible dirty fireballs is at most comparable to that of the known population of long-duration GRBs.", "date": "2018-02-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "854", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L13", "id_number": "CaltechAUTHORS:20180209-095826158", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180209-095826158", "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": "Ministerio de Educaci\u00f3n y Ciencia (MEC)", "grant_number": "AYA 2014-58381-P" }, { "agency": "Juan de la Cierva Incorporac\u00edon", "grant_number": "IJCI-2015-261" }, { "agency": "NSF", "grant_number": "AST-1545949" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/2041-8213/aaaa62", "primary_object": { "basename": "1712.00949.pdf", "url": "https://authors.library.caltech.edu/records/f75cs-3r893/files/1712.00949.pdf" }, "related_objects": [ { "basename": "Ho_2018_ApJL_854_L13.pdf", "url": "https://authors.library.caltech.edu/records/f75cs-3r893/files/Ho_2018_ApJL_854_L13.pdf" } ], "pub_year": "2018", "author_list": "Ho, Anna Y. Q.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/1qdz3-mxf03", "eprint_id": 84653, "eprint_status": "archive", "datestamp": "2023-08-19 07:41:20", "lastmod": "2023-10-18 16:31:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "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": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T." } }, { "id": "Cook-D-O", "name": { "family": "Cook", "given": "D. O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Ho-Anna-Y-Q", "name": { "family": "Ho", "given": "A. Y. Q." }, "orcid": "0000-0002-9017-3567" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" } ] }, "title": "iPTF Survey for Cool Transients", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general supernovae: individual (SN 2017lf, AT 2017bkj, AT 2017be) surveys", "note": "\u00a9 2018 Astronomical Society of the Pacific. \n\nReceived 2017 July 18. Accepted 2017 December 20. Published 2018 February 1. \n\nWe thank Mislav Balokovic, Kevin Burdge, Kishalay De, George Djorgovski, Andrew Drake, Marianne Heida, Nikita Kamraj, and Harish Vedantham for taking observations used in this paper. We thank the anonymous referee and Chris Kochanek for helpful comments. \n\nA.A.M. is supported by a grant from the Large Synoptic Survey Telescope Corporation, which funds the Data Science Fellowship Program. J.S and F.T. gratefully acknowledge the support from the Knut and Alice Wallenberg Foundation. R.A., M.B., A.G., and R.F. acknowledge support from the Swedish Research Council and the Swedish Space Board. \n\nThe Intermediate Palomar Transient Factory project is 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. 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. 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. These results made use of the Discovery Channel Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale. This 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. This work is partly based on observations made with DOLoRes@TNG.\n\nPublished - Adams_2018_PASP_130_034202.pdf
Submitted - 1711.10501.pdf
", "abstract": "We performed a wide-area (2000 deg^2) g and I band experiment as part of a two month extension to the Intermediate Palomar Transient Factory. We discovered 36 extragalactic transients including iPTF17lf, a highly reddened local SN Ia, iPTF17bkj, a new member of the rare class of transitional Ibn/IIn supernovae, and iPTF17be, a candidate luminous blue variable outburst. We do not detect any luminous red novae and place an upper limit on their rate. We show that adding a slow-cadence I band component to upcoming surveys such as the Zwicky Transient Facility will improve the photometric selection of cool and dusty transients.", "date": "2018-02-01", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "130", "number": "985", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 034202", "id_number": "CaltechAUTHORS:20180202-104540651", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180202-104540651", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" }, { "agency": "John and Ginger Giovale" } ] }, "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/aaa356", "primary_object": { "basename": "1711.10501.pdf", "url": "https://authors.library.caltech.edu/records/1qdz3-mxf03/files/1711.10501.pdf" }, "related_objects": [ { "basename": "Adams_2018_PASP_130_034202.pdf", "url": "https://authors.library.caltech.edu/records/1qdz3-mxf03/files/Adams_2018_PASP_130_034202.pdf" } ], "pub_year": "2018", "author_list": "Adams, S. M.; Blagorodnova, N.; et el." }, { "id": "https://authors.library.caltech.edu/records/3m5d3-ses78", "eprint_id": 84604, "eprint_status": "archive", "datestamp": "2023-08-21 22:40:42", "lastmod": "2023-10-18 16:23:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "Po-Chieh" }, "orcid": "0000-0001-8894-0854" }, { "id": "Yu-Chang-Hsien", "name": { "family": "Yu", "given": "Chang-Hsien" } }, { "id": "Lee-Chien-De", "name": { "family": "Lee", "given": "Chien-De" }, "orcid": "0000-0002-3142-7299" }, { "id": "Lin-Chie-Cheng", "name": { "family": "Lin", "given": "Chien-Cheng" } }, { "id": "Hsia-Chih-Hao", "name": { "family": "Hsia", "given": "Chih-Hao" } }, { "id": "Chang-Chang-Kao", "name": { "family": "Chang", "given": "Chang-Kao" } }, { "id": "Chen-I-Chenn", "name": { "family": "Chen", "given": "I-Chenn" }, "orcid": "0000-0002-1497-9884" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Chen-Wen-Ping", "name": { "family": "Chen", "given": "Wen-Ping" }, "orcid": "0000-0003-0262-272X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Searching for Be Stars in the Open Clusters with PTF/iPTF. I. Cluster Sample and Be Star Candidates", "ispublished": "pub", "full_text_status": "public", "keywords": "open clusters and associations: general; stars: emission-line, Be; stars: general; surveys", "note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 June 6. Accepted 2017 December 26. Published 2018 January 29. \n\nThis work is supported in part by the Ministry of Science and Technology of Taiwan under grants MOST 105-2119-M-008-003 (W.-H.I.), MOST 103-2112-M-008-024-MY3 (W.-P.C.), MOST 104-2112-M-008-012-MY3 (C.-C.N.), MOST 104-2112-M-008-014-MY3 (C.-K.C), and MOST 106-2917-I-564-042 (C.-C.L.). This work is also supported by the Science and Technology Development Fund of Macau (project codes: 039/2013/A2 and 017/2014/A1). 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 research has made use of the WEBDA database, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University.\n\nPublished - Yu_2018_AJ_155_91.pdf
", "abstract": "We conducted a search for Be star candidates in open clusters using H\u03b1 imaging photometry of the Palomar Transient Factory Survey to investigate some connections among Be star phenomena, cluster environments, and ages. Stellar members of clusters were identified by spatial distributions, near-infrared magnitudes and colors, and by proper motions. Among 104 open clusters, we identified 96 Be star candidates in 32 clusters; 11 of our candidates have been reported in previous studies. We found that the clusters with age 7.5 < log(t(year)) \u2a7d 8.5 tend to have more Be star candidates; there is about a 40% occurrence rate within this age bin. The clusters in this age bin also tend to have a higher Be fraction N(Be)/N(Be+B-type). These results suggest that the environments of young and intermediate clusters are favorable to the formation of Be phenomena. Spatial distribution of Be star candidates with different ages implies that they do not form preferentially in the central regions. Furthermore, we showed that the mid-infrared (MIR) colors of the Be star candidates are similar to known Be stars, which could be caused by free\u2013free emission or bound-free emission. Some Be star candidates might have no circumstellar dust according to their MIR colors. Finally, among 96 Be candidates, we discovered that one Be star candidate FSR 0904-1 exhibits long-term variability on the timescale of ~2000 days with an amplitude of 0.2\u20130.3 mag, indicating a long timescale of disk evolution.", "date": "2018-02", "date_type": "published", "publication": "Astronomical Journal", "volume": "155", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 91", "id_number": "CaltechAUTHORS:20180131-131424122", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180131-131424122", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST-105-2119-M-008-003" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 103-2112-M-008-024-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 104-2112-M-008-012-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 104-2112-M-008-014-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 106-2917-I-564-042" }, { "agency": "Macau Science and Technology Development Fund", "grant_number": "039/2013/A2" }, { "agency": "Macau Science and Technology Development Fund", "grant_number": "017/2014/A1" }, { "agency": "NSF" }, { "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": "10.3847/1538-3881/aaa45b", "primary_object": { "basename": "Yu_2018_AJ_155_91.pdf", "url": "https://authors.library.caltech.edu/records/3m5d3-ses78/files/Yu_2018_AJ_155_91.pdf" }, "pub_year": "2018", "author_list": "Yu, Po-Chieh; Yu, Chang-Hsien; et el." }, { "id": "https://authors.library.caltech.edu/records/s851c-yvq60", "eprint_id": 84356, "eprint_status": "archive", "datestamp": "2023-08-21 22:35:39", "lastmod": "2023-10-18 16:09:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Piro-A-L", "name": { "family": "Piro", "given": "A. L." }, "orcid": "0000-0001-6806-0673" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "B. D." }, "orcid": "0000-0002-7856-3570" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Dhawan-S", "name": { "family": "Dhawan", "given": "S." } }, { "id": "Ferretti-R", "name": { "family": "Ferretti", "given": "R." }, "orcid": "0000-0001-7814-5814" }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "O. D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "McCully-C", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Early Observations of the Type Ia Supernova iPTF 16abc: A Case of Interaction with Nearby, Unbound Material and/or Strong Ejecta Mixing", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: observational; supernovae: general; supernovae: individual (iPTF 16abc; SN 2011fe); surveys", "note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2017 August 23. Accepted 2017 December 5. Published 2018 January 11. \n\nThis study has benefited from the suggestions of an anonymous referee. We are deeply grateful to R. C. Thomas for indulging a slew of questions regarding C ii in SNe. Similarly, it is our pleasure to buy a beer for R. Amanullah and U. Feindt for discussions regarding SALT2. \n\nThis paper utilizes the LCO infrastructure for rapid and regular monitoring of SNe, and we thank S. Valenti and I. Arcavi for their development efforts. Figure 3 would not have been possible without S. Blondin generously sharing the data from Blondin et al. (2012). \n\nMuch of the analysis presented herein would not have been possible without the help of several observers. We thank M. West for taking the first spectrum of iPTF 16abc as a ToO on the DCT. We also thank P. GuhaThakurta, E. C. Cunningham, K. A. Plant, H. Jang, and J. Torres for executing a Keck ToO as part of the UC/Caltech partnership, and also the Gemini service observers for executing our ToO observations. Additionally, J. Cohen, N. Suzuki, V. Ravi, R. Walters, A. Ho, H. Vedanthamand, K. De, and L. Yan helped obtain data for this paper. \n\nA.A.M. is funded by the Large Synoptic Survey Telescope Corporation in support of the Data Science Fellowship Program. Y.C. acknowledges support from a postdoctoral fellowship at the eScience Institute, University of Washington. \n\nD.A.H., C.M., and G.H. are supported by NSF-1313484. \n\nThe Intermediate Palomar Transient Factory project is 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. This work was supported by the GROWTH project funded by the National Science Foundation under grant no. 1545949. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work makes use of observations from the LCO network. These results made use of the Discovery Channel Telescope at Lowell Observatory. Lowell is a private, nonprofit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The upgrade of the DeVeny optical spectrograph has been funded by a generous grant from John and Ginger Giovale. 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 Astrof\u00edsica de Canarias.\n\nFacilities: DCT - , Gemini:Gillett - , Hale - , Keck:I - , Keck:II - , LCOGT - , PO:1.2m - , PO:1.5m - , NOT - , VLT - , Swift - , OANSPM:HJT - .\n\nPublished - Miller_2018_ApJ_852_100.pdf
", "abstract": "Early observations of Type Ia supernovae (SNe Ia) provide a unique probe of their progenitor systems and explosion physics. Here we report the intermediate Palomar Transient Factory (iPTF) discovery of an extraordinarily young SN Ia, iPTF 16abc. By fitting a power law to our early light curve, we infer that first light for the SN, that is, when the SN could have first been detected by our survey, occurred only 0.15 \u00b1_(0.07)^(0.15) days before our first detection. In the ~24 hr after discovery, iPTF 16abc rose by ~2 mag, featuring a near-linear rise in flux for \u22733 days. Early spectra show strong C ii absorption, which disappears after ~7 days. Unlike the extensively observed Type Ia SN 2011fe, the (B-V)_0 colors of iPTF 16abc are blue and nearly constant in the days after explosion. We show that our early observations of iPTF 16abc cannot be explained by either SN shock breakout and the associated, subsequent cooling or the SN ejecta colliding with a stellar companion. Instead, we argue that the early characteristics of iPTF 16abc, including (i) the rapid, near-linear rise, (ii) the nonevolving blue colors, and (iii) the strong C ii absorption, are the result of either ejecta interaction with nearby, unbound material or vigorous mixing of radioactive ^(56)Ni in the SN ejecta, or a combination of the two. In the next few years, dozens of very young normal SNe Ia will be discovered, and observations similar to those presented here will constrain the white dwarf explosion mechanism.", "date": "2018-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "852", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 100", "id_number": "CaltechAUTHORS:20180117-090820881", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180117-090820881", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Data Science Fellowship Program" }, { "agency": "University of Washington" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "John and Ginger Giovale" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/aaa01f", "primary_object": { "basename": "Miller_2018_ApJ_852_100.pdf", "url": "https://authors.library.caltech.edu/records/s851c-yvq60/files/Miller_2018_ApJ_852_100.pdf" }, "pub_year": "2018", "author_list": "Miller, A. A.; Cao, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/n1ajr-fz780", "eprint_id": 84704, "eprint_status": "archive", "datestamp": "2023-08-19 07:10:41", "lastmod": "2023-10-18 16:37:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "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" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Smadja-G", "name": { "family": "Smadja", "given": "G." } }, { "id": "Tao-C", "name": { "family": "Tao", "given": "C." } } ] }, "title": "PTF11mnb: First analog of supernova 2005bf. Long-rising, double-peaked supernova Ic from a massive progenitor", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general / supernovae: individual: PTF11mnb, SN 2005bf, iPTF15dtg", "note": "\u00a9 2018 ESO. \n\nReceived 10 October 2016. Accepted 12 October 2017. \n\nWe gratefully acknowledge the support from the Knut and\nAlice Wallenberg Foundation. Based on observations obtained with the Samuel Oschin 48-inch Telescope and the 60-inch Telescope at the Palomar Observatory as part of the intermediate Palomar Transient Factory (iPTF) 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. The Oskar Klein Centre is funded by the Swedish Research Council. We thank I. Arcavi, A. Horesh, T. Kupfer, D. Levitan, T. Matheson, G. Smadja, S. Tendulkar, and D. Xu for their help with the spectral observations and their preliminary reductions. We thank Y. Cao, J. Surace, R. Laher, F. Masci, U. Rebbapragada, and P.W\u00f3zniak for their contribution to the iPTF project. This work is partly based on observations made with DOLoRes@TNG. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 725161, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva and ISF grants, WIS-UK \"making connections\", and Kimmel and YeS awards. G.S. acknowledges support from the Lyon Institute of Origins under grant ANR-10-LABX-66.\n\nPublished - aa29874-16.pdf
", "abstract": "Aims. We study PTF11mnb, a He-poor supernova (SN) whose light curves resemble those of SN 2005bf, a peculiar double-peaked stripped-envelope (SE) SN, until the declining phase after the main peak. We investigate the mechanism powering its light curve and the nature of its progenitor star.\n\nMethods. Optical photometry and spectroscopy of PTF11mnb are presented. We compared light curves, colors and spectral properties to those of SN 2005bf and normal SE SNe. We built a bolometric light curve and modeled this light curve with the SuperNova Explosion Code (SNEC) hydrodynamical code explosion of a MESA progenitor star and semi-analytic models.\n\nResults. The light curve of PTF11mnb turns out to be similar to that of SN 2005bf until ~50 d when the main (secondary) peaks occur at \u221218.5 mag. The early peak occurs at ~20 d and is about 1.0 mag fainter. After the main peak, the decline rate of PTF11mnb is remarkably slower than what was observed in SN 2005bf, and it traces well the ^(56)Co decay rate. The spectra of PTF11mnb reveal a SN Ic and have no traces of He unlike in the case of SN Ib 2005bf, although they have velocities comparable to those of SN 2005bf. The whole evolution of the bolometric light curve is well reproduced by the explosion of a massive (M_(ej) = 7.8 M_\u2299), He-poor star characterized by a double-peaked ^(56)Ni distribution, a total ^(56)Ni mass of 0.59 M_\u2299, and an explosion energy of 2.2 \u00d7 10^(51) erg. Alternatively, a normal SN Ib/c explosion (M(^(56)Ni)\u2009=\u20090.11 M_\u2299, EK = 0.2 \u00d7 10^(51) erg, M_(ej) = 1 M_\u2299) can power the first peak while a magnetar, with a magnetic field characterized by B = 5.0 \u00d7 10^(14) G, and a rotation period of P = 18.1 ms, provides energy for the main peak. The early g-band light curve can be fit with a shock-breakout cooling tail or an extended envelope model from which a radius of at least 30 R_\u2299 is obtained.\n\nConclusions. We presented a scenario where PTF11mnb was the explosion of a massive, He-poor star, characterized by a double-peaked ^(56)Ni distribution. In this case, the ejecta mass and the absence of He imply a large ZAMS mass (~85 M_\u2299) for the progenitor, which most likely was a Wolf-Rayet star, surrounded by an extended envelope formed either by a pre-SN eruption or due to a binary configuration. Alternatively, PTF11mnb could be powered by a SE SN with a less massive progenitor during the first peak and by a magnetar afterward.", "date": "2018-01", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "609", "publisher": "EDP Sciences", "pagerange": "Art. No. A106", "id_number": "CaltechAUTHORS:20180207-082158154", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-082158154", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "European Research Council (ERC)", "grant_number": "725161" }, { "agency": "Israeli Committee for Planning and Funding" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Lyon Institute of Origins", "grant_number": "ANR-10-LABX-66" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1051/0004-6361/201629874", "primary_object": { "basename": "aa29874-16.pdf", "url": "https://authors.library.caltech.edu/records/n1ajr-fz780/files/aa29874-16.pdf" }, "pub_year": "2018", "author_list": "Taddia, F.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/fhpdv-abe70", "eprint_id": 83956, "eprint_status": "archive", "datestamp": "2023-08-19 06:56:08", "lastmod": "2023-10-18 14:33:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Whitesides-L", "name": { "family": "Whitesides", "given": "L." } }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Cook-D-O", "name": { "family": "Cook", "given": "D. O." }, "orcid": "0000-0002-6877-7655" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" } ] }, "title": "iPTF 16asu: A Luminous, Rapidly Evolving, and High-velocity Supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: general \u2013 shock waves \u2013 stars: magnetars \u2013 supernovae: general \u2013 supernovae: individual (iPTF 16asu)", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 June 14; revised 2017 October 10; accepted 2017 November 6; published 2017 December 18. \n\nWe thank the anonymous referee for constructive comments that improved the manuscript. We thank Iair Arcavi, Maria Drout, Avishay Gal-Yam, Raffaella Margutti, and Maryam Modjaz for helpful discussions and comments. R. L. acknowledges helpful discussions at the Munich Institute for Astro- and Particle Physics (MIAPP) workshop \"Superluminous Supernovae in the Next Decade,\" supported by the MIAPP, of the DFG cluster of excellence \"Origin and Structure of the Universe.\" We thank Harish Vedantham, Vikram Ravi, and Anna Ho for assisting with the observations presented in this paper. The Intermediate Palomar Transient Factory project is 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. This work was supported by the GROWTH project, funded by the National Science Foundation under Grant No. 1545949. This work is partially based on data acquired with the Swift GO program 1215281 (Grant No. NNX16AN84G, PI: R. Lunnan). Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. A. C. acknowledges support from the National Science Foundation CAREER Award No. 1455090. D. S. and D. F. gratefully acknowledge support from RSF Grant No. 17-12-01378. This work made use of the data products generated by the New York University SN group and released under DOI:10.5281/zenodo.58767, available at https://github.com/nyusngroup/SESNspectraLib 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 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. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacilities: PO: 1.2 m - , PO: 1.5 m - , PO: Hale - , Keck: I - KECK I Telescope, Keck: II - KECK II Telescope, NOT - Nordic Optical Telescope, TNG - Telescopio Nazionale Galileo, Swift - Swift Gamma-Ray Burst Mission, VLA.\n\nPublished - Whitesides_2017_ApJ_851_107.pdf
Submitted - 1706.05018.pdf
", "abstract": "Wide-field surveys are discovering a growing number of rare transients whose physical origin is not yet well understood. Here we present optical and UV data and analysis of intermediate Palomar Transient Factory (iPTF) 16asu, a luminous, rapidly evolving, high-velocity, stripped-envelope supernova (SN). With a rest-frame rise time of just four days and a peak absolute magnitude of M_g = -20.4 mag, the light curve of iPTF 16asu is faster and more luminous than that of previous rapid transients. The spectra of iPTF 16asu show a featureless blue continuum near peak that develops into an SN Ic-BL spectrum on the decline. We show that while the late-time light curve could plausibly be powered by ^(56)Ni decay, the early emission requires a different energy source. Nondetections in the X-ray and radio strongly constrain the energy coupled to relativistic ejecta to be at most comparable to the class of low-luminosity gamma-ray bursts (GRBs). We suggest that the early emission may have been powered by either a rapidly spinning-down magnetar or by shock breakout in an extended envelope of a very energetic explosion. In either scenario a central engine is required, making iPTF 16asu an intriguing transition object between superluminous SNe, SNe Ic-BL, and low-luminosity GRBs.", "date": "2017-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "851", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20171219-083803156", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171219-083803156", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Munich Institute for Astro- and Particle Physics (MIAPP)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NASA", "grant_number": "NNX16AN84G" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1455090" }, { "agency": "Russian Science Foundation", "grant_number": "17-12-01378" }, { "agency": "W. M. Keck Foundation" } ] }, "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": "10.3847/1538-4357/aa99de", "primary_object": { "basename": "1706.05018.pdf", "url": "https://authors.library.caltech.edu/records/fhpdv-abe70/files/1706.05018.pdf" }, "related_objects": [ { "basename": "Whitesides_2017_ApJ_851_107.pdf", "url": "https://authors.library.caltech.edu/records/fhpdv-abe70/files/Whitesides_2017_ApJ_851_107.pdf" } ], "pub_year": "2017", "author_list": "Whitesides, L.; Lunnan, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/5xawz-13597", "eprint_id": 83942, "eprint_status": "archive", "datestamp": "2023-08-21 22:14:56", "lastmod": "2023-10-18 14:32:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aartsen-M-G", "name": { "family": "Aartsen", "given": "M. G." } }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E." }, "orcid": "0000-0001-8018-5348" } ] }, "title": "Multiwavelength follow-up of a rare IceCube neutrino multiplet", "ispublished": "pub", "full_text_status": "public", "keywords": "Astroparticle physics; Neutrinos; Gamma-ray burst; Supernovae; Galaxies: active; X-rays: bursts", "note": "\u00a9 ESO 2017. \n\nReceived 14 February 2017; accepted 30 July 2017. \n\nNeil Gehrels sadly died during the late stage of the production of this paper. As Swift PI he was an enthusiastic supporter of multi-messenger observations; he will be sorely missed. The IceCube Collaboration acknowledges the support from the following agencies: US National Science Foundation - Office of Polar Programs, US National Science Foundation - Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin - Madison, the Open Science Grid (OSG) grid infrastructure; US Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada,WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRSFWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Villum Fonden, Danish National Research Foundation (DNRF), Denmark This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. Funding for the Swift project in the UK is provided by the UK Space Agency. Part of this work was facilitated by the GROWTH project, a partnership in international research and education, NSF PIRE Grant No. 1545949. ASAS-SN is supported by NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Mt. Cuba Astronomical Foundation, and by George Skestos. 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. The HAWC Collaboration acknowledges the support from: the US National Science Foundation (NSF); the US Department of Energy Office of High- Energy Physics; the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT), M\u00e9xico (grants 271051, 232656, 260378, 179588, 239762, 254964, 271737, 258865, 243290, 132197), Laboratorio Nacional HAWC de rayos gamma; L'OREAL Fellowship for Women in Science 2014; Red HAWC, M\u00e9xico; DGAPA-UNAM (grants IG100317, IN111315, IN111716-3, IA102715, 109916, IA102917); VIEP-BUAP; PIFI 2012, 2013, PROFOCIE 2014, 2015;the University of Wisconsin Alumni Research Foundation; the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory; Polish Science Centre grant DEC-2014/13/B/ST9/945; Coordinaci\u00f3n de la Investigaci\u00f3n Cient\u00edfica de la Universidad Michoacana. We thank Luciano D\u00edaz and Eduardo Murrieta for technical support of the HAWC detector. Support for I. Arcavi was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. D. A. Howell, C. McCully, and G. Hosseinzadeh are supported by NSF-1313484. This work makes use of observations from the LCO network. VERITAS research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, and by NSERC in Canada. VERITAS acknowledges the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. E. O. Ofek and A. Gal-Yam acknowledge a Minerva grant.\n\nPublished - aa30620-17.pdf
Submitted - 1702.06131.pdf
", "abstract": "On February 17, 2016, the IceCube real-time neutrino search identified, for the first time, three muon neutrino candidates arriving within 100\u2009s of one another, consistent with coming from the same point in the sky. Such a triplet is expected once every 13.7\u2009years as a random coincidence of background events. However, considering the lifetime of the follow-up program the probability of detecting at least one triplet from atmospheric background is 32%. Follow-up observatories were notified in order to search for an electromagnetic counterpart. Observations were obtained by Swift's X-ray telescope, by ASAS-SN, LCO and MASTER at optical wavelengths, and by VERITAS in the very-high-energy gamma-ray regime. Moreover, the Swift BAT serendipitously observed the location 100\u2009s after the first neutrino was detected, and data from the Fermi LAT and HAWC observatory were analyzed. We present details of the neutrino triplet and the follow-up observations. No likely electromagnetic counterpart was detected, and we discuss the implications of these constraints on candidate neutrino sources such as gamma-ray bursts, core-collapse supernovae and active galactic nucleus flares. This study illustrates the potential of and challenges for future follow-up campaigns.", "date": "2017-11-24", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "607", "publisher": "EDP Sciences", "pagerange": "Art. No. A115", "id_number": "CaltechAUTHORS:20171215-110713919", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171215-110713919", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Wisconsin Alumni Research Foundation" }, { "agency": "Grid Laboratory of Wisconsin (GLOW)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "National Energy Research Scientific Computing Center (NERSC)" }, { "agency": "Louisiana Optical Network Initiative (LONI)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "WestGrid" }, { "agency": "Compute/Calcul Canada" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish Polar Research Secretariat" }, { "agency": "Swedish National Infrastructure for Computing (SNIC)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Helmholtz-Allianz f\u00fcr Astroteilchenphysik" }, { "agency": "Research Department of Plasmas with Complex Interactions" }, { "agency": "Fonds de la Recherche Scientifique (FNRS)" }, { "agency": "Fonds Wetenschappelijk Onderzoek (FWO)" }, { "agency": "Agentschap voor Innovatie door Wetenschap en Technologie (IWT-Belgium)" }, { "agency": "Belgian Federal Science Policy Office (BELSPO)" }, { "agency": "University of Oxford" }, { "agency": "Marsden Fund of the Royal Society of New Zealand" }, { "agency": "Australian Research Council" }, { "agency": "Japan Society for Promotion of Science (JSPS)" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Villum Fonden" }, { "agency": "Danish National Research Foundation" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NSF", "grant_number": "AST-1515927" }, { "agency": "NSF", "grant_number": "AST-0908816" }, { "agency": "Center for Cosmology and AstroParticle Physics (CCAPP)" }, { "agency": "Mt. Cuba Astronomical Foundation" }, { "agency": "George Skestos" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "K\u014d Enerug\u012b Kasokuki Kenky\u016b Kik\u014d (KEK)" }, { "agency": "Japan Aerospace Exploration Agency (JAXA)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "271051" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "232656" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "260378" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "179588" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "239762" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "254964" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "271737" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "258865" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "243290" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "132197" }, { "agency": "Laboratorio Nacional HAWC de Rayos Gamma" }, { "agency": "L'OREAL Fellowship for Women in Science" }, { "agency": "Direcci\u00f3n General Asuntos del Personal Acad\u00e9mico, Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)", "grant_number": "IG100317" }, { "agency": "Direcci\u00f3n General Asuntos del Personal Acad\u00e9mico, Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)", "grant_number": "IN111315" }, { "agency": "Direcci\u00f3n General Asuntos del Personal Acad\u00e9mico, Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)", "grant_number": "IN111716-3" }, { "agency": "Direcci\u00f3n General Asuntos del Personal Acad\u00e9mico, Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)", "grant_number": "IA102715" }, { "agency": "Direcci\u00f3n General Asuntos del Personal Acad\u00e9mico, Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)", "grant_number": "109916" }, { "agency": "Direcci\u00f3n General Asuntos del Personal Acad\u00e9mico, Universidad Nacional Aut\u00f3noma de M\u00e9xico (DGAPA-UNAM)", "grant_number": "IA102917" }, { "agency": "Vicerrector\u00eda de Investigaci\u00f3n y Estudios de Posgrado, Benem\u00e9rita Universidad Aut\u00f3noma de Puebla (VIEP-BUAP)" }, { "agency": "Programa Integral de Fortalecimiento Institucional (PIFI)" }, { "agency": "Programa de Fortalecimiento de la Calidad en Instituciones Educativas (PROFOCIE)" }, { "agency": "National Science Centre (Poland)", "grant_number": "DEC-2014/13/B/ST9/945" }, { "agency": "Coordinaci\u00f3n de la Investigaci\u00f3n Cient\u00edfica de la Universidad Michoacana" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "Smithsonian Institution" }, { "agency": "Minerva Grant" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "corp_creators": { "items": [ "IceCube Collaboration", "ASAS-SN Collaboration", "Astrophysical Multimessenger Observatory Network Collaboration", "Fermi LAT Collaboration", "HAWC Collaboration", "LCO Collaboration", "MASTER Collaboration", "Swift Collaboration", "VERITAS Collaboration" ] }, "doi": "10.1051/0004-6361/201730620", "primary_object": { "basename": "1702.06131.pdf", "url": "https://authors.library.caltech.edu/records/5xawz-13597/files/1702.06131.pdf" }, "related_objects": [ { "basename": "aa30620-17.pdf", "url": "https://authors.library.caltech.edu/records/5xawz-13597/files/aa30620-17.pdf" } ], "pub_year": "2017", "author_list": "Aartsen, M. G. and Bellm, E." }, { "id": "https://authors.library.caltech.edu/records/gzmfp-ffm97", "eprint_id": 95652, "eprint_status": "archive", "datestamp": "2023-08-19 06:06:56", "lastmod": "2023-10-20 20:25:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bar-I", "name": { "family": "Bar", "given": "Ira" } }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "Paul" }, "orcid": "0000-0002-7572-9088" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Nelemans-G", "name": { "family": "Nelemans", "given": "Gijs" } } ] }, "title": "A Spectroscopic Search for White Dwarf Companions to 101 Nearby M Dwarfs", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: general \u2013 stars: late-type \u2013 white dwarfs", "note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 March 21; revised 2017 October 1; accepted 2017 October 3; published 2017 November 14.\n\nWe would like to thank Barak Zackay for many insightful discussions. This work used the astronomy & astrophysics package for Matlab (Ofek 2014), the SIMBAD database, operated at CDS, Strasbourg, France, and used data obtained from the Weizmann interactive supernova data repository (http://wiserep.weizmann.ac.il). This work also made use of the data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. This work has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory, made use of the tables for evolutionary sequences of WD atmospheres of Holberg & Bergeron (2006), Kowalski & Saumon (2006), Tremblay et al. (2011), and Bergeron et al. (2011; http://www.astro.umontreal.ca/~bergeron/CoolingModels/), and made use of the observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. We acknowledge support from the Weizmann Institute, in particular the Kimmel Award.\n\nPublished - Bar_2017_ApJ_850_34.pdf
Submitted - 1703.07650.pdf
", "abstract": "Recent studies of the stellar population in the solar neighborhood (<20 pc) suggest that there are undetected white dwarfs (WDs) in multiple systems with main-sequence companions. Detecting these hidden stars and obtaining a more complete census of nearby WDs is important for our understanding of stellar and galactic evolution, as well as the study of explosive phenomena. In an attempt to uncover these hidden WDs, we present intermediate resolution spectroscopy over the wavelength range of 3000\u201325000 \u00c5 of 101 nearby M dwarfs (dMs), observed with the Very Large Telescope X-Shooter spectrograph. For each star we search for a hot component superimposed on the dM spectrum. X-Shooter has excellent blue sensitivity and thus can reveal a faint hot WD despite the brightness of its red companion. Visual examination shows no clear evidence of a WD in any of the spectra. We place upper limits on the effective temperatures of WDs that may still be hiding by fitting dM templates to the spectra and modeling the WD spectra. On average our survey is sensitive to WDs hotter than about 5300 K. This suggests that the frequency of WD companions of T_(eff) \u2273 5300 K with separation of the order of \u227e50 au among the local dM population is <3% at the 95% confidence level. The reduced spectra are made available via the WISeREP repository.", "date": "2017-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "850", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 34", "id_number": "CaltechAUTHORS:20190521-145846352", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190521-145846352", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-98034" }, { "agency": "NSF" }, { "agency": "Weizmann Institute" }, { "agency": "Kimmel Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/1538-4357/aa91d4", "primary_object": { "basename": "1703.07650.pdf", "url": "https://authors.library.caltech.edu/records/gzmfp-ffm97/files/1703.07650.pdf" }, "related_objects": [ { "basename": "Bar_2017_ApJ_850_34.pdf", "url": "https://authors.library.caltech.edu/records/gzmfp-ffm97/files/Bar_2017_ApJ_850_34.pdf" } ], "pub_year": "2017", "author_list": "Bar, Ira; Vreeswijk, Paul; et el." }, { "id": "https://authors.library.caltech.edu/records/wnmac-2bk34", "eprint_id": 83147, "eprint_status": "archive", "datestamp": "2023-08-19 06:00:51", "lastmod": "2023-10-17 22:56:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Bahnolzer-S", "name": { "family": "Bahnolzer", "given": "Sophianna" } }, { "id": "He-Kevin", "name": { "family": "He", "given": "Kevin" }, "orcid": "0000-0001-5806-0370" }, { "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" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "The Outer Halo of the Milky Way as Probed by RR Lyr Variables from the Palomar Transient Facility", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: halo \u2013 Galaxy: kinematics and dynamics \u2013 stars: variables: RR Lyrae", "note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 April 26; revised 2017 September 26; accepted 2017 September 28; published 2017 November 9.\n\nBased in part on observations obtained at the W. M. Keck Observatory, which is operated jointly by the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration.\n\nWe are grateful to the many people who have worked to make the Keck Telescope and its instruments a reality and to operate and maintain the Keck Observatory. The authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible.\n\nWe thank the referee for helpful detailed comments that improved this paper.\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 Intermediate Palomar Transient Factory project is 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 PTF database (DR3) is now publicly available at https://www.ptf.caltech.edu/news/DR3. It includes photometry through 2015 January 28.\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/.\n\nSDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.\n\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\nJ.G.C. and B.S. acknowledge NSF grant AST-0908139 to J.G.C. for partial support during the initial early stages of this project. S.R.B. and K.H. thank the Caltech Summer Undergraduate Research Fellowship (SURF) program for support.\n\nPublished - Cohen_2017_ApJ_849_150.pdf
Submitted - 1710.01276.pdf
", "abstract": "RR Lyrae stars are ideal massless tracers that can be used to study the total mass and dark matter content of the outer halo of the Milky Way (MW). This is because they are easy to find in the light-curve databases of large stellar surveys and their distances can be determined with only knowledge of the light curve. We present here a sample of 112 RR Lyr stars beyond 50 kpc in the outer halo of the MW, excluding the Sgr streams, for which we have obtained moderate-resolution spectra with Deimos on the Keck II Telescope. Four of these have distances exceeding 100 kpc. These were selected from a much larger set of 447 candidate RR Lyr stars that were data-mined using machine-learning techniques applied to the light curves of variable stars in the Palomar Transient Facility database. The observed radial velocities taken at the phase of the variable corresponding to the time of observation were converted to systemic radial velocities in the Galactic standard of rest. From our sample of 112 RR Lyr stars we determine the radial velocity dispersion in the outer halo of the MW to be ~90 km s^(\u22121) at 50 kpc, falling to about 65 km s^(\u22121) near 100 kpc once a small number of major outliers are removed. With reasonable estimates of the completeness of our sample of 447 candidates and assuming a spherical halo, we find that the stellar density in the outer halo declines as r^(-4).", "date": "2017-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "849", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 150", "id_number": "CaltechAUTHORS:20171113-103138961", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171113-103138961", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-0908139" }, { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" } ] }, "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": "10.3847/1538-4357/aa9120", "primary_object": { "basename": "1710.01276.pdf", "url": "https://authors.library.caltech.edu/records/wnmac-2bk34/files/1710.01276.pdf" }, "related_objects": [ { "basename": "Cohen_2017_ApJ_849_150.pdf", "url": "https://authors.library.caltech.edu/records/wnmac-2bk34/files/Cohen_2017_ApJ_849_150.pdf" } ], "pub_year": "2017", "author_list": "Cohen, Judith G.; Sesar, Branimir; et el." }, { "id": "https://authors.library.caltech.edu/records/7g49g-4m104", "eprint_id": 82089, "eprint_status": "archive", "datestamp": "2023-08-21 22:05:13", "lastmod": "2023-10-17 22:01:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dahm-S-E", "name": { "family": "Dahm", "given": "S. E." }, "orcid": "0000-0002-2968-2418" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "L. A." } } ] }, "title": "Interpretation of a Variable Reflection Nebula Associated with HBC 340 and HBC 341 in NGC 1333", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2017 June 9. Accepted 2017 August 26. Published 2017 October 5. \n\nWe have made use of the Digitized Sky Surveys, which were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166, the SIMBAD database operated at CDS, Strasbourg, France, and the 2MASS, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/California Institute of Technology, funded by NASA 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. 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 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, 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 Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. The authors gratefully acknowledge the efforts and dedication of the W. M. Keck Observatory staff and the NASA Infrared Telescope Facility staff for their support in making the observations presented herein. S.E.D. also wishes to thank Ethan Dahm for assisting with the HIRES observations made on 2015 October 30. Finally, the authors thank Bo Reipurth who served as the referee for this paper. His insightful comments and recommendations greatly improved the manuscript.\n\nPublished - Dahm_2017_AJ_154_177.pdf
Submitted - 1709.01503.pdf
", "abstract": "We present multi-epoch, R-band imaging obtained from the Palomar Transient Factory of a small, fan-shaped reflection nebula in NGC 1333 that experiences prominent brightness fluctuations. Photometry of HBC 340 (K7e) and HBC 341 (M5e), a visual pair of late-type, young stellar objects lying near the apex of the nebula, demonstrates that while both are variable, the former has brightened by more than two magnitudes following a deep local minimum in 2014 September. Keck high-dispersion (R ~ 45,000\u201366,000), optical spectroscopy of HBC 340 suggests that the protostar is a spectroscopic binary (HBC 340Aa + HBC 340Ab). Both HBC 340 and HBC 341 exhibit strong H\u03b1 and forbidden line emission, consistent with accretion and outflow. We conclude that the brightness fluctuations in the reflection nebula represent light echos produced by varying incident radiation emanating from HBC 340. The short-term variability observed in the protostar is attributed to irregular accretion activity, while correlated, dipping behavior on a several hundred day timescale may be due to eclipse-like events caused by orbiting circumstellar material. Archival Hubble Space Telescope imaging of the region reveals a second, faint (F814W ~ 20.3 mag) companion to HBC 340 that lies 1farcs02 (~235 au) east of the protostar. If associated, this probable substellar mass object (20\u201350 Jupiter masses), HBC 340B, is likely unrelated to the observed brightness variations. The sustained brightening of HBC 340 since late 2014 can be explained by an EXor-like outburst, the recovery from a long duration eclipse event caused by obscuring circumstellar dust, or by the gradual removal of extincting material from along the line of sight. Our analysis here favors one of the extinction scenarios.", "date": "2017-11", "date_type": "published", "publication": "Astronomical Journal", "volume": "154", "number": "5", "publisher": "American Astronomical Society", "pagerange": "Art. No. 177", "id_number": "CaltechAUTHORS:20171004-152440377", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171004-152440377", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG W-2166" }, { "agency": "NSF" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" }, { "agency": "Eotvos Lorand University (ELTE)" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Gordon and Betty Moore Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-3881/aa89eb", "primary_object": { "basename": "1709.01503.pdf", "url": "https://authors.library.caltech.edu/records/7g49g-4m104/files/1709.01503.pdf" }, "related_objects": [ { "basename": "Dahm_2017_AJ_154_177.pdf", "url": "https://authors.library.caltech.edu/records/7g49g-4m104/files/Dahm_2017_AJ_154_177.pdf" } ], "pub_year": "2017", "author_list": "Dahm, S. E. and Hillenbrand, L. A." }, { "id": "https://authors.library.caltech.edu/records/eq252-zc190", "eprint_id": 77109, "eprint_status": "archive", "datestamp": "2023-08-19 05:34:39", "lastmod": "2023-10-25 21:53:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Adams-Scott-M", "name": { "family": "Adams", "given": "S. M." }, "orcid": "0000-0001-5855-5939" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Kne\u017eevi\u0107-S", "name": { "family": "Kne\u017eevi\u0107", "given": "S." }, "orcid": "0000-0003-1416-8069" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Petrushevska-T", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "U. D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Color Me Intrigued: the Discovery of iPTF 16fnm, a Supernova 2002cx-like Object", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: observational \u2013 surveys \u2013 supernovae: general \u2013 supernovae: individual (SN 2002cx, SN 2005hk, iPTF 16fnm)", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 March 27; revised 2017 September 11; accepted 2017 September 11; published 2017 October 12. \n\nThis study has benefited from the suggestions of an anonymous referee. We thank K. Shen for a useful discussion on the color evolution of SNe Ia. R. Amanullah pointed us to several useful papers on the color evolution of SNe Ia, for which we are grateful. We wish to recognize J. Nordin, who helped us examine SEDm spectra. Finally, we thank J. D. Neill and A. Y. Q. Ho for providing detailed notes on the manuscript prior to submission. \n\nA.A.M. is funded by the Large Synoptic Survey Telescope Corporation in support of the Data Science Fellowship Program. \n\nThe Intermediate Palomar Transient Factory project is 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. This work was supported by the GROWTH project funded by the National Science Foundation under grant No. 1545949. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. \n\nSome of 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. \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\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 research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. \n\nFacilities: PO:1.2m - Palomar Observatory's 1.2 meter Samuel Oschin Telescope, PO:1.5 m (SEDm) - , Hale (DBSP) - , NOT (ALFOSC) - , Keck:I (LRIS) - .\n\nPublished - Miller_2017_ApJ_848_59.pdf
Submitted - 1703.07449.pdf
", "abstract": "Modern wide-field, optical time-domain surveys must solve a basic optimization problem: maximize the number of transient discoveries or minimize the follow-up needed for the new discoveries. Here, we describe the Color Me Intrigued experiment, the first from the intermediate Palomar Transient Factory (iPTF) to search for transients simultaneously in the g_(PTF) and R_(PTF) bands. During the course of this experiment, we discovered iPTF 16fnm, a new member of the 02cx-like subclass of Type Ia supernovae (SNe). iPTF 16fnm peaked at M_(gPTF) = -15.09 \u00b1 0.17 mag, making it the second-least-luminous known SN Ia. iPTF 16fnm exhibits all the hallmarks of the 02cx-like class: (i) low luminosity at peak, (ii) low ejecta velocities, and (iii) a non-nebular spectrum several months after peak. Spectroscopically, iPTF 16fnm exhibits a striking resemblance to two other low-luminosity 02cx-like SNe: SN 2007qd and SN 2010ae. iPTF 16fnm and SN 2005hk decline at nearly the same rate, despite a 3 mag difference in brightness at peak. When considering the full subclass of 02cx-like SNe, we do not find evidence for a tight correlation between peak luminosity and decline rate in either the g' or r' band. We measure the relative rate of 02cx-like SNe to normal SNe Ia and find r_(N02cx)/N_(Ia) = 33^(+158)_(-25)%. We further examine the g' \u2212 r' evolution of 02cx-like SNe and find that their unique color evolution can be used to separate them from 91bg-like and normal SNe Ia. This selection function will be especially important in the spectroscopically incomplete Zwicky Transient Facility/Large Synoptic Survey Telescope (LSST) era. Finally, we close by recommending that LSST periodically evaluate, and possibly update, its observing cadence to maximize transient science.", "date": "2017-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "848", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 59", "id_number": "CaltechAUTHORS:20170501-143925844", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170501-143925844", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Large Synoptic Survey Telescope Corporation" }, { "agency": "Data Science Fellowship Program" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/aa8c7e", "primary_object": { "basename": "1703.07449.pdf", "url": "https://authors.library.caltech.edu/records/eq252-zc190/files/1703.07449.pdf" }, "related_objects": [ { "basename": "Miller_2017_ApJ_848_59.pdf", "url": "https://authors.library.caltech.edu/records/eq252-zc190/files/Miller_2017_ApJ_848_59.pdf" } ], "pub_year": "2017", "author_list": "Miller, A. A.; Kasliwal, M. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/vjrpm-bkc79", "eprint_id": 82706, "eprint_status": "archive", "datestamp": "2023-08-19 04:55:49", "lastmod": "2023-10-17 22:37:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "A." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Moriya-T-J", "name": { "family": "Moriya", "given": "T. J." }, "orcid": "0000-0003-1169-1954" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "A." }, "orcid": "0000-0003-2082-1626" }, { "id": "Roy-R", "name": { "family": "Roy", "given": "R." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" } ] }, "title": "The bumpy light curve of Type IIn supernova iPTF13z over 3 years", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual: iPTF13z \u2013 galaxies: individual: SDSS J160200.05+211442.3", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 14 October 2017; Accepted 24 March 2017; Published online 29 August 2017. \n\nThanks to John Telting, Auni Somero, Paul Vreeswijk, Ofer Yaron, Kunal Mooley, Ragnhild Lunnan, Danny Khazov, and Gina Duggan for making observations of iPTF13z. Thanks to Peter Lundqvist and Mattias Ergon for discussions. Thanks to Andrew Drake and Ashish Mahabal for assisting with access to the Catalina Real-time Transient Survey images. We gratefully acknowledge the support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. This research used a computer bought with a grant from the Alva and Lennart Dahlmark Foundation. T.J.M. is supported by the Grant-in-Aid for Research Activity Start-up of the Japan Society for the Promotion of Science (16H07413). EOO is the incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva and ISF grants, WIS-UK \"making connections\", and Kimmel and YeS awards. The intermediate Palomar Transient Factory (iPTF) project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Centre, 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. 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. This work was supported by the GROWTH project funded by the National Science Foundation under Grant No. 1545949. This research used 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. This research used observations obtained with the Apache Point Observatory 3.5-m telescope, which is owned and operated by the Astrophysical Research Consortium. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research used the SIMBAD and VizieR databases operated at CDS, Strasbourg, France. This research used the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research used NASA's Astrophysics Data System.\n\nPublished - aa29906-16.pdf
Submitted - 1703.09679.pdf
", "abstract": "A core-collapse (CC) supernova (SN) of Type IIn is dominated by the interaction of SN ejecta with the circumstellar medium (CSM). Some SNe IIn (e.g. SN 2006jd) have episodes of re-brightening (\"bumps\") in their light curves. We present iPTF13z, a Type IIn SN discovered on 2013 February 1 by the intermediate Palomar Transient Factory (iPTF). This SN showed at least five bumps in its declining light curve between 130 and 750 days after discovery. We analyse this peculiar behaviour and try to infer the properties of the CSM, of the SN explosion, and the nature of the progenitor star. We obtained multi-band optical photometry for over 1000 days after discovery with the P48 and P60 telescopes at Palomar Observatory. We obtained low-resolution optical spectra during the same period. We did an archival search for progenitor outbursts. We analyse the photometry and the spectra, and compare iPTF13z to other SNe IIn. In particular we derive absolute magnitudes, colours, a pseudo-bolometric light curve, and the velocities of the different components of the spectral lines. A simple analytical model is used to estimate the properties of the CSM. iPTF13z had a light curve peaking at Mr \u2272 \u2212 18.3 mag. The five bumps during its decline phase had amplitudes ranging from 0.4 to 0.9 mag and durations between 20 and 120 days. The most prominent bumps appeared in all the different optical bands, when covered. The spectra of this SN showed typical SN IIn characteristics, with emission lines of H\u03b1 (with broad component FWHM ~ 10^3 \u2013 10^4 km s^(-1) and narrow component FWHM ~ 10^2 km s^(-1)) and He\u2009I, but also with Fe\u2009II, Ca\u2009II, Na\u2009I D and H\u03b2 P Cygni profiles (with velocities of ~ 10^3km s^(-1)). A pre-explosion outburst was identified lasting \u2273 50 days, with M_r \u2248 \u2212 15 mag around 210 days before discovery. Large, variable progenitor mass-loss rates (\u22730.01M\u2299 yr^(-1)) and CSM densities (\u227310^(-16) g cm^(-3)) are derived. The SN was hosted by a metal-poor dwarf galaxy at redshift z = 0.0328. We suggest that the light curve bumps of iPTF13z arose from SN ejecta interacting with denser regions in the CSM, possibly produced by the eruptions of a luminous blue variable progenitor star.", "date": "2017-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "605", "publisher": "EDP Sciences", "pagerange": "Art. No. A6", "id_number": "CaltechAUTHORS:20171026-142545167", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171026-142545167", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "Alva and Lennart Dahlmark Foundation" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "16H07413" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Quantum Universe I-Core Program" }, { "agency": "Israeli Committee for Planning and Funding" }, { "agency": "Kimmel Award" }, { "agency": "YeS Award" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201629906", "primary_object": { "basename": "1703.09679.pdf", "url": "https://authors.library.caltech.edu/records/vjrpm-bkc79/files/1703.09679.pdf" }, "related_objects": [ { "basename": "aa29906-16.pdf", "url": "https://authors.library.caltech.edu/records/vjrpm-bkc79/files/aa29906-16.pdf" } ], "pub_year": "2017", "author_list": "Nyholm, A.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/w7829-tba88", "eprint_id": 79532, "eprint_status": "archive", "datestamp": "2023-08-19 04:52:04", "lastmod": "2023-10-26 16:16:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yang-Michael-Ting-Chang", "name": { "family": "Yang", "given": "Michael Ting-Chang" } }, { "id": "Chou-Yi", "name": { "family": "Chou", "given": "Yi" } }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Hu-Chin-Ping", "name": { "family": "Hu", "given": "Chin-Ping" } }, { "id": "Su-Yi-Hao", "name": { "family": "Su", "given": "Yi-Hao" } }, { "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": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "Andrew J." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "Stanislav G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "Matthew J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Donalek-C", "name": { "family": "Donalek", "given": "Ciro" } } ] }, "title": "Long-term Periodicities of Cataclysmic Variables with Synoptic Surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "(stars:) novae \u2013 cataclysmic variables \u2013 (stars:) binaries (including multiple): close \u2013 surveys \u2013 catalogs \u2013 methods: data analysis \u2013 methods: observational", "note": "\u00a9 2017 The Astronomical Society of the Pacific. \n\nReceived 2017 May 21; accepted 2017 June 20; published 2017 July 20. \n\nM.T.-C.Y. is grateful to have the anonymous referee for the precious comments and suggestions. M.T.-C.Y. thanks the Ministry of Science and Technology (MOST) of Taiwan for support through the grant MOST 104-2119-M-008-024 (TANGO Project, as the courtesy of W.H.Ip.), NSC 102-2112-M-008-020-MY3, and MOST 105-2112-M-008-012. PTF is a collaboration project in science 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. C.R.T.S. was supported by the NSF grants of AST-1313422, AST-1413600, and AST-1518308.\n\nSubmitted - 1706.06731.pdf
", "abstract": "A systematic study on the long-term periodicities of known Galactic cataclysmic variables (CVs) was conducted. Among 1580 known CVs, 344 sources were matched and extracted from the Palomar Transient Factory (PTF) data repository. The PTF light curves were combined with the Catalina Real-Time Transient Survey (CRTS) light curves and analyzed. Ten targets were found to exhibit long-term periodic variability, which is not frequently observed in the CV systems. These long-term variations are possibly caused by various mechanisms, such as the precession of the accretion disk, hierarchical triple star system, magnetic field change of the companion star, and other possible mechanisms. We discuss the possible mechanisms in this study. If the long-term period is less than several tens of days, the disk precession period scenario is favored. However, the hierarchical triple star system or the variations in magnetic field strengths are most likely the predominant mechanisms for longer periods.", "date": "2017-09", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "129", "number": "979", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 094202", "id_number": "CaltechAUTHORS:20170728-091458187", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170728-091458187", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2119-M-008-024" }, { "agency": "National Science Foundation of China", "grant_number": "102-2112-M-008-020-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "105-2112-M-008-012" }, { "agency": "NSF", "grant_number": "AST-1313422" }, { "agency": "NSF", "grant_number": "AST-1413600" }, { "agency": "NSF", "grant_number": "AST-1518308" } ] }, "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/aa7a99", "primary_object": { "basename": "1706.06731.pdf", "url": "https://authors.library.caltech.edu/records/w7829-tba88/files/1706.06731.pdf" }, "pub_year": "2017", "author_list": "Yang, Michael Ting-Chang; Chou, Yi; et el." }, { "id": "https://authors.library.caltech.edu/records/fxv2k-1g668", "eprint_id": 79247, "eprint_status": "archive", "datestamp": "2023-08-21 21:27:53", "lastmod": "2023-10-26 14:44:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "B. D." }, "orcid": "0000-0002-7856-3570" }, { "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" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" } ] }, "title": "iPTF16fnl: A Faint and Fast Tidal Disruption Event in an E+A Galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: nuclei; stars: individual (iPTF16fnl)", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2017 February 17. Accepted 2017 May 24. Published 2017 July 20. \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under grant No. 1545949. We thank the Gemini Fast Turnaround program (PI: T. Hung). S.G. is supported in part by NSF CAREER grant 1454816 and NASA Swift Cycle 12 grant NNX16AN85G. A.Y.Q.H. was supported by a National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. A.J.C.T. acknowledges support from the Spanish Ministry Project AYA 2015-71718-R. Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. G.H. is supported by the National Science Foundation (NSF) under grant No. 1313484. This work makes use of observations from the LCO network. G.H. is supported by the National Science Foundation (NSF) under grant No. 1313484. This work makes use of observations from the LCO network. \n\nWe acknowledge the use of public data from the Swift data archive. The CSS survey is funded by the National Aeronautics and Space Administration under grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182. L.A.N.L. participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program. 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. Part of this work is based on observations obtained at the Gemini observatory under the Fast Turnaround program. The Gran Telescopio Canarias (GTC) is operated on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. 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. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. V.A.F. is supported by the Russian Science Foundation under grant 14-50-00043. \n\nFacilities: DCT, Gemini North, GTC, Hale, JCMT, Keck:I, Keck:II, LCOGT, PO:1.2m, PO:1.5m, PS1, VLT. \n\nSoftware: AstroPy, EMCEE (Foreman-Mackey et al. 2013), IRAF, LMFIT, pPXF (Cappellari 2017), PTFIDE (Masci et al. 2017), PYRAF, UVOTSOURCE.\n\nPublished - Blagorodnova_2017_ApJ_844_46.pdf
Submitted - 1703.00965.pdf
", "abstract": "We present ground-based and Swift observations of iPTF16fnl, a likely tidal disruption event (TDE) discovered by the intermediate Palomar Transient Factory (iPTF) survey at 66.6 Mpc. The light curve of the object peaked at an absolute mag M_g =- 17.2. The maximum bolometric luminosity (from optical and UV) was L_p \u2243 (1.0 \u00b1 0.15) x 10^(43) erg s^(\u22121), an order of magnitude fainter than any other optical TDE discovered so far. The luminosity in the first 60 days is consistent with an exponential decay, with L \u221d e^(-(t-t_0)/\u03c4, where t_0 = 57631.0 (MJD) and \u03c4 \u2243 15 days. The X-ray shows a marginal detection at L_X = 2.4_(-1.1)^(1.9) x 10^(39) erg s^(\u22121) (Swift X-ray Telescope). No radio counterpart was detected down to 3\u03c3, providing upper limits for monochromatic radio luminosities of vL_v < 2.3 x 10^(36) erg s^(\u22121) and vL_v < 1.7 x 10^(37) erg s^(\u22121) (Very Large Array, 6.1 and 22 GHz). The blackbody temperature, obtained from combined Swift UV and optical photometry, shows a constant value of 19,000 K. The transient spectrum at peak is characterized by broad He ii and H\u03b1 emission lines, with FWHMs of about 14,000 km s^(\u22121) and 10,000 km s^(\u22121), respectively. He i lines are also detected at \u03bb\u03bb 5875 and 6678. The spectrum of the host is dominated by strong Balmer absorption lines, which are consistent with a post-starburst (E+A) galaxy with an age of ~650 Myr and solar metallicity. The characteristics of iPTF16fnl make it an outlier on both luminosity and decay timescales, as compared to other optically selected TDEs. The discovery of such a faint optical event suggests a higher rate of tidal disruptions, as low-luminosity events may have gone unnoticed in previous searches.", "date": "2017-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "844", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 46", "id_number": "CaltechAUTHORS:20170720-093554732", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170720-093554732", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "NASA", "grant_number": "NNX16AN85G" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)", "grant_number": "AYA 2015-71718-R" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Chinese Academy of Sciences", "grant_number": "XDB09000000" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Russian Science Foundation", "grant_number": "14-50-00043" } ] }, "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": "10.3847/1538-4357/aa7579", "primary_object": { "basename": "1703.00965.pdf", "url": "https://authors.library.caltech.edu/records/fxv2k-1g668/files/1703.00965.pdf" }, "related_objects": [ { "basename": "Blagorodnova_2017_ApJ_844_46.pdf", "url": "https://authors.library.caltech.edu/records/fxv2k-1g668/files/Blagorodnova_2017_ApJ_844_46.pdf" } ], "pub_year": "2017", "author_list": "Blagorodnova, N.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/ahaj9-cpm89", "eprint_id": 78524, "eprint_status": "archive", "datestamp": "2023-08-19 03:52:47", "lastmod": "2023-10-26 00:10:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "van-Roestel-J", "name": { "family": "van Roestel", "given": "J." }, "orcid": "0000-0002-2626-2872" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "P. J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "D." } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Bloemen-S", "name": { "family": "Bloemen", "given": "S." } }, { "id": "Marsh-T-R", "name": { "family": "Marsh", "given": "T. R." }, "orcid": "0000-0002-2498-7589" }, { "id": "Dhillon-V-S", "name": { "family": "Dhillon", "given": "V. S." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D." }, "orcid": "0000-0003-4401-0430" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "PTF1 J085713+331843, a new post-common-envelope binary in the orbital period gap of cataclysmic variables", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing \u2013 stars: late-type \u2013white dwarfs", "note": "\u00a9 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2017 March 10. Received 2017 February 27; in original form 2016 December 22. Published: 14 March 2017. \n\nWe thank the anonymous referee for his/her helpful comments improving this manuscript, and thank T. Kupfer and C. Knigge for many useful discussions. \n\nThe results presented in this paper are based on observations collected with ULTRACAM, supported by STFC grants, at the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Institutions de Astrofisica de Canarias. \n\nThe results are based on observations of the Palomar Transient Factory. The Palomar Transient Factory is a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkely National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. \n\nThe results are based on observations collected at the Palomar Observatory with the 200 inch Hale Telescope, operated by the California institute of Technology, its divisions Caltech Optical Observations, the Jet Propulsion Laboratory (operated for NASA) and Cornell University. \n\nSome of the data presented here were obtained by the Catalina Real-time Transient Survey (CRTS). CRTS are supported by the U.S. National Science Foundation under grants AST-0909182 and CNS-0540369. The CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. \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\nWe thank K. Verbeek for the use of the white dwarf\u2013red dwarf model spectra that are partially made from white dwarf model spectra kindly given to us by D. Koester. \n\nJvR acknowledges support by the Netherlands Research School of Astronomy (NOVA) and Foundation for Fundamental Research on Matter (FOM). This paper was finalized during a stay by the lead authors at the Kavli Institute for Theoretical Physics, Santa Barbara, which is supported in part by the National Science Foundation under Grant No. NSF PHY-1125915.\n\nPublished - stx625.pdf
Submitted - 1704.01182.pdf
", "abstract": "We report the discovery and analysis of PTF1 J085713+331843, a new eclipsing post-common-envelope detached white-dwarf\u2013red-dwarf binary with a 2.5 h orbital period discovered by the Palomar Transient Factory. ULTRACAM multicolour photometry over multiple orbital periods reveals a light curve with a deep flat-bottomed primary eclipse and a strong reflection effect. Phase-resolved spectroscopy shows broad Balmer absorption lines from the DA white dwarf and phase-dependent Balmer emission lines originating on the irradiated side of the red dwarf. The temperature of the DA white dwarf is T_(WD) = 25\u2009700 \u00b1 400\u2009K and the spectral type of the red dwarf is M3\u2013M5. A combined modelling of the light curve and the radial velocity variations results in a white dwarf mass of \nM_(WD)=0.61^(+0.18)_(\u22120.17)M\u2299 and radius of R_(WD)=0.0175^(+0.0012)_(\u22120.0011)R\u2299, and a red dwarf mass and radius of \nM_(RD)=0.19^(+0.10)_(\u22120.08)M\u2299 and R_(RD)=0.24^(+0.04)_(\u22120.04)R\u2299. The system is either a detached cataclysmic variable or has emerged like from the common-envelope phase at nearly its current orbital period. In \u223c70 Myr, this system will become a cataclysmic variable in the period gap.", "date": "2017-07", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "468", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "3109-3122", "id_number": "CaltechAUTHORS:20170623-141442582", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170623-141442582", "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-0909182" }, { "agency": "NSF", "grant_number": "CNS-0540369" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" }, { "agency": "Nederlandse Onderzoekschool Voor Astronomie (NOVA)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "NSF", "grant_number": "PHY-1125915" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1093/mnras/stx625", "primary_object": { "basename": "1704.01182.pdf", "url": "https://authors.library.caltech.edu/records/ahaj9-cpm89/files/1704.01182.pdf" }, "related_objects": [ { "basename": "stx625.pdf", "url": "https://authors.library.caltech.edu/records/ahaj9-cpm89/files/stx625.pdf" } ], "pub_year": "2017", "author_list": "van Roestel, J.; Groot, P. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/99d8k-rmz92", "eprint_id": 78038, "eprint_status": "archive", "datestamp": "2023-08-21 21:13:58", "lastmod": "2023-10-25 23:41:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hung-T-K", "name": { "family": "Hung", "given": "T." } }, { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Roth-N", "name": { "family": "Roth", "given": "N." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "McCully-C", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "Revisiting Optical Tidal Disruption Events with iPTF16axa", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; black hole physics; galaxies: nuclei; ultraviolet: general", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2017 March 1. Accepted 2017 May 13. Published 2017 June 8. \n\nWe thank the anonymous referee for helpful comments regarding the manuscript. T.H. thanks T. Holoien and C. Bonnerot for providing data from their papers. S.G. is supported in part by NSF CAREER grant 1454816, NASA Swift Cycle 12 grant NNX16AN85G, and NASA Keck Grant 1568615. N.R. acknowledges the support of a Joint Space-Science Institute prize postdoctoral fellowship. A.H. acknowledges the support of a grant from the I-CORE program \"From the Big Bang to Planets.\" Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. These results made use of the Discovery Channel Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.\n\nPublished - Hung_2017_ApJ_842_29.pdf
Submitted - 1703.01299v2.pdf
", "abstract": "We report the discovery by the intermediate Palomar Transient Factory (iPTF) of a candidate tidal disruption event (TDE) iPTF16axa at z = 0.108 and present its broadband photometric and spectroscopic evolution from three months of follow-up observations with ground-based telescopes and Swift. The light curve is well fitted with a t^(\u22125/3) decay, and we constrain the rise time to peak to be <49 rest-frame days after disruption, which is roughly consistent with the fallback timescale expected for the ~5 \u00d7 10^6 M_\u2299 black hole inferred from the stellar velocity dispersion of the host galaxy. The UV and optical spectral energy distribution is well described by a constant blackbody temperature of T ~ 3 \u00d7 10^4 K over the monitoring period, with an observed peak luminosity of 1.1 \u00d7 10^(44) erg s^(\u22121). The optical spectra are characterized by a strong blue continuum and broad He ii and H\u03b1 lines, which are characteristic of TDEs. We compare the photometric and spectroscopic signatures of iPTF16axa with 11 TDE candidates in the literature with well-sampled optical light curves. Based on a single-temperature fit to the optical and near-UV photometry, most of these TDE candidates have peak luminosities confined between log(L [erg s^(\u22121)]) = 43.4\u201344.4, with constant temperatures of a few \u00d710^4 K during their power-law declines, implying blackbody radii on the order of 10 times the tidal disruption radius, that decrease monotonically with time. For TDE candidates with hydrogen and helium emission, the high helium-to-hydrogen ratios suggest that the emission arises from high-density gas, where nebular arguments break down. We find no correlation between the peak luminosity and the black hole mass, contrary to the expectations for TDEs to have M \u221d M_(BH)^(-1/2).", "date": "2017-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "842", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 29", "id_number": "CaltechAUTHORS:20170609-064008817", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170609-064008817", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "NASA", "grant_number": "NNX16AN85G" }, { "agency": "NASA", "grant_number": "1568615" }, { "agency": "Joint Space-Science Institute" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/aa7337", "primary_object": { "basename": "1703.01299v2.pdf", "url": "https://authors.library.caltech.edu/records/99d8k-rmz92/files/1703.01299v2.pdf" }, "related_objects": [ { "basename": "Hung_2017_ApJ_842_29.pdf", "url": "https://authors.library.caltech.edu/records/99d8k-rmz92/files/Hung_2017_ApJ_842_29.pdf" } ], "pub_year": "2017", "author_list": "Hung, T.; Gezari, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/xq7z7-hp952", "eprint_id": 77407, "eprint_status": "archive", "datestamp": "2023-08-19 03:06:37", "lastmod": "2023-10-25 23:00:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Lin-Zhong-Yi", "name": { "family": "Lin", "given": "Zhong-Yi" }, "orcid": "0000-0003-3827-8991" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Ye-Quanzhi", "name": { "family": "Ye", "given": "Quan-Zhi" }, "orcid": "0000-0002-4838-7676" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Lee-Hee-Jae", "name": { "family": "Lee", "given": "Hee-Jae" } }, { "id": "Moon-Hong-Kyu", "name": { "family": "Moon", "given": "Hong-Kyu" } } ] }, "title": "Confirmation of Large Super-fast Rotator (144977) 2005 EC_(127)", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: individual (144977) 2005 EC127", "note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2017 April 2; revised 2017 April 24; accepted 2017 April 27; published 2017 May 10.\n\nThis work is supported in part by the Ministry of Science and Technology of Taiwan under grants MOST 104-2112-M-008-014-MY3, MOST 104-2119-M-008-024, and MOST 105-2112-M-008-002-MY3, and also by Macau Science and Technology Fund No. 017/2014/A1 of MSAR. We are thankful for the indispensable support provided by the staff of the Lulin Observatory and the staff of the Palomar Observatory. We thank the anonymous referee for useful suggestions and comments.\n\nPublished - Chang_2017_ApJL_840_L22.pdf
Submitted - 1704.08451.pdf
", "abstract": "(144977) 2005 EC_(127) is a V-/A-type inner-main-belt asteroid with a diameter of 0.6 \u00b1 0.1 km. Asteroids of this size are believed to have rubble-pile structure, and therefore cannot have a rotation period shorter than 2.2 hr. However, our measurements show that asteroid 2005 EC_(127) completes one rotation in 1.65 \u00b1 0.01 hr with a peak-to-peak light-curve variation of ~0.5 mag. Therefore, this asteroid is identified as a large super-fast rotator. Either a rubble-pile asteroid with a bulk density of \u03c1 ~ 6 g cm^(\u22123) or an asteroid with an internal cohesion of 47 \u00b1 30 Pa can explain 2005 EC_(127). However, the scenario of high bulk density is very unlikely for asteroids. To date, only six large super-fast rotators, including 2005 EC_(127), have been reported, and this number is very small when compared with the much more numerous fast rotators. We also note that none of the six reporting large SFRs are classified as C-type asteroids.", "date": "2017-05-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "840", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L22", "id_number": "CaltechAUTHORS:20170512-104233877", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170512-104233877", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 104-2112-M-008-014-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 104-2119-M-008-024" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 105-2112-M-008-002-MY3" }, { "agency": "Macau Science and Technology", "grant_number": "017/2014/A1" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/2041-8213/aa6ff5", "primary_object": { "basename": "1704.08451.pdf", "url": "https://authors.library.caltech.edu/records/xq7z7-hp952/files/1704.08451.pdf" }, "related_objects": [ { "basename": "Chang_2017_ApJL_840_L22.pdf", "url": "https://authors.library.caltech.edu/records/xq7z7-hp952/files/Chang_2017_ApJL_840_L22.pdf" } ], "pub_year": "2017", "author_list": "Chang, Chan-Kao; Lin, Hsing-Wen; et el." }, { "id": "https://authors.library.caltech.edu/records/g2r19-n3163", "eprint_id": 77213, "eprint_status": "archive", "datestamp": "2023-08-21 21:00:03", "lastmod": "2023-10-25 21:58:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Brown-P", "name": { "family": "Brown", "given": "P." } }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "J." }, "orcid": "0000-0001-5703-2108" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "J." }, "orcid": "0000-0001-5754-4007" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Far-ultraviolet to Near-infrared Spectroscopy of a Nearby Hydrogen-poor Superluminous Supernova Gaia16apd", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: massive; supernovae: individual (Gaia16apd)", "note": "\u00a9 2017 American Astronomical Society. \n\nReceived 2016 November 7. Accepted 2017 March 30. Published 2017 May 4. \n\nWe thank Daniel Kasen for very helpful discussion and for making his model spectra available. Vikram Ravi is acknowledged for obtaining some spectra used in this paper. We are grateful to the HST staff for the prompt scheduling of these ToO observations. We acknowledge ESA Gaia, DPAC, and the Photometric Science Alerts Team.11 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. M.M.K. acknowledges support by the GROWTH project funded by the National Science Foundation under PIRE Grant No 1545949. E.O.O. is an incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation, Minerva, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva, and ISF grants, WIS-UK \"making connections,\" and Kimmel and YeS awards. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacilities: Swift - Swift Gamma-Ray Burst Mission, HST (COS - , STIS) - , Keck (LRIS - , MOSFIRE) - , Palomar - . \n\nSoftware: Astropy, SEDONA, syn++.\n\nPublished - Yan_2017_ApJ_840_57.pdf
Submitted - 1611.02782.pdf
", "abstract": "We report the first maximum-light far-ultraviolet (FUV) to near-infrared (NIR) spectra (1000 \u00c5 \u2212 1.62 \u03bcm, rest) of a hydrogen-poor superluminous supernova, Gaia16apd. At z = 0.1018, it is the second closest and the UV brightest SLSN-I, with 17.4 mag in Swift UVW2 band at \u221211 days pre-maximum. The coordinated observations with HST, Palomar, and Keck were taken at \u22122 to +25 days. Assuming an exponential (or t^2) form, we derived the rise time of 33 days and the peak bolometric luminosity of 3 \u00d7 10^(44) erg s^(\u22121). At the maximum, the photospheric temperature and velocity are 17,000 K and 14,000 km s^(\u22121), respectively. The inferred radiative and kinetic energy are roughly 1 \u00d7 10^(51) and 2 \u00d7 10^(52) erg. Gaia16apd is extremely UV luminous, and emits 50% of its total luminosity at 1000\u20132500 \u00c5. Compared to the UV spectra (normalized at 3100 \u00c5) of well studied SN1992A (Ia), SN2011fe (Ia), SN1999em (IIP), and SN1993J (IIb), it has orders of magnitude more FUV emission. This excess is interpreted primarily as a result of weaker metal-line blanketing due to a much lower abundance of iron group elements in the outer ejecta. Because these elements originate either from the natal metallicity of the star, or have been newly produced, our observation provides direct evidence that little of these freshly synthesized material, including ^(56)Ni, were mixed into the outer ejecta, and the progenitor metallicity is likely sub-solar. This disfavors Pair-instability Supernova models with helium core masses \u2a7e 90, M_\u2609, where substantial ^(56)Ni material is produced. A higher photospheric temperature definitely contributes to the FUV excess from Gaia16apd. Compared with Gaia16apd, we find PS1-11bam is also UV luminous.", "date": "2017-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "840", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 57", "id_number": "CaltechAUTHORS:20170505-093241168", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170505-093241168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ)" }, { "agency": "Israel Science Foundation" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "MINERVA (Israel)" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa6b02", "primary_object": { "basename": "1611.02782.pdf", "url": "https://authors.library.caltech.edu/records/g2r19-n3163/files/1611.02782.pdf" }, "related_objects": [ { "basename": "Yan_2017_ApJ_840_57.pdf", "url": "https://authors.library.caltech.edu/records/g2r19-n3163/files/Yan_2017_ApJ_840_57.pdf" } ], "pub_year": "2017", "author_list": "Yan, Lin; Quimby, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/n2t3d-drt13", "eprint_id": 73163, "eprint_status": "archive", "datestamp": "2023-08-19 02:47:55", "lastmod": "2023-10-24 15:05:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Groh-J-H", "name": { "family": "Groh", "given": "J. H." } }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Rubin-A-E", "name": { "family": "Rubin", "given": "A." } }, { "id": "Szabo-P", "name": { "family": "Szabo", "given": "P." } }, { "id": "Sapir-N", "name": { "family": "Sapir", "given": "N." } }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Khazov-D", "name": { "family": "Khazov", "given": "D." } }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "O. D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Gnat-O", "name": { "family": "Gnat", "given": "O." } }, { "id": "Kelly-P-L", "name": { "family": "Kelly", "given": "P. L." }, "orcid": "0000-0003-3142-997X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P. R." }, "orcid": "0000-0002-9919-3310" }, { "id": "Lee-William-H-K", "name": { "family": "Lee", "given": "W. H." } }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "U. D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Sullivan-M", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Sougmagnac-M-T", "name": { "family": "Soumagnac", "given": "M. T." } } ] }, "title": "Confined dense circumstellar material surrounding a regular type II supernova", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 Macmillan Publishers Limited, part of Springer Nature. \n\nReceived 15 October 2016; Accepted 03 January 2017; Published online 13 February 2017. \n\nWe are grateful to the staff at the various observatories where data were obtained, as well as to N. E. Groeneboom, K. I. Clubb, M. L. Graham, D. Sand, A. A. Djupvik, I. Shivvers, J. C. Mauerhan and A. Waszczak for assistance with observations. We thank E. Waxman for valuable discussions. A.G.-Y.'s group is supported by the EU/FP7 via an ERC grant, the Quantum Universe I-Core programme by the Israeli Committee for planning and budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK 'making connections' programme; and by Kimmel, ARCHES and Yes awards. D.A.P. acknowledges support from Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute, and from a Marie Curie Individual Fellowship as part of the Horizon 2020 European Union (EU) Framework Programme for Research and Innovation (H2020-MSCA-IF-2014-660113). J.H.G. acknowledges support from an AMBIZIONE grant of the Swiss NSF. E.O.O. is supported by the Arye Dissentshik career development chair, Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core programme. M.M.K. acknowledges support from the National Science Foundation for the GROWTH project funded under Grant No. 1545949. A.V.F.'s research is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and US NSF grant AST-1211916. Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development programme. Supernova research at the Oskar Klein Centre is supported by the Swedish Research Council and by the Knut and Alice Wallenberg Foundation. K.M. acknowledges support from a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). Some data were obtained with the Nordic Optical Telescope, which is operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain. We thank the RATIR project team, the staff of the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and the software support team from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional and the operation of both are funded through National Aeronautics and Space Administration (NASA) grants NNX09AH71G, NNX09AT02G, NNX10AI27G and NNX12AE66G, CONACyT (INFR-2009-01-122785, CB-2008-101958), UNAM PAPIIT (IN113810 and IG100414) and UCMEXUS-CONACyT. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with NASA.\n\nContributions:\nO.Y. initiated the study, conducted analysis and wrote the manuscript. D.A.P. is PI of the first-night Keck programme, obtained and reduced the Keck/LRIS spectra, and contributed to the analysis of the early-time data. A.G.-Y. is PI of iPTF early-time SN II studies, managed the project, and contributed to analysis and manuscript preparation. J.H.G. performed modelling and analysis of the early spectra. A.H. is PI of the VLA radio programme, provided radio observations, reduction, and analysis, and contributed to figures and manuscript preparation. E.O.O. contributed to analysis of early-time data, mass-loss estimates, Swift-XRT reductions and manuscript preparation. S.R.K. is PI of PTF and of Palomar and Keck follow-up programmes. J.S. provided NOT spectroscopy and contributed to analysis and manuscript preparation. C.F. contributed to analysis of line profiles, estimates of physical properties, and X-ray and radio data interpretation. A.R. performed analysis of the multiband photometry fits to RW11 shock-cooling models. P.S. performed SBO models and contributed to analysis of X-ray emission. N.S. contributed to analysis of SBO properties, early-time spectral modelling, and X-ray emission. F.T. provided and reduced NOT data. S.B.C. reduced Swift and Palomar 60-inch data, and contributed to spectroscopic reduction and analysis. S.V. provided LCOGT multiband photometry and reduced FTS-FLOYDS spectroscopy. I.A. provided LCOGT multiband photometry and reduced FTS-FLOYDS spectroscopy. D.A.H. is PI of the LCOGT follow-up programme. M.M.K. is a PTF builder and provided APO data. P.M.V. contributed to spectroscopic reductions, analysis and figure preparation. D.K. contributed to analysis of the early flash-ionized spectra and to figure preparation. O.D.F. provided RATIR multiband photometry. Y.C. is a PTF builder and performed spectroscopic observations and reductions. O.G. contributed to radiative-transfer analysis of the early-time emission-line spectra. P.L.K. contributed to Keck-II/DEIMOS spectroscopic reductions. P.E.N. is a PTF builder and contributed to manuscript preparation. A.V.F. provided Keck and Lick data, and edited the manuscript. R.R.L. is a developer of the image reduction pipeline. P.R.W. is a PTF builder, involved with machine-learning development. W.H.L. is PI of the RATIR proposals. U.D.R. is a PTF builder, involved with machine-learning development. K.M. is PI of the WHT ToO spectroscopic time, and performed WHT-ISIS spectroscopic reductions. M.S. is PI of the WHT follow-up effort. M.T.S. is a member of the iPTF human monitoring (scanners) team. \n\nThe authors declare no competing financial interests.\n\nSubmitted - 1701.02596.pdf
Supplemental Material - nphys4025-s1.pdf
", "abstract": "With the advent of new wide-field, high-cadence optical transient surveys, our understanding of the diversity of core-collapse supernovae has grown tremendously in the last decade. However, the pre-supernova evolution of massive stars, which sets the physical backdrop to these violent events, is theoretically not well understood and difficult to probe observationally. Here we report the discovery of the supernova iPTF\u200913dqy = SN\u20092013fs\u2009 a mere ~3\u2009h after explosion. Our rapid follow-up observations, which include multiwavelength photometry and extremely early (beginning at ~6\u2009h post-explosion) spectra, map the distribution of material in the immediate environment (\u227210^(15)\u2009cm) of the exploding star and establish that it was surrounded by circumstellar material (CSM) that was ejected during the final ~1\u2009yr prior to explosion at a high rate, around 10^(\u22123) solar masses per year. The complete disappearance of flash-ionized emission lines within the first several days requires that the dense CSM be confined to within \u227210^(15)\u2009cm, consistent with radio non-detections at 70\u2013100\u2009days. The observations indicate that iPTF\u200913dqy was a regular type II supernova; thus, the finding that the probable red supergiant progenitor of this common explosion ejected material at a highly elevated rate just prior to its demise suggests that pre-supernova instabilities may be common among exploding massive stars.", "date": "2017-05", "date_type": "published", "publication": "Nature Physics", "volume": "13", "number": "5", "publisher": "Nature Publishing Group", "pagerange": "510-517", "id_number": "CaltechAUTHORS:20161222-154313025", "issn": "1745-2473", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161222-154313025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "Yes Award" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51296.01-A" }, { "agency": "Marie Curie Fellowship", "grant_number": "H2020-MSCA-IF-2014-660113" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Arye Dissentshik career development chair" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Swedish Research Council" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "NASA", "grant_number": "NNX09AH71G" }, { "agency": "NASA", "grant_number": "NNX09AT02G" }, { "agency": "NASA", "grant_number": "NNX10AI27G" }, { "agency": "NASA", "grant_number": "NNX12AE66G" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "INFR-2009-01-122785" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "CB-2008-101958" }, { "agency": "University of California Institute for Mexico and the United States (UC MEXUS)" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Google" }, { "agency": "JPL Research and Technology Development Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nphys4025", "primary_object": { "basename": "nphys4025-s1.pdf", "url": "https://authors.library.caltech.edu/records/n2t3d-drt13/files/nphys4025-s1.pdf" }, "related_objects": [ { "basename": "1701.02596.pdf", "url": "https://authors.library.caltech.edu/records/n2t3d-drt13/files/1701.02596.pdf" } ], "pub_year": "2017", "author_list": "Yaron, O.; Perley, D. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/q98a4-0x079", "eprint_id": 76786, "eprint_status": "archive", "datestamp": "2023-08-19 02:41:55", "lastmod": "2023-10-25 16:51:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Lawrence-D-J", "name": { "family": "Lawrence", "given": "D." } }, { "id": "M\u00f6rtsell-E", "name": { "family": "M\u00f6rtsell", "given": "E." } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Brandeker-A", "name": { "family": "Brandeker", "given": "A." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Ferretti-R", "name": { "family": "Ferretti", "given": "R." }, "orcid": "0000-0001-7814-5814" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Hangard-L", "name": { "family": "Hangard", "given": "L." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "H." }, "orcid": "0000-0001-8242-9983" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Papadogiannakis-S", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Petrushevska-T", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" }, { "id": "Ravi-Vikram", "name": { "family": "Ravi", "given": "V." }, "orcid": "0000-0002-7252-5485" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Wilson-D-M", "name": { "family": "Wilson", "given": "D. M." }, "orcid": "0000-0001-6002-423X" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" } ] }, "title": "iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Association for the Advancement of Science. \n\nReceived for publication 25 October 2016; accepted for publication 24 March 2017. \n\nSupported by the Swedish National Science Council and the Swedish National Space Board (A.G., R.A., and E.M.); U.S. Department of Energy (DOE) grant DE-AC02-05CH11231 (P.E.N.); European Research Council grant 615929 (M.S.); NASA (S.R.K.); and NSF grant 1545949. The iPTF Swedish collaboration is funded through a grant from the Knut and Alice Wallenberg foundation. This research used resources of the National Energy Research Scientific Computing Center, supported by DOE contract DE-AC02-05CH11231. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA grant HST-GO-14862.002. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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. The Space Telescope Science Data Analysis System (STSDAS) and the command language PyRAF are products of the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA) for NASA. Part of the processing was carried out off-line using the commercial software package MATLAB and Statistics Toolbox Release 2013a, The MathWorks Inc., Natick, MA. Photometric data used in this paper are available in tables S1, S2, and S5, spectroscopic data are available at public repository WISeREP (33) (http://wiserep.weizmann.ac.il) under the ID \"SN 2016geu\"; the positions of the SN images used in the lensing model are provided in table S4.\n\nSubmitted - 1611.00014.pdf
Supplemental Material - aal2729_Goobar_SM.pdf
", "abstract": "We report the discovery of a multiply imaged, gravitationally lensed type Ia supernova, iPTF16geu (SN 2016geu), at redshift z = 0.409. This phenomenon was identified because the light from the stellar explosion was magnified more than 50 times by the curvature of space around matter in an intervening galaxy. We used high-spatial-resolution observations to resolve four images of the lensed supernova, approximately 0.3 arc seconds from the center of the foreground galaxy. The observations probe a physical scale of ~1 kiloparsec, smaller than is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration imply close alignment between the lines of sight to the supernova and to the lens. The relative magnifications of the four images provide evidence for substructures in the lensing galaxy.", "date": "2017-04-21", "date_type": "published", "publication": "Science", "volume": "356", "number": "6335", "publisher": "American Association for the Advancement of Science", "pagerange": "291-295", "id_number": "CaltechAUTHORS:20170420-143345464", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170420-143345464", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish National Science Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "NASA", "grant_number": "HST-GO-14862.002" }, { "agency": "W. M. Keck Foundation" } ] }, "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": "10.1126/science.aal2729", "primary_object": { "basename": "1611.00014.pdf", "url": "https://authors.library.caltech.edu/records/q98a4-0x079/files/1611.00014.pdf" }, "related_objects": [ { "basename": "aal2729_Goobar_SM.pdf", "url": "https://authors.library.caltech.edu/records/q98a4-0x079/files/aal2729_Goobar_SM.pdf" } ], "pub_year": "2017", "author_list": "Goobar, A.; Amanullah, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/6h451-jw951", "eprint_id": 95835, "eprint_status": "archive", "datestamp": "2023-08-19 02:29:29", "lastmod": "2023-10-20 20:37:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pian-E", "name": { "family": "Pian", "given": "E." } }, { "id": "Tomasella-L", "name": { "family": "Tomasella", "given": "L." } }, { "id": "Cappellaro-E", "name": { "family": "Cappellaro", "given": "E." }, "orcid": "0000-0001-5008-8619" }, { "id": "Benetti-S", "name": { "family": "Benetti", "given": "S." }, "orcid": "0000-0002-3256-0016" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Baltay-C", "name": { "family": "Baltay", "given": "C." } }, { "id": "Branchesi-M", "name": { "family": "Branchesi", "given": "M." } }, { "id": "Brocato-E", "name": { "family": "Brocato", "given": "E." } }, { "id": "Campana-S", "name": { "family": "Campana", "given": "S." } }, { "id": "Copperwheat-C-M", "name": { "family": "Copperwheat", "given": "C." } }, { "id": "Covino-S", "name": { "family": "Covino", "given": "S." } }, { "id": "D'Avanzo-P", "name": { "family": "D'Avanzo", "given": "P." } }, { "id": "Ellman-N", "name": { "family": "Ellman", "given": "N." } }, { "id": "Grado-A", "name": { "family": "Grado", "given": "A." }, "orcid": "0000-0002-0501-8256" }, { "id": "Melandri-A", "name": { "family": "Melandri", "given": "A." } }, { "id": "Palazzi-E", "name": { "family": "Palazzi", "given": "E." } }, { "id": "Piascik-A-S", "name": { "family": "Piascik", "given": "A." } }, { "id": "Piranomonte-S", "name": { "family": "Piranomonte", "given": "S." } }, { "id": "Rabinowitz-D-L", "name": { "family": "Rabinowitz", "given": "D." } }, { "id": "Raimondo-G", "name": { "family": "Raimondo", "given": "G." } }, { "id": "Smartt-S-J", "name": { "family": "Smartt", "given": "S. J." }, "orcid": "0000-0002-8229-1731" }, { "id": "Steele-I-A", "name": { "family": "Steele", "given": "I. A." }, "orcid": "0000-0001-8397-5759" }, { "id": "Stritzinger-M-D", "name": { "family": "Stritzinger", "given": "M." }, "orcid": "0000-0002-5571-1833" }, { "id": "Yang-S", "name": { "family": "Yang", "given": "S." } }, { "id": "Ascenzi-S", "name": { "family": "Ascenzi", "given": "S." }, "orcid": "0000-0001-5116-6789" }, { "id": "Della-Valle-M", "name": { "family": "Della Valle", "given": "M." }, "orcid": "0000-0003-3142-5020" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Getman-F", "name": { "family": "Getman", "given": "F." } }, { "id": "Greco-G", "name": { "family": "Greco", "given": "G." } }, { "id": "Inserra-C", "name": { "family": "Inserra", "given": "C." }, "orcid": "0000-0002-3968-4409" }, { "id": "Kankare-E", "name": { "family": "Kankare", "given": "E." }, "orcid": "0000-0001-8257-3512" }, { "id": "Limatola-L", "name": { "family": "Limatola", "given": "L." }, "orcid": "0000-0002-1896-8605" }, { "id": "Nicastro-L", "name": { "family": "Nicastro", "given": "L." } }, { "id": "Pastorello-A", "name": { "family": "Pastorello", "given": "A." } }, { "id": "Pulone-L", "name": { "family": "Pulone", "given": "L." } }, { "id": "Stamerra-A", "name": { "family": "Stamerra", "given": "A." } }, { "id": "Stella-L", "name": { "family": "Stella", "given": "L." } }, { "id": "Stratta-G", "name": { "family": "Stratta", "given": "G." } }, { "id": "Tartaglia-L", "name": { "family": "Tartaglia", "given": "L." }, "orcid": "0000-0003-3433-1492" }, { "id": "Turatto-M", "name": { "family": "Turatto", "given": "M." } } ] }, "title": "Optical photometry and spectroscopy of the low-luminosity, broad-lined Ic supernova iPTF15dld", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: massive, supernovae: individual: iPTF15dld (LSQ15bfp, PS15clr), galaxies: starburst", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 December 9. Received 2016 December 8; in original form 2016 October 29. Published: 13 December 2016.\n\nWe acknowledge data from the Pan-STARRS1 telescope that is supported by NASA under grant no. NNX12AR65G and grant no. NNX14AM74G issued through the NEO Observation Program. We acknowledge funding from ASI INAF grant I/088/06/0, from the Italian Ministry of Education and Research and the Scuola Normale Superiore, and from INAF project: 'Gravitational Wave Astronomy with the first detections of aLIGO and aVIRGO experiments' (PI: E. Brocato). GR is partially supported by the PRIN INAF-2014 'EXCALIBURS: EXtragalactic distance scale CALIBration Using first-Rank Standard candles' (PI: G. Clementini). L. Tomasella, EC and SB are partially supported by the PRIN-INAF 2014 project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'. MS gratefully acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. MB, GG and GS acknowledge financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F. We thank the staff of the Copernico telescope, LT, NTT, TNG, NOT and LSQ, in particular W. Boschin, D. Carosati, S. Dalle Ave, L. Di Fabrizio, A. Fiorenzano, P. Ochner, T. Pursimo and T. Reynolds. We are grateful to S. Valenti for sending archival supernova data in digital form, P. Nugent for his support of this project, L. Singer for his critical reading of the manuscript and to our referee for constructive suggestions. This research is based on observations made with the Copernico telescope (Asiago, Italy) of INAF - Osservatorio Astronomico di Padova; with the NTT at the European Organization for Astronomical Research in the Southern hemisphere, Chile, as part of the Public ESO Spectroscopic Survey for Transient Objects Survey (PESSTO) ESO programmes 188.D-3003, 191.D-0935; with the Telescopio Nazionale Galileo, operated by the Fundaci\u00f3n Galileo Galilei of INAF, with the Liverpool Telescope, operated by Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council, and with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association, all three on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. This research has made use of the Weizmann Interactive Supernova data Repository (http://wiserep.weizmann.ac.il), and it 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.\n\nAccepted Version - 1612.03275.pdf
", "abstract": "Core-collapse stripped-envelope supernova (SN) explosions reflect the diversity of physical parameters and evolutionary paths of their massive star progenitors. We have observed the Type Ic SN iPTF15dld (z = 0.047), reported by the Palomar Transient Factory. Spectra were taken starting 20 rest-frame days after maximum luminosity and are affected by a young stellar population background. Broad spectral absorption lines associated with the SN are detected over the continuum, similar to those measured for broad-lined, highly energetic SNe Ic. The light curve and maximum luminosity are instead more similar to those of low luminosity, narrow-lined Ic SNe. This suggests a behaviour whereby certain highly stripped-envelope SNe do not produce a large amount of ^(56)Ni, but the explosion is sufficiently energetic that a large fraction of the ejecta is accelerated to higher than usual velocities. We estimate SN iPTF15dld had a main-sequence progenitor of 20\u201325 M\u2299, produced a ^(56)Ni mass of \u223c0.1\u20130.2 M\u2299, had an ejecta mass of [2\u201310] M\u2299, and a kinetic energy of [1\u201318] \u00d7 10^(51) erg.", "date": "2017-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "466", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1848-1856", "id_number": "CaltechAUTHORS:20190528-153917372", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190528-153917372", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AR65G" }, { "agency": "NASA", "grant_number": "NNX14AM74G" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/088/06/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Danish Agency for Science and Technology and Innovation" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "RBFR12PM1F" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stw3247", "primary_object": { "basename": "1612.03275.pdf", "url": "https://authors.library.caltech.edu/records/6h451-jw951/files/1612.03275.pdf" }, "pub_year": "2017", "author_list": "Pian, E.; Tomasella, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/wm0rj-vwf41", "eprint_id": 95837, "eprint_status": "archive", "datestamp": "2023-08-19 01:59:45", "lastmod": "2023-10-20 20:37:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Villarroel-B", "name": { "family": "Villarroel", "given": "Beatriz" } }, { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "Anders" } }, { "id": "Karlsson-T", "name": { "family": "Karlsson", "given": "Torgny" } }, { "id": "Comer\u00f3n-S", "name": { "family": "Comer\u00f3n", "given": "S\u00e9bastien" } }, { "id": "Korn-A-J", "name": { "family": "Korn", "given": "Andreas J." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "id": "Zackrisson-E", "name": { "family": "Zackrisson", "given": "Erik" }, "orcid": "0000-0003-1096-2636" } ] }, "title": "AGN Luminosity and Stellar Age: Two Missing Ingredients for AGN Unification as Seen with iPTF Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 galaxies: nuclei \u2013 supernovae: general \u2013 surveys", "note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 August 18; revised 2017 January 19; accepted 2017 January 29; published 2017 March 8.\n\nB.V. wishes to thank Kjell Lundgren for early discussions about the work. She also wishes to thank Martin Gaskell and Robert R.J. Antonucci and for many constructive and helpful comments, and finally to acknowledge A. Magnard, C. Franck, G. von Rivia, and J. Pianist for inspiring discussions. A.N. wishes to thank Ariel Goobar for useful suggestions. B.V. was funded and supported by the Center of Interdisciplinary Mathematics (Uppsala Universitet) and Erik and M\u00e4rta Holmbergs donation from the Kungliga Fysiografiska S\u00e4llskapet. Supernova research at the Oskar Klein Centre is supported by the Swedish Research Council and by the Knut and Alice Wallenberg Foundation. The intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Centre, 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. 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 also heavily relies on the Sloan Digital Sky Survey (SDSS). Funding for SDSS-II has been provided by the Alfred P Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.\n\nAccepted Version - 1701.08647.pdf
", "abstract": "Active galactic nuclei (AGNs) are extremely powerful cosmic objects, driven by accretion of hot gas upon super-massive black holes. The zoo of AGN classes is divided into two major groups, with Type-1 AGNs displaying broad Balmer emission lines and Type-2 narrow ones. For a long time it was believed that a Type-2 AGN is a Type-1 AGN viewed through a dusty kiloparsec-sized torus, but an emerging body of observations suggests more than just the viewing angle matters. Here we report significant differences in supernova (SN) counts and classes in the first study to date of SNe near Type-1 and Type-2 AGN host galaxies, using data from the intermediate Palomar Transient Factory, the Sloan Digital Sky Survey Data Release 7, and Galaxy Zoo. We detect many more SNe in Type-2 AGN hosts (size of effect ~5.1\u03c3) compared to Type-1 hosts, which shows that the two classes of AGN are located inside host galaxies with different properties. In addition, Type-1 and Type-2 AGNs that are dominated by star formation according to Wide-field Infrared Survey Explorer colors m_(W1)\u2212m_(W2) < 0.5 and are matched in 22 \u03bcm absolute magnitude differ by a factor of ten in L[O III] \u03bb5007 luminosity, suggesting that when residing in similar types of host galaxies Type-1 AGNs are much more luminous. Our results demonstrate two more factors that play an important role in completing the current picture: the age of stellar populations and the AGN luminosity. This has immediate consequences for understanding the many AGN classes and galaxy evolution.", "date": "2017-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "837", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 110", "id_number": "CaltechAUTHORS:20190528-155748288", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190528-155748288", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Uppsala Universitet" }, { "agency": "Kungliga Fysiografiska S\u00e4llskapet" }, { "agency": "Swedish Research Council" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "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" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "Palomar-Transient-Factory", "value": "Palomar Transient Factory" } ] }, "doi": "10.3847/1538-4357/aa5d5a", "primary_object": { "basename": "1701.08647.pdf", "url": "https://authors.library.caltech.edu/records/wm0rj-vwf41/files/1701.08647.pdf" }, "pub_year": "2017", "author_list": "Villarroel, Beatriz; Nyholm, Anders; et el." }, { "id": "https://authors.library.caltech.edu/records/y9qcs-1k259", "eprint_id": 76615, "eprint_status": "archive", "datestamp": "2023-08-19 01:47:45", "lastmod": "2023-10-25 16:09:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soraisam-M-D", "name": { "family": "Soraisam", "given": "Monika D." } }, { "id": "Gilfanov-M", "name": { "family": "Gilfanov", "given": "Marat" } }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Shafter-A-W", "name": { "family": "Shafter", "given": "Allen W." } }, { "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": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" } ] }, "title": "A novel method for transient detection in high-cadence optical surveys Its application for a systematic search for novae in M31", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis, surveys, novae, cataclysmic variables, galaxies: individual: M 31", "note": "\u00a9 2017 ESO. \n\nReceived: 21 July 2016. Accepted: 28 November 2016. \n\nM.D.S. is grateful to Niels Oppermann (CITA) for helpful discussions on the Bayesian treatment of obtaining the probability distribution of false matches. M.D.S. thanks the California Institute of Technology, where a portion of this work was completed, for its hospitality. M.D.S. was supported, in part, by the GROWTH internship program funded by the National Science Foundation under Grant No. 1545949. A.W.S. is grateful to the NSF for financial support through grant AST-1009566. M.G. acknowledges partial support by Russian Scientific Foundation (RSF), project 14-22-00271.\n\nPublished - aa29368-16.pdf
Submitted - 1612.00116.pdf
", "abstract": "Context. In the present era of large-scale surveys in the time domain, the processing of data, from procurement up to the detection of sources, is generally automated. One of the main challenges in the astrophysical analysis of their output is contamination by artifacts, especially in the regions of high surface brightness of unresolved emission.\nAims. We present a novel method for identifying candidates for variable and transient sources from the outputs of optical time-domain survey data pipelines. We use the method to conduct a systematic search for novae in the intermediate Palomar Transient Factory (iPTF) observations of the bulge part of M\u200931 during the second half of 2013.\nMethods. We demonstrate that a significant fraction of artifacts produced by the iPTF pipeline form a locally uniform background of false detections approximately obeying Poissonian statistics, whereas genuine variable and transient sources, as well as artifacts associated with bright stars, result in clusters of detections whose spread is determined by the source localization accuracy. This makes the problem analogous to source detection on images produced by grazing incidence X-ray telescopes, enabling one to utilize the arsenal of powerful tools developed in X-ray astronomy. In particular, we use a wavelet-based source detection algorithm from the Chandra data analysis package CIAO.\nResults. Starting from ~2.5 \u00d7 10^5 raw detections made by the iPTF data pipeline, we obtain approximately 4000 unique source candidates. Cross-matching these candidates with the source-catalog of a deep reference image of the same field, we find counterparts for ~90% of the candidates. These sources are either artifacts due to imperfect PSF matching or genuine variable sources. The remaining approximately 400 detections are transient sources. We identify novae among these candidates by applying selection cuts to their lightcurves based on the expected properties of novae. Thus, we recovered all 12 known novae (not counting one that erupted toward the end of the survey) registered during the time span of the survey and discovered three nova candidates. Our method is generic and can be applied to mining any target out of the artifacts in optical time-domain data. As it is fully automated, its incompleteness can be accurately computed and corrected for.", "date": "2017-03", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "599", "publisher": "EDP Sciences", "pagerange": "Art. No. A48", "id_number": "CaltechAUTHORS:20170417-142352019", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170417-142352019", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "1545949" }, { "agency": "NSF", "grant_number": "AST-1009566" }, { "agency": "Russian Science Foundation", "grant_number": "14-22-00271" } ] }, "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": "10.1051/0004-6361/201629368", "primary_object": { "basename": "1612.00116.pdf", "url": "https://authors.library.caltech.edu/records/y9qcs-1k259/files/1612.00116.pdf" }, "related_objects": [ { "basename": "aa29368-16.pdf", "url": "https://authors.library.caltech.edu/records/y9qcs-1k259/files/aa29368-16.pdf" } ], "pub_year": "2017", "author_list": "Soraisam, Monika D.; Gilfanov, Marat; et el." }, { "id": "https://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" }, "pub_year": "2017", "author_list": "Waszczak, Adam; Prince, Thomas A.; et el." }, { "id": "https://authors.library.caltech.edu/records/yn8a4-45584", "eprint_id": 75572, "eprint_status": "archive", "datestamp": "2023-08-19 01:46:25", "lastmod": "2023-10-25 15:09:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Marsh-F-M", "name": { "family": "Marsh", "given": "F. M." } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A. A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E. C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "A. J." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" } ] }, "title": "Characterization of 9380 contact binaries from the CRTS Variable Sources Catalogue", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys, binaries: eclipsing, stars: magnetic field", "note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 August 19. Received 2016 August 18; in original form 2016 June 20. \n\nThis work made use of data products from the CSS survey. The CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the US National Science Foundation under grants AST-0909182, AST-1313422, AST-1413600, and AST-1518308. \n\nThis work made use of data products from the SDSS-III survey. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. \n\nSDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. \n\nI would like to acknowledge the California Institute of Technology Summer Undergraduate Research Fellowship program for their financial support. I thank an anonymous reviewer for providing comments which greatly improved the paper. I thank James Davenport and Lynne Hillenbrand for their helpful comments, Jake VanderPlas for his help with gatspy, and John McBride for his help preparing the manuscript.\n\nPublished - stw2110.pdf
Supplemental Material - stw2110_Supp.zip
", "abstract": "We construct a sample of 9380 contact binaries (W UMa systems) by using the Catalina Real-Time Transient Survey Variables Sources Catalogue. By measuring brightness change rates, light-curve statistics, and temperatures for this sample, we improve the understanding of contact binary light-curve characteristics, and luminosity variability on decadal time-scales. We show that binaries with convective outer envelopes have a different distribution of light-curve amplitudes and magnitude differences between eclipse minima than binaries with radiative outer envelopes. We find that more than 2000 binaries exhibit a linear change in mean brightness over the 8-yr timespan of observations with at least 3\u03c3 significance. We note that 25.9 per cent of binaries with convective outer envelopes exhibit a significant change in brightness, while only 10.5 per cent of radiative binaries exhibit a significant change in brightness. In 205 binaries (2.2 per cent), we find that a sinusoid model better describes the luminosity trend within the 8-yr observation timespan. For these binaries, we report the amplitudes and periods (as estimated using observed half-periods) of this sinusoidal brightness variation and discuss possible mechanisms driving the variation.", "date": "2017-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "465", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "4678-4689", "id_number": "CaltechAUTHORS:20170331-095838217", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-095838217", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "NSF", "grant_number": "AST-1313422" }, { "agency": "NSF", "grant_number": "AST-1413600" }, { "agency": "NSF", "grant_number": "AST-1518308" }, { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "Palomar-Transient-Factory", "value": "Palomar Transient Factory" }, { "id": "Astronomy-Department", "value": "Astronomy Department" } ] }, "doi": "10.1093/mnras/stw2110", "primary_object": { "basename": "stw2110.pdf", "url": "https://authors.library.caltech.edu/records/yn8a4-45584/files/stw2110.pdf" }, "related_objects": [ { "basename": "stw2110_Supp.zip", "url": "https://authors.library.caltech.edu/records/yn8a4-45584/files/stw2110_Supp.zip" } ], "pub_year": "2017", "author_list": "Marsh, F. M.; Prince, T. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/dh56b-cpe15", "eprint_id": 80586, "eprint_status": "archive", "datestamp": "2023-08-19 01:52:35", "lastmod": "2023-10-17 16:32:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas" }, "orcid": "0000-0001-5390-8563" } ] }, "title": "The unblinking eye on the sky", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2017 Macmillan Publishers Limited, part of Springer Nature. \n\nPublished: 2 March 2017.", "abstract": "The Zwicky Transient Facility (ZTF) is a next-generation optical synoptic survey motivated by the search for rare and fast-evolving optical transients. ZTF succeeds the Palomar Transient Factory (PTF) survey and the intermediate Palomar Transient Factory (iPTF) survey on the 48-inch Samuel Oschin Schmidt Telescope (P48) at Palomar Observatory. The PTF began operations in 2009, emphasizing large area surveys to characterize the optical transient sky. The iPTF has operated for the past four years, emphasizing same-night multicolour follow-up of transient candidates, most recently using a novel ultralow-resolution spectrograph on the robotic Palomar 60-inch telescope (P60). The survey camera on the P48 (CFH12K, originally used on the Canada\u2013France\u2013Hawaii Telescope) had a field of view of eight deg^2.", "date": "2017-03", "date_type": "published", "publication": "Nature Astronomy", "volume": "1", "number": "3", "publisher": "Nature Publishing Group", "pagerange": "Art. No. 0071", "id_number": "CaltechAUTHORS:20170817-160656851", "issn": "2397-3366", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170817-160656851", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/s41550-017-0071", "pub_year": "2017", "author_list": "Bellm, Eric and Kulkarni, Shrinivas" }, { "id": "https://authors.library.caltech.edu/records/yzsa4-04e10", "eprint_id": 74452, "eprint_status": "archive", "datestamp": "2023-08-19 01:36:18", "lastmod": "2023-10-24 22:39:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "Griffin" }, "orcid": "0000-0002-0832-2974" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Duggan-G-E", "name": { "family": "Duggan", "given": "Gina" }, "orcid": "0000-0002-9256-6735" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi" }, "orcid": "0000-0002-5619-4938" }, { "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": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Type Ibn Supernovae Show Photometric Homogeneity and Spectral Diversity at Maximum Light", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (PTF11rfh, PTF12ldy, iPTF14aki, SN 2015U, iPTF15ul, SN 2015G, iPTF15akq)", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 August 3; revised 2016 August 29; accepted 2016 August 31; published 2017 February 16. \n\nThis work 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 intermediate Palomar Transient Factory (iPTF) project, a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin\u2013Milwaukee, 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; the New Technology Telescope, operated by the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of PESSTO, ESO program 191.D-0935(C); the Las Cumbres Observatory Global Telescope Network; both the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association, and the Telescopio Nazionale Galileo, operated by the Fundaci\u00f3n Galileo Galilei of the Italian Istituto Nazionale di Astrofisica, at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrof\u00edsica de Canarias; the Lick Observatory owned and operated by the University of California; and the W. M. Keck Observatory, which was made possible by the generous financial support of the W. M. Keck Foundation and is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). We thank the staffs at all of these observatories for their assistance with the observations. \n\nWe thank Lars Bildsten and Matteo Cantiello for useful discussions, and all those whose observations and data reduction contributed to this work. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The authors made extensive use of the Astropy package Astropy Collaboration et al. (2013) for data analysis. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. LANL participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program. \n\nG.H., D.A.H., and C.M. are supported by the National Science Foundation (NSF) under Grant No. 1313484. \n\nA.P., S.B., and N.E.R. are partially supported by PRIN-INAF 2014 with the project \"Transient universe: unveiling new types of stellar explosions with PESSTO.\" \n\nJ.S., C.F., E.K., and F.T. gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. \n\nM.F., A.G.-Y., and M.S. acknowledge support from the European Union FP7 programme through ERC grant numbers 320360, 307260, and 615929, respectively. A.G.-Y. is also supported by the Quantum universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and YeS awards. \n\nA.C. acknowledges support from NSF CAREER award #1455090. \n\nM.M.K. acknowledges support from NSF PIRE program grant 1545949. \n\nThe supernova research of A.V.F.'s group at UC Berkeley is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST\u20131211916. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google.\n\nPublished - Hosseinzadeh_2017_ApJ_836_158.pdf
Submitted - 1608.01998.pdf
", "abstract": "Type Ibn supernovae (SNe) are a small yet intriguing class of explosions whose spectra are characterized by low-velocity helium emission lines with little to no evidence for hydrogen. The prevailing theory has been that these are the core-collapse explosions of very massive stars embedded in helium-rich circumstellar material (CSM). We report optical observations of six new SNe Ibn: PTF11rfh, PTF12ldy, iPTF14aki, iPTF15ul, SN 2015G, and iPTF15akq. This brings the sample size of such objects in the literature to 22. We also report new data, including a near-infrared spectrum, on the Type Ibn SN 2015U. In order to characterize the class as a whole, we analyze the photometric and spectroscopic properties of the full Type Ibn sample. We find that, despite the expectation that CSM interaction would generate a heterogeneous set of light curves, as seen in SNe IIn, most Type Ibn light curves are quite similar in shape, declining at rates around 0.1 mag day^(\u22121) during the first month after maximum light, with a few significant exceptions. Early spectra of SNe Ibn come in at least two varieties, one that shows narrow P Cygni lines and another dominated by broader emission lines, both around maximum light, which may be an indication of differences in the state of the progenitor system at the time of explosion. Alternatively, the spectral diversity could arise from viewing-angle effects or merely from a lack of early spectroscopic coverage. Together, the relative light curve homogeneity and narrow spectral features suggest that the CSM consists of a spatially confined shell of helium surrounded by a less dense extended wind.", "date": "2017-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "836", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 158", "id_number": "CaltechAUTHORS:20170222-081843865", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-081843865", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "European Research Council (ERC)", "grant_number": "320360" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "YeS Award" }, { "agency": "NSF", "grant_number": "AST-1455090" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/836/2/158", "primary_object": { "basename": "1608.01998.pdf", "url": "https://authors.library.caltech.edu/records/yzsa4-04e10/files/1608.01998.pdf" }, "related_objects": [ { "basename": "Hosseinzadeh_2017_ApJ_836_158.pdf", "url": "https://authors.library.caltech.edu/records/yzsa4-04e10/files/Hosseinzadeh_2017_ApJ_836_158.pdf" } ], "pub_year": "2017", "author_list": "Hosseinzadeh, Griffin; Cao, Yi; et el." }, { "id": "https://authors.library.caltech.edu/records/cxbgs-c1y16", "eprint_id": 95840, "eprint_status": "archive", "datestamp": "2023-08-19 01:37:03", "lastmod": "2023-10-20 20:37:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zackay-B", "name": { "family": "Zackay", "given": "Barak" } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" } ] }, "title": "How to COAAD Images. II. A Coaddition Image that is Optimal for Any Purpose in the Background-dominated Noise Limit", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak \u2013 instrumentation: high angular resolution \u2013 methods: data analysis \u2013 methods: statistical \u2013 techniques: image processing \u2013 techniques: photometric", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2015 December 6; revised 2016 October 21; accepted 2016 December 28; published 2017 February 21. \n\nWe thank Avishay Gal-Yam, Guy Nir, Ora Zackay, Maayane Soumagnac, Adam Rubin, Frank Masci, Dovi Poznanski, and Assaf Horesh for their comments and suggestions. We thank Guy Nir and Ilan Manulis for help with obtaining the speckle images presented here. B.Z. is grateful for receiving the Clore fellowship. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF).\n\nSubmitted - 1512.06879.pdf
", "abstract": "Image coaddition is one of the most basic operations that astronomers perform. In Paper I, we presented the optimal ways to coadd images in order to detect faint sources and to perform flux measurements under the assumption that the noise is approximately Gaussian. Here, we build on these results and derive from first principles a coaddition technique that is optimal for any hypothesis testing and measurement (e.g., source detection, flux or shape measurements, and star/galaxy separation), in the background-noise-dominated case. This method has several important properties. The pixels of the resulting coadded image are uncorrelated. This image preserves all the information (from the original individual images) on all spatial frequencies. Any hypothesis testing or measurement that can be done on all the individual images simultaneously, can be done on the coadded image without any loss of information. The PSF of this image is typically as narrow, or narrower than the PSF of the best image in the ensemble. Moreover, this image is practically indistinguishable from a regular single image, meaning that any code that measures any property on a regular astronomical image can be applied to it unchanged. In particular, the optimal source detection statistic derived in Paper I is reproduced by matched filtering this image with its own PSF. This coaddition process, which we call proper coaddition, can be understood as the maximum signal-to-noise ratio measurement of the Fourier transform of the image, weighted in such a way that the noise in the entire Fourier domain is of equal variance. This method has important implications for multi-epoch seeing-limited deep surveys, weak lensing galaxy shape measurements, and diffraction-limited imaging via speckle observations. The last topic will be covered in depth in future papers. We provide an implementation of this algorithm in MATLAB.", "date": "2017-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "836", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 188", "id_number": "CaltechAUTHORS:20190529-074656999", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-074656999", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Weizmann Institute of Science" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/1538-4357/836/2/188", "primary_object": { "basename": "1512.06879.pdf", "url": "https://authors.library.caltech.edu/records/cxbgs-c1y16/files/1512.06879.pdf" }, "pub_year": "2017", "author_list": "Zackay, Barak and Ofek, Eran O." }, { "id": "https://authors.library.caltech.edu/records/c57s0-9y491", "eprint_id": 95841, "eprint_status": "archive", "datestamp": "2023-08-19 01:37:11", "lastmod": "2023-10-20 20:38:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zackay-B", "name": { "family": "Zackay", "given": "Barak" } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" } ] }, "title": "How to COAAD Images. I. Optimal Source Detection and Photometry of Point Sources Using Ensembles of Images", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 gravitational lensing: weak \u2013 methods: data analysis \u2013 surveys \u2013 techniques: image processing \u2013 techniques: photometric", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2015 December 6; revised 2016 October 21; accepted 2016 December 28; published 2017 February 21. \n\nWe thank Avishay Gal-Yam, Assaf Horesh, Frank Masci, William Newman, and Ora Zackay for discussions. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. B.Z. is grateful for receiving the Clore fellowship. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF).\n\nSubmitted - 1512.06872.pdf
", "abstract": "Stacks of digital astronomical images are combined in order to increase image depth. The variable seeing conditions, sky background, and transparency of ground-based observations make the coaddition process nontrivial. We present image coaddition methods that maximize the signal-to-noise ratio (S/N) and optimized for source detection and flux measurement. We show that for these purposes, the best way to combine images is to apply a matched filter to each image using its own point-spread function (PSF) and only then to sum the images with the appropriate weights. Methods that either match the filter after coaddition or perform PSF homogenization prior to coaddition will result in loss of sensitivity. We argue that our method provides an increase of between a few and 25% in the survey speed of deep ground-based imaging surveys compared with weighted coaddition techniques. We demonstrate this claim using simulated data as well as data from the Palomar Transient Factory data release 2. We present a variant of this coaddition method, which is optimal for PSF or aperture photometry. We also provide an analytic formula for calculating the S/N for PSF photometry on single or multiple observations. In the next paper in this series, we present a method for image coaddition in the limit of background-dominated noise, which is optimal for any statistical test or measurement on the constant-in-time image (e.g., source detection, shape or flux measurement, or star\u2013galaxy separation), making the original data redundant. We provide an implementation of these algorithms in MATLAB.", "date": "2017-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "836", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 187", "id_number": "CaltechAUTHORS:20190529-075432034", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-075432034", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Weizmann Institute of Science" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "Palomar-Transient-Factory", "value": "Palomar Transient Factory" } ] }, "doi": "10.3847/1538-4357/836/2/187", "primary_object": { "basename": "1512.06872.pdf", "url": "https://authors.library.caltech.edu/records/c57s0-9y491/files/1512.06872.pdf" }, "pub_year": "2017", "author_list": "Zackay, Barak and Ofek, Eran O." }, { "id": "https://authors.library.caltech.edu/records/gh5td-07e45", "eprint_id": 95839, "eprint_status": "archive", "datestamp": "2023-08-19 01:30:12", "lastmod": "2023-10-20 20:37:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tartaglia-L", "name": { "family": "Tartaglia", "given": "L." }, "orcid": "0000-0003-3433-1492" }, { "id": "Fraser-M", "name": { "family": "Fraser", "given": "M." }, "orcid": "0000-0003-2191-1674" }, { "id": "Sand-D-J", "name": { "family": "Sand", "given": "D. J." }, "orcid": "0000-0003-4102-380X" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Smartt-S-J", "name": { "family": "Smartt", "given": "S. J." }, "orcid": "0000-0002-8229-1731" }, { "id": "McCully-C", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Anderson-J-P", "name": { "family": "Anderson", "given": "J. P." }, "orcid": "0000-0003-0227-3451" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Elias-Rosa-N", "name": { "family": "Elias-Rosa", "given": "N." }, "orcid": "0000-0002-1381-9125" }, { "id": "Galbany-L", "name": { "family": "Galbany", "given": "L." }, "orcid": "0000-0002-1296-6887" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Haislip-J-B", "name": { "family": "Haislip", "given": "J" } }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Inserra-C", "name": { "family": "Inserra", "given": "C." }, "orcid": "0000-0002-3968-4409" }, { "id": "Jha-S-W", "name": { "family": "Jha", "given": "S. W." }, "orcid": "0000-0001-8738-6011" }, { "id": "Kankare-E", "name": { "family": "Kankare", "given": "E." }, "orcid": "0000-0001-8257-3512" }, { "id": "Lundqvist-P", "name": { "family": "Lundqvist", "given": "P." }, "orcid": "0000-0002-3664-8082" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Mattila-S", "name": { "family": "Mattila", "given": "S." }, "orcid": "0000-0001-7497-2994" }, { "id": "Reichart-D-E", "name": { "family": "Reichart", "given": "D." }, "orcid": "0000-0002-5060-3673" }, { "id": "Smith-K-W", "name": { "family": "Smith", "given": "K. W." } }, { "id": "Smith-M", "name": { "family": "Smith", "given": "M." }, "orcid": "0000-0002-3321-1432" }, { "id": "Stritzinger-M-D", "name": { "family": "Stritzinger", "given": "M." }, "orcid": "0000-0002-5571-1833" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Tomasella-L", "name": { "family": "Tomasella", "given": "L." } } ] }, "title": "Progenitor and Early Evolution of the Type IIb SN 2016gkg", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (2016gkg)", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 2; revised 2017 January 11; accepted 2017 January 25; published 2017 February 10. \n\nBased on data from: ESO as part of PESSTO (197.D-1075.191.D-0935) and under programme 097.D-0762(A). Gemini Observatory under GS-2016B-Q-22 (PI: Sand). The Nordic Optical Telescope of the Instituto de Astrof\u00edsica de Canarias. The European Organisation for Astronomical Research in the southern hemisphere under ESO programme 198.A-0915(A). FOSCGUI is a graphic user interface aimed at extracting SN spectroscopy and photometry obtained with FOSC-like instruments, developed by E. Cappellaro. D.J.S. acknowledges NSF grants AST-1412504 and AST-1517649. S.J.S. acknowledges EU/FP7-ERC grant 29122. M.F. acknowledges the support of a Royal Society\u2014Science Foundation Ireland University Research Fellowship. L.G. was supported in part by the US National Science Foundation under grant AST-1311862. M.S. acknowledges support from EU/FP7-ERC grant number 615929. K.M. acknowledges support from STFC through an Ernest Rutherford Fellowship. D.A.H., C.M., and G.H. are funded by NSF AST-1313484. Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. N.E.R. acknowledges financial support by the 1994 PRIN-INAF 2014 (project \"Transient universe: unveiling new types of stellar explosions with PESSTO\") and by MIUR PRIN 2010-2011, \"The dark universe and the cosmic evolution of baryons: from current surveys to Euclid.\" M.S. acknowledges support from the Danish Agency for Science and Technology and Innovation via a Sapere Aude Level 2 grant, the Villum foundation, and the Instrumentcenter for Danish Astrophysics (IDA).\n\nSubmitted - 1611.00419.pdf
", "abstract": "We report initial observations and analysis on the Type IIb SN 2016gkg in the nearby galaxy NGC 613. SN 2016gkg exhibited a clear double-peaked light curve during its early evolution, as evidenced by our intensive photometric follow-up campaign. SN 2016gkg shows strong similarities with other Type IIb SNe, in particular, with respect to the He I emission features observed in both the optical and near-infrared. SN 2016gkg evolved faster than the prototypical Type IIb SN 1993J, with a decline similar to that of SN 2011dh after the first peak. The analysis of archival Hubble Space Telescope images indicate a pre-explosion source at SN 2016gkg's position, suggesting a progenitor star with a ~mid-F spectral type and initial mass 15-20 M\u2299, depending on the distance modulus adopted for NGC 613. Modeling the temperature evolution within 5 days of explosion, we obtain a progenitor radius of ~48-124 R\u2299, smaller than that obtained from the analysis of the pre-explosion images (240-320 R\u2299).", "date": "2017-02-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "836", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L12", "id_number": "CaltechAUTHORS:20190528-161442964", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190528-161442964", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1412504" }, { "agency": "NSF", "grant_number": "AST-1517649" }, { "agency": "European Research Council (ERC)", "grant_number": "29122" }, { "agency": "Royal Society" }, { "agency": "Science Foundation Ireland" }, { "agency": "NSF", "grant_number": "AST-1311862" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NSF", "grant_number": "AST-1313484" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Danish Agency for Science and Technology and Innovation" }, { "agency": "Villum Foundation" }, { "agency": "Instrumentcenter for Danish Astrophysics" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/2041-8213/aa5c7f", "primary_object": { "basename": "1611.00419.pdf", "url": "https://authors.library.caltech.edu/records/gh5td-07e45/files/1611.00419.pdf" }, "pub_year": "2017", "author_list": "Tartaglia, L.; Fraser, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/zt7z7-yyk21", "eprint_id": 74294, "eprint_status": "archive", "datestamp": "2023-08-19 01:29:26", "lastmod": "2023-10-24 22:27:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Hangard-L", "name": { "family": "Hangard", "given": "L." } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Parrent-J-T", "name": { "family": "Parrent", "given": "J. T." } }, { "id": "McCully-C", "name": { "family": "McCully", "given": "C." }, "orcid": "0000-0001-5807-7893" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Mulchaey-J-S", "name": { "family": "Mulchaey", "given": "J. S." } }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "S." }, "orcid": "0000-0001-6760-3074" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Fruchter-A-S", "name": { "family": "Fruchter", "given": "A. S." } }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Koda-Jin", "name": { "family": "Koda", "given": "J." }, "orcid": "0000-0002-8762-7863" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Yagi-Masafumi", "name": { "family": "Yagi", "given": "M." } }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" } ] }, "title": "Two New Calcium-rich Gap Transients in Group and Cluster Environments", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (PTF11kmb, PTF12bho, PTF10hcw, SN 2005E)", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 23; revised 2016 December 20; accepted 2016 December 21; published 2017 February 8. \n\nR.L. thanks Andrew Wetzler, Wen-fai Fong, Mark Sullivan, Dan Milisavljevic, Giorgos Leloudas, Jesper Sollerman, and Ryan Chornock for useful discussions and acknowledges helpful interactions with Lars Bildsten, Eliot Quataert, and Dan Kasen at a PTF Theory Network retreat funded by the Gordon and Betty Moore Foundation through Grant GBMF5076. We thank J. Silverman, B. Dilday, J. Bloom, B. Sesar, D. Levitan, P. Groot, D. Perley, A. Horesh, K. Mooley, and D. Xu for assisting with the observations presented in this paper. The Intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin\u2013Milwaukee, 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. Support for HST Program GO-13864 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the AURA, Inc., under NASA contract NAS 5-26555. We thank F. Yuan, M. Sullivan, D. Perley, R. M. Quimby, and S. B. Cenko for their contributions to the HST proposal. This work was supported by the GROWTH project funded by the National Science Foundation under Grant 1545949. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva and ISF grants, WIS-UK \"making connections,\" and Kimmel and YeS awards. A.V.F. is grateful for financial support from the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. D.A.H. and C.M. are supported by NSF grant AST-313484. 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. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacilities: PO:1.2m, PO:1.5m, PO:Hale, Keck:I, Keck:II, Subaru, HST.\n\nPublished - Lunnan_2017_ApJ_836_60.pdf
Submitted - 1612.00454.pdf
", "abstract": "We present the Palomar Transient Factory discoveries and the photometric and spectroscopic observations of PTF11kmb and PTF12bho. We show that both transients have properties consistent with the class of calcium-rich gap transients, specifically lower peak luminosities and rapid evolution compared to ordinary supernovae, and a nebular spectrum dominated by [Ca II] emission. A striking feature of both transients is their host environments: PTF12bho is an intracluster transient in the Coma Cluster, while PTF11kmb is located in a loose galaxy group, at a physical offset ~150 kpc from the most likely host galaxy. Deep Subaru imaging of PTF12bho rules out an underlying host system to a limit of M_R > -8.0 mag, while Hubble Space Telescope imaging of PTF11kmb reveals a marginal counterpart that, if real, could be either a background galaxy or a globular cluster. We show that the offset distribution of Ca-rich gap transients is significantly more extreme than that seen for SNe Ia or even short-hard gamma-ray bursts (sGRBs). Thus, if the offsets are caused by a kick, they require higher kick velocities and/or longer merger times than sGRBs. We also show that almost all Ca-rich transients found to date are in group and cluster environments with elliptical host galaxies, indicating a very old progenitor population; the remote locations could partially be explained by these environments having the largest fraction of stars in the intragroup/intracluster light following galaxy\u2013galaxy interactions.", "date": "2017-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "836", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 60", "id_number": "CaltechAUTHORS:20170214-095909820", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170214-095909820", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "YeS Award" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NSF", "grant_number": "AST-313484" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" } ] }, "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": "10.3847/1538-4357/836/1/60", "primary_object": { "basename": "Lunnan_2017_ApJ_836_60.pdf", "url": "https://authors.library.caltech.edu/records/zt7z7-yyk21/files/Lunnan_2017_ApJ_836_60.pdf" }, "related_objects": [ { "basename": "1612.00454.pdf", "url": "https://authors.library.caltech.edu/records/zt7z7-yyk21/files/1612.00454.pdf" } ], "pub_year": "2017", "author_list": "Lunnan, R.; Kasliwal, M. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/9k8b6-np546", "eprint_id": 73787, "eprint_status": "archive", "datestamp": "2023-08-19 01:21:15", "lastmod": "2023-10-24 16:27:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gezari-S", "name": { "family": "Gezari", "given": "S." }, "orcid": "0000-0003-3703-5154" }, { "id": "Hung-T-K", "name": { "family": "Hung", "given": "T." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K." }, "orcid": "0000-0002-2557-5180" }, { "id": "Kong-Albert-K-H", "name": { "family": "Kong", "given": "A. K. H." }, "orcid": "0000-0002-5105-344X" }, { "id": "Cantwell-T-M", "name": { "family": "Cantwell", "given": "T. M." } }, { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "P. C." }, "orcid": "0000-0001-8894-0854" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "C.-C." }, "orcid": "0000-0001-8771-7554" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "iPTF Discovery of the Rapid \"Turn-on\" of a Luminous Quasar", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks \u2013 black hole physics \u2013 galaxies: active \u2013 surveys", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 4; revised 2016 December 13; accepted 2016 December 13; published 2017 January 24. \n\nWe thank the anonymous referee for their helpful comments that improved the manuscript. S.G. is supported in part by NSF CAREER grant 1454816 and NASA Swift Cycle 12 grant NNX16AN85G. S.G. thanks Mike Koss for help with the X-ray data archives. These results made use of the Discovery Channel Telescope at Lowell Observatory. Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University, and Yale University. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. K.M.'s research is supported by the Oxford Centre for Astrophysical Surveys, which is funded through generous support from the Hintze Family Charitable Foundation. The AMI telescope gratefully acknowledges support from the European Research Council under grant ERC-2012- StG-307215 LODESTONE, the UK Science and Technology Facilities Council (STFC), and the University of Cambridge. We thank the AMI staff for scheduling the observations.\n\nPublished - Gezari_2017_ApJ_835_144.pdf
Submitted - 1612.04830v1.pdf
", "abstract": "We present a radio-quiet quasar at z = 0.237 discovered \"turning on\" by the intermediate Palomar Transient Factory (iPTF). The transient, iPTF 16bco, was detected by iPTF in the nucleus of a galaxy with an archival Sloan Digital Sky Survey spectrum with weak narrow-line emission characteristic of a low-ionization nuclear emission-line region (LINER). Our follow-up spectra show the dramatic appearance of broad Balmer lines and a power-law continuum characteristic of a luminous (L_(bol) \u2248 10^(45) erg s^(\u22121)) type 1 quasar 12 yr later. Our photometric monitoring with PTF from 2009\u20132012 and serendipitous X-ray observations from the XMM-Newton Slew Survey in 2011 and 2015 constrain the change of state to have occurred less than 500 days before the iPTF detection. An enhanced broad H\u03b1/[O III] \u03bb5007 line ratio in the type 1 state relative to other changing-look quasars also is suggestive of the most rapid change of state yet observed in a quasar. We argue that the >10 increase in Eddington ratio inferred from the brightening in UV and X-ray continuum flux is more likely due to an intrinsic change in the accretion rate of a preexisting accretion disk than an external mechanism such as variable obscuration, microlensing, or the tidal disruption of a star. However, further monitoring will be helpful in better constraining the mechanism driving this change of state. The rapid \"turn-on\" of the quasar is much shorter than the viscous infall timescale of an accretion disk and requires a disk instability that can develop around a ~ 10^8 M_\u2299 black hole on timescales less than 1 yr.", "date": "2017-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 144", "id_number": "CaltechAUTHORS:20170127-143119431", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-143119431", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1454816" }, { "agency": "NASA", "grant_number": "NNX16AN85G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Oxford Centre for Astrophysical Surveys" }, { "agency": "Hintze Family Charitable Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "307215" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "University of Cambridge" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Astronomy-Department" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/1538-4357/835/2/144", "primary_object": { "basename": "1612.04830v1.pdf", "url": "https://authors.library.caltech.edu/records/9k8b6-np546/files/1612.04830v1.pdf" }, "related_objects": [ { "basename": "Gezari_2017_ApJ_835_144.pdf", "url": "https://authors.library.caltech.edu/records/9k8b6-np546/files/Gezari_2017_ApJ_835_144.pdf" } ], "pub_year": "2017", "author_list": "Gezari, S.; Hung, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/mpsdx-2xf13", "eprint_id": 73788, "eprint_status": "archive", "datestamp": "2023-08-22 19:40:15", "lastmod": "2023-10-24 16:27:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "van-Roestel-J", "name": { "family": "van Roestel", "given": "Jan" }, "orcid": "0000-0002-2626-2872" }, { "id": "Brooks-J", "name": { "family": "Brooks", "given": "Jared" } }, { "id": "Geier-S", "name": { "family": "Geier", "given": "Stephan" }, "orcid": "0000-0002-3948-9339" }, { "id": "Marsh-T-R", "name": { "family": "Marsh", "given": "Tom R." }, "orcid": "0000-0002-2498-7589" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Bloemen-S", "name": { "family": "Bloemen", "given": "Steven" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Heber-U", "name": { "family": "Heber", "given": "Ulrich" }, "orcid": "0000-0001-7798-6769" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Dyer-M-J", "name": { "family": "Dyer", "given": "Martin J." } }, { "id": "Dhillon-V-S", "name": { "family": "Dhillon", "given": "Vik S." } }, { "id": "Green-M", "name": { "family": "Green", "given": "Matthew" } }, { "id": "Irawati-P", "name": { "family": "Irawati", "given": "Puji" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Littlefair-S-P", "name": { "family": "Littlefair", "given": "Stuart P." }, "orcid": "0000-0001-7221-855X" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "David L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" }, { "id": "Rattansoon-S", "name": { "family": "Rattansoon", "given": "Somsawat" } }, { "id": "Pettini-M", "name": { "family": "Pettini", "given": "Max" }, "orcid": "0000-0002-5139-4359" } ] }, "title": "PTF1 J082340.04+081936.5: A Hot Subdwarf B Star with a Low-mass White Dwarf Companion in an 87-minute Orbit", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; stars: individual (PTF1 J082340.04+081936.5); subdwarfs; white dwarfs", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 November 14; revised 2016 December 5; accepted 2016 December 6; published 2017 January 23. \n\nThis work was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. J.v.R. acknowledges support by the Netherlands Research School of Astronomy (NOVA) and the foundation for Fundamental Research on Matter (FOM). T.R.M. acknowledges the support from the Science and Technology Facilities Council (STFC), ST/L00733. This research was partially funded by the Gordon and Betty Moore Foundation through Grant GBMF5076 to Lars Bildsten. This work was supported by the National Science Foundation under grants PHY 11-25915, AST 11-09174, and AST 12-05574. This work was supported in part by the National Science Foundation under Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics where parts of this paper was written. We thank the referee for helpful and timely comments. \n\nObservations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the PTF project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some results presented in this paper are based on observations made with the WHT operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Institutio de Astrofisica de Canarias. \n\nSoftware: PyRAF (Bellm & Sesar 2016), MAKEE (http://www.astro.caltech.edu/tb/ipac staff/tab/makee/), Gatspy (VanderPlas & Ivezi\u0107 2015), LCURVE (Copperwheat et al. 2010), emcee (Foreman-Mackey et al. 2013), MESA (Paxton et al. 2011, 2013, 2015), FITSB2 (Napiwotzki et al. 2004).\n\nPublished - Kupfer_2017_ApJ_835_131.pdf
Accepted Version - 1612.02019.pdf
", "abstract": "We present the discovery of the hot subdwarf B star (sdB) binary PTF1 J082340.04+081936.5. The system has an orbital period of P_(orb) = 87.49668(1) minutes (0.060761584(10) days), making it the second-most compact sdB binary known. The light curve shows ellipsoidal variations. Under the assumption that the sdB primary is synchronized with the orbit, we find a mass of M_(sdB) = 0.45_(-0.07)^(+0.09) M_\u2299, a companion white dwarf mass of M_(WD) = 0.46_(-0.09)^(+0.12) M_\u2299, and a mass ratio of q = M_(WD)/M_(sdB) = 1.03_(-0.08)^(+0.10). The future evolution was calculated using the MESA stellar evolution code. Adopting a canonical sdB mass of M_(sdB) = 0.47 M_\u2299, we find that the sdB still burns helium at the time it will fill its Roche lobe if the orbital period was less than 106 minutes at the exit from the last common envelope (CE) phase. For longer CE exit periods, the sdB will have stopped burning helium and turned into a C/O white dwarf at the time of contact. Comparing the spectroscopically derived log g and T_(eff) with our MESA models, we find that an sdB model with a hydrogen envelope mass of 5 x 10^(-4) M_\u2299 matches the measurements at a post-CE age of 94 Myr, corresponding to a post-CE orbital period of 109 minutes, which is close to the limit to start accretion while the sdB is still burning helium.", "date": "2017-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 131", "id_number": "CaltechAUTHORS:20170127-143159985", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-143159985", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L00733" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF5076" }, { "agency": "NSF", "grant_number": "PHY 11-25915" }, { "agency": "NSF", "grant_number": "AST 11-09174" }, { "agency": "NSF", "grant_number": "AST 12-05574" }, { "agency": "NSF", "grant_number": "PHYS-1066293" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/835/2/131", "primary_object": { "basename": "1612.02019.pdf", "url": "https://authors.library.caltech.edu/records/mpsdx-2xf13/files/1612.02019.pdf" }, "related_objects": [ { "basename": "Kupfer_2017_ApJ_835_131.pdf", "url": "https://authors.library.caltech.edu/records/mpsdx-2xf13/files/Kupfer_2017_ApJ_835_131.pdf" } ], "pub_year": "2017", "author_list": "Kupfer, Thomas; van Roestel, Jan; et el." }, { "id": "https://authors.library.caltech.edu/records/4eyzq-s4g76", "eprint_id": 73792, "eprint_status": "archive", "datestamp": "2023-08-22 19:37:51", "lastmod": "2023-10-24 16:27:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Kulkarni-M-K", "name": { "family": "Kulkarni", "given": "M. K." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Preparing for Advanced LIGO: A Star\u2013Galaxy Separation Catalog for the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: statistics; methods: data analysis; methods: statistical; stars: statistics; surveys", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 August 30; revised 2016 November 16; accepted 2016 December 2; published 2017 January 16. \n\nThis project started as part of an undergraduate research project at the California Institute of Technology. We thank T. Prince for funding M.K.K. during the summer of 2015. \n\nWe are extremely grateful to A. Thakar and the entire SDSS CasJobs Helpdesk for assistance in performing the large cross-match between PTF and SDSS spectroscopic sources. Without their assistance this study would not have been possible. Without the patience and aid of R. Lupton we would not have been able to recreate the SDSS photometric classifier. We are in debt to M. M. Kasliwal, who endured countless conversations on the appropriate threshold for point-source classification. With gratitude, we salute S. B. Cenko for useful suggestions on the comparison of the NERSC catalog and the PTF RF catalog. Finally, we thank the anonymous referee for suggestions that improved this manuscript. \n\nA.A.M. acknowledges support for this work by NASA from 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\nFunding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. \n\nFacilities: Sloan, PO:1.2m.\n\nPublished - Miller_2017_AJ_153_73.pdf
", "abstract": "The search for fast optical transients, such as the expected electromagnetic counterparts to binary neutron star mergers, is riddled with false positives (FPs) ranging from asteroids to stellar flares. While moving objects are readily rejected via image pairs separated by ~1 hr, stellar flares represent a challenging foreground, significantly outnumbering rapidly evolving explosions. Identifying stellar sources close to and fainter than the transient detection limit can eliminate these FPs. Here, we present a method to reliably identify stars in deep co-adds of Palomar Transient Factory (PTF) imaging. Our machine-learning methodology utilizes the random forest (RF) algorithm, which is trained using > 3 x 10^6 sources with Sloan Digital Sky Survey (SDSS) spectra. When evaluated on an independent test set, the PTF RF model outperforms the SExtractor star classifier by ~4%. For faint sources (r' \u2265 21 mag), which dominate the field population, the PTF RF model produces a ~19% improvement over SExtractor. To avoid false negatives in the PTF transient-candidate stream, we adopt a conservative stellar classification threshold, corresponding to a galaxy misclassification rate of 0.005. Ultimately, 1.70 x 10^8 objects are included in our PTF point-source catalog, of which only ~10^6 are expected to be galaxies. We demonstrate that the PTF RF catalog reveals transients that otherwise would have been missed. To leverage its superior image quality, we additionally create an SDSS point-source catalog, which is also tuned to have a galaxy misclassification rate of 0.005. These catalogs have been incorporated into the PTF real-time pipelines to automatically reject stellar sources as non-extragalactic transients.", "date": "2017-02", "date_type": "published", "publication": "Astronomical Journal", "volume": "153", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 73", "id_number": "CaltechAUTHORS:20170127-151845228", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-151845228", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51325.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-3881/153/2/73", "primary_object": { "basename": "Miller_2017_AJ_153_73.pdf", "url": "https://authors.library.caltech.edu/records/4eyzq-s4g76/files/Miller_2017_AJ_153_73.pdf" }, "pub_year": "2017", "author_list": "Miller, A. A.; Kulkarni, M. K.; et el." }, { "id": "https://authors.library.caltech.edu/records/9pnv4-jrw44", "eprint_id": 73569, "eprint_status": "archive", "datestamp": "2023-08-19 01:08:20", "lastmod": "2023-10-24 15:28:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "Paul M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "Ragnhild" }, "orcid": "0000-0001-9454-4639" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" } ] }, "title": "On the Early-time Excess Emission in Hydrogen-poor Superluminous Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (PTF 12dam, iPTF 13dcc)", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 September 21; revised 2016 November 29; accepted 2016 November 29; published 2017 January 18. \n\nThe Dark Cosmology Centre is funded by the DNRF. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, GIF, Minerva, and ISF grants, WIS-UK \"making connections,\" and Kimmel and ARCHES awards. Support for D.A.P. was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. M.S. acknowledges support from EU/FP7-ERC grant 615929. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation, Minerva, and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. Support for I.A. was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. A.V.F.'s supernova group at UC Berkeley is supported through NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. 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\nPublished - Vreeswijk_2017_ApJ_835_58.pdf
Submitted - 1609.08145v3.pdf
", "abstract": "We present the light curves of the hydrogen-poor superluminous supernovae (SLSNe I) PTF 12dam and iPTF 13dcc, discovered by the (intermediate) Palomar Transient Factory. Both show excess emission at early times and a slowly declining light curve at late times. The early bump in PTF 12dam is very similar in duration (~10 days) and brightness relative to the main peak (2\u20133 mag fainter) compared to that observed in other SLSNe I. In contrast, the long-duration (>30 days) early excess emission in iPTF 13dcc, whose brightness competes with that of the main peak, appears to be of a different nature. We construct bolometric light curves for both targets, and fit a variety of light-curve models to both the early bump and main peak in an attempt to understand the nature of these explosions. Even though the slope of the late-time decline in the light curves of both SLSNe is suggestively close to that expected from the radioactive decay of ^(56)Ni and ^(56)Co, the amount of nickel required to power the full light curves is too large considering the estimated ejecta mass. The magnetar model including an increasing escape fraction provides a reasonable description of the PTF 12dam observations. However, neither the basic nor the double-peaked magnetar model is capable of reproducing the light curve of iPTF 13dcc. A model combining a shock breakout in an extended envelope with late-time magnetar energy injection provides a reasonable fit to the iPTF 13dcc observations. Finally, we find that the light curves of both PTF 12dam and iPTF 13dcc can be adequately fit with the model involving interaction with the circumstellar medium.", "date": "2017-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 58", "id_number": "CaltechAUTHORS:20170120-095849262", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170120-095849262", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Danish National Research Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Funding" }, { "agency": "Israel Science Foundation" }, { "agency": "GIF (Israel)" }, { "agency": "MINERVA (Israel)" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51296.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF6-170148" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "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": "10.3847/1538-4357/835/1/58", "primary_object": { "basename": "1609.08145v3.pdf", "url": "https://authors.library.caltech.edu/records/9pnv4-jrw44/files/1609.08145v3.pdf" }, "related_objects": [ { "basename": "Vreeswijk_2017_ApJ_835_58.pdf", "url": "https://authors.library.caltech.edu/records/9pnv4-jrw44/files/Vreeswijk_2017_ApJ_835_58.pdf" } ], "pub_year": "2017", "author_list": "Vreeswijk, Paul M.; Perley, Daniel A.; et el." }, { "id": "https://authors.library.caltech.edu/records/9dg5t-y8516", "eprint_id": 95842, "eprint_status": "archive", "datestamp": "2023-08-19 01:09:25", "lastmod": "2023-10-20 20:38:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jerkstrand-A", "name": { "family": "Jerkstrand", "given": "A." } }, { "id": "Smartt-S-J", "name": { "family": "Smartt", "given": "S. J." }, "orcid": "0000-0002-8229-1731" }, { "id": "Inserra-C", "name": { "family": "Inserra", "given": "C." }, "orcid": "0000-0002-3968-4409" }, { "id": "Nicholl-M", "name": { "family": "Nicholl", "given": "M." }, "orcid": "0000-0002-2555-3192" }, { "id": "Chen-Ting-Wan", "name": { "family": "Chen", "given": "T.-W." }, "orcid": "0000-0002-1066-6098" }, { "id": "Kr\u00fchler-T", "name": { "family": "Kr\u00fchler", "given": "T." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taubenberger-S", "name": { "family": "Taubenberger", "given": "S." }, "orcid": "0000-0002-4265-1958" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Kankare-E", "name": { "family": "Kankare", "given": "E." }, "orcid": "0000-0001-8257-3512" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Fraser-M", "name": { "family": "Fraser", "given": "M." }, "orcid": "0000-0003-2191-1674" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Cartier-R", "name": { "family": "Cartier", "given": "R." } }, { "id": "Young-D-R", "name": { "family": "Young", "given": "D. R." } } ] }, "title": "Long-duration superluminous supernovae at late times", "ispublished": "pub", "full_text_status": "public", "keywords": "nuclear reactions, nucleosynthesis, abundances \u2013 supernovae: general \u2013 supernovae: individual (SN 2007bi, LSQ14an, SN 2015bn) \u2013 radiative transfer", "note": "\u00a9 2017 The American Astronomical Society.\n\nReceived 2016 August 9; revised 2016 November 28; accepted 2016 November 28; published 2017 January 16.\n\nWe thank S. Blinnikov, C. Fransson, A. Kozyreva, P Mazzali, and C. Harris for discussion. A.J. thanks the organisers and participants of MIAPP conference \"The Physics of Supernovae\" and the workshop \"Supernovae: The Outliers\" for stimulating discussions. A.J. acknowledges funding by the European Union's Framework Programme for Research and Innovation Horizon 2020 under Marie Sklodowska-Curie grant agreement No 702538, and Science and Technology Facilities Council DIRAC computing grants ACSP45 and ACSP74. 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)/ERfC Grant agreement no [291222]. Agreements 307260, 320360, and 615929 are also acknowledged. SJS acknowledges funding from STFC grants ST/I001123/1 and ST/L000709/1. This work is based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO program 188.D-3003, 191.D-0935 and on the VLT ESO Programmes 094.A-0645, 096.D-0191and 296.D-5042. K.M. acknowledges support from the STFC through an Ernest Rutherford Fellowship. S.T. acknowledges support by TRR 33 The Dark universe of the German Research Foundation. T.-W.C. and T.K. acknowledge the support through the Sofia Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation of Germany. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We have made use of the Weizmann interactive supernova data repository-http://wiserep.weizmann.ac.il. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE) and the Los Alamos National Laboratory.\n\nAccepted Version - 1608.02994.pdf
", "abstract": "Nebular-phase observations and spectral models of Type Ic superluminous supernovae (SLSNe) are presented. LSQ14an and SN 2015bn both display late-time spectra similar to galaxy-subtracted spectra of SN 2007bi, and the class shows strong similarity with broad-lined SNe Ic such as SN 1998bw. Near-infrared observations of SN 2015bn show a strong Ca II triplet, O I 9263, O I 1.13 \u03bcm, and Mg I 1.50 \u03bcm, but no distinct He, Si, or S emission. The high Ca II NIR/[Ca II] 7291, 7323 ratio of ~2 indicates a high electron density of n_e \u2273 10^8 cm\u22123. Spectral models of oxygen-zone emission are investigated to put constraints on the emitting region. Models require M(O-zone) \u2273 10 M\u2299 to produce enough [O I] 6300, 6364 luminosity, irrespective of the powering situation and the density. The high oxygen-zone mass, supported by high estimated magnesium masses, points to explosions of massive CO cores, requiring M_(ZAMS) \u2273 40 M\u2299. Collisions of pair-instability pulsations do not provide enough mass to account for the emission. [O II] and [O III] lines emerge naturally in many models, which strengthens the identification of broad [O II] 7320, 7330, [O III] 4363, and [O III] 4959, 5007 in some spectra. A small filling factor f \u227e 0.01 for the O/Mg zone is needed to produce enough luminosity in Mg I] 4571, Mg I 1.504 \u03bcm, and O I recombination lines, which shows that the ejecta is clumped. We review the constraints from the nebular spectral modeling in the context of the various scenarios proposed for SLSNe.", "date": "2017-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "835", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 13", "id_number": "CaltechAUTHORS:20190529-080042785", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-080042785", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "702538" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ACSP45" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ACSP74" }, { "agency": "European Research Council (ERC)", "grant_number": "291222" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "European Research Council (ERC)", "grant_number": "320360" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I001123/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000709/1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TRR 33" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" }, { "agency": "Eotvos Lorand University (ELTE)" }, { "agency": "Los Alamos National Laboratory" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/1538-4357/835/1/13", "primary_object": { "basename": "1608.02994.pdf", "url": "https://authors.library.caltech.edu/records/9dg5t-y8516/files/1608.02994.pdf" }, "pub_year": "2017", "author_list": "Jerkstrand, A.; Smartt, S. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/5np34-y3f75", "eprint_id": 73295, "eprint_status": "archive", "datestamp": "2023-08-22 19:30:48", "lastmod": "2023-10-24 15:12:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blagorodnova-N", "name": { "family": "Blagorodnova", "given": "N." }, "orcid": "0000-0003-0901-1606" }, { "id": "Kotak-R", "name": { "family": "Kotak", "given": "R." }, "orcid": "0000-0001-5455-3653" }, { "id": "Polshaw-J", "name": { "family": "Polshaw", "given": "J." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Cody-A-M", "name": { "family": "Cody", "given": "A. M." }, "orcid": "0000-0002-3656-6706" }, { "id": "Doran-G-B", "name": { "family": "Doran", "given": "G. B." } }, { "id": "Elias-Rosa-N", "name": { "family": "Elias-Rosa", "given": "N." }, "orcid": "0000-0002-1381-9125" }, { "id": "Fraser-M", "name": { "family": "Fraser", "given": "M." }, "orcid": "0000-0003-2191-1674" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Gonzalez-Fernandez-C", "name": { "family": "Gonzalez-Fernandez", "given": "C." } }, { "id": "Harmanen-J", "name": { "family": "Harmanen", "given": "J." } }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "J." }, "orcid": "0000-0001-5754-4007" }, { "id": "Kankare-E", "name": { "family": "Kankare", "given": "E." }, "orcid": "0000-0001-8257-3512" }, { "id": "Kudritzki-R-P", "name": { "family": "Kudritzki", "given": "R.-P." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Magnier-E-A", "name": { "family": "Magnier", "given": "E. A." }, "orcid": "0000-0002-7965-2815" }, { "id": "Manulis-I", "name": { "family": "Manulis", "given": "I." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Mattila-S", "name": { "family": "Mattila", "given": "S." }, "orcid": "0000-0001-7497-2994" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ochner-P", "name": { "family": "Ochner", "given": "P." } }, { "id": "Pastorello-A", "name": { "family": "Pastorello", "given": "A." } }, { "id": "Reynolds-T-M", "name": { "family": "Reynolds", "given": "T." } }, { "id": "Smith-K", "name": { "family": "Smith", "given": "K." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Terreran-G", "name": { "family": "Terreran", "given": "G." } }, { "id": "Tomasella-L", "name": { "family": "Tomasella", "given": "L." } }, { "id": "Turatto-M", "name": { "family": "Turatto", "given": "M." } }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" }, { "id": "Zaggia-S", "name": { "family": "Zaggia", "given": "S." }, "orcid": "0000-0001-6081-379X" } ] }, "title": "Common Envelope Ejection for a Luminous Red Nova in M101", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; novae, cataclysmic variables; stars: individual (M101 OT2015-1, PSN J14021678+5426205); stars: massive; stars: winds, outflows", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 July 22; revised 2016 October 21; accepted 2016 October 26; published 2017 January 6. \n\nThe research leading to these results has received funding from the European Union Seventh Framework Programme ([FP7/2007-2013] under grant agreement no. 264895. This work was partly supported by the European Union FP7 programme through ERC grant no. 320360. This work was supported, in whole or in part, by the European Science Foundation under the GREAT ESF RNP programme. This work was supported by the GROWTH project funded by the National Science Foundation under grant no. 1545949. LANL participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program. 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. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada\u2013France\u2013Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This paper makes use of data obtained from the Isaac Newton Group Archive, which is maintained as part of the CASU Astronomical Data Centre at the Institute of Astronomy, Cambridge. This work is partly 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. This work is partly based on observations made with the William Hershell Telescope 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 Astrofsica de Canarias. The Gran Telescopio Canarias (GTC) operated on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is partly based on data from Copernico 1.82 m telescope operated by INAF Osservatorio Astronomico di Padova. NER, AP, GT, and MT are partially supported by the PRIN-INAF 2014 with the project \"Transient universe: unveiling new types of stellar explosions with PESSTO.\" Finally, NBM would like to thank the anonymous referee, who helped to improve the manuscript, Robert G. Izzard, Philipp Podsiadlowski, Lars Bildsten, E. Sterl Phinney, and Noam Soker for helpful discussions, and Pablo and Lucia Solis, and Israel Zenteno for the motivation. \n\nFacilities: Asiago:Copernico - Asiago Observatory's Copernico Telescope, CFHT - , GTC - , Hale - , ING:Newton - , ING:Herschel - , Keck:I - , LBT - , Liverpool:2m - , NOT - , PO:1.2m - , PO:1.5m - , PS1 - , Sloan - , Spitzer - , UKIRT. - \n\nSoftware: BPASS v1.0, BPASS v2.0, EMCEE (Foreman-Mackey et al. 2013), IRAF, NOTCAM (v2.54), PTFIDE (Masci et al. 2016), PYRAF, SNOoPY.\n\nPublished - Blagorodnova_2017_ApJ_834_107.pdf
", "abstract": "We present the results of optical, near-infrared, and mid-infrared observations of M101 OT2015-1 (PSN J14021678+5426205), a luminous red transient in the Pinwheel galaxy (M101), spanning a total of 16 years. The light curve showed two distinct peaks with absolute magnitudes M_r \u2264 -12.4 and M_r \u2243 -12, on 2014 November 11 and 2015 February 17, respectively. The spectral energy distributions during the second maximum show a cool outburst temperature of \u2248 3700 K and low expansion velocities (\u2248-300 km s^(\u22121)) for the H i, Ca ii, Ba ii, and K i lines. From archival data spanning 15\u20138 years before the outburst, we find a single source consistent with the optically discovered transient, which we attribute to being the progenitor; it has properties consistent with being an F-type yellow supergiant with L ~ 8.7 x 10^4 L_\u2299, T_(eff) \u2248 7000 K, and an estimated mass of M_1 = 18 \u00b1 1 M_\u2299. This star has likely just finished the H-burning phase in the core, started expanding, and is now crossing the Hertzsprung gap. Based on the combination of observed properties, we argue that the progenitor is a binary system, with the more evolved system overfilling the Roche lobe. Comparison with binary evolution models suggests that the outburst was an extremely rare phenomenon, likely associated with the ejection of the common envelope of a massive star. The initial mass of the primary fills the gap between the merger candidates V838 Mon (5\u221210 M_\u2299) and NGC 4490-OT (30 M_\u2299).", "date": "2017-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "834", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20170106-105020459", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170106-105020459", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "264895 GENIUS" }, { "agency": "European Research Council (ERC)", "grant_number": "320360" }, { "agency": "European Science Foundation" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-INAF 2014" } ] }, "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": "10.3847/1538-4357/834/2/107", "primary_object": { "basename": "Blagorodnova_2017_ApJ_834_107.pdf", "url": "https://authors.library.caltech.edu/records/5np34-y3f75/files/Blagorodnova_2017_ApJ_834_107.pdf" }, "pub_year": "2017", "author_list": "Blagorodnova, N.; Kotak, R.; et el." }, { "id": "https://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" }, "pub_year": "2017", "author_list": "Masci, Frank J.; Laher, Russ R.; et el." }, { "id": "https://authors.library.caltech.edu/records/dvd2a-bmg21", "eprint_id": 72858, "eprint_status": "archive", "datestamp": "2023-08-19 00:26:34", "lastmod": "2023-10-23 23:01:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Charisi-M", "name": { "family": "Charisi", "given": "M." }, "orcid": "0000-0003-3579-2522" }, { "id": "Bartos-I", "name": { "family": "Bartos", "given": "I." }, "orcid": "0000-0001-5607-3637" }, { "id": "Haiman-Z", "name": { "family": "Haiman", "given": "Z." }, "orcid": "0000-0003-3633-5403" }, { "id": "Price-Whelan-A-M", "name": { "family": "Price-Whelan", "given": "A. M." }, "orcid": "0000-0003-0872-7098" }, { "id": "Graham-M-J", "name": { "family": "Graham", "given": "M. J." }, "orcid": "0000-0002-3168-0139" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E. C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "M\u00e1rka-S", "name": { "family": "M\u00e1rka", "given": "S." } } ] }, "title": "A population of short-period variable quasars from PTF as supermassive black hole binary candidates", "ispublished": "pub", "full_text_status": "public", "keywords": "quasars: supermassive black holes", "note": "\u00a9 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 July 22. Received 2016 July 21. In original form 2016 April 5. First published online July 28, 2016. \n\nWe thank Jules Halpern and Daniel D'Orazio for useful discussions, Ying Zu for assisting with the Javelin code, and Marcel Agueros for providing the light curves and the stellar rotation periods from the Praesepe cluster for an initial test to our Lomb\u2013Scargle algorithm. \n\nFor our analysis, we made use of the High Performace Computing cluster Yeti at Columbia University. Additional resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. This work was supported in part by NASA grants NNX11AE05G and NNX15AB19G (to ZH). MJG acknowledges support from NSF grant AST-1518308. \n\nThis paper is based on observations obtained with the Samuel Oschin Telescope as part of the PTF 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. \n\nThe CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the US National Science Foundation under grants AST-0909182 and AST-1313422. \n\nThis paper was approved for publication by the LIGO Scientific Collaboration, with document number LIGO-P1600113.\n\nPublished - MNRAS-2016-Charisi-2145-71.pdf
Submitted - 1604.01020v2.pdf
", "abstract": "Supermassive black hole binaries (SMBHBs) at sub-parsec separations should be common in galactic nuclei, as a result of frequent galaxy mergers. Hydrodynamical simulations of circum-binary discs predict strong periodic modulation of the mass accretion rate on time-scales comparable to the orbital period of the binary. As a result, SMBHBs may be recognized by the periodic modulation of their brightness. We conducted a statistical search for periodic variability in a sample of 35 383 spectroscopically confirmed quasars in the photometric data base of the Palomar Transient Factory (PTF). We analysed Lomb\u2013Scargle periodograms and assessed the significance of our findings by modelling each individual quasar's variability as a damped random walk (DRW). We identified 50 quasars with significant periodicity beyond the DRW model, typically with short periods of a few hundred days. We find 33 of these to remain significant after a re-analysis of their periodograms including additional optical data from the intermediate-PTF and the Catalina Real-Time Transient Survey. Assuming that the observed periods correspond to the redshifted orbital periods of SMBHBs, we conclude that our findings are consistent with a population of unequal-mass SMBHBs, with a typical mass ratio as low as q \u2261 M_2/M_1 \u2248 0.01.", "date": "2016-12-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "463", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2145-2171", "id_number": "CaltechAUTHORS:20161215-144147982", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161215-144147982", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX11AE05G" }, { "agency": "NASA", "grant_number": "NNX15AB19G" }, { "agency": "NSF", "grant_number": "AST-1518308" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "NSF", "grant_number": "AST-1313422" } ] }, "other_numbering_system": { "items": [ { "id": "LIGO-P1600113", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "LIGO" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stw1838", "primary_object": { "basename": "1604.01020v2.pdf", "url": "https://authors.library.caltech.edu/records/dvd2a-bmg21/files/1604.01020v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2016-Charisi-2145-71.pdf", "url": "https://authors.library.caltech.edu/records/dvd2a-bmg21/files/MNRAS-2016-Charisi-2145-71.pdf" } ], "pub_year": "2016", "author_list": "Charisi, M.; Bartos, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/xwqjt-d1q43", "eprint_id": 72887, "eprint_status": "archive", "datestamp": "2023-08-19 00:14:53", "lastmod": "2023-10-23 23:22:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "Po-Chieh" }, "orcid": "0000-0001-8894-0854" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Yang-Ting-Chang", "name": { "family": "Yang", "given": "Ting-Chang" } }, { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam" }, "orcid": "0000-0001-9515-478X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" } ] }, "title": "The Palomar Transient Factory and RR Lyrae: The Metallicity\u2013Light Curve Relation Based on ab-type RR Lyrae in the Kepler Field", "ispublished": "pub", "full_text_status": "public", "keywords": "distance scale \u2013 stars: abundances \u2013 stars: variables: RR Lyrae", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 August 19; revised 2016 October 11; accepted 2016 October 27; published 2016 December 15. \n\nWe thank the referee for valuable input that improved the manuscript. We acknowledge Wee Siang Edmund Yuen, a 2015 summer student at the National Central University, for carrying out the preliminary analysis of the PTF data for RR Lyrae in the Kepler field. C.C.N. is thankful for the funding from the Ministry of Science and Technology (Taiwan) under grants 104-2112-M-008-012-MY3 and 104-2119-M-008-024. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nFacility: PO:1.2m.\n\nPublished - Ngeow_2016_ApJS_227_30.pdf
", "abstract": "The wide-field synoptic sky surveys, known as the Palomar Transient Factory (PTF) and the intermediate Palomar Transient Factory (iPTF), will accumulate a large number of known and new RR Lyrae. These RR Lyrae are good tracers to study the substructure of the Galactic halo if their distance, metallicity, and galactocentric velocity can be measured. Candidates of halo RR Lyrae can be identified from their distance and metallicity before requesting spectroscopic observations for confirmation. This is because both quantities can be obtained via their photometric light curves, because the absolute V-band magnitude for RR Lyrae is correlated with metallicity, and the metallicity can be estimated using a metallicity\u2013light curve relation. To fully utilize the PTF and iPTF light-curve data in related future work, it is necessary to derive the metallicity\u2013light curve relation in the native PTF/iPTF R-band photometric system. In this work, we derived such a relation using the known ab-type RR Lyrae located in the Kepler field, and it is found to be [Fe/H]_(PTF) = -4.089-7.346P + 1.280\u03c6_(31) (where P is pulsational period and \u03c6_(31) is one of the Fourier parameters describing the shape of the light curve), with a dispersion of 0.118 dex. We tested our metallicity\u2013light curve relation with new spectroscopic observations of a few RR Lyrae in the Kepler field, as well as several data sets available in the literature. Our tests demonstrated that the derived metallicity\u2013light curve relation could be used to estimate metallicities for the majority of the RR Lyrae, which are in agreement with the published values.", "date": "2016-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "227", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 30", "id_number": "CaltechAUTHORS:20161216-091221197", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161216-091221197", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2112-M-008-012-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "104-2119-M-008-024" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/1538-4365/227/2/30", "primary_object": { "basename": "Ngeow_2016_ApJS_227_30.pdf", "url": "https://authors.library.caltech.edu/records/xwqjt-d1q43/files/Ngeow_2016_ApJS_227_30.pdf" }, "pub_year": "2016", "author_list": "Ngeow, Chow-Choong; Yu, Po-Chieh; et el." }, { "id": "https://authors.library.caltech.edu/records/5nvhc-gs971", "eprint_id": 72631, "eprint_status": "archive", "datestamp": "2023-08-22 19:12:31", "lastmod": "2023-10-23 22:47:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Large Super-Fast Rotator Hunting Using the Intermediate Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: general; surveys", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 June 26. Accepted 2016 August 25. Published 2016 December 2. \n\nWe would like to thank the anonymous referee for useful suggestions and comments. This work is supported in part by the National Science Council of Taiwan under the grants MOST 104-2112-M-008-014-MY3 and MOST 104-2119-M-008-024, and also by the Macau Science and Technology Fund No. 017/2014/A1 of MSAR. This publication makes use of data products from 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. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services that are specific to NEOWISE that are contributed by the International Astronomical Union's Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University.\n\nPublished - Chang_2016_ApJS_227_20.pdf
Submitted - 1608.07910v1.pdf
", "abstract": "In order to look for large super-fast rotators, in late 2014 and early 2015, five dedicated surveys covering ~188 deg2 in the ecliptic plane have been carried out in the R-band, with ~10 minute cadence using the intermediate Palomar Transient Factory. Among 1029 reliable rotation periods obtained from the surveys, we discovered 1 new large super-fast rotator, (40511) 1999 RE88, and 18 other candidates. (40511) 1999 RE88 is an S-type inner main-belt asteroid with a diameter of D = 1.9 \u00b1 0.3 km, a rotation period of P = 1.96 \u00b1 0.01 hr, and a light curve amplitude of \u0394m ~ 1.0 mag. To maintain such fast rotation, an internal cohesive strength of ~780 Pa is required. Combining all known large super-fast rotators, their cohesive strengths all fall in the range of 100\u20131000 Pa of lunar regolith. However, the number of large super-fast rotators seems to be far less than the whole asteroid population. This might indicate a peculiar asteroid group for them. Although the detection efficiency for a long rotation period is greatly reduced due to our two-day observation time span, the spin-rate distributions of this work show consistent results with Chang et al. (2015), after considering the possible observational bias in our surveys. It shows a number decrease with an increase of spin rate for asteroids with a diameter of 3 \u2264 D \u2264 15 km, and a number drop at a spin rate of f = 5 rev day^(\u22121) for asteroids with D \u2264 3 km.", "date": "2016-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "227", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 20", "id_number": "CaltechAUTHORS:20161207-120923097", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161207-120923097", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Council (Taipei)", "grant_number": "MOST 104-2112-M-008-014-MY3MOST 104-2112-M-008-014-MY3" }, { "agency": "National Science Council (Taipei)", "grant_number": "MOST 104-2119-M-008-024" }, { "agency": "Macau Science and Technology Fund", "grant_number": "017/2014/A1" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0067-0049/227/2/20", "primary_object": { "basename": "Chang_2016_ApJS_227_20.pdf", "url": "https://authors.library.caltech.edu/records/5nvhc-gs971/files/Chang_2016_ApJS_227_20.pdf" }, "related_objects": [ { "basename": "1608.07910v1.pdf", "url": "https://authors.library.caltech.edu/records/5nvhc-gs971/files/1608.07910v1.pdf" } ], "pub_year": "2016", "author_list": "Chang, Chan-Kao; Lin, Hsing-Wen; et el." }, { "id": "https://authors.library.caltech.edu/records/ckfrq-zdb97", "eprint_id": 72193, "eprint_status": "archive", "datestamp": "2023-08-19 00:06:38", "lastmod": "2023-10-23 18:01:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Papadogiannakis-S", "name": { "family": "Papadogiannakis", "given": "S." }, "orcid": "0000-0003-0783-3323" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "Brian D." }, "orcid": "0000-0002-7856-3570" } ] }, "title": "SN2002es-like Supernovae from Different Viewing Angles", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (SN2002es, iPTF14atg, iPTF14dpk)", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 June 17; revised 2016 September 11; accepted 2016 September 12; published 2016 November 18. \n\nY.C. and P.E.N. acknowledge support from the DOE under grant DE-AC02-05CH11231, Analytical Modeling for Extreme-Scale Computing Environments. Y.C. also acknowledges support by the GROWTH project funded by the National Science Foundation under Grant No 1545949. A.G.-Y. is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I-Core programme by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" programme; and by Kimmel and ARCHES awards. \n\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. 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\nPublished - Cao_2016_ApJ_832_86.pdf
Submitted - 1606.05655v1.pdf
", "abstract": "In this article, we compare optical light curves of two SN2002es-like Type Ia supernovae (SNe), iPTF14atg and iPTF14dpk, from the intermediate Palomar Transient Factory. Although the two light curves resemble each other around and after maximum, they show distinct early-phase rise behavior in the r-band. On the one hand, iPTF14atg revealed a slow and steady rise that lasted for 22 days with a mean rise rate of 0.2\u20130.3 mag day^(-1), before it reached the R-band peak (\u221218.05 mag). On the other hand, iPTF14dpk rose rapidly to \u221217 mag within a day of discovery with a rise rate > 1.8 mag day^(-1) , and then rose slowly to its peak (\u221218.19 mag) with a rise rate similar to iPTF14atg. The apparent total rise time of iPTF14dpk is therefore only 16 days. We show that emission from iPTF14atg before \u221217 days with respect to its maximum can be entirely attributed to radiation produced by collision between the SN and its companion star. Such emission is absent from iPTF14dpk probably because of an unfavored viewing angle, provided that SN2002es-like events arise from the same progenitor channel. We further show that an SN2002es-like SN may experience a dark phase after the explosion but before its radioactively powered light curve becomes visible. This dark phase may be lit by radiation from supernova\u2013companion interaction.", "date": "2016-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "832", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 86", "id_number": "CaltechAUTHORS:20161121-100334709", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161121-100334709", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "Weizmann-UK Program" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/832/1/86", "primary_object": { "basename": "Cao_2016_ApJ_832_86.pdf", "url": "https://authors.library.caltech.edu/records/ckfrq-zdb97/files/Cao_2016_ApJ_832_86.pdf" }, "related_objects": [ { "basename": "1606.05655v1.pdf", "url": "https://authors.library.caltech.edu/records/ckfrq-zdb97/files/1606.05655v1.pdf" } ], "pub_year": "2016", "author_list": "Cao, Yi; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/kcwfk-c3y79", "eprint_id": 70659, "eprint_status": "archive", "datestamp": "2023-08-20 14:19:15", "lastmod": "2023-10-20 23:18:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Intermediate Palomar Transient Factory: Realtime Image Subtraction Pipeline", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys methods: observational (stars:) supernovae: general", "note": "\u00a9 2016 Astronomical Society of the Pacific. \n\nReceived 2016 June 6; accepted 2016 August 2; published 2016 September 30. \n\nWe thank J. Sollerman for useful suggestions to improve the manuscript. Y.C. and P.E.N. acknowledge support from the DOE under grant DE-AC02-05CH11231, Analytical Modeling for Extreme-Scale Computing Environments. Y.C. and M.M.K. also acknowledge support by the GROWTH project, funded by the National Science Foundation under grant No. 1545949. The intermediate Palomar Transient Factory project is a scientific collaboration (PI: S. R. Kulkarni) among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin\u2013Milwaukee, 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\nSubmitted - 1608.01006v1.pdf
", "abstract": "A fast-turnaround pipeline for realtime data reduction plays an essential role in discovering and permitting follow-up observations to young supernovae and fast-evolving transients in modern time-domain surveys. In this paper, we present the realtime image subtraction pipeline in the intermediate Palomar Transient Factory. By using high-performance computing, efficient databases, and machine-learning algorithms, this pipeline manages to reliably deliver transient candidates within 10 minutes of images being taken. Our experience in using high-performance computing resources to process big data in astronomy serves as a trailblazer to dealing with data from large-scale time-domain facilities in the near future.", "date": "2016-11", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "128", "number": "969", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 114502", "id_number": "CaltechAUTHORS:20160929-104335598", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160929-104335598", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "OISE-1545949" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/1538-3873/128/969/114502", "primary_object": { "basename": "1608.01006v1.pdf", "url": "https://authors.library.caltech.edu/records/kcwfk-c3y79/files/1608.01006v1.pdf" }, "pub_year": "2016", "author_list": "Cao, Yi; Nugent, Peter E.; et el." }, { "id": "https://authors.library.caltech.edu/records/m4dek-77t09", "eprint_id": 71225, "eprint_status": "archive", "datestamp": "2023-08-20 14:14:56", "lastmod": "2023-10-23 15:30:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lau-Ryan-M", "name": { "family": "Lau", "given": "Ryan M." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Bond-H-E", "name": { "family": "Bond", "given": "Howard E." }, "orcid": "0000-0003-1377-7145" }, { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "Ori D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Carlon-R", "name": { "family": "Carlon", "given": "Robert" } }, { "id": "Cody-A-M", "name": { "family": "Cody", "given": "Ann Marie" }, "orcid": "0000-0002-3656-6706" }, { "id": "Contreras-C", "name": { "family": "Contreras", "given": "Carlos" } }, { "id": "Dykhoff-D", "name": { "family": "Dykhoff", "given": "Devin" } }, { "id": "Gehrz-R-D", "name": { "family": "Gehrz", "given": "Robert" }, "orcid": "0000-0003-1319-4089" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "Eric" } }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob" }, "orcid": "0000-0001-5754-4007" }, { "id": "Khan-Rubab", "name": { "family": "Khan", "given": "Rubab" } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Monard-L-A-G", "name": { "family": "Monard", "given": "L. A. G." } }, { "id": "Monson-A-J", "name": { "family": "Monson", "given": "Andrew J." }, "orcid": "0000-0002-0048-2586" }, { "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": "Ressler-M-E", "name": { "family": "Ressler", "given": "Michael E." } } ] }, "title": "Rising from the Ashes: Mid-infrared Re-brightening of the Impostor SN 2010da in NGC 300", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter \u2013 dust, extinction \u2013 stars: evolution \u2013 stars: mass-loss \u2013 supernovae: individual (SN 2010da) \u2013 X-rays: binaries", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 May 6; revised 2016 July 25; accepted 2016 July 26; published 2016 October 18. \n\nThis work made use of observations from the Spitzer Space Telescope operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA (PIDS 1083, 40204, 61002, 80015A, 80196, 80015, 10136, 10139, 11063, and 11053). Ground-based observations presented were obtained from the Bronberg Observatory, the SMARTS Consortium 1.3 m telescope at CTIO, the 1 m Swope telescope at LCO, the Mount Lemmon Observing Facility, operated by the University of Minnesota, and the Magellan Baade Telescope at LCO. This work was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.J. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. R.D.G. and his group at MLOF were supported, in part, by the United States Air Force. \n\nR.L. thanks Drew Clausen for enlightening discussions on high-mass X-ray binaries. R.L. also thanks Scott Adams for insightful comments and the anonymous referee for the valuable suggestions and corrections. H.E.B. thanks the STScI Director's Discretionary Research Fund for supporting STScI's participation in the SMARTS Consortium. We appreciate the excellent work of the CTIO/SMARTS service observers who obtained the ANDICAM images during many long clear Tololo nights: Juan Espinoza, Alberto Miranda, Mauricio Rojas, and Jacqueline Seron.\n\nPublished - Lau_2016_ApJ_830_142.pdf
Submitted - 1605.06750v1.pdf
", "abstract": "We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the \"impostor\" supernova (SN) 2010da in NGC 300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN 2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS) 14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN 2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ~10% decrease at 4.5 \u03bcm between 2003 November and 2007 December. A sharp increase in the 3.6 \u03bcm flux followed by a rapid decrease measured ~150 days before and ~80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (~2000 days), the 3.6 and 4.5 \u03bcm emission increased to over a factor of two times the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN 2010da. We analyze the evolution of the dust temperature (T_d ~ 700\u20131000 K), mass (M_d ~ 0.5\u20133.8 \u00d7 10^(\u22127) M\u2299), luminosity (L_(IR) ~ 1.3\u20133.5 \u00d7 10^4 L\u2299), and the equilibrium temperature radius (R_(eq) ~ 6.4\u201312.2 au) in order to resolve the nature of SN 2010da. We address the leading interpretation of SN 2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN 2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN 2010da progenitor occupies a similar region on a mid-IR color\u2013magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e > 0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN 2010da may be associated with a newly formed HMXB system.", "date": "2016-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "830", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 142", "id_number": "CaltechAUTHORS:20161018-122908941", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161018-122908941", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "United States Air Force" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0004-637X/830/2/142", "primary_object": { "basename": "1605.06750v1.pdf", "url": "https://authors.library.caltech.edu/records/m4dek-77t09/files/1605.06750v1.pdf" }, "related_objects": [ { "basename": "Lau_2016_ApJ_830_142.pdf", "url": "https://authors.library.caltech.edu/records/m4dek-77t09/files/Lau_2016_ApJ_830_142.pdf" } ], "pub_year": "2016", "author_list": "Lau, Ryan M.; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/rgvqy-htv96", "eprint_id": 95843, "eprint_status": "archive", "datestamp": "2023-08-20 14:11:14", "lastmod": "2023-10-20 20:38:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zackay-B", "name": { "family": "Zackay", "given": "Barak" } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" } ] }, "title": "Proper image subtraction\u2014optimal transient detection, photometry, and hypothesis testing", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: micro \u2013 methods: data analysis \u2013 methods: statistical \u2013 surveys \u2013 techniques:\nimage processing \u2013 techniques: photometric", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 January 11; revised 2016 May 23; accepted 2016 June 15; published 2016 October 4. \n\nWe thank Ora Zackay, Zeljko Ivesic, Robert Lupton, and Assaf Horesh for many discussions. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. B.Z. is grateful for receiving the Clore fellowship. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). A.G. acknowledges support from the I-Core program \"The Quantum universe,\" as well as from the Kimmel Award.\n\nSubmitted - 1601.02655.pdf
", "abstract": "Transient detection and flux measurement via image subtraction stand at the base of time domain astronomy. Due to the varying seeing conditions, the image subtraction process is non-trivial, and existing solutions suffer from a variety of problems. Starting from basic statistical principles, we develop the optimal statistic for transient detection, flux measurement, and any image-difference hypothesis testing. We derive a closed-form statistic that: (1) is mathematically proven to be the optimal transient detection statistic in the limit of background-dominated noise, (2) is numerically stable, (3) for accurately registered, adequately sampled images, does not leave subtraction or deconvolution artifacts, (4) allows automatic transient detection to the theoretical sensitivity limit by providing credible detection significance, (5) has uncorrelated white noise, (6) is a sufficient statistic for any further statistical test on the difference image, and, in particular, allows us to distinguish particle hits and other image artifacts from real transients, (7) is symmetric to the exchange of the new and reference images, (8) is at least an order of magnitude faster to compute than some popular methods, and (9) is straightforward to implement. Furthermore, we present extensions of this method that make it resilient to registration errors, color-refraction errors, and any noise source that can be modeled. In addition, we show that the optimal way to prepare a reference image is the proper image coaddition presented in Zackay & Ofek. We demonstrate this method on simulated data and real observations from the PTF data release 2. We provide an implementation of this algorithm in MATLAB and Python.", "date": "2016-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "830", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 27", "id_number": "CaltechAUTHORS:20190529-081531406", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-081531406", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Weizmann Institute of Science" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Kimmel Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0004-637x/830/1/27", "primary_object": { "basename": "1601.02655.pdf", "url": "https://authors.library.caltech.edu/records/rgvqy-htv96/files/1601.02655.pdf" }, "pub_year": "2016", "author_list": "Zackay, Barak; Ofek, Eran O.; et el." }, { "id": "https://authors.library.caltech.edu/records/2bnkm-qx607", "eprint_id": 70750, "eprint_status": "archive", "datestamp": "2023-08-22 18:52:28", "lastmod": "2023-10-20 23:28:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Yang-L", "name": { "family": "Yang", "given": "L." } }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "A." }, "orcid": "0000-0003-2082-1626" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Graham-M-L", "name": { "family": "Graham", "given": "M. L." }, "orcid": "0000-0002-9154-3136" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" } ] }, "title": "Host-Galaxy Properties of 32 Low-Redshift Superluminous Supernovae from the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: abundances; galaxies: dwarf; galaxies: photometry; supernovae: general", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 April 27; revised 2016 July 13; accepted 2016 July 19; published 2016 October 3. \n\nWe thank the anonymous referee for a careful reading of the submitted paper and for providing valuable comments. D.A.P. acknowledges support from a Marie Sklodowska-Curie Individual Fellowship within the Horizon 2020 European Union (EU) Framework Programme for Research and Innovation (H2020-MSCA-IF-2014-660113). Support for this work was also provided by the National Aeronautics and Space Administration (NASA) through an award issued by JPL/Caltech, and through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The Dark Cosmology Centre has been funded by the DNRF. D.A.P. thanks the Aspen Center for Physics for its hospitality and for enabling productive discussion of SLSN models and optical surveys during summer programs in 2014 (\"Fast & Furious\") and 2015 (\"The Dynamic Universe\") and particularly acknowledges R. Chornock's useful presentation on SLSN diversity. A.V.F. also thanks the Aspen Center for its hospitality during programs in 2014 and 2016 (\"Emergence, Evolution, and Effects of Black Holes in the Universe\"). Participation in these programs was supported by National Science Foundation (NSF) Grant No. PHYS-1066293. D.A.P. acknowledges useful discussions about dwarf-galaxy star formation histories and surveys with A. Wetzel and dwarf-galaxy stellar populations with D. Baade, on SLSN hosts with T. Chen, on metallicity determinations with M. Modjaz, and extensive input from G. Leloudas. We acknowledge useful feedback on the paper from D. A. Kann and D. Cook. We thank Y. Cao, S. Kulkarni, and M. Kasliwal for some observations. We also thank the entire PTF collaboration for their input in building this successful survey, including J. Bloom for developing and implementing the machine-learning techniques used to identify transients. \n\nA.G.Y. is supported by the EU/FP7 via ERC grant no. 307260, \"The Quantum Universe\" I-Core program by the Israeli Committee for planning and budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and YeS awards. A.V.F. is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, Gary and Cynthia Bengier, the Christopher R. Redlich Fund, and NASA/HST grants AR-12850 and AR-14295 from STScI. \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. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. This paper also includes data based on observations made with the NASA/ESA Hubble Space Telescope and obtained from the Hubble Legacy Archive, which is a collaboration between STScI/NASA, the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). 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 use data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California at Los Angeles and the Jet Propulsion Laboratory/California Institute of Technology, funded by NASA.\n\nPublished - apj_830_1_13.pdf
Submitted - 1604.08207v3.pdf
", "abstract": "We present ultraviolet through near-infrared photometry and spectroscopy of the host galaxies of all superluminous supernovae (SLSNe) discovered by the Palomar Transient Factory prior to 2013 and derive measurements of their luminosities, star formation rates, stellar masses, and gas-phase metallicities. We find that Type I (hydrogen-poor) SLSNe (SLSNe I) are found almost exclusively in low-mass (M_* < 2 x 10^9 M_\u2299) and metal-poor (12 + log_(10)[O/H] < 8.4) galaxies. We compare the mass and metallicity distributions of our sample to nearby galaxy catalogs in detail and conclude that the rate of SLSNe I as a fraction of all SNe is heavily suppressed in galaxies with metallicities \u22730.5 Z_\u2299. Extremely low metallicities are not required and indeed provide no further increase in the relative SLSN rate. Several SLSN I hosts are undergoing vigorous starbursts, but this may simply be a side effect of metallicity dependence: dwarf galaxies tend to have bursty star formation histories. Type II (hydrogen-rich) SLSNe (SLSNe II) are found over the entire range of galaxy masses and metallicities, and their integrated properties do not suggest a strong preference for (or against) low-mass/low-metallicity galaxies. Two hosts exhibit unusual properties: PTF 10uhf is an SLSN I in a massive, luminous infrared galaxy at redshift z = 0.29, while PTF 10tpz is an SLSN II located in the nucleus of an early-type host at z = 0.04.", "date": "2016-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "830", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 13", "id_number": "CaltechAUTHORS:20161003-095119926", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161003-095119926", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "H2020-MSCA-IF-2014-660113" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51296.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Danish National Research Foundation" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weismann-UK" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "NASA", "grant_number": "AR-12850" }, { "agency": "NASA", "grant_number": "AR-14295" }, { "agency": "Space Telescope Science Institute" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "AutoScope Corporation" }, { "agency": "Lick Observatory" }, { "agency": "University of California" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Google" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/830/1/13", "primary_object": { "basename": "1604.08207v3.pdf", "url": "https://authors.library.caltech.edu/records/2bnkm-qx607/files/1604.08207v3.pdf" }, "related_objects": [ { "basename": "apj_830_1_13.pdf", "url": "https://authors.library.caltech.edu/records/2bnkm-qx607/files/apj_830_1_13.pdf" } ], "pub_year": "2016", "author_list": "Perley, D. A.; Quimby, R. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/d8cz2-3bw59", "eprint_id": 70848, "eprint_status": "archive", "datestamp": "2023-08-22 18:52:42", "lastmod": "2023-10-20 23:34:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johns-Krull-C-M", "name": { "family": "Johns-Krull", "given": "Christopher M." } }, { "id": "Prato-L", "name": { "family": "Prato", "given": "Lisa" } }, { "id": "McLane-J-N", "name": { "family": "McLane", "given": "Jacob N." } }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David R." }, "orcid": "0000-0002-5741-3047" }, { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "Julian C." }, "orcid": "0000-0003-2192-5371" }, { "id": "Chen-Wei", "name": { "family": "Chen", "given": "Wei" } }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "John R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles A." }, "orcid": "0000-0002-5627-5471" }, { "id": "Frazier-S-A", "name": { "family": "Frazier", "given": "Sarah A." } }, { "id": "Boden-A-F", "name": { "family": "Boden", "given": "Andrew F." } }, { "id": "Morales-Calder\u00f3n-M", "name": { "family": "Morales-Calder\u00f3n", "given": "Mar\u00eda" } }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa M." }, "orcid": "0000-0001-6381-515X" } ] }, "title": "H\u03b1 Variability in PTFO8-8695 and the Possible Direct Detection of Emission from a 2 Million Year Old Evaporating Hot Jupiter", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; line: profiles; stars: atmospheres; stars: formation; stars: magnetic field; stars: pre-main sequence", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 September 14; revised 2016 May 11; accepted 2016 May 19; published 2016 October 3. \n\nL.P. and C.M.J.-K. wish to acknowledge partial support for this research from the NASA Origins of Solar Systems program through grant number 07-SSO07-86 made to Lowell Observatory. CMJ-K also wishes to acknowledge partial support for this work from the National Science Foundation through grant number 1212122 made to Rice University. This work was funded in part through the 2013\u20132014 NAU/NASA Space Grant Undergraduate Research Internship for Jacob N. McLane. Finally, we wish to thank an anonymous referee for several useful comments that improved the original manuscript.\n\nPublished - Johns-Krull_2016_ApJ_830_15.pdf
Submitted - 1606.02701v1.pdf
", "abstract": "We use high time cadence, high spectral resolution optical observations to detect excess H\u03b1 emission from the 2\u20133 Myr old weak-lined T Tauri star PTFO 8-8695. This excess emission appears to move in velocity as expected if it were produced by the suspected planetary companion to this young star. The excess emission is not always present, but when it is, the predicted velocity motion is often observed. We have considered the possibility that the observed excess emission is produced by stellar activity (flares), accretion from a disk, or a planetary companion; we find the planetary companion to be the most likely explanation. If this is the case, the strength of the H\u03b1 line indicates that the emission comes from an extended volume around the planet, likely fed by mass loss from the planet which is expected to be overflowing its Roche lobe.", "date": "2016-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "830", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20161005-072304972", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161005-072304972", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "07-SSO07-86" }, { "agency": "NSF", "grant_number": "AST-1212122" }, { "agency": "Northern Arizona University" }, { "agency": "NASA Space Grant Undergraduate Research Internship" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/830/1/15", "primary_object": { "basename": "1606.02701v1.pdf", "url": "https://authors.library.caltech.edu/records/d8cz2-3bw59/files/1606.02701v1.pdf" }, "related_objects": [ { "basename": "Johns-Krull_2016_ApJ_830_15.pdf", "url": "https://authors.library.caltech.edu/records/d8cz2-3bw59/files/Johns-Krull_2016_ApJ_830_15.pdf" } ], "pub_year": "2016", "author_list": "Johns-Krull, Christopher M.; Prato, Lisa; et el." }, { "id": "https://authors.library.caltech.edu/records/j956p-5xt52", "eprint_id": 63957, "eprint_status": "archive", "datestamp": "2023-08-22 18:51:54", "lastmod": "2023-10-17 18:31:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Palliyaguru-N-T", "name": { "family": "Palliyaguru", "given": "N." }, "orcid": "0000-0002-4828-0262" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" } ] }, "title": "Radio observations of a sample of broad-lined type Ic supernovae discovered by PTF/iPTF: A search for relativistic explosions", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: general; radiation mechanisms: non-thermal; supernovae: general", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2015 December 3; revised 2016 July 13; accepted 2016 July 13; published 2016 October 10. \n\nA.C. thanks P. Chandra for graciously providing the data for the average long GRB radio light curve showing in Figure 4. A.C. acknowledges support from the NSF CAREER award #1455090. A.C. and N.P. acknowledge partial support from NASA/Swift Cycle 10 and 11 GI via grants NNX15AB79G and NNX16AC12G. A.G.Y.'s team is supported by the EU/FP7 via ERC grant No. 307260 the Quantum universe I-Core program by the Israeli Committee for planning and budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards. K.M. acknowledges support from the STFC through an Ernest Rutherford Fellowship. M.M.K. acknowledges partial support from the GROWTH project via NSF grant 1545949. M.S. acknowledges support from the Royal Society and EU/FP7-ERC grant No. 615929. The Karl G. Jansky Very Large Array is operated by NRAO, for the NSF under cooperative agreement by Associated Universities, Inc. W. M. Keck Observatory, is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias. The authors acknowledge the High Performance Computing Center (HPCC) at Texas Tech University at Lubbock (http://cmsdev.ttu.edu/hpcc) for providing HPC resources that have contributed to the research results reported within this paper. This research also 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\nPublished - Corsi_2016_ApJ_830_42.pdf
Submitted - 1512.01303.pdf
", "abstract": "Long duration \u03b3-ray bursts are a rare subclass of stripped-envelope core-collapse supernovae (SNe) that launch collimated relativistic outflows (jets). All \u03b3-ray-burst-associated SNe are spectroscopically Type Ic, with broad-lines, but the fraction of broad-lined SNe Ic harboring low-luminosity \u03b3-ray bursts remains largely unconstrained. Some SNe should be accompanied by off-axis \u03b3-ray burst jets that initially remain invisible, but then emerge as strong radio sources (as the jets decelerate). However, this critical prediction of the jet model for \u03b3-ray bursts has yet to be verified observationally. Here, we present K. G. Jansky Very Large Array observations of 15 broad-lined SNe of Type Ic discovered by the Palomar Transient Factory in an untargeted manner. Most of the SNe in our sample exclude radio emission observationally similar to that of the radio-loud, relativistic SN 1998bw. We constrain the fraction of 1998bw-like broad-lined SNe Ic to be \u227e41% (99.865% confidence). Most of the events in our sample also exclude off-axis jets similar to GRB 031203 and GRB 030329, but we cannot rule out off-axis \u03b3-ray bursts expanding in a low-density wind environment. Three SNe in our sample are detected in the radio. PTF11qcj and PTF14dby show late-time radio emission with average ejecta speeds of \u22480.3\u20130.4 c, on the dividing line between relativistic and \"ordinary\" SNe. The speed of PTF11cmh radio ejecta is poorly constrained. We estimate that \u227e85% 99.865% confidence) of the broad-lined SNe Ic in our sample may harbor off-axis \u03b3-ray bursts expanding in media with densities in the range probed by this study.", "date": "2016-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "830", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 42", "id_number": "CaltechAUTHORS:20160126-073528823", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160126-073528823", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1455090" }, { "agency": "NASA", "grant_number": "NNX15AB79G" }, { "agency": "NASA", "grant_number": "NNX16AC12G" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee Quantum Universe I-Core program" }, { "agency": "Israel Science Foundation" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK Program" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/830/1/42", "primary_object": { "basename": "1512.01303.pdf", "url": "https://authors.library.caltech.edu/records/j956p-5xt52/files/1512.01303.pdf" }, "related_objects": [ { "basename": "Corsi_2016_ApJ_830_42.pdf", "url": "https://authors.library.caltech.edu/records/j956p-5xt52/files/Corsi_2016_ApJ_830_42.pdf" } ], "pub_year": "2016", "author_list": "Corsi, A.; Gal-Yam, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/01c5q-aem42", "eprint_id": 71947, "eprint_status": "archive", "datestamp": "2023-08-20 14:08:43", "lastmod": "2023-10-23 17:42:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Palliyaguru-N-T", "name": { "family": "Palliyaguru", "given": "N. T." }, "orcid": "0000-0002-4828-0262" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Mishra-N", "name": { "family": "Mishra", "given": "N." } }, { "id": "Singer-L-P", "name": { "family": "Singer", "given": "L. P." }, "orcid": "0000-0001-9898-5597" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J. A." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Radio Follow-up of Gravitational-wave Triggers during Advanced LIGO O1", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational waves \u2013 radiation mechanisms: general \u2013 radio continuum: general", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 August 22; Accepted 2016 September 14; Published 2016 September 28. \n\nA.C. thanks K. Hotokezaka and S. Nissanke for graciously providing the theoretical radio light curves of NS\u2013NS mergers. A.C. acknowledges support from the NSF CAREER award #1455090. A.C. and N.P. acknowledge partial support from NASA/Swift Cycle 11 GI via grant NNX16AC12G. M.M.K. acknowledges partial support from the GROWTH project funded by the NSF under Grant #1545949. N.M. acknowledges support from the TTU Clark Scholars program. A.G.-Y. acknowledges support from the European Union FP7 programme through ERC grant #307260, the Quantum universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; and by Kimmel and YeS awards. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Intermediate Palomar Transient Factory project is 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. 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\nPublished - Palliyaguru_2016_ApJL_829_L28.pdf
Submitted - 1608.06518v2.pdf
", "abstract": "We present radio follow-up observations carried out with the Karl G. Jansky Very Large Array during the first observing run (O1) of the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO). A total of three gravitational-wave triggers were followed-up during the \u2248\n4 months of O1, from 2015 September to 2016 January. Two of these triggers, GW150914 and GW151226, are binary black hole (BH) merger events of high significance. A third trigger, G194575, was subsequently declared as an event of no interest (i.e., a false alarm). Our observations targeted selected optical transients identified by the intermediate Palomar Transient Factory in the Advanced LIGO error regions of the three triggers, and a limited region of the gravitational-wave localization area of G194575 not accessible to optical telescopes due to Sun constraints, where a possible high-energy transient was identified. No plausible radio counterparts to GW150914 and GW151226 were found, in agreement with expectations for binary BH mergers. We show that combining optical and radio observations is key to identifying contaminating radio sources that may be found in the follow-up of gravitational-wave triggers, such as emission associated with star formation and active galactic nuclei. We discuss our results in the context of the theoretical predictions for radio counterparts to gravitational-wave transients, and describe our future plans for the radio follow-up of Advanced LIGO (and Virgo) triggers.", "date": "2016-10-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "829", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L28", "id_number": "CaltechAUTHORS:20161111-110633320", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161111-110633320", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1455090" }, { "agency": "NASA", "grant_number": "NNX16AC12G" }, { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "Texas Tech University" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Kimmel Award" }, { "agency": "YeS Award" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/2041-8205/829/2/L28", "primary_object": { "basename": "1608.06518v2.pdf", "url": "https://authors.library.caltech.edu/records/01c5q-aem42/files/1608.06518v2.pdf" }, "related_objects": [ { "basename": "Palliyaguru_2016_ApJL_829_L28.pdf", "url": "https://authors.library.caltech.edu/records/01c5q-aem42/files/Palliyaguru_2016_ApJL_829_L28.pdf" } ], "pub_year": "2016", "author_list": "Palliyaguru, N. T.; Corsi, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/ychen-44s68", "eprint_id": 71133, "eprint_status": "archive", "datestamp": "2023-08-20 13:52:45", "lastmod": "2023-10-23 15:21:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kao-Wil", "name": { "family": "Kao", "given": "Wil" } }, { "id": "Kaplan-D-L", "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" }, { "id": "Ene-Irina", "name": { "family": "Ene", "given": "Irina" } }, { "id": "KIim-Kyu-Bin", "name": { "family": "Kim", "given": "Kyu Bin" } }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "Photometric variability of candidate white dwarf binary systems from Palomar Transient Factory archival data", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close binaries: eclipsing white dwarfs", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 June 14. Received 2016 June 14. In original form 2015 September 10. First published online June 16, 2016. \n\nPart of this work was performed by TAP while at the Aspen Center for Physics, which is supported by NSF Grant #1066293. WK and KBK were each funded by a Summer Undergraduate Research Fellowship at the California Institute of Technology. \n\nThe CRTS survey is supported by the US National Science Foundation under grants AST-0909182. Observations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the PTF 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. Additional observations were obtained using the DBSP spectrograph on the Palomar 200-inch Hale telescope operated by Caltech. \n\nWe thank Nathaniel Butler for providing the main framework of the L-S python script and Detlev Koester for providing us with his WD model atmospheres. We are in debt to Mike Yang for assisting in the retrieval of CRTS data and Ashish Mahabal for the verification of eclipses in CRTS light curves. Furthermore, the constructive comments from Eric Bellm, Thomas Kupfer, and Avi Shporer are much appreciated. We would also like to thank the referee for careful reading of the manuscript and providing many valuable suggestions that certainly helped improve the paper. \n\nWK thanks the productive discussions with Marten van Kerkwijk, as well as the time of Hung Yu (Ben) Ling and Alexander Papanicolaou, who never failed to provide seemingly useless advice that turned out as thought provoking as caffeine. Last but not least, a special mention must go to Yi Cao, Adam Miller, and other members of the iPTF collaboration at Caltech, who generously shared their telescope time with us. \n\nThis research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France, and has benefited much from NASA's Astrophysics Data System.\n\nPublished - MNRASKao,W.etal.pdf
Submitted - 1606.04627v2.pdf
", "abstract": "We present a sample of 59 periodic variables from the Palomar Transient Factory, selected from published catalogues of white dwarf (WD) candidates. The variability can likely be attributed to ellipsoidal variation of the tidally distorted companion induced by the gravity of the primary (WD or hot subdwarf) or to the reflection of hot emission by a cooler companion. We searched 11\u2009311 spectroscopically or photometrically selected WD candidates from three hot star/WD catalogues, using the Lomb\u2013Scargle periodogram to single out promising sources. We present period estimates for the candidates, 45 of which were not previously identified as periodic variables, and find that most have a period shorter than a few days. Additionally, we discuss the eclipsing systems in our sample and present spectroscopic data on selected sources.", "date": "2016-09-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "461", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2747-2761", "id_number": "CaltechAUTHORS:20161017-074029367", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161017-074029367", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" }, { "agency": "NSF", "grant_number": "AST-0909182" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stw1434", "primary_object": { "basename": "1606.04627v2.pdf", "url": "https://authors.library.caltech.edu/records/ychen-44s68/files/1606.04627v2.pdf" }, "related_objects": [ { "basename": "MNRASKao,W.etal.pdf", "url": "https://authors.library.caltech.edu/records/ychen-44s68/files/MNRASKao,W.etal.pdf" } ], "pub_year": "2016", "author_list": "Kao, Wil; Kaplan, David L.; et el." }, { "id": "https://authors.library.caltech.edu/records/gbkqe-y7766", "eprint_id": 70655, "eprint_status": "archive", "datestamp": "2023-08-22 18:44:55", "lastmod": "2023-10-20 23:18:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Singer-L-P", "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "id": "Chen-Hsin-Yu", "name": { "family": "Chen", "given": "Hsin-Yu" } }, { "id": "Holz-D-E", "name": { "family": "Holz", "given": "Daniel E." } }, { "id": "Farr-W-M", "name": { "family": "Farr", "given": "Will M." }, "orcid": "0000-0003-1540-8562" }, { "id": "Price-L-R", "name": { "family": "Price", "given": "Larry R." } }, { "id": "Raymond-V", "name": { "family": "Raymond", "given": "Vivien" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } }, { "id": "Cannizzo-J-K", "name": { "family": "Cannizzo", "given": "John" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Nissanke-S", "name": { "family": "Nissanke", "given": "Samaya" } }, { "id": "Coughlin-M-W", "name": { "family": "Coughlin", "given": "Michael" }, "orcid": "0000-0002-8262-2924" }, { "id": "Farr-B", "name": { "family": "Farr", "given": "Ben" } }, { "id": "Urban-A-L", "name": { "family": "Urban", "given": "Alex L." } }, { "id": "Vitale-S", "name": { "family": "Vitale", "given": "Salvatore" } }, { "id": "Veitch-J", "name": { "family": "Veitch", "given": "John" } }, { "id": "Graff-P", "name": { "family": "Graff", "given": "Philip" } }, { "id": "Berry-C-P-L", "name": { "family": "Berry", "given": "Christopher P. L." } }, { "id": "Mohapatra-S", "name": { "family": "Mohapatra", "given": "Satya" } }, { "id": "Mandel-I", "name": { "family": "Mandel", "given": "Ilya" }, "orcid": "0000-0002-6134-8946" } ] }, "title": "Going the Distance: Mapping Host Galaxies of LIGO and Virgo Sources in Three Dimensions Using Local Cosmography and Targeted Follow-up", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: distances and redshifts; gravitational waves; surveys", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 March 23; revised 2016 July 28; accepted 2016 July 29; published 2016 September 21. \n\nWe thank the Aspen Center for Physics and NSF grant #1066293 for hospitality during the conception, writing, and editing of this paper. We thank P. Shawhan and F. Tombesi for detailed feedback on the manuscript. Supplementary material, including a sample of reconstructed GW volume FITS files, will be made available at https://dcc.ligo.org/P1500071/public/html. See the Supplement (Singer et al. 2016) in the journal for more details. This is LIGO document P1500071-v7.\n\nPublished - apjl_829_1_L15.pdf
Submitted - 1603.07333v4.pdf
", "abstract": "The Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) discovered gravitational waves (GWs) from a binary black hole merger in 2015 September and may soon observe signals from neutron star mergers. There is considerable interest in searching for their faint and rapidly fading electromagnetic (EM) counterparts, though GW position uncertainties are as coarse as hundreds of square degrees. Because LIGO's sensitivity to binary neutron stars is limited to the local universe, the area on the sky that must be searched could be reduced by weighting positions by mass, luminosity, or star formation in nearby galaxies. Since GW observations provide information about luminosity distance, combining the reconstructed volume with positions and redshifts of galaxies could reduce the area even more dramatically. A key missing ingredient has been a rapid GW parameter estimation algorithm that reconstructs the full distribution of sky location and distance. We demonstrate the first such algorithm, which takes under a minute, fast enough to enable immediate EM follow-up. By combining the three-dimensional posterior with a galaxy catalog, we can reduce the number of galaxies that could conceivably host the event by a factor of 1.4, the total exposure time for the Swift X-ray Telescope by a factor of 2, the total exposure time for a synoptic optical survey by a factor of 2, and the total exposure time for a narrow-field optical telescope by a factor of 3. This encourages us to suggest a new role for small field of view optical instruments in performing targeted searches of the most massive galaxies within the reconstructed volumes.", "date": "2016-09-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "829", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L15", "id_number": "CaltechAUTHORS:20160929-081821795", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160929-081821795", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" } ] }, "other_numbering_system": { "items": [ { "id": "P1500071-v7", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/2041-8205/829/1/L15", "primary_object": { "basename": "1603.07333v4.pdf", "url": "https://authors.library.caltech.edu/records/gbkqe-y7766/files/1603.07333v4.pdf" }, "related_objects": [ { "basename": "apjl_829_1_L15.pdf", "url": "https://authors.library.caltech.edu/records/gbkqe-y7766/files/apjl_829_1_L15.pdf" } ], "pub_year": "2016", "author_list": "Singer, Leo P.; Chen, Hsin-Yu; et el." }, { "id": "https://authors.library.caltech.edu/records/cb84p-vye63", "eprint_id": 95844, "eprint_status": "archive", "datestamp": "2023-08-20 13:47:23", "lastmod": "2023-10-20 20:38:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yuan-Fang", "name": { "family": "Yuan", "given": "Fang" } }, { "id": "Jerkstrand-A", "name": { "family": "Jerkstrand", "given": "A." } }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Seitenzahl-I-R", "name": { "family": "Seitenzahl", "given": "I. R." } }, { "id": "Pastorello-A", "name": { "family": "Pastorello", "given": "A." } }, { "id": "Schulze-S", "name": { "family": "Schulze", "given": "S." }, "orcid": "0000-0001-6797-1889" }, { "id": "Chen-Ting-Wan", "name": { "family": "Chen", "given": "T.-W." }, "orcid": "0000-0002-1066-6098" }, { "id": "Childress-M-J", "name": { "family": "Childress", "given": "M. J." } }, { "id": "Fraser-M-P", "name": { "family": "Fraser", "given": "M." } }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Kotak-R", "name": { "family": "Kotak", "given": "R." }, "orcid": "0000-0001-5455-3653" }, { "id": "Ruiter-A-J", "name": { "family": "Ruiter", "given": "A. J." } }, { "id": "Schmidt-B-P", "name": { "family": "Schmidt", "given": "B. P." }, "orcid": "0000-0001-6589-1287" }, { "id": "Smartt-S-J", "name": { "family": "Smartt", "given": "S. J." }, "orcid": "0000-0002-8229-1731" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Terreran-G", "name": { "family": "Terreran", "given": "G." } }, { "id": "Tucker-B-E", "name": { "family": "Tucker", "given": "B. E." } }, { "id": "Barbarino-C", "name": { "family": "Barbarino", "given": "C." }, "orcid": "0000-0002-3821-6144" }, { "id": "Benetti-S", "name": { "family": "Benetti", "given": "S." }, "orcid": "0000-0002-3256-0016" }, { "id": "Elias-Rosa-N", "name": { "family": "Elias-Rosa", "given": "N." }, "orcid": "0000-0002-1381-9125" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Inserra-C", "name": { "family": "Inserra", "given": "C." }, "orcid": "0000-0002-3968-4409" }, { "id": "Kankare-E", "name": { "family": "Kankare", "given": "E." }, "orcid": "0000-0001-8257-3512" }, { "id": "Lee-M-Y", "name": { "family": "Lee", "given": "M. Y." } }, { "id": "Li-Kwan-Lok", "name": { "family": "Li", "given": "K. L." }, "orcid": "0000-0001-8229-2024" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Margheim-S", "name": { "family": "Margheim", "given": "S." } }, { "id": "Mehner-A", "name": { "family": "Mehner", "given": "A." }, "orcid": "0000-0002-9564-3302" }, { "id": "Ochner-P", "name": { "family": "Ochner", "given": "P." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Tomasella-L", "name": { "family": "Tomasella", "given": "L." } }, { "id": "Young-D-R", "name": { "family": "Young", "given": "D. R." } } ] }, "title": "450 d of Type II SN 2013ej in optical and near-infrared", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general, supernovae: individual: SN 2013ej", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2016 June 10. Received 2016 June 10; in original form 2016 April 18. Published: 15 June 2016.\n\nThe authors would like to thank Melissa Graham for scheduling the LCOGT observations. This paper is based on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programme ID 188.D-3003. The paper is partially based on observations collected at Copernico and Schmidt telescopes (Asiago, Italy) of the INAF \u2013 Osservatorio Astronomico di Padova. Some observations have been obtained also with the 1.22 m telescope + B&C spectrograph operated in Asiago by the Department of Physics and Astronomy of the University of Padova. This paper is partly based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil).\n\nThis research was made possible through the use of the APASS, funded by the Robert Martin Ayers Sciences Fund. 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\nParts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. IRS was supported by the ARC Laureate Grant FL0992131. SB, AP, NER and GT are partially supported by the PRIN-INAF 2014 project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'. SSchulze acknowledges support from CONICYT-Chile FONDECYT 3140534, Basal-CATA PFB-06/2007, and Project IC120009 'Millennium Institute of Astrophysics (MAS)' of Initiative Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. KM acknowledges support from the STFC through an Ernest Rutherford Fellowship. MS acknowledges support from STFC grant ST/L000679/1 and EU/FP7-ERC grant no. [615929]. AGY is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I- CORE Program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF grants; by the Weizmann-UK making connections programme; and by Kimmel and ARCHES awards.\n\nSupplemental Material - stw1419_Supplementary_Data.zip
", "abstract": "We present optical and near-infrared photometric and spectroscopic observations of SN 2013ej, in galaxy M74, from 1 to 450\u2009d after the explosion. SN 2013ej is a hydrogen-rich supernova, classified as a Type IIL due to its relatively fast decline following the initial peak. It has a relatively high peak luminosity (absolute magnitude MV = \u221217.6) but a small ^(56)Ni production of \u223c0.023 M\u2299. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H_\u03b1 profile typical for a Type IIL. During transition to the radioactive decay tail at \u223c100\u2009d, we find the SN to grow bluer in B \u2212 V colour, in contrast to some other Type II supernovae. At late times, the bolometric light curve declined faster than expected from ^(56)Co decay and we observed unusually broad and asymmetric nebular emission lines. Based on comparison of nebular emission lines most sensitive to the progenitor core mass, we find our observations are best matched to synthesized spectral models with a M_(ZAMS) = 12\u201315 M\u2299progenitor. The derived mass range is similar to but not higher than the mass estimated for Type IIP progenitors. This is against the idea that Type IIL are from more massive stars. Observations are consistent with the SN having a progenitor with a relatively low-mass envelope.", "date": "2016-09-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "461", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "2003-2018", "id_number": "CaltechAUTHORS:20190529-082821644", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-082821644", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Robert Martin Ayers Sciences Fund" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Australian Research Council", "grant_number": "CE110001020" }, { "agency": "Australian Research Council", "grant_number": "FL0992131" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN-INAF 2014" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3140534" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo", "grant_number": "IC120009" }, { "agency": "European Research Council (ERC)", "grant_number": "320360" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000679/1" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stw1419", "primary_object": { "basename": "stw1419_Supplementary_Data.zip", "url": "https://authors.library.caltech.edu/records/cb84p-vye63/files/stw1419_Supplementary_Data.zip" }, "pub_year": "2016", "author_list": "Yuan, Fang; Jerkstrand, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/zv6k3-28p56", "eprint_id": 96111, "eprint_status": "archive", "datestamp": "2023-08-20 13:46:51", "lastmod": "2023-10-20 20:52:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rubin-A", "name": { "family": "Rubin", "given": "Adam" }, "orcid": "0000-0003-4557-0632" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" } ] }, "title": "Unsupervised clustering of Type II supernova light curves", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 9; revised 2016 June 15; accepted 2016 June 16; published 2016 September 12. \n\nWe thank Y. Cao for reducing the spectrum of iPTF13blq. We thank A. Tanay and B. Zackay for helpful discussions. A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum universe I-CORE Program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards.\n\nSubmitted - 1602.01446.pdf
", "abstract": "As new facilities come online, the astronomical community will be provided with extremely large data sets of well-sampled light curves (LCs) of transients. This motivates systematic studies of the LCs of supernovae (SNe) of all types, including the early rising phase. We performed unsupervised k-means clustering on a sample of 59 R-band SN II LCs and find that the rise to peak plays an important role in classifying LCs. Our sample can be divided into three classes: slowly rising (II-S), fast rise/slow decline (II-FS), and fast rise/fast decline (II-FF). We also identify three outliers based on the algorithm. The II-FF and II-FS classes are disjoint in their decline rates, while the II-S class is intermediate and \"bridges the gap.\" This may explain recent conflicting results regarding II-P/II-L populations. The II-FS class is also significantly less luminous than the other two classes. Performing clustering on the first two principal component analysis components gives equivalent results to using the full LC morphologies. This indicates that Type II LCs could possibly be reduced to two parameters. We present several important caveats to the technique, and find that the division into these classes is not fully robust. Moreover, these classes have some overlap, and are defined in the R band only. It is currently unclear if they represent distinct physical classes, and more data is needed to study these issues. However, we show that the outliers are actually composed of slowly evolving SN IIb, demonstrating the potential of such methods. The slowly evolving SNe IIb may arise from single massive progenitors.", "date": "2016-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "828", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 111", "id_number": "CaltechAUTHORS:20190604-131727395", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190604-131727395", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0004-637x/828/2/111", "primary_object": { "basename": "1602.01446.pdf", "url": "https://authors.library.caltech.edu/records/zv6k3-28p56/files/1602.01446.pdf" }, "pub_year": "2016", "author_list": "Rubin, Adam and Gal-Yam, Avishay" }, { "id": "https://authors.library.caltech.edu/records/5f2nr-enh29", "eprint_id": 95962, "eprint_status": "archive", "datestamp": "2023-08-20 13:46:43", "lastmod": "2023-10-20 20:45:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rubin-A", "name": { "family": "Rubin", "given": "Adam" }, "orcid": "0000-0003-4557-0632" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" } ] }, "title": "Unsupervised clustering of Type II supernova light curves", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 9; revised 2016 June 15; accepted 2016 June 16; published 2016 September 12. \n\nWe thank Y. Cao for reducing the spectrum of iPTF13blq. We thank A. Tanay and B. Zackay for helpful discussions. A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum universe I-CORE Program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards.\n\nSubmitted - 1602.01446.pdf
", "abstract": "As new facilities come online, the astronomical community will be provided with extremely large data sets of well-sampled light curves (LCs) of transients. This motivates systematic studies of the LCs of supernovae (SNe) of all types, including the early rising phase. We performed unsupervised k-means clustering on a sample of 59 R-band SN II LCs and find that the rise to peak plays an important role in classifying LCs. Our sample can be divided into three classes: slowly rising (II-S), fast rise/slow decline (II-FS), and fast rise/fast decline (II-FF). We also identify three outliers based on the algorithm. The II-FF and II-FS classes are disjoint in their decline rates, while the II-S class is intermediate and \"bridges the gap.\" This may explain recent conflicting results regarding II-P/II-L populations. The II-FS class is also significantly less luminous than the other two classes. Performing clustering on the first two principal component analysis components gives equivalent results to using the full LC morphologies. This indicates that Type II LCs could possibly be reduced to two parameters. We present several important caveats to the technique, and find that the division into these classes is not fully robust. Moreover, these classes have some overlap, and are defined in the R band only. It is currently unclear if they represent distinct physical classes, and more data is needed to study these issues. However, we show that the outliers are actually composed of slowly evolving SN IIb, demonstrating the potential of such methods. The slowly evolving SNe IIb may arise from single massive progenitors.", "date": "2016-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "828", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 111", "id_number": "CaltechAUTHORS:20190531-074021836", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190531-074021836", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0004-637x/828/2/111", "primary_object": { "basename": "1602.01446.pdf", "url": "https://authors.library.caltech.edu/records/5f2nr-enh29/files/1602.01446.pdf" }, "pub_year": "2016", "author_list": "Rubin, Adam and Gal-Yam, Avishay" }, { "id": "https://authors.library.caltech.edu/records/5b7gr-c9m72", "eprint_id": 95964, "eprint_status": "archive", "datestamp": "2023-08-20 13:40:23", "lastmod": "2023-10-20 20:45:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Ergon-M", "name": { "family": "Ergon", "given": "M." } }, { "id": "Fraser-M", "name": { "family": "Fraser", "given": "M." }, "orcid": "0000-0003-2191-1674" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Jerkstrand-A", "name": { "family": "Jerkstrand", "given": "A." } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Bufano-F", "name": { "family": "Bufano", "given": "F." } }, { "id": "Elias-Rosa-N", "name": { "family": "Elias-Rosa", "given": "N." }, "orcid": "0000-0002-1381-9125" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D." }, "orcid": "0000-0002-3714-672X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Kotak-R", "name": { "family": "Kotak", "given": "R." }, "orcid": "0000-0001-5455-3653" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P." }, "orcid": "0000-0001-6876-8284" }, { "id": "Milisavljevic-D", "name": { "family": "Milisavljevic", "given": "D." }, "orcid": "0000-0002-0763-3885" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Nyholm-A", "name": { "family": "Nyholm", "given": "A." } }, { "id": "Pian-E", "name": { "family": "Pian", "given": "E." } }, { "id": "Smartt-S-J", "name": { "family": "Smartt", "given": "S." }, "orcid": "0000-0002-8229-1731" } ] }, "title": "PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual: PTF12os \u2013 galaxies: individual: NGC 5806 \u2013 techniques: image processing \u2013 supernovae: individual: iPTF13bvn", "note": "\u00a9 2016 ESO. Article published by EDP Sciences. \n\nReceived 8 February 2016; Accepted 26 May 2016; Published online 22 September 2016. \n\nWe gratefully acknowledge support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. 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. We acknowledge help from Rob Fesen, Craig Wheeler, and Shazrene Mohamed with the SALT data, as well as Jeffrey Silverman for help with the Keck data. We thank Alastair Bruce for assistance with the WHT observing and data reduction. We especially thank Shri Kulkarni, Mansi Kasliwal, Yi Cao, Anna-Lisa de Cia, Jerod Parrent, Assaf Horesh, Tom Matheson, Melissa Graham, Dan Perley, Eric Bellm, Ofer Yaron, Yen-Chen Pan and Kelsey Clubb for help with observations and/or reductions within the PTF effort. We also acknowledge observers, organizers, and data reducers who participated in the BLP 2012P campaign, in particular Andrea Pastorello, Max Stritzinger, Cosimo Inserra, Flora Cellier-Holzem, Luca Borsato, Valerio Nascimbeni, Stefano Benetti, and Stefan Taubenberger. We thank Doug Leonard for discussions regarding complementary MLO data. This work is partly 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. We acknowledge the exceptional support we received from the NOT staff throughout this campaign. Also based in part on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u0131sica de Canarias, in the island of La Palma. This work is based in part on observations from the LCOGT network. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. CAFOS, AFOSC, and EFOSC2 data were taken within the European supernova collaboration involved in the ESO-NTT large programme 184.D-1140 led by Stefano Benetti. Partially based on observations collected at Copernico telescope (Asiago, Italy) of the INAF \u2212 Osservatorio Astronomico di Padova, and the 2.2 m Telescope of the Centro Astronomico Hispano-Aleman, Calar Alto, Spain. Based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina), and Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil). The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-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. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT). This 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. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Based in part on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme 093.D-0199(A). We are grateful for the assistance of the staff members at all observatories where we obtained data.A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for Planning and Budgeting; by Minerva and ISF grants; by the Weizmann-UK making connections program; and by Kimmel and ARCHES awards. A.V.F.'s research is supported by NASA/HST grant AR-14295 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555; additional financial assistance was provided by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. N.E.R. is supported by the PRIN-INAF 2014 with the project: Transient Universe: unveiling new types of stellar explosions with PESSTO. This work was partly supported by the European Union FP7 program though ERC grant number 320360. We acknowledge funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement n\u00b0 [291222].\n\nAccepted Version - 1606.03074.pdf
", "abstract": "Context. We investigate two stripped-envelope supernovae (SNe) discovered in the nearby galaxy NGC 5806 by the (intermediate) Palomar Transient Factory [(i)PTF]. These SNe, designated PTF12os/SN 2012P and iPTF13bvn, exploded within ~520 days of one another at a similar distance from the host-galaxy center. We classify PTF12os as a Type IIb SN based on our spectral sequence; iPTF13bvn has previously been classified as Type Ib having a likely progenitor with zero age main sequence (ZAMS) mass below ~17 M_\u2299. Because of the shared and nearby host, we are presented with a unique opportunity to compare these two SNe. \n\nAims. Our main objective is to constrain the explosion parameters of iPTF12os and iPTF13bvn, and to put constraints on the SN progenitors. We also aim to spatially map the metallicity in the host galaxy, and to investigate the presence of hydrogen in early-time spectra of both SNe. \n\nMethods. We present comprehensive datasets collected on PTF12os and iPTF13bvn, and introduce a new automatic reference-subtraction photometry pipeline (FPipe) currently in use by the iPTF. We perform a detailed study of the light curves (LCs) and spectral evolution of the SNe. The bolometric LCs are modeled using the hydrodynamical code HYDE. We analyze early spectra of both SNe to investigate the presence of hydrogen; for iPTF13bvn we also investigate the regions of the Paschen lines in infrared spectra. We perform spectral line analysis of helium and iron lines to map the ejecta structure of both SNe. We use nebular models and late-time spectroscopy to constrain the ZAMS mass of the progenitors. We also perform image registration of ground-based images of PTF12os to archival HST images of NGC 5806 to identify a potential progenitor candidate. \n\nResults. We find that our nebular spectroscopy of iPTF13bvn remains consistent with a low-mass progenitor, likely having a ZAMS mass of ~12M_\u2299. Our late-time spectroscopy of PTF12os is consistent with a ZAMS mass of ~15M\u2299. We successfully identify a source in pre-explosion HST images coincident with PTF12os. The colors and absolute magnitude of this object are consistent between pre-explosion and late-time HST images, implying it is a cluster of massive stars. Our hydrodynamical modeling suggests that the progenitor of PTF12os had a compact He core with a mass of 3.25^(+0.77)_(-0.56)M_\u2299 at the time of the explosion, which had a total kinetic energy of 0.54^(+0.41)_(-0.25) \u00d710^(51) erg and synthesized 0.063^(+0.020)_(-0.011)M_\u2299 of strongly mixed \u2009^(56)Ni. Spectral comparisons to the Type IIb SN 2011dh indicate that the progenitor of PTF12os was surrounded by a thin hydrogen envelope with a mass lower than 0.02M_\u2299. We also find tentative evidence that the progenitor of iPTF13bvn could have been surrounded by a small amount of hydrogen prior to the explosion. This result is supported by possible weak signals of hydrogen in both optical and infrared spectra.", "date": "2016-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "593", "publisher": "EDP Sciences", "pagerange": "Art. No. A68", "id_number": "CaltechAUTHORS:20190531-075922693", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190531-075922693", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201628275", "primary_object": { "basename": "1606.03074.pdf", "url": "https://authors.library.caltech.edu/records/5b7gr-c9m72/files/1606.03074.pdf" }, "pub_year": "2016", "author_list": "Fremling, C.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/c0f1v-77315", "eprint_id": 70656, "eprint_status": "archive", "datestamp": "2023-08-22 18:36:06", "lastmod": "2023-10-20 23:18:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Singer-L-P", "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "id": "Chen-Hsin-Yu", "name": { "family": "Chen", "given": "Hsin-Yu" } }, { "id": "Holz-D-E", "name": { "family": "Holz", "given": "Daniel E." } }, { "id": "Farr-W-M", "name": { "family": "Farr", "given": "Will M." }, "orcid": "0000-0003-1540-8562" }, { "id": "Price-L-R", "name": { "family": "Price", "given": "Larry R." } }, { "id": "Raymond-V", "name": { "family": "Raymond", "given": "Vivien" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } }, { "id": "Cannizzo-J-K", "name": { "family": "Cannizzo", "given": "John" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Nissanke-S", "name": { "family": "Nissanke", "given": "Samaya" } }, { "id": "Coughlin-M-W", "name": { "family": "Coughlin", "given": "Michael" }, "orcid": "0000-0002-8262-2924" }, { "id": "Farr-B", "name": { "family": "Farr", "given": "Ben" } }, { "id": "Urban-A-L", "name": { "family": "Urban", "given": "Alex L." } }, { "id": "Vitale-S", "name": { "family": "Vitale", "given": "Salvatore" } }, { "id": "Veitch-J", "name": { "family": "Veitch", "given": "John" } }, { "id": "Graff-P", "name": { "family": "Graff", "given": "Philip" } }, { "id": "Berry-C-P-L", "name": { "family": "Berry", "given": "Christopher P. L." } }, { "id": "Mohapatra-S", "name": { "family": "Mohapatra", "given": "Satya" } }, { "id": "Mandel-I", "name": { "family": "Mandel", "given": "Ilya" }, "orcid": "0000-0002-6134-8946" } ] }, "title": "Supplement: \"Going the Distance: Mapping Host Galaxies of LIGO and Virgo Sources in Three Dimensions Using Local Cosmography and Targeted Follow-up\" (2016, ApJL, 829, L15)", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; galaxies: distances and redshifts; gravitational waves; surveys", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 May 13; accepted 2016 August 5; published 2016 September 21. \n\nWe thank the Aspen Center for Physics and NSF grant #1066293 for hospitality during the conception, writing, and editing of this paper. We thank P Shawhan and F Tombesi for detailed feedback on the manuscript. The online data release is available at https://dcc.ligo.org/P1500071/public/html. This is LIGO document P1500071-v7. \n\nSoftware: Astropy (Robitaille et al. 2013), GNU Scientific Library (Galassi & Gough 2009), HEALPix (G\u00f3rski et al. 2005), Matplotlib (Hunter 2007), Yt (Turk et al. 2011).\n\nPublished - apjs_226_1_10.pdf
Submitted - 1605.04242v3.pdf
", "abstract": "This is a supplement to the Letter of Singer et al., in which we demonstrated a rapid algorithm for obtaining joint 3D estimates of sky location and luminosity distance from observations of binary neutron star mergers with Advanced LIGO and Virgo. We argued that combining the reconstructed volumes with positions and redshifts of possible host galaxies can provide large-aperture but small field of view instruments with a manageable list of targets to search for optical or infrared emission. In this Supplement, we document the new HEALPix-based file format for 3D localizations of gravitational-wave transients. We include Python sample code to show the reader how to perform simple manipulations of the 3D sky maps and extract ranked lists of likely host galaxies. Finally, we include mathematical details of the rapid volume reconstruction algorithm.", "date": "2016-09", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "226", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 10", "id_number": "CaltechAUTHORS:20160929-082925782", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160929-082925782", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" } ] }, "other_numbering_system": { "items": [ { "id": "P1500071-v7", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0067-0049/226/1/10", "primary_object": { "basename": "1605.04242v3.pdf", "url": "https://authors.library.caltech.edu/records/c0f1v-77315/files/1605.04242v3.pdf" }, "related_objects": [ { "basename": "apjs_226_1_10.pdf", "url": "https://authors.library.caltech.edu/records/c0f1v-77315/files/apjs_226_1_10.pdf" } ], "pub_year": "2016", "author_list": "Singer, Leo P.; Chen, Hsin-Yu; et el." }, { "id": "https://authors.library.caltech.edu/records/s0k9v-yqv34", "eprint_id": 72121, "eprint_status": "archive", "datestamp": "2023-08-20 13:11:03", "lastmod": "2023-10-23 17:56:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Karamehmetoglu-E", "name": { "family": "Karamehmetoglu", "given": "E." }, "orcid": "0000-0001-6209-838X" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "B." }, "orcid": "0000-0002-7856-3570" }, { "id": "Ergon-M", "name": { "family": "Ergon", "given": "M." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P. R." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 ESO. \n\nReceived: 13 April 2016. Accepted: 31 May 2016. \n\nWe gratefully acknowledge the support from the Knut and Alice Wallenberg Foundation. This 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. This paper made use of Lowell Observatory's Discovery Channel Telescope (DCT). Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. The Large Monolithic Imager (LMI) on DCT was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). LANL participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program. 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. We thank N. Blagorodnova, E. Bellm, Y. Cao, G. Duggan, S. Kulkarni, J. Jencson, P. Nugent, for their precious help with the observations of iPTF15dtg and contribution to iPTF. We thank L. Yan for her comments on the paper. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the intermediate Palomar Transient Factory (iPTF) 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. A. Corsi acknowledges support from NSF CAREER Award #1455090.\n\nPublished - aa28703-16.pdf
", "abstract": "Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H- (and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (~10\u221215 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D).\n\nAims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (~30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star.\n\nMethods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission.\n\nResults. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (~10 M_\u2299) and strong ^(56)Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended (\u2273500 R_\u2299), low-mass (\u22730.045 M_\u2299) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored.\n\nConclusions. The large ejecta mass and the presence of H- and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive (\u227335 M_\u2299) WR star that experienced strong mass loss.", "date": "2016-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "592", "publisher": "EDP Sciences", "pagerange": "Art .No. A89", "id_number": "CaltechAUTHORS:20161117-112958640", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161117-112958640", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Discovery Communications" }, { "agency": "NSF", "grant_number": "AST-1005313" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1455090" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201628703", "primary_object": { "basename": "aa28703-16.pdf", "url": "https://authors.library.caltech.edu/records/s0k9v-yqv34/files/aa28703-16.pdf" }, "pub_year": "2016", "author_list": "Taddia, F.; Fremling, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/1mdcm-3cw87", "eprint_id": 96115, "eprint_status": "archive", "datestamp": "2023-08-20 13:13:34", "lastmod": "2023-10-20 20:52:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Liu-Yuan", "name": { "family": "Liu", "given": "Yuan" } } ] }, "title": "Finding binary active galactic nuclei candidates by the centroid shift in imaging surveys. II. Testing the method with SDSS J233635.75-010733.7", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 astrometry \u2013 methods: data analysis", "note": "\u00a9 2016 ESO. Article published by EDP Sciences. \n\nReceived 4 March 2016; Accepted 27 June 2016; Published online 25 July 2016. \n\nThe author thanks the referee for useful comments that clarified the paper. Some data in this work were obtained as part of the Palomar Transient Factory (PTF) project. This work is supported by the National Natural Science Foundation of China under grant Nos. 11573027, 11103019, 11133002, and 11103022.\n\nAccepted Version - 1607.00898.pdf
", "abstract": "We have previously proposed selecting binary active galactic nuclei (AGNs) candidates using the centroid shift of the images that is induced by the non-synchronous variations of the two nuclei. In this paper, a known binary AGN (SDSS J233635.75-010733.7) is employed to verify the functioning of this method. Using 162 exposures in the R band of the Palomar Transient Factory (PTF), an excess of dispersion in the positional distribution of the binary AGN is detected, although the two nuclei cannot be resolved in the images of PTF. We also propose a new method to compare the position of the binary AGN in PTF g and R band and find that the difference is highly significant even with only 20 exposures. This new method is efficient for two nuclei with different spectral energy distributions such as type I + type II AGN or an off-set AGN. Large-scale surveys such as the Panoramic Survey Telescope and Rapid Response System, and the Large Synoptic Survey Telescope are expected to discover a large sample of binary AGN candidates with these methods.", "date": "2016-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "592", "publisher": "EDP Sciences", "pagerange": "Art. No. L4", "id_number": "CaltechAUTHORS:20190604-142205284", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190604-142205284", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201628430", "primary_object": { "basename": "1607.00898.pdf", "url": "https://authors.library.caltech.edu/records/1mdcm-3cw87/files/1607.00898.pdf" }, "pub_year": "2016", "author_list": "Liu, Yuan" }, { "id": "https://authors.library.caltech.edu/records/v0ga0-vw051", "eprint_id": 72144, "eprint_status": "archive", "datestamp": "2023-08-20 13:11:29", "lastmod": "2023-10-23 17:58:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ferretti-R", "name": { "family": "Ferretti", "given": "R." }, "orcid": "0000-0001-7814-5814" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Butler-R-P", "name": { "family": "Butler", "given": "R. P." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Doran-G-B", "name": { "family": "Doran", "given": "G." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Freeland-E-E", "name": { "family": "Freeland", "given": "E." } }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Lundqvist-P", "name": { "family": "Lundqvist", "given": "P." }, "orcid": "0000-0002-3664-8082" }, { "id": "Mattila-S", "name": { "family": "Mattila", "given": "S." }, "orcid": "0000-0001-7497-2994" }, { "id": "Nordin-J", "name": { "family": "Nordin", "given": "J." } }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Petrushevska-T", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Vogt-S-S", "name": { "family": "Vogt", "given": "S. S." } }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "Time-varying sodium absorption in the Type Ia supernova 2013gh", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general, supernovae: individual: SN 2013gh, dust, extinction, circumstellar matter, supernovae: individual: iPTF 13dge", "note": "\u00a9 2016 ESO. \n\nReceived: 19 February 2016. Accepted: 2 May 2016. Published online: 18 July 2016. \n\nWe would like to thank Alexis Brandeker for assisting us with the UVES data, Jesper Sollerman for his helpful comments, and Daniela Vergani for sharing graphs of the VLA H I data. R.A. and A.G. acknowledge support from the Swedish Research Council and the Swedish Space Board. The Oskar Klein Centre is funded by the Swedish Research Council. A.V.F.'s research was funded by US NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. \n\nThis work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 091.D-0352(A). We made use of Swift/UVOT data reduced by P. J. Brown and released in the Swift Optical/Ultraviolet Supernova Archive (SOUSA). SOUSA is supported by NASA's Astrophysics Data Analysis Program through grant NNX13AF35G. This work is 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 makes use of observations from the LCOGT network. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. This research 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. LANL participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - aa28351-16.pdf
Submitted - 1605.01738v1.pdf
", "abstract": "Context. Temporal variability of narrow absorption lines in high-resolution spectra of Type Ia supernovae (SNe Ia) is studied to search for circumstellar matter. Time series which resolve the profiles of absorption lines such as Na I D or Ca II H&K are expected to reveal variations due to photoionisation and subsequent recombination of the gases. The presence, composition, and geometry of circumstellar matter may hint at the elusive progenitor system of SNe Ia and could also affect the observed reddening law.\n\nAims. To date, there are few known cases of time-varying Na I D absorption in SNe Ia, all of which occurred during relatively late phases of the supernova (SN) evolution. Photoionisation, however, is predicted to occur during the early phases of SNe Ia, when the supernovae peak in the ultraviolet. We attempt, therefore, to observe early-time absorption-line variations by obtaining high-resolution spectra of SNe before maximum light.\n\nMethods. We have obtained photometry and high-resolution spectroscopy of SNe Ia 2013gh and iPTF 13dge, to search for absorption-line variations. Furthermore, we study interstellar absorption features in relation to the observed photometric colours of the SNe.\n\nResults. Both SNe display deep Na I D and Ca II H&K absorption features. Furthermore, small but significant variations are detected in a feature of the Na I D profile of SN 2013gh. The variations are consistent with either geometric effects of rapidly moving or patchy gas clouds or photoionisation of Na I gas at R \u2248 10^(19) cm from the explosion.\n\nConclusions. Our analysis indicates that it is necessary to focus on early phases to detect photoionisation effects of gases in the circumstellar medium of SNe Ia. Different absorbers such as Na I and Ca II can be used to probe for matter at different distances from the SNe. The nondetection of variations during early phases makes it possible to put limits on the abundance of the species at those distances.", "date": "2016-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "592", "publisher": "EDP Sciences", "pagerange": "Art. No. A40", "id_number": "CaltechAUTHORS:20161118-070440638", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161118-070440638", "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": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "NASA", "grant_number": "NNX13AF35G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201628351", "primary_object": { "basename": "1605.01738v1.pdf", "url": "https://authors.library.caltech.edu/records/v0ga0-vw051/files/1605.01738v1.pdf" }, "related_objects": [ { "basename": "aa28351-16.pdf", "url": "https://authors.library.caltech.edu/records/v0ga0-vw051/files/aa28351-16.pdf" } ], "pub_year": "2016", "author_list": "Ferretti, R.; Amanullah, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/j35km-ygd63", "eprint_id": 70407, "eprint_status": "archive", "datestamp": "2023-08-20 12:54:57", "lastmod": "2023-10-20 22:55:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kaplan-D-L", "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Tom A." }, "orcid": "0000-0002-8850-3627" } ] }, "title": "PSR J1024\u20130719: A Millisecond Pulsar in an Unusual Long-period Orbit", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: general \u2013 pulsars: individual (PSR J1024\u20130719) \u2013 stars: distances", "note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2016 March 31; accepted 2016 May 10; published 2016 July 25.\n\nWe thank J. Creighton, C. Bassa, and S. Phinney for useful discussions. The NANOGrav project receives support from National Science Foundation (NSF) PIRE program award number 0968296 and NSF Physics Frontiers Center award number 1430284. P.S.R.'s work at NRL is supported by the Chief of Naval Research. Pulsar research at UBC is supported by an NSERC Discovery Grant and by the Canadian Institute for Advanced Research. 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nFacilities: GBT - Green Bank Telescope, PO:1.5m - Palomar Observatory's 1.5 meter Telescope, Hale (Double Beam Spectrograph) - , VLT:Antu (FORS1) - .\n\nPublished - apj_826_1_86.pdf
Submitted - 1604.00131v3.pdf
", "abstract": "PSR J1024\u20130719 is a millisecond pulsar that was long thought to be isolated. However, puzzling results concerning its velocity, distance, and low rotational period derivative have led to a reexamination of its properties. We present updated radio timing observations along with new and archival optical data which show that PSR J1024\u20130719 is most likely in a long-period (2\u201320 kyr) binary system with a low-mass (\u22480.4 M\u2299), low-metallicity (z \u2248 -0.9 dex) main-sequence star. Such a system can explain most of the anomalous properties of this pulsar. We suggest that this system formed through a dynamical exchange in a globular cluster that ejected it into a halo orbit, which is consistent with the low observed metallicity for the stellar companion. Further astrometric and radio timing observations such as measurement of the third period derivative could strongly constrain the range of orbital parameters.", "date": "2016-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "826", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 86", "id_number": "CaltechAUTHORS:20160916-150307252", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160916-150307252", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-0968296" }, { "agency": "NSF", "grant_number": "PHY-1430284" }, { "agency": "Chief of Naval Research" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "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": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0004-637X/826/1/86", "primary_object": { "basename": "1604.00131v3.pdf", "url": "https://authors.library.caltech.edu/records/j35km-ygd63/files/1604.00131v3.pdf" }, "related_objects": [ { "basename": "apj_826_1_86.pdf", "url": "https://authors.library.caltech.edu/records/j35km-ygd63/files/apj_826_1_86.pdf" } ], "pub_year": "2016", "author_list": "Kaplan, David L.; Kupfer, Thomas; et el." }, { "id": "https://authors.library.caltech.edu/records/egmvs-82509", "eprint_id": 71774, "eprint_status": "archive", "datestamp": "2023-08-20 12:55:24", "lastmod": "2023-10-23 15:14:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. 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M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Duggan-G-E", "name": { "family": "Duggan", "given": "G." }, "orcid": "0000-0002-9256-6735" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T." } }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E." }, "orcid": "0000-0001-8018-5348" }, { "id": "Cook-D", "name": { "family": "Cook", "given": "D." } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "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" } ] }, "title": "Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational waves \u2013 methods: observational", "note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2016 February 29; revised 2016 April 26; accepted 2016 May 2; published 2016 July 20.\n\nThe authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector, and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educaci\u00f3 Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources.\n\nThe Australian SKA Pathfinder is part of the Australia Telescope National Facility which is managed by CSIRO. The operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. Establishment of the Murchison Radio-astronomy Observatory was funded by the Australian Government and the Government of Western Australia. ASKAP uses advanced supercomputing resources at the Pawsey Supercomputing Centre. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site.\n\nA.J.C.T. acknowledges support from the Junta de Andaluc\u00eda (Project P07-TIC-03094) and Univ. of Auckland and NIWA for installing of the Spanish BOOTES-3 station in New Zealand, and support from the Spanish Ministry Projects AYA2012-39727-C03-01 and 2015-71718R.\n\nFunding for the DES Projects has been provided by the United States Department of Energy, the United States 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, the 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, Funda\u00e7\u00e3o Carlos Chagas Filho de Amparo \u00e0 Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00edfico e Tecnol\u00f3gico and the Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey.\n\nThe Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ\u00e9ticas, Medioambientales y Tecnol\u00f3gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen\u00f6ssische Technische Hochschule (ETH) Z\u00fcrich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci\u00e8ncies de l'Espai (IEEC/CSIC), the Institut de F\u00edsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00e4t M\u00fcnchen and the associated Excellence Cluster universe, the University of Michigan, the National Optical Astronomy Observatory, 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.\n\nThe DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.\n\nThe Fermi LAT Collaboration acknowledges support for LAT development, operation, and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. The Fermi GBM Collaboration acknowledges the support of NASA in the United States and DRL in Germany.\n\nGRAWITA acknowledges the support of INAF for the project \"Gravitational Wave Astronomy with the first detections of adLIGO and adVIRGO experiments.\"\n\nThis work exploited data by INTEGRAL, an ESA project with instruments and science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), and with the participation of Russia and the USA. The SPI ACS detector system has been provided by MPE Garching/Germany. We acknowledge the German INTEGRAL support through DLR grant 50 OG 1101.\n\nIPN work is supported in the US under NASA Grant NNX15AU74G.\n\nThis work is partly based on observations obtained with the Samuel Oschin 48 in Telescope and the 60 in Telescope at the Palomar Observatory as part of the Intermediate Palomar Transient Factory (iPTF) 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. M.M.K. and Y.C. acknowledge funding from the National Science Foundation PIRE program grant 1545949. A.A.M. acknowledges support from the Hubble Fellowship HST-HF-51325.01. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.\n\nJ-GEM is financially supported by KAKENHI Grant No. 24103003, 15H00774, and 15H00788 of MEXT Japan, 15H02069 and 15H02075 of JSPS, and the \"Optical and Near-Infrared Astronomy Inter-University Cooperation Program\" supported by MEXT.\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\nLOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, which are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. R. Fender acknowledges support from ERC Advanced Investigator Grant 267697.\n\nMASTER Global Robotic Net is supported in parts by Lomonosov Moscow State University Development programm, Moscow Union OPTICA, Russian Science Foundation 16-12-00085, RFBR15-02-07875, National Research Foundation of South Africa.\n\nWe thank JAXA and RIKEN for providing MAXI data. The MAXI team is partially supported by KAKENHI grant Nos. 24103002, 24540239, 24740186, and 23000004 of MEXT, Japan.\n\nThis work uses the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for the operation of the MWA is provided by the Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. The MWA acknowledges the iVEC Petabyte Data Store and the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University.\n\nPan-STARRS is supported by the University of Hawaii and the National Aeronautics and Space Administration's Planetary Defense Office under grant No. NNX14AM74G. The Pan-STARRS-LIGO effort is in collaboration with the LIGO Consortium and supported by Queen's University Belfast. The Pan-STARRS1 Sky Surveys 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, and 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 grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This work is based (in part) on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programs 188.D-3003, 191.D-0935.\n\nSome of the data presented herein were obtained at the Palomar Observatory, California Institute of Technology.\n\nS.J.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement No. [291222] and STFC grants ST/I001123/1 and ST/L000709/1. M.F. is supported by the European Union FP7 programme through ERC grant No. 320360. K.M. acknowledges support from the STFC through an Ernest Rutherford Fellowship.\n\nF.O.E. acknowledges support from FONDECYT through postdoctoral grant 3140326.\n\nParts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project No. CE110001020.\n\nFunding for Swift is provided by NASA in the US, by the UK Space Agency in the UK, and by the Agenzia Spaziale Italiana (ASI) in Italy. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We acknowledge the use of public data from the Swift data archive.\n\nThe TOROS Collaboration acknowledges support from Ministerio de Ciencia y Tecnolog\u00eda (MinCyT) and Consejo Nacional de Investigaciones Cientificas y Tecnol\u00f3gicas (CONICET) from Argentina and grants from the USA NSF PHYS 1156600 and NSF HRD 1242090.\n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nVST and VISTA observations were performed at the European Southern Observatory, Paranal, Chile. We acknowledge ESO personnel for their assistance during the observing runs.\n\nPublished - Abbott_2016_ApJL_826_L13.pdf
Submitted - 1602.08492v4.pdf
Supplemental Material - Abbott_2016_ApJS_225_8.pdf
", "abstract": "A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams.", "date": "2016-07-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "826", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L13", "id_number": "CaltechAUTHORS:20161107-124939230", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161107-124939230", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max-Planck Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Australian Research Council" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Council of Scientific and Industrial Research of India" }, { "agency": "Department of Science and Technology, India" }, { "agency": "Science and Engineering Research Board (SERB)" }, { "agency": "Ministry of Human Resource Development, India" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia i Competitivitat" }, { "agency": "Conselleria d'Educaci\u00f3 Cultura i Universitats" }, { "agency": "National Science Centre of Poland" }, { "agency": "European Commission" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Ministry of Economic Development and Innovation, Province of Ontario" }, { "agency": "National Science and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (MCTI)" }, { "agency": "Russian Foundation for Basic Research" }, { "agency": "Leverhulme Trust" }, { "agency": "Research Corporation" }, { "agency": "Ministry of Science and Technology (MOST)" }, { "agency": "Kavli Foundation" }, { "agency": "Australian Government" }, { "agency": "Government of Western Australia" }, { "agency": "Junta de Andaluc\u00eda", "grant_number": "P07-TIC-03094" }, { "agency": "Spanish Ministerio de Ciencia y Tecnolog\u00eda", "grant_number": "AYA2012-39727-C03-01" }, { "agency": "Spanish Ministerio de Ciencia y Tecnolog\u00eda", "grant_number": "2015-71718R" }, { "agency": "NSF", "grant_number": "AST-1138766" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "AYA2012-39559" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "ESP2013-48274" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "FPA2013-47986" }, { "agency": "Centro de Excelencia Severo Ochoa", "grant_number": "SEV-2012-0234" }, { "agency": "European Research Council", "grant_number": "240672" }, { "agency": "European Research Council", "grant_number": "291329" }, { "agency": "European Research Council", "grant_number": "306478" }, { "agency": "NASA", "grant_number": "NNX15AU74G" }, { "agency": "NSF", "grant_number": "1545949" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-51325.01" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24103003" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "15H00774" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "15H00788" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H02069" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H02075" }, { "agency": "European Research Council", "grant_number": "267697" }, { "agency": "Russian Science Foundation", "grant_number": "16-12-00085" }, { "agency": "Russian Foundation for Basic Research", "grant_number": "15-02-07875" }, { "agency": "National Research Foundation of South Africa" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24103002" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24540239" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "24740186" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "23000004" }, { "agency": "NASA", "grant_number": "NNX14AM74G" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "European Research Council", "grant_number": "291222" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I001123/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000709/1" }, { "agency": "European Research Council", "grant_number": "320360" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3140326" }, { "agency": "Australian Research Council", "grant_number": "CE110001020" }, { "agency": "NSF", "grant_number": "PHYS-1156600" }, { "agency": "NSF", "grant_number": "HRD-1242090" } ] }, "other_numbering_system": { "items": [ { "id": "LIGO-P1600137-v2", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "LIGO" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration", "Intermediate Palomar Transient Factory Collaboration", "PESSTO Collaboration" ] }, "doi": "10.3847/2041-8205/826/1/L13", "primary_object": { "basename": "1602.08492v4.pdf", "url": "https://authors.library.caltech.edu/records/egmvs-82509/files/1602.08492v4.pdf" }, "related_objects": [ { "basename": "Abbott_2016_ApJL_826_L13.pdf", "url": "https://authors.library.caltech.edu/records/egmvs-82509/files/Abbott_2016_ApJL_826_L13.pdf" }, { "basename": "Abbott_2016_ApJS_225_8.pdf", "url": "https://authors.library.caltech.edu/records/egmvs-82509/files/Abbott_2016_ApJS_225_8.pdf" } ], "pub_year": "2016", "author_list": "Abbott, B. P.; Abbott, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/kmhag-4de18", "eprint_id": 70230, "eprint_status": "archive", "datestamp": "2023-08-22 18:17:45", "lastmod": "2023-10-20 21:58:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Folatelli-G", "name": { "family": "Folatelli", "given": "Gast\u00f3n" } }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Kuncarayakti-H", "name": { "family": "Kuncarayakti", "given": "Hanindyo" } }, { "id": "Maeda-Keiichi", "name": { "family": "Maeda", "given": "Keiichi" }, "orcid": "0000-0003-2611-7269" }, { "id": "Bersten-M-C", "name": { "family": "Bersten", "given": "Melina C." } }, { "id": "Nomoto-Ken'ichi", "name": { "family": "Nomoto", "given": "Ken'ichi" }, "orcid": "0000-0001-9553-0685" }, { "id": "Pignata-G", "name": { "family": "Pignata", "given": "Giuliano" }, "orcid": "0000-0003-0006-0188" }, { "id": "Hamuy-M", "name": { "family": "Hamuy", "given": "Mario" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Zheng-Weikang", "name": { "family": "Zheng", "given": "WeiKang" }, "orcid": "0000-0002-2636-6508" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Clubb-K-I", "name": { "family": "Clubb", "given": "Kelsey I." } }, { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Elias-Rosa-N", "name": { "family": "Elias-Rosa", "given": "Nancy" }, "orcid": "0000-0002-1381-9125" }, { "id": "Foley-R-J", "name": { "family": "Foley", "given": "Ryan J." } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" } ] }, "title": "Disappearance of the Progenitor of Supernova iPTF13bvn", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 5806); stars: evolution; supernovae: general; supernovae: individual (iPTF13bvn)", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 April 22; revised 2016 May 25; accepted 2016 June 2; published 2016 July 5. \n\nThis research is supported by grants GO-13684, GO-13822, and AR-14295 from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. A.V.F.'s group is also grateful for funding through NSF grant AST-1211916, the TABASGO Foundation (KAIT and research support), the Sylvia & Jim Katzman Foundation, Clark and Sharon Winslow, and the Christopher R. Redlich Fund. This research is supported by the WPI Initiative MEXT (Japan), the Japan Society for the Promotion of Science (JSPS) KAKENHI grants 26800100 (K.M.) 23224004, and 26400222 (K.N.), and by the JSPS Open Partnership Bilateral Joint Research Project between Japan and Chile (K.M.). M.H., G.P., and H.K. acknowledge support from the Millennium Institute of Astrophysics (grant IC120009). H.K. also acknowledges FONDECYT grant 3140563. N.E.R. is supported by PRIN-INAF 2014. R.J.F. acknowledges support from NSF grant AST\u20131518052 and the Alfred P. Sloan Foundation. A.A.M. acknowledges support by NASA (Hubble Fellowship grant HST-HF-51325.01, under contract NAS 5-26555). Many UC Berkeley undergraduate students helped obtain Lick/Nickel data. Research at Lick Observatory is partially supported by a generous gift from Google.\n\nPublished - apjl_825_2_L22.pdf
Submitted - 1604.06821v2.pdf
", "abstract": "Supernova (SN) iPTF13bvn in NGC 5806 was the first Type Ib SN to have been tentatively associated with a progenitor in pre-explosion images. We performed deep ultraviolet (UV) and optical Hubble Space Telescope observations of the SN site ~740 days after explosion. We detect an object in the optical bands that is fainter than the pre-explosion object. This dimming is likely not produced by dust absorption in the ejecta; thus, our finding confirms the connection of the progenitor candidate with the SN. The object in our data is likely dominated by the fading SN, implying that the pre-SN flux is mostly due to the progenitor. We compare our revised pre-SN photometry with previously proposed models. Although binary progenitors are favored, models need to be refined. In particular, to comply with our deep UV detection limit, any companion star must be less luminous than a late-O star or substantially obscured by newly formed dust. A definitive progenitor characterization will require further observations to disentangle the contribution of a much fainter SN and its environment.", "date": "2016-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "825", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L22", "id_number": "CaltechAUTHORS:20160909-092857171", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160909-092857171", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "GO-13684" }, { "agency": "NASA", "grant_number": "GO-13822" }, { "agency": "NASA", "grant_number": "AR-14295" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Clark and Sharon Winslow Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26800100" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "23224004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26400222" }, { "agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo", "grant_number": "IC120009" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3140563" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NSF", "grant_number": "AST\u20131518052" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51325.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Google" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/2041-8205/825/2/L22", "primary_object": { "basename": "1604.06821v2.pdf", "url": "https://authors.library.caltech.edu/records/kmhag-4de18/files/1604.06821v2.pdf" }, "related_objects": [ { "basename": "apjl_825_2_L22.pdf", "url": "https://authors.library.caltech.edu/records/kmhag-4de18/files/apjl_825_2_L22.pdf" } ], "pub_year": "2016", "author_list": "Folatelli, Gast\u00f3n; Van Dyk, Schuyler D.; et el." }, { "id": "https://authors.library.caltech.edu/records/x58x3-yfq87", "eprint_id": 69334, "eprint_status": "archive", "datestamp": "2023-08-20 12:27:45", "lastmod": "2023-10-20 16:48:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gopalan-G", "name": { "family": "Gopalan", "given": "Giri" } }, { "id": "Plavchan-P", "name": { "family": "Plavchan", "given": "Peter" }, "orcid": "0000-0002-8864-1667" }, { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "Julian" }, "orcid": "0000-0003-2192-5371" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David" }, "orcid": "0000-0002-5741-3047" }, { "id": "von-Braun-K", "name": { "family": "von Braun", "given": "Kaspar" }, "orcid": "0000-0002-5823-4630" }, { "id": "Kane-S-R", "name": { "family": "Kane", "given": "Stephen R." }, "orcid": "0000-0002-7084-0529" } ] }, "title": "Application of the Trend Filtering Algorithm for Photometric Time Series Data", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis \u2013 methods: statistical", "note": "\u00a9 2016 The Astronomical Society of the Pacific. \n\nReceived 2015 October 3; accepted 2016 March 18; published 2016 June 23. \n\nG.G. would like to acknowledge the gracious support of the Caltech Summer Undergraduate Research Fellowship program for supporting this work during the summer of 2009.\n\nSubmitted - 1603.06001v1.pdf
", "abstract": "Detecting transient light curves (e.g., transiting planets) requires high-precision data, and thus it is important to effectively filter systematic trends affecting ground-based wide-field surveys. We apply an implementation of the Trend Filtering Algorithm (TFA) to the 2MASS calibration catalog and select Palomar Transient Factory (PTF) photometric time series data. TFA is successful at reducing the overall dispersion of light curves, however, it may over-filter intrinsic variables and increase \"instantaneous\" dispersion when a template set is not judiciously chosen. In an attempt to rectify these issues we modify the original TFA from the literature by including measurement uncertainties in its computation, including ancillary data correlated with noise, and algorithmically selecting a template set using clustering algorithms as suggested by various authors. This approach may be particularly useful for appropriately accounting for variable photometric precision surveys and/or combined data sets. In summary, our contributions are to provide a MATLAB software implementation of TFA and a number of modifications tested on synthetics and real data, summarize the performance of TFA and various modifications on real ground-based data sets (2MASS and PTF), and assess the efficacy of TFA and modifications using synthetic light curve tests consisting of transiting and sinusoidal variables. While the transiting variables test indicates that these modifications confer no advantage to transit detection, the sinusoidal variables test indicates potential improvements in detection accuracy.", "date": "2016-06-23", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "128", "number": "966", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 084504", "id_number": "CaltechAUTHORS:20160729-153020557", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160729-153020557", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/1538-3873/128/966/084504", "primary_object": { "basename": "1603.06001v1.pdf", "url": "https://authors.library.caltech.edu/records/x58x3-yfq87/files/1603.06001v1.pdf" }, "pub_year": "2016", "author_list": "Gopalan, Giri; Plavchan, Peter; et el." }, { "id": "https://authors.library.caltech.edu/records/eqnr9-1sy79", "eprint_id": 69103, "eprint_status": "archive", "datestamp": "2023-08-22 18:08:04", "lastmod": "2023-10-20 16:32:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "T." } }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E." }, "orcid": "0000-0001-8018-5348" }, { "id": "Cook-D", "name": { "family": "Cook", "given": "D." } }, { "id": "Duggan-G-E", "name": { "family": "Duggan", "given": "G. E." }, "orcid": "0000-0002-9256-6735" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "A. A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "iPTF Search for an Optical Counterpart to Gravitational-wave Transient GW150914", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational waves; methods: observational; techniques: spectroscopic; surveys", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 February 28; revised 2016 May 25; accepted 2016 May 26; published 2016 June 17. \n\nBased on observations obtained with the Samuel Oschin\nTelescope 48 inch and the 60 inch Telescope at the Palomar\nObservatory as part of the iPTF 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. M.M.K., R.L., and Y.C. acknowledge support from the National Science Foundation PIRE program grant 1545949. A.A.M. acknowledges support from the Hubble Fellowship HST-HF-51325.01. P.E.N. and Y.C. acknowledge support from the DOE under grant DE-AC02-05CH11231, Analytical Modeling for Extreme-Scale Computing Environments. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. A.C. and N.P. acknowledge support from NSF CAREER award 1455090. \nPart of the research was carried out at the Jet Propulsion\nLaboratory, California Institute of Technology, under a\ncontract with NASA. M.M.K. thanks Brian Metzger for\nproviding us theoretical light curves for neutron-powered\nprecursors. We thank the referee for constructive feedback.\n\nPublished - apjl_824_2_L24.pdf
Submitted - 1602.08764v2.pdf
", "abstract": "The intermediate Palomar Transient Factory (iPTF) autonomously responded to and promptly tiled the error region of the first gravitational-wave event GW150914 to search for an optical counterpart. Only a small fraction of the total localized region was immediately visible in the northern night sky, due both to Sun-angle and elevation constraints. Here, we report on the transient candidates identified and rapid follow-up undertaken to determine the nature of each candidate. Even in the small area imaged of 126 deg^2, after extensive filtering, eight candidates were deemed worthy of additional follow-up. Within two hours, all eight were spectroscopically classified by the Keck II telescope. Curiously, even though such events are rare, one of our candidates was a superluminous supernova. We obtained radio data with the Jansky Very Large Array and X-ray follow-up with the Swift satellite for this transient. None of our candidates appear to be associated with the gravitational-wave trigger, which is unsurprising given that GW150914 came from the merger of two stellar-mass black holes. This end-to-end discovery and follow-up campaign bodes well for future searches in this post-detection era of gravitational waves.", "date": "2016-06-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "824", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L24", "id_number": "CaltechAUTHORS:20160719-073716715", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160719-073716715", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OISE-1545949" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51325.01" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "AST-1455090" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/2041-8205/824/2/L24", "primary_object": { "basename": "1602.08764v2.pdf", "url": "https://authors.library.caltech.edu/records/eqnr9-1sy79/files/1602.08764v2.pdf" }, "related_objects": [ { "basename": "apjl_824_2_L24.pdf", "url": "https://authors.library.caltech.edu/records/eqnr9-1sy79/files/apjl_824_2_L24.pdf" } ], "pub_year": "2016", "author_list": "Kasliwal, M. M.; Cao, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/ayzb1-h1j28", "eprint_id": 68891, "eprint_status": "archive", "datestamp": "2023-09-15 05:29:54", "lastmod": "2023-10-23 21:18:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-Eran-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Cenko-S-Bradley", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Shaviv-Nir-J", "name": { "family": "Shaviv", "given": "N. J." }, "orcid": "0000-0003-3894-8422" }, { "id": "Duggan-Gina-E", "name": { "family": "Duggan", "given": "G." }, "orcid": "0000-0002-9256-6735" }, { "id": "Strotjohann-Nora-Linn", "name": { "family": "Strotjohann", "given": "N.-L." }, "orcid": "0000-0002-4667-6730" }, { "id": "Rubin-Alan-E", "name": { "family": "Rubin", "given": "A." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Gal-Yam-Avishay", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Nugent-Peter-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Sollerman-Jesper", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fransson-Claes", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Filippenko-Alexei-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Perley-Daniel-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Yaron-Ofer", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "PTF 13efv - An outburst 500 days prior to the SNHunt 275 explosion and its radiative efficiency", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (PTF13efv, SNHunt275)", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 September 21; accepted 2016 March 7; published 2016 June 3. \n\nWe thank M. Graham, P. Kelly, A. Bostroem, I. Shivvers, and W. Zheng for their help obtaining some of the optical spectra. We are also grateful to the staffs of the Palomar, Lick, and Keck Observatories for their excellent assistance. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), the Israel Science Foundation, Minerva, Weizmann-UK, and the I-Core program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF). N.J.S. is grateful for the IBM Einstein Fellowship. A.G.Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards. M.S. acknowledges support from the Royal Society and EU/FP7-ERC grant No. 615929. A.V.F.'s research is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916.\n\nPublished - apj_824_1_6.pdf
Submitted - 1605.02450v1.pdf
", "abstract": "The progenitors of some supernovae (SNe) exhibit outbursts with super-Eddington luminosities prior to their final explosions. This behavior is common among SNe IIn, but the driving mechanisms of these precursors are not yet well-understood. SNHunt 275 was announced as a possible new SN during 2015 May. Here we report on pre-explosion observations of the location of this event by the Palomar Transient Factory (PTF) and report the detection of a precursor about 500 days prior to the 2015 May activity (PTF 13efv). The observed velocities in the 2015 transient and its 2013 precursor absorption spectra are low (1000\u20132000 km s^(\u22121)), so it is not clear yet if the recent activity indeed marks the final disruption of the progenitor. Regardless of the nature of this event, we use the PTF photometric and spectral observations, as well as Swift-UVOT observations, to constrain the efficiency of the radiated energy relative to the total kinetic energy of the precursor. We find that, using an order-of-magnitude estimate and under the assumption of spherical symmetry, the ratio of the radiated energy to the kinetic energy is in the range of 4 \u00d7 10^(\u22122) to 3.4 \u00d7 10^3.", "date": "2016-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "824", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 6", "id_number": "CaltechAUTHORS:20160707-105410507", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160707-105410507", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Google" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Kimmel Award" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "ARCHES Award" }, { "agency": "IBM Einstein Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/824/1/6", "primary_object": { "basename": "1605.02450v1.pdf", "url": "https://authors.library.caltech.edu/records/ayzb1-h1j28/files/1605.02450v1.pdf" }, "related_objects": [ { "basename": "apj_824_1_6.pdf", "url": "https://authors.library.caltech.edu/records/ayzb1-h1j28/files/apj_824_1_6.pdf" } ], "pub_year": "2016", "author_list": "Ofek, E. O.; Cenko, S. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/ejxj7-v8266", "eprint_id": 63958, "eprint_status": "archive", "datestamp": "2023-08-20 12:00:27", "lastmod": "2023-10-17 18:31:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." } }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Nordin-J", "name": { "family": "Nordin", "given": "Jakob" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Fox-O-D", "name": { "family": "Fox", "given": "Ori" }, "orcid": "0000-0003-2238-1572" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "E. Y." } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "Brian D." }, "orcid": "0000-0002-7856-3570" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Lee-William-H", "name": { "family": "Lee", "given": "William H." } }, { "id": "Chotard-N", "name": { "family": "Chotard", "given": "Nicolas" } } ] }, "title": "Absence of Fast-moving Iron in an Intermediate Type Ia Supernova between Normal and Super-Chandrasekhar", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual (iPTF13asv) \u2013 ultraviolet: general", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2016 January 4; accepted 2016 April 10; published 2016 June 1. \n\nThis research is partly supported by the Swift Guest Investigator program and by the National Science Foundation. Y.C. and M.M.K. acknowledge support from the National Science Foundation PIRE program grant 1545949. A.G. and R.A. acknowledge support from the Swedish Research Council and the Swedish Space Board. E.Y.H. acknowledges the support provided by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. \n\nSome observations were obtained with the SuperNova Integral Field Spectrograph on the University of Hawaii 2.2 m telescope as part of the Nearby Supernova Factory II project, a scientific collaboration between the Centre de Recherche Astronomique de Lyon, Institut de Physique Nucl'eaire de Lyon, Laboratoire de Physique Nucl'eaire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and Centre de Physique des Particules de Marseille. \n\nSome data in this paper 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\nWe also thank the RATIR project team and the staff of the Observatorio Astron\u00f3mico Nacional on Sierra San Pedro M\u00e1rtir. RATIR is a collaboration between the University of California, the Universidad Nacional Aut\u00f3noma de M\u00e9xico, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector and hardware and software support from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astron\u00f3mico Nacional on Sierra San Pedro M\u00e1rtir and the operation of both is funded through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants LN 260369, and UNAM PAPIIT grant IG100414. \n\nA portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright 2016 California Institute of Technology. All Rights Reserved. US Government Support Acknowledged.\n\nPublished - Cao_2016_ApJ_823_147.pdf
Submitted - 1601.00686v2.pdf
", "abstract": "In this paper, we report observations of a peculiar SN Ia iPTF13asv (a.k.a., SN2013cv) from the onset of the explosion to months after its peak. The early-phase spectra of iPTF13asv show an absence of iron absorption, indicating that synthesized iron elements are confined to low-velocity regions of the ejecta, which, in turn, implies a stratified ejecta structure along the line of sight. Our analysis of iPTF13asv's light curves and spectra shows that it is an intermediate case between normal and super-Chandrasekhar events. On the one hand, its light curve shape (B-band \u0394m_(15) = 1.03 \u00b1 0.01) and overall spectral features resemble those of normal SNe Ia. On the other hand, its large peak optical and UV luminosity (M_B = -19.84 mag, M_(uvm2) = -15.5 mag) and its low but almost constant Si II velocities of about 10,000 km s^(\u22121) are similar to those in super-Chandrasekhar events, and its persistent carbon signatures in the spectra are weaker than those seen commonly in super-Chandrasekhar events. We estimate a ^(56)Ni mass of 0.81 \u00b1 ^(+0.10)_(-0.18) M\u2299 and a total ejecta mass of 1.59^(+0.45)_(-0.12)M\u2299. The large ejecta mass of iPTF13asv and its stratified ejecta structure together seemingly favor a double-degenerate origin.", "date": "2016-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "823", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 147", "id_number": "CaltechAUTHORS:20160126-080342517", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160126-080342517", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Danish Agency for Science and Technology and Innovation" }, { "agency": "NASA", "grant_number": "NNX09AH71G" }, { "agency": "NASA", "grant_number": "NNX09AT02G" }, { "agency": "NASA", "grant_number": "NNX10AI27G" }, { "agency": "NASA", "grant_number": "NNX12AE66G" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "LN 260369" }, { "agency": "Universidad Nacional Aut\u00f3noma de M\u00e9xico (UNAM)", "grant_number": "IG100414" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/823/2/147", "primary_object": { "basename": "1601.00686v2.pdf", "url": "https://authors.library.caltech.edu/records/ejxj7-v8266/files/1601.00686v2.pdf" }, "related_objects": [ { "basename": "Cao_2016_ApJ_823_147.pdf", "url": "https://authors.library.caltech.edu/records/ejxj7-v8266/files/Cao_2016_ApJ_823_147.pdf" } ], "pub_year": "2016", "author_list": "Cao, Yi; Johansson, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/qz3qx-44q88", "eprint_id": 67667, "eprint_status": "archive", "datestamp": "2023-08-20 11:42:52", "lastmod": "2023-10-18 21:22:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Prentice-S-J", "name": { "family": "Prentice", "given": "S. J." } }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Pian-E", "name": { "family": "Pian", "given": "E." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Rubin-A", "name": { "family": "Rubin", "given": "A." }, "orcid": "0000-0003-4557-0632" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Zheng-W", "name": { "family": "Zheng", "given": "W." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" } ] }, "title": "The bolometric light curves and physical parameters of stripped-envelope supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 February 4. Received 2016 February 2. In original form 2015 December 4. First published online February 8, 2016. \n\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 US Department of Energy under Contract No. DE-AC02-05CH11231. AVF's research was funded by NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. A.G.Y. is supported by the EU/FP7 via ERC grant no. 307260, \"The Quantum Universe\" I-Core program by the Israeli Committee for planning and budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and YeS awards.\n\nPublished - MNRAS-2016-Prentice-2973-3002.pdf
Submitted - 1602.01736v2.pdf
", "abstract": "The optical and optical/near-infrared pseudobolometric light curves of 84 stripped-envelope supernovae (SNe) are constructed using a consistent method and a standard cosmology. The light curves are analysed to derive temporal characteristics and peak luminosity L_p, enabling the construction of a luminosity function. Subsequently, the mass of ^(56)Ni synthesised in the explosion, along with the ratio of ejecta mass to ejecta kinetic energy, are found. Analysis shows that host-galaxy extinction is an important factor in accurately determining luminosity values as it is significantly greater than Galactic extinction in most cases. It is found that broad-lined SNe Ic (SNe Ic-BL) and gamma-ray burst SNe are the most luminous subtypes with a combined median L_p, in erg s^(\u22121), of log(L_p) = 42.99 compared to 42.51 for SNe Ic, 42.50 for SNe Ib, and 42.36 for SNe IIb. It is also found that SNe Ic-BL synthesise approximately twice the amount of ^(56)Ni compared with SNe Ic, Ib, and IIb, with median M_(Ni) = 0.34, 0.16, 0.14, and 0.11 M_\u2299, respectively. SNe Ic-BL, and to a lesser extent SNe Ic, typically rise from L_p/2 to L_p more quickly than SNe Ib/IIb; consequently, their light curves are not as broad.", "date": "2016-05-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "458", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2973-3002", "id_number": "CaltechAUTHORS:20160606-073147446", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160606-073147446", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weismann-UK" }, { "agency": "Kimmel Award" }, { "agency": "YeS awards" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stw299", "primary_object": { "basename": "MNRAS-2016-Prentice-2973-3002.pdf", "url": "https://authors.library.caltech.edu/records/qz3qx-44q88/files/MNRAS-2016-Prentice-2973-3002.pdf" }, "related_objects": [ { "basename": "1602.01736v2.pdf", "url": "https://authors.library.caltech.edu/records/qz3qx-44q88/files/1602.01736v2.pdf" } ], "pub_year": "2016", "author_list": "Prentice, S. J.; Mazzali, P. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/f1x8e-2s302", "eprint_id": 67638, "eprint_status": "archive", "datestamp": "2023-08-20 11:35:54", "lastmod": "2023-10-18 21:20:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Andrews-J-E", "name": { "family": "Andrews", "given": "Jennifer E." }, "orcid": "0000-0003-0123-0062" }, { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Mauerhan-J-C", "name": { "family": "Mauerhan", "given": "Jon C." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Bond-H-E", "name": { "family": "Bond", "given": "Howard E." }, "orcid": "0000-0003-1377-7145" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Clubb-K-I", "name": { "family": "Clubb", "given": "Kelsey I." } }, { "id": "Graham-M-L", "name": { "family": "Graham", "given": "Melissa L." }, "orcid": "0000-0002-9154-3136" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Jencson-J-E", "name": { "family": "Jencson", "given": "Jacob" }, "orcid": "0000-0001-5754-4007" }, { "id": "Bally-J", "name": { "family": "Bally", "given": "John" }, "orcid": "0000-0001-8135-6612" }, { "id": "Ubeda-L", "name": { "family": "Ubeda", "given": "Leonardo" } }, { "id": "Sabbi-E", "name": { "family": "Sabbi", "given": "Elena" }, "orcid": "0000-0003-2954-7643" } ] }, "title": "Massive star mergers and the recent transient in NGC 4490: a more massive cousin of V838 Mon and V1309 Sco", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: general circumstellar matter stars: evolution stars: massive stars: winds, outflows", "note": "\u00a9 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2016 January 25. Received 2016 January 7; in original form 2015 September 16. \n\nSome of the data reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. We thank the staffs at Lick and MMT Observatories for their assistance with the observations. We also appreciate the help of Jeff Silverman for some of the Lick observations. Data from Steward Observatory facilities were obtained as part of the observing programme AZTEC: Arizona Transient Exploration and Characterization. Lindsey Kabot assisted with early stages of the MMT spectral data reduction. The work presented here is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These are based in part on observations associated with programme #13364 (Legacy ExtraGalactic UV Survey, LEGUS). This paper has made use of the higher level data products provided by the LEGUS team. \n\nNS and JEA received partial support from National Science Foundation (NSF) grants AST-1210599 and AST-1312221. MMK acknowledges support from the Carnegie-Princeton fellowship. Funding for this effort was provided in part by the Spitzer SPIRITS Cycles 10\u201312 exploration science programme. The supernova research of AVF's group at U.C. Berkeley presented here is supported by Gary & Cynthia Bengier, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. JJ is supported by an NSF Graduate Research Fellowship under Grant No. DGE-1144469.\n\nPublished - MNRAS-2016-Smith-950-62.pdf
", "abstract": "The Galactic transient V1309 Sco was the result of a merger in a low-mass star system, while V838 Mon was thought to be a similar merger event from a more massive B-type progenitor. In this paper, we study a recent optical and infrared (IR) transient discovered in the nearby galaxy NGC\u20094490 named NGC\u20094490-OT2011 (NGC\u20094490-OT hereafter), which appeared similar to these merger events (unobscured progenitor, irregular multi-peaked light curve, increasingly red colour, similar optical spectrum, IR excess at late times), but which had a higher peak luminosity and longer duration in outburst. NGC\u20094490-OT has less in common with the class of SN 2008S-like transients. A progenitor detected in pre-eruption Hubble Space Telescope (HST) images, combined with upper limits in the IR, requires a luminous and blue progenitor that has faded in late-time HST images. The same source was detected by Spitzer and ground-based data as a luminous IR (2\u20135 \u03bcm) transient, indicating a transition to a self-obscured state qualitatively similar to the evolution seen in other stellar mergers and in luminous blue variables. The post-outburst dust-obscured source is too luminous and too warm at late times to be explained with an IR echo, suggesting that the object survived the event. The luminosity of the enshrouded IR source is similar to that of the progenitor. Compared to proposed merger events, the more massive progenitor of NGC\u20094490-OT seems to extend a correlation between stellar mass and peak luminosity, and may suggest that both of these correlate with duration. We show that spectra of NGC\u20094490-OT and V838 Mon also resemble light-echo spectra of \u03b7 Car, prompting us to speculate that \u03b7 Car may be an extreme extension of this phenomenon.", "date": "2016-05-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "458", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "950-962", "id_number": "CaltechAUTHORS:20160603-083351085", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160603-083351085", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "AST-1210599" }, { "agency": "NSF", "grant_number": "AST-1312221" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Spitzer SPIRITS" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "AutoScope Corporation" }, { "agency": "Lick Observatory" }, { "agency": "University of California" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Google" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stw219", "primary_object": { "basename": "MNRAS-2016-Smith-950-62.pdf", "url": "https://authors.library.caltech.edu/records/f1x8e-2s302/files/MNRAS-2016-Smith-950-62.pdf" }, "pub_year": "2016", "author_list": "Smith, Nathan; Andrews, Jennifer E.; et el." }, { "id": "https://authors.library.caltech.edu/records/b8db2-4zm47", "eprint_id": 67740, "eprint_status": "archive", "datestamp": "2023-08-22 17:52:45", "lastmod": "2023-10-18 21:39:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "Po-Chieh" }, "orcid": "0000-0001-8894-0854" }, { "id": "Lin-Chie-Cheng", "name": { "family": "Lin", "given": "Chien-Cheng" } }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "id": "Lee-Chien-De", "name": { "family": "Lee", "given": "Chien-De" }, "orcid": "0000-0002-3142-7299" }, { "id": "Konidaris-N-P", "name": { "family": "Konidaris", "given": "Nick" }, "orcid": "0000-0003-1905-2815" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Chen-Wen-Ping", "name": { "family": "Chen", "given": "Wen-Ping" }, "orcid": "0000-0003-0262-272X" }, { "id": "Chen-Hui-Chen", "name": { "family": "Chen", "given": "Hui-Chen" } }, { "id": "Malkan-M-A", "name": { "family": "Malkan", "given": "Matthew A." }, "orcid": "0000-0001-6919-1237" }, { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Huang-Li-Ching", "name": { "family": "Huang", "given": "Li-Ching" } }, { "id": "Cheng-Yu-Chi", "name": { "family": "Cheng", "given": "Yu-Chi" } }, { "id": "Edelson-R", "name": { "family": "Edelson", "given": "Rick" } }, { "id": "Ritter-A", "name": { "family": "Ritter", "given": "Andreas" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Be Stars in the Open Cluster NGC 6830", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: star clusters: individual (NGC 6830); instrumentation: spectrographs; stars: emission-line, Be", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 November 11; accepted 2016 February 24; published 2016 April 20. \n\nWe thank the referee for constructive comments. We are also grateful to the staff of Lulin and Lick Observatory for helping with the observations. This work is supported, in part, by the National Science Council and the Ministry of Science and Technology of Taiwan under grants MOST 104-2119-M-008-024 (W.-H.I.), MOST 103-2112-M-008-024-MY3 (W.-P.C.), MOST 104-2112-M-008-012-MY3 (C.-C.N.), and NSC 103-2917-I-564-004 (P.-C.Y.). The Lulin Observatory is funded by the Ministry of Science and Technology of Taiwan, and operated by National Central University of Taiwan. The Lick Observatory is funded by Google Inc. and operated by the University of California. 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 - aj_151_5_121.pdf
Submitted - 1604.02276v1.pdf
", "abstract": "We report the discovery of two new Be stars, and re-identify one known Be star in the open cluster NGC 6830. Eleven H\u03b1 emitters were discovered using the H\u03b1 imaging photometry of the Palomar Transient Factory Survey. Stellar membership of the candidates was verified with photometric and kinematic information using 2MASS data and proper motions. The spectroscopic confirmation was carried out by using the Shane 3 m telescope at the Lick observatory. Based on their spectral types, three H\u03b1 emitters were confirmed as Be stars with H\u03b1 equivalent widths greater than \u221210 \u00c5. Two objects were also observed by the new spectrograph spectral energy distribution-machine (SED-machine) on the Palomar 60-inch Telescope. The SED-machine results show strong H\u03b1 emission lines, which are consistent with the results of the Lick observations. The high efficiency of the SED-machine can provide rapid observations for Be stars in a comprehensive survey in the future.", "date": "2016-05", "date_type": "published", "publication": "Astronomical Journal", "volume": "151", "number": "5", "publisher": "American Astronomical Society", "pagerange": "Art. No. 121", "id_number": "CaltechAUTHORS:20160607-131223777", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160607-131223777", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 104-2119-M-008-024" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 103-2112-M-001-030-MY3" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "MOST 104-2112-M-008-012-MY3" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC 103- 2917-I-564-004" }, { "agency": "Google Inc." }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-6256/151/5/121", "primary_object": { "basename": "1604.02276v1.pdf", "url": "https://authors.library.caltech.edu/records/b8db2-4zm47/files/1604.02276v1.pdf" }, "related_objects": [ { "basename": "aj_151_5_121.pdf", "url": "https://authors.library.caltech.edu/records/b8db2-4zm47/files/aj_151_5_121.pdf" } ], "pub_year": "2016", "author_list": "Yu, Po-Chieh; Lin, Chien-Cheng; et el." }, { "id": "https://authors.library.caltech.edu/records/e770q-jr878", "eprint_id": 64148, "eprint_status": "archive", "datestamp": "2023-08-20 11:02:53", "lastmod": "2023-10-17 19:33:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Migotto-K", "name": { "family": "Migotto", "given": "K." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Armen-S", "name": { "family": "Armen", "given": "S." } }, { "id": "Duggan-G-E", "name": { "family": "Duggan", "given": "G." }, "orcid": "0000-0002-9256-6735" }, { "id": "Ergon-M", "name": { "family": "Ergon", "given": "M." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "C." }, "orcid": "0000-0001-8532-3594" }, { "id": "Hosseinzadeh-G", "name": { "family": "Hosseinzadeh", "given": "G." }, "orcid": "0000-0002-0832-2974" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "Leonard-D-C", "name": { "family": "Leonard", "given": "D. C." } }, { "id": "Lunnan-R", "name": { "family": "Lunnan", "given": "R." }, "orcid": "0000-0001-9454-4639" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F. J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Moon-Dae-Sik", "name": { "family": "Moon", "given": "D.-S." }, "orcid": "0000-0003-4200-5064" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wozniak", "given": "P. R." }, "orcid": "0000-0002-9919-3310" } ] }, "title": "Long-rising Type II supernovae from Palomar Transient Factory and Caltech Core-Collapse Project", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 Galaxy: abundances", "note": "\u00a9 2016 ESO. \n\nReceived 23 November 2015. Accepted 23 January 2016. \n\nWe thank the staffs of the various observatories (Palomar, Lick, Keck, etc.) where data for this study were obtained. The Oskar Klein Centre is funded by the Swedish Research Council. We gratefully acknowledge the support from the Knut and Alice Wallenberg Foundation. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards. A.V.F.'s research is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. D.C.L. and S.F.A. acknowledge support from NSF grants AST-1009571 and AST-1210311, under which part of this research (photometry data collected at MLO) was carried out. We thank Joseph Fedrow, Alyssa Del Rosario, Chuck Horst, and David Jaimes for assistance with the MLO observations. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. This research has made use of the APASS database, located at the AAVSO web site; funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We acknowledge contributions to CCCP by S. B. Cenko, D. Fox, D. Sand, and A. Soderberg. We acknowledge M. Sullivan and K. Sharon for helping with the CCCP spectral observations. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development program.\n\nPublished - aa27811-15.pdf
Submitted - 1601.07368v1.pdf
", "abstract": "Context. Supernova (SN) 1987A was a peculiar hydrogen-rich event with a long-rising (~ 84 d) light curve, stemming from the explosion of a compact blue supergiant star. Only a few similar events have been presented in the literature in recent decades. Aims. We present new data for a sample of six long-rising Type II SNe (SNe II), three of which were discovered and observed by the Palomar Transient Factory (PTF) and three observed by the Caltech Core-Collapse Project (CCCP). Our aim is to enlarge this\nsmall family of long-rising SNe II, characterizing their differences in terms of progenitor and explosion parameters. We also study the metallicity of their environments. \n\nMethods. Optical light curves, spectra, and host-galaxy properties of these SNe are presented and analyzed. Detailed comparisons with known SN 1987A-like events in the literature are shown, with particular emphasis on the absolute magnitudes, colors, expansion velocities, and host-galaxy metallicities. Bolometric properties are derived from the multiband light curves. By modeling the early time emission with scaling relations derived from the SuperNova Explosion Code (SNEC) models of MESA progenitor stars, we estimate the progenitor radii of these transients. The modeling of the bolometric light curves also allows us to estimate other progenitor and explosion parameters, such as the ejected ^(56)Ni mass, the explosion energy, and the ejecta mass. \n\nResults. We present PTF12kso, a long-rising SN II that is estimated to have the largest amount of ejected ^(56)Ni mass measured for this class. PTF09gpn and PTF12kso are found at the lowest host metallicities observed for this SN group. The variety of early light curve luminosities depends on the wide range of progenitor radii of these SNe, from a few tens of R_\u2299 (SN 2005ci) up to thousands\n(SN 2004ek) with some intermediate cases between 100 R_\u2299 (PTF09gpn) and 300 R_\u2299 (SN 2004em).\n\nConclusions. We confirm that long-rising SNe II with light-curve shapes closely resembling that of SN 1987A generally arise from blue supergiant (BSG) stars. However, some of them, such as SN 2004em, likely have progenitors with larger radii (~ 300 R_\u2299, typical of yellow supergiants) and can thus be regarded as intermediate cases between normal SNe IIP and SN 1987A-like SNe. Some\nextended red supergiant (RSG) stars such as the progenitor of SN 2004ek can also produce long-rising SNe II if they synthesized a large amount of ^(56 0Ni in the explosion. Low host metallicity is confirmed as a characteristic of the SNe arising from compact BSG stars.", "date": "2016-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "588", "publisher": "EDP Sciences", "pagerange": "Art. No. A5", "id_number": "CaltechAUTHORS:20160202-082620745", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160202-082620745", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NSF", "grant_number": "AST-1009571" }, { "agency": "NSF", "grant_number": "AST-1210311" }, { "agency": "NSF", "grant_number": "AST-1302771" }, { "agency": "Robert Martin Ayers Sciences Fund" }, { "agency": "Google" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201527811", "primary_object": { "basename": "aa27811-15.pdf", "url": "https://authors.library.caltech.edu/records/e770q-jr878/files/aa27811-15.pdf" }, "related_objects": [ { "basename": "1601.07368v1.pdf", "url": "https://authors.library.caltech.edu/records/e770q-jr878/files/1601.07368v1.pdf" } ], "pub_year": "2016", "author_list": "Taddia, F.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/a9xh2-a0706", "eprint_id": 63963, "eprint_status": "archive", "datestamp": "2023-08-20 10:57:18", "lastmod": "2023-10-17 18:31:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rubin-A", "name": { "family": "Rubin", "given": "Adam" }, "orcid": "0000-0003-4557-0632" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" } ] }, "title": "Type II supernova energetics and comparison of light curves to shock-cooling models", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 The American Astronomical Society. Received 2015 September 7; accepted 2015 November 23; published 2016 March 16.\n\nWe thank E. Waxman for helpful discussions. We are grateful to the staffs at the many observatories where data for this study were collected (Palomar, Lick, Keck, etc.). We thank J. Silverman, G. Duggan, A. Miller, A. Waszczak, E. Bellm, K. Mooley, J. Van Roestel, A. Cucchiara, R. J. Foley, M. T. Kandrashoff, B. Sesar, I. Shivvers, J. S. Bloom, D. Xu, J. Surace, and L. Magill for helping with some of the observations and data reduction. Specifically for assistance with the MLO observations, we acknowledge N. Duong, T. Fetherolf, S. Brunker, R. Dixon, and A. Rachubo. A.G.Y. is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I-CORE Program by the Israeli Committee for Planning and Budgeting and the Israel Science Foundation (ISF); by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), ISF, Minerva, Weizmann-UK, and the I-CORE Program of the Planning and Budgeting Committee and the ISF. M.S. acknowledges support from the Royal Society and EU/FP7-ERC grant no [615929]. K.M. is grateful for a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). D.C.L., S.F.A., J.C.H., and J.M.F. are supported by NSF grants AST-1009571 and AST-1210311,\nunder which part of this research (photometry data collected at MLO) was carried out. The supernova research of A.V.F.'s group at U.C. Berkeley presented herein is supported by Gary & Cynthia Bengier, the Christopher\nR. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group\nin the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. This research has made use of the APASS database, located at the AAVSO web site. Funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration. Copyright 2015 California Institute of Technology. All Rights Reserved. US Government Support Acknowledged. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and\nDevelopment program.\n\nPublished - apj_820_1_33.pdf
Submitted - 1512.00733.pdf
", "abstract": "During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band Type II SN light curves that are well monitored during their rise, having > 5 detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1-3 days. We show that\nthe energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the model of Rabinak & Waxman (2011), while the progenitor radius cannot be determined based on R-band data alone. We find that Type II SN explosion energies span a range of\nE/M = (0.2-20)x10^(51) erg/(10 M_\u2609), and have a mean energy per unit mass of \u3008E/M\u3009 = 0.85x10^(51)erg/(10 M_\u2609), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of ^(56)Ni produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the\ndecline rate (\u0394m_(15)), the decline rate is weakly correlated with the rise time, and the rise time is not\nsignificantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events.", "date": "2016-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "820", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 33", "id_number": "CaltechAUTHORS:20160126-092427530", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160126-092427530", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation (ISF)" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel award" }, { "agency": "ARCHES award" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Marie Curie Intra-European Fellowship" }, { "agency": "NSF", "grant_number": "AST-1009571" }, { "agency": "NSF", "grant_number": "AST-1210311" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Google" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Robert Martin Ayers Sciences Fund" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/820/1/33", "primary_object": { "basename": "apj_820_1_33.pdf", "url": "https://authors.library.caltech.edu/records/a9xh2-a0706/files/apj_820_1_33.pdf" }, "related_objects": [ { "basename": "1512.00733.pdf", "url": "https://authors.library.caltech.edu/records/a9xh2-a0706/files/1512.00733.pdf" } ], "pub_year": "2016", "author_list": "Rubin, Adam; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/jfm20-yf848", "eprint_id": 62660, "eprint_status": "archive", "datestamp": "2023-08-20 10:57:11", "lastmod": "2023-10-25 17:18:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ganot-N", "name": { "family": "Ganot", "given": "Noam" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sagiv-I", "name": { "family": "Sagiv", "given": "Ilan" } }, { "id": "Waxman-E", "name": { "family": "Waxman", "given": "Eli" }, "orcid": "0000-0002-9038-5877" }, { "id": "Lapid-O", "name": { "family": "Lapid", "given": "Ofer" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Chelouche-D", "name": { "family": "Chelouche", "given": "Doron" } }, { "id": "Rafter-S", "name": { "family": "Rafter", "given": "Stephen" } }, { "id": "Behar-E", "name": { "family": "Behar", "given": "Ehud" } }, { "id": "Laor-A", "name": { "family": "Laor", "given": "Ari" } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Nakar-U", "name": { "family": "Nakar", "given": "Udi" } }, { "id": "Maoz-D", "name": { "family": "Maoz", "given": "Dan" } }, { "id": "Trakhtenbrot-B", "name": { "family": "Trakhtenbrot", "given": "Benny" }, "orcid": "0000-0002-3683-7297" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Thomas A." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Gezari-S", "name": { "family": "Gezari", "given": "Suvi" }, "orcid": "0000-0003-3703-5154" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" } ] }, "title": "The detection rate of early UV emission from supernovae: A dedicated GALEX/PTF survey and calibrated theoretical estimates", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 December 19. Accepted 2016 February 4. Published 2016 March 17. \n\nThis research was supported by grants from the Israeli Space Agency (ISA) and the Ministry of Science, Technology and Space (MOS). Additional funding was provided by the EU via ERC grant 307260, the ISF, and a Kimmel award.\n\nPublished - apj_820_1_57.pdf
Submitted - 1412.4063v2.pdf
", "abstract": "The radius and surface composition of an exploding massive star, as well as the explosion energy per unit mass, can be measured using early UV observations of core collapse supernovae (SNe). We present the first results from a simultaneous GALEX/PTF search for early UV emission from SNe. Six Type II SNe and one Type II superluminous SN (SLSN-II) are clearly detected in the GALEX NUV data. We compare our detection rate with theoretical estimates based on early, shock-cooling UV light curves calculated from models that fit existing Swift and GALEX observations well, combined with volumetric SN rates. We find that our observations are in good agreement with calculated rates assuming that red supergiants (RSGs) explode with fiducial radii of 500R_\u2299, explosion energies of 10^(51) erg, and ejecta masses of 10 M_\u2299. Exploding blue supergiants and Wolf-Rayet stars are poorly constrained. We describe how such observations can be used to derive the progenitor radius, surface composition and explosion energy per unit\nmass of such SN events, and we demonstrate why UV observations are critical for such measurements. We use the fiducial RSG parameters to estimate the detection rate of SNe during the shock-cooling phase (< 1 d after explosion)\nfor several ground-based surveys (PTF, ZTF, and LSST). We show that the proposed wide-field UV explorer ULTRASAT mission, is expected to find > 100 SNe per year (~ 0.5 SN per deg^2), independent of host galaxy extinction, down\nto an NUV detection limit of 21.5mag AB. Our pilot GALEX/PTF project thus convincingly demonstrates that a dedicated, systematic SN survey at the NUV band is a compelling method to study how massive stars end their life.", "date": "2016-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "820", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 57", "id_number": "CaltechAUTHORS:20151207-145315969", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151207-145315969", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israeli Space Agency" }, { "agency": "Ministry of Science, Technology and Space (Israel)" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israel Science Foundation" }, { "agency": "Kimmel Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "ULTRASAT Science Team", "WTTH Consortium", "GALEX Science Team", "Palomar Transient Factory Collaboration" ] }, "doi": "10.3847/0004-637X/820/1/57", "primary_object": { "basename": "1412.4063v2.pdf", "url": "https://authors.library.caltech.edu/records/jfm20-yf848/files/1412.4063v2.pdf" }, "related_objects": [ { "basename": "apj_820_1_57.pdf", "url": "https://authors.library.caltech.edu/records/jfm20-yf848/files/apj_820_1_57.pdf" } ], "pub_year": "2016", "author_list": "Ganot, Noam; Gal-Yam, Avishay; et el." }, { "id": "https://authors.library.caltech.edu/records/rjxfm-8be26", "eprint_id": 96124, "eprint_status": "archive", "datestamp": "2023-08-20 10:47:58", "lastmod": "2023-10-20 20:52:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Wolf-W-M", "name": { "family": "Wolf", "given": "William M." }, "orcid": "0000-0002-6828-0630" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "Giorgos" }, "orcid": "0000-0002-8597-0756" }, { "id": "Hardin-D", "name": { "family": "Hardin", "given": "Delphine" } }, { "id": "Prajs-S", "name": { "family": "Prajs", "given": "Szymon" } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Svirski-G", "name": { "family": "Svirski", "given": "Gilad" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Katz-B", "name": { "family": "Katz", "given": "Boaz" } }, { "id": "McCully-C", "name": { "family": "McCully", "given": "Curtis" }, "orcid": "0000-0001-5807-7893" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "Chris" }, "orcid": "0000-0003-1731-0497" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "Stefano" }, "orcid": "0000-0001-8818-0795" }, { "id": "Astier-P", "name": { "family": "Astier", "given": "Pierre" } }, { "id": "Balland-C", "name": { "family": "Balland", "given": "Cristophe" } }, { "id": "Carlberg-R-G", "name": { "family": "Carlberg", "given": "Ray G." } }, { "id": "Conley-A-J", "name": { "family": "Conley", "given": "Alex" } }, { "id": "Fouchez-D", "name": { "family": "Fouchez", "given": "Dominique" } }, { "id": "Guy-J", "name": { "family": "Guy", "given": "Julien" } }, { "id": "Pain-R", "name": { "family": "Pain", "given": "Reynald" } }, { "id": "Palanque-Delabrouille-N", "name": { "family": "Palanque-Delabrouille", "given": "Nathalie" } }, { "id": "Perrett-K", "name": { "family": "Perrett", "given": "Kathy" } }, { "id": "Pritchet-C-J", "name": { "family": "Pritchet", "given": "Chris J." } }, { "id": "Regnault-N", "name": { "family": "Regnault", "given": "Nicolas" } }, { "id": "Rich-James", "name": { "family": "Rich", "given": "James" } }, { "id": "Ruhlmann-Kleider-V", "name": { "family": "Ruhlmann-Kleider", "given": "Vanina" } } ] }, "title": "Rapidly Rising Transients in the Supernova - Superluminous Supernova Gap", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual (PTF10iam, SNLS04D4ec, SNLS05D2bk, SNLS06D1hc, Dougie)", "note": "\u00a9 2016 The American Astronomical Society. \n\nReceived 2015 September 1; accepted 2016 January 14; published 2016 February 25. \n\nWe thank J. Silverman and J. Johansson for helpful discussions and S. Sim and M. Kromer for sharing their white dwarf detonation models. This paper is based on observations obtained at the Cerro Paranal Observatory (ESO program 176.A-0589) and with the Samuel Oschin Telescope as part of the Palomar Transient Factory project. We are grateful for the assistance of the staffs at the various observatories where data were obtained. This work made use of the astronomy & astrophysics package for Matlab (Ofek 2014). Some of the work presented here is supported by the National Science Foundation under Grant No. 1313484. I.A. and A.G. acknowledge support by the Israeli Science Foundation and an EU/FP7/ERC grant. A.G. further acknowledges grants from the BSF, GIF, and Minerva, as well as the \"Quantum universe\" I-Core program of the planning and budgeting committee and the ISF, and a Kimmel Investigator award. The work of W.M.W. and L.B. was supported by the National Science Foundation under grants PHY 11-25915 and AST 11-09174. The Dark Cosmology Centre is funded by the Danish National Research Foundation. 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. Some data are based on observations obtained at the Gemini Observatory 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), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia, Tecnologia e Inovao (Brazil), and Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina). This work made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. 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\nAccepted Version - 1511.00704.pdf
", "abstract": "We present observations of four rapidly rising (t_(rise) \u2248 10 days) transients with peak luminosities between those of supernovae (SNe) and superluminous SNe (M_(peak) \u2248 \u221220)\u2014one discovered and followed by the Palomar Transient Factory (PTF) and three by the Supernova Legacy Survey. The light curves resemble those of SN 2011kl, recently shown to be associated with an ultra-long-duration gamma-ray burst (GRB), though no GRB was seen to accompany our SNe. The rapid rise to a luminous peak places these events in a unique part of SN phase space, challenging standard SN emission mechanisms. Spectra of the PTF event formally classify it as an SN II due to broad H\u03b1emission, but an unusual absorption feature, which can be interpreted as either high velocity H\u03b1(though deeper than in previously known cases) or Si II (as seen in SNe Ia), is also observed. We find that existing models of white dwarf detonations, CSM interaction, shock breakout in a wind (or steeper CSM), and magnetar spin down cannot readily explain the observations. We consider the possibility that a \"Type 1.5 SN\" scenario could be the origin of our events. More detailed models for these kinds of transients and more constraining observations of future such events should help to better determine their nature.", "date": "2016-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "819", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 35", "id_number": "CaltechAUTHORS:20190604-150226384", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190604-150226384", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.3847/0004-637x/819/1/35", "primary_object": { "basename": "1511.00704.pdf", "url": "https://authors.library.caltech.edu/records/rjxfm-8be26/files/1511.00704.pdf" }, "pub_year": "2016", "author_list": "Arcavi, Iair; Wolf, William M.; et el." }, { "id": "https://authors.library.caltech.edu/records/e8qt3-j7571", "eprint_id": 66597, "eprint_status": "archive", "datestamp": "2023-08-20 10:41:32", "lastmod": "2023-10-18 18:37:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Moquist-P", "name": { "family": "Moquist", "given": "P." } }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Rubin-A-E", "name": { "family": "Rubin", "given": "A." } }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Graham-M-L", "name": { "family": "Graham", "given": "M. L." }, "orcid": "0000-0002-9154-3136" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Pan-Yen-Chen", "name": { "family": "Pan", "given": "Y.-C." } }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" } ] }, "title": "Metallicity from Type II supernovae from the (i)PTF", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 Galaxy: abundances", "note": "\u00a9 2016 ESO. \n\nReceived 16 December 2015; Accepted 7 February 2016. \n\nWe gratefully acknowledge the support from the Knut and Alice Wallenberg Foundation. The Oskar Klein Centre is funded by the Swedish Research Council. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards. A.V.F.'s research is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. We are grateful to the staffs at the many observatories where data for this study were collected (Palomar, Lick, Keck, etc.). We thank R. Foley, J. Bloom, Green, N. Cucchiara, A. Horesh, K. I. Clubb, M. T. Kandrashoff, K. Maguire, A. De Cia, S. Tang, B. Zackay, B. Sesar, A. Waszczak, I. Shivvers, who helped with some of the observations and data reduction. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. This 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. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. D.X. acknowledges the support of the One-Hundred-Talent Program from the National Astronomical Observatories, Chinese Academy of Sciences. This work is partly based on the Bachelor thesis by P. Moquist.\n\nPublished - aa27983-15.pdf
Submitted - 1602.01433v2.pdf
", "abstract": "Type IIP supernovae (SNe IIP) have recently been proposed as metallicity (Z) probes. The spectral models of Dessart et al. (2014, MNRAS, 440, 1856) showed that the pseudo-equivalent width of Fe\u2009II \u03bb5018 (pEW_(5018)) during the plateau phase depends on the primordial Z, but there was a paucity of SNe IIP exhibiting pEW_(5018) that were compatible with Z < 0.4 Z\u2299. This lack might be due to some physical property of the SN II population or to the fact that those SNe have been discovered in luminous, metal-rich targeted galaxies. Here we use SN II observations from the untargeted (intermediate) Palomar Transient Factory [(i)PTF] survey, aiming to investigate the pEW_(5018) distribution of this SN population and, in particular, to look for the presence of SNe II at lower Z. We perform pEW_(5018) measurements on the spectra of a sample of 39 (i)PTF SNe II, selected to have well-constrained explosion epochs and light-curve properties. Based on the comparison with the pEW_(5018) spectral models, we subgrouped our SNe into four Z bins from Z \u2248 0.1 Z\u2299 up to Z \u2248 2 Z\u2299. We also independently investigated the Z of the hosts by using their absolute magnitudes and colors and, in a few cases, using strong-line diagnostics from spectra. We searched for possible correlations between SN observables, such as their peak magnitudes and the Z inferred from pEW_(5018). We found 11 events with pEW_(5018) that were small enough to indicate Z \u2248 0.1 Z\u2299. The trend of pEW_(5018) with Z matches the Z estimates obtained from the host-galaxy photometry, although the significance of the correlation is weak. We also found that SNe with brighter peak magnitudes have smaller pEW_(5018) and occur at lower Z.", "date": "2016-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "587", "publisher": "EDP Sciences", "pagerange": "Art. No. L7", "id_number": "CaltechAUTHORS:20160502-143626914", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160502-143626914", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Swedish Research Council" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Google" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "AST-1302771" }, { "agency": "Chinese Academy of Sciences" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201527983", "primary_object": { "basename": "1602.01433v2.pdf", "url": "https://authors.library.caltech.edu/records/e8qt3-j7571/files/1602.01433v2.pdf" }, "related_objects": [ { "basename": "aa27983-15.pdf", "url": "https://authors.library.caltech.edu/records/e8qt3-j7571/files/aa27983-15.pdf" } ], "pub_year": "2016", "author_list": "Taddia, F.; Moquist, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/3zdzs-p7649", "eprint_id": 63939, "eprint_status": "archive", "datestamp": "2023-08-20 10:25:33", "lastmod": "2023-10-17 18:30:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K. P." }, "orcid": "0000-0002-2557-5180" }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "G." }, "orcid": "0000-0002-7083-4049" }, { "id": "Bourke-S-A", "name": { "family": "Bourke", "given": "S." } }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Myers-Steven-Theodore", "name": { "family": "Myers", "given": "S. T." } }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "D. B." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E." }, "orcid": "0000-0001-8018-5348" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "The Caltech-NRAO Stripe 82 Survey (CNSS) Paper. I. The Pilot Radio Transient Survey in 50 deg^2", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs \u2013 galaxies: active \u2013 radio continuum: galaxies \u2013 stars: activity \u2013 supernovae: general \u2013 surveys", "note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2015 April 29; accepted 2015 December 2; published 2016 February 11.\n\nThe authors extend sincere thanks to Joan Wrobel and other scheduling staff at the NRAO in Socorro for extensive help with the scheduling of the VLA observations, and to James Robnett and other computing staff for their untiring assistance with the data storage and allocation of computing resources. The authors also wish to thank Luis Ho, Branimir Sesar, Eran Ofek, Sanjay Bhatnagar, Urvashi Rau, Kumar Golap, Vivek Dhawan, Craig Walker, Talvikki Hovatta, Tim Pearson, Anthony Readhead, Chuck Steidel, and Allison Strom for insightful discussions. The contribution of PTF collaboration members to optical data processing and optical follow-up observations relevant for this project is acknowledged. K.P.M. is grateful to NRAO for the Grote Reber Fellowship, and to Yamini Jangir for going over this manuscript and providing useful suggestions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. S.R.K.'s research in part is supported by NASA and NSF. 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. This research has made extensive use of ADS, CDS (Vizier and SIMBAD), NED, SDSS, and IRSA. We thank the anonymous referee for comments that helped in improving certain parts of the manuscript.\n\nPublished - Mooley_2016_ApJ_818_105.pdf
Submitted - 1601.01693.pdf
", "abstract": "We have commenced a multiyear program, the Caltech-NRAO Stripe 82 Survey (CNSS), to search for radio transients with the Jansky VLA in the Sloan Digital Sky Survey Stripe 82 region. The CNSS will deliver five epochs over the entire ~270 deg^2 of Stripe 82, an eventual deep combined map with an rms noise of ~40 \u03bcJy and catalogs at a frequency of 3 GHz, and having a spatial resolution of 3''. This first paper presents the results from an initial pilot survey of a 50 deg^2 region of Stripe 82, involving four epochs spanning logarithmic timescales between 1 week and 1.5 yr, with the combined map having a median rms noise of 35 \u03bcJy. This pilot survey enabled the development of the hardware and software for rapid data processing, as well as transient detection and follow-up, necessary for the full 270 deg^2 survey. Data editing, calibration, imaging, source extraction, cataloging, and transient identification were completed in a semi-automated fashion within 6 hr of completion of each epoch of observations, using dedicated computational hardware at the NRAO in Socorro and custom-developed data reduction and transient detection pipelines. Classification of variable and transient sources relied heavily on the wealth of multiwavelength legacy survey data in the Stripe 82 region, supplemented by repeated mapping of the region by the Palomar Transient Factory. A total of 3.9^(+0.5)_(-0.9)% of the few thousand detected point sources were found to vary by greater than 30%, consistent with similar studies at 1.4 and 5 GHz. Multiwavelength photometric data and light curves suggest that the variability is mostly due to shock-induced flaring in the jets of active galactic nuclei (AGNs). Although this was only a pilot survey, we detected two bona fide transients, associated with an RS CVn binary and a dKe star. Comparison with existing legacy survey data (FIRST, VLA-Stripe 82) revealed additional highly variable and transient sources on timescales between 5 and 20 yr, largely associated with renewed AGN activity. The rates of such AGNs possibly imply episodes of enhanced accretion and jet activity occurring once every ~40,000 yr in these galaxies. We compile the revised radio transient rates and make recommendations for future transient surveys and joint radio-optical experiments.", "date": "2016-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "818", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 105", "id_number": "CaltechAUTHORS:20160125-142728419", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160125-142728419", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Radio Astronomy Observatory" }, { "agency": "NASA" }, { "agency": "NSF" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/818/2/105", "primary_object": { "basename": "Mooley_2016_ApJ_818_105.pdf", "url": "https://authors.library.caltech.edu/records/3zdzs-p7649/files/Mooley_2016_ApJ_818_105.pdf" }, "related_objects": [ { "basename": "1601.01693.pdf", "url": "https://authors.library.caltech.edu/records/3zdzs-p7649/files/1601.01693.pdf" } ], "pub_year": "2016", "author_list": "Mooley, K. P.; Hallinan, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/swgv9-thc30", "eprint_id": 62656, "eprint_status": "archive", "datestamp": "2023-08-20 10:14:44", "lastmod": "2023-10-25 17:18:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Toy-V-L", "name": { "family": "Toy", "given": "V. L." } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "E." }, "orcid": "0000-0001-8018-5348" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Singer-L-P", "name": { "family": "Singer", "given": "L." }, "orcid": "0000-0001-9898-5597" } ] }, "title": "Optical and near-infrared observations of SN 2013dx associated with GRB 130702A", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: individual (GRB 130702A) \u2013 supernovae: individual (SN 2013dx)", "note": "\u00a9 2016. The American Astronomical Society. Received 2015 July 30; accepted 2015 December 22; published 2016 February 9.\n\nWe gratefully acknowledge S. Schulze, F. Olivares E., A.\nMelandri, M. Modjaz, Y. Liu, and E. Pian for generously\nsharing their raw data, which significantly improved the\nanalysis for this paper. We also thank J. Lyman, M. Modjaz,\nR. Thomas, and the anonymous referee for useful feedback on\nthe manuscript.\nThis work was supported by the National Aeronautics and\nSpace Administration (NASA) Headquarters under the NASA\nEarth and Space Science Fellowship Program (Grant\nNNX12AL70H to V.T.). V.T. and S.V. were partially\nsupported by NSF/ATI grant 1207785. The research of\nA.V.F.\u02bcs group at UC Berkeley has been funded by (NSF)\ngrant AST-1211916, Gary and Cynthia Bengier, the Richard\nand Rhoda Goldman Fund, the TABASGO Foundation, and\nthe Christopher R. Redlich Fund. J.M.S. is supported by an\nNSF Astronomy and Astrophysics Postdoctoral Fellowship\nunder award AST-1302771. A.G.Y. is supported by the EU/\nFP7 via ERC grant no. 307260, the Quantum universe I-Core\nprogram by the Israeli Committee for planning and budgeting\nand the ISF; by Minerva and ISF grants; by the Weizmann-UK\n\"making connections\" program; and by Kimmel and ARCHES\nawards. A.C. acknowledges support from the NASA-Swift GI\nprogram via grants 13-SWIFT13-0030 and 14-SWIFT14-0024.\nE.T. acknowledges support for this project under the Fermi\nGuest Investigator Program. The work of D.S. was carried out\nat the Jet Propulsion Laboratory, California Institute of\nTechnology, under a contract with NASA. We also acknowledge\nthe help of K. Markey, E. Alduena, A. Alduena, and S.\nKuo from Walden School for their help with the Palomar\nobservations on 2013 July 8.\nWe thank the RATIR project team and the staff of the\nObservatorio Astron\u00f3mico Nacional on Sierra San Pedro\nM\u00e1rtir. RATIR is a collaboration between the University of\nCalifornia, the Universidad Nacional Auton\u00f3ma de M\u00e9xico,\nNASA Goddard Space Flight Center, and Arizona State\nUniversity, benefiting from the loan of an H2RG detector\nand hardware and software support from Teledyne Scientific\nand Imaging. RATIR, the automation of the Harold L. Johnson\nTelescope of the Observatorio Astron\u00f3mico Nacional on\nSierra San Pedro M\u00e1rtir, and the operation of both are\nfunded through NASA grants NNX09AH71G, NNX09AT02G,\nNNX10AI27G, and NNX12AE66G, CONACyT grants INFR-\n2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant\nIG100414, and UC MEXUS-CONACyT grant CN 09-283.\nThese results made use of Lowell Observatory\u02bcs Discovery\nChannel Telescope. Lowell operates the DCT in partnership\nwith Boston University, Northern Arizona University, the\nUniversity of Maryland, and the University of Toledo. Partial\nsupport of the DCT was provided by Discovery Communications.\nLMI was built by Lowell Observatory using funds from\nthe NSF (AST-1005313). The Liverpool Telescope is operated\non the island of La Palma by Liverpool John Moores\nUniversity in the Spanish Observatorio del Roque de los\nMuchachos of the Instituto de Astrofisica de Canarias with\nfinancial support from the UK Science and Technology\nFacilities Council. Some of the data presented herein were\nobtained at the W. M. Keck Observatory, which is operated as\na scientific partnership among the California Institute of\nTechnology, the University of California, and NASA; the\nobservatory was made possible by the generous financial\nsupport of the W. M. Keck Foundation. This research has made use of the VizieR catalog access tool,\nCDS, Strasbourg, France. This publication also uses data\nproducts from the Two Micron All Sky Survey, which is a joint\nproject of the University of Massachusetts and the Infrared\nProcessing and Analysis Center/California Institute of Technology,\nfunded by NASA and the NSF. Funding for SDSS-III\nhas been provided by the Alfred P. Sloan Foundation, the\nParticipating Institutions, the NSF, and the U.S. Department of\nEnergy Office of Science. The SDSS-III website is http://\nwww.sdss3.org/. SDSS-III is managed by the Astrophysical\nResearch Consortium for the Participating Institutions of the\nSDSS-III Collaboration including the University of Arizona,\nthe Brazilian Participation Group, Brookhaven National\nLaboratory, Carnegie Mellon University, University of Florida,\nthe French Participation Group, the German Participation\nGroup, Harvard University, the Instituto de Astrofisica de\nCanarias, the Michigan State/Notre Dame/JINA Participation\nGroup, Johns Hopkins University, Lawrence Berkeley National\nLaboratory, Max Planck Institute for Astrophysics, Max Planck\nInstitute for Extraterrestrial Physics, New Mexico State\nUniversity, New York University, Ohio State University,\nPennsylvania State University, University of Portsmouth,\nPrinceton University, the Spanish Participation Group, University\nof Tokyo, University of Utah, Vanderbilt University,\nUniversity of Virginia, University of Washington, and Yale\nUniversity.\n\nPublished - Toy_2016p79.pdf
Submitted - 1508.00575v1.pdf
", "abstract": "We present optical and near-infrared (NIR) light curves and optical spectra of SN 2013dx, associated with the nearby (redshift 0.145) gamma-ray burst GRB 130702A. The prompt isotropic gamma-ray energy released from GRB 130702A is measured to be E_(yiso)=6.4_(-1.0)^(+1.3) x 10^(50) erg (1 keV to 10 MeV in the rest frame), placing it intermediate between low-luminosity GRBs like GRB 980425/SN 1998bw and the broader cosmological population. We compare the observed g'r'i'z' light curves of SN 2013dx to a SN 1998bw template, finding that SN 2013dx evolves ~20% faster (steeper rise time), with a comparable peak luminosity. Spectroscopically, SN 2013dx resembles other broad-lined SNe Ic, both associated with (SN 2006aj and SN 1998bw) and lacking (SN 1997ef, SN 2007I, and SN 2010ah) gamma-ray emission, with photospheric velocities around peak of ~ 21,000 km s^(\u22121). We construct a quasi-bolometric g'r'i'z'yJ) light curve for SN 2013dx, only the fifth GRB-associated SN with extensive NIR coverage and the third with a bolometric light curve extending beyond \u0394t > 40 days. Together with the measured photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a ^(56)Ni mass of M_(Ni)= 0.37 \u00b1 0.01 M_\u2609, an ejecta mass of M_(ej) = 3.1 \u00b1 0.1 M_\u2609, and a kinetic energy of E_K = 8.2 \u00b1 0.43 x 10^(51) erg (statistical uncertainties only), consistent with previous GRB-associated supernovae. When considering the ensemble population of GRB-associated supernovae, we find no correlation between the mass of synthesized 56Ni and high-energy properties, despite clear predictions from numerical simulations that M_(Ni) should correlate with the degree of asymmetry. On the other hand, M_(Ni) clearly correlates with the kinetic energy of the supernova ejecta across a wide range of core-collapse events.", "date": "2016-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "818", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 79", "id_number": "CaltechAUTHORS:20151207-131630440", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151207-131630440", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NASA Earth and Space Science Fellowship Program", "grant_number": "NNX12AL70H" }, { "agency": "NSF", "grant_number": "ATI-1207785" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "NSF Astronomy and Astrophysics Postdoctoral Fellowship", "grant_number": "AST-1302771" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "Israeli Committee for planning and budgeting" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "NASA", "grant_number": "13-SWIFT13-0030" }, { "agency": "NASA", "grant_number": "14-SWIFT14-0024" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NNX09AH71G" }, { "agency": "NASA", "grant_number": "NNX09AT02G" }, { "agency": "NASA", "grant_number": "NNX10AI27G" }, { "agency": "NASA", "grant_number": "NNX12AE66G" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "INFR-2009-01-122785" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "CB-2008-101958" }, { "agency": "UNAM PAPIIT", "grant_number": "IG100414" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "CN 09-283" }, { "agency": "Discovery Communications" }, { "agency": "NSF", "grant_number": "AST-1005313" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Israel Science Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "ARCHES Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/818/1/79", "primary_object": { "basename": "1508.00575v1.pdf", "url": "https://authors.library.caltech.edu/records/swgv9-thc30/files/1508.00575v1.pdf" }, "related_objects": [ { "basename": "Toy_2016p79.pdf", "url": "https://authors.library.caltech.edu/records/swgv9-thc30/files/Toy_2016p79.pdf" } ], "pub_year": "2016", "author_list": "Toy, V. L.; Perley, D. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/6shtm-c3v05", "eprint_id": 63956, "eprint_status": "archive", "datestamp": "2023-08-20 10:14:50", "lastmod": "2023-10-17 18:31:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Khazov-D", "name": { "family": "Khazov", "given": "D." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D." }, "orcid": "0000-0001-8472-1996" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Flash Spectroscopy: Emission Lines from the Ionized Circumstellar Material around <10-Day-Old Type II Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2015 June 23; accepted 2015 November 30; published 2016 February 2.\n\nWe would like to acknowledge A. Miller, D. Poznanski, J. Bloom, K. Clubb, D. Murray, S. Tang, S. Geier, V. Van Eylen, and J. Parrent for help with the observations. We are grateful to the staffs at the various observatories and telescopes with which we collected data (Lick, Palomar, Keck, Gemini, NOT, Apache Point, Kitt Peak, HET) for their excellent assistance. An anonymous referee careful read our manuscript and provided valuable comments.\n\nA.G.-Y. is supported by the EU/FP7 via ERC grant no. 307260, the Quantum universe I-Core program by the Israeli Committee for planning and budgeting, and the ISF, Minerva and ISF grants, WIS-UK \"making connections,\" and the Kimmel and ARCHES awards. J.M.S. is supported by a National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. A.V.F.'s research was made possible by NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. M.S. acknowledges support from the Royal Society and EU/FP7-ERC grant No. [615929]. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development program. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration. US Government Support Acknowledged.\n\nResearch at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based in part on observations obtained at the Gemini Observatory under program GN-2010B-Q-13, 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 NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina).\n\nPublished - Khazov_2016_ApJ_818_3.pdf
Submitted - 1512.00846.pdf
", "abstract": "Supernovae (SNe) embedded in dense circumstellar material (CSM) may show prominent emission lines in their early-time spectra (\u226410 days after the explosion), owing to recombination of the CSM ionized by the shock-breakout flash. From such spectra (\"flash spectroscopy\"), we can measure various physical properties of the CSM, as well as the mass-loss rate of the progenitor during the year prior to its explosion. Searching through the Palomar Transient Factory (PTF and iPTF) SN spectroscopy databases from 2009 through 2014, we found 12 SNe II showing flash-ionized (FI) signatures in their first spectra. All are younger than 10 days. These events constitute 14% of all 84 SNe in our sample having a spectrum within 10 days from explosion, and 18% of SNe II observed at ages <5 days, thereby setting lower limits on the fraction of FI events. We classified as \"blue/featureless\" (BF) those events having a first spectrum that is similar to that of a blackbody, without any emission or absorption signatures. It is possible that some BF events had FI signatures at an earlier phase than observed, or that they lack dense CSM around the progenitor. Within 2 days after explosion, 8 out of 11 SNe in our sample are either BF events or show FI signatures. Interestingly, we found that 19 out of 21 SNe brighter than an absolute magnitude M_R = \u221218.2 belong to the FI or BF groups, and that all FI events peaked above M_R = \u221217.6 mag, significantly brighter than average SNe II.", "date": "2016-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "818", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 3", "id_number": "CaltechAUTHORS:20160126-070703893", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160126-070703893", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee Quantum Universe I-Core program" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israeli Science Foundation" }, { "agency": "MINERVA" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel award" }, { "agency": "ARCHES award" }, { "agency": "NSF", "grant_number": "AST-1302771" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL" }, { "agency": "Google" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.3847/0004-637X/818/1/3", "primary_object": { "basename": "1512.00846.pdf", "url": "https://authors.library.caltech.edu/records/6shtm-c3v05/files/1512.00846.pdf" }, "related_objects": [ { "basename": "Khazov_2016_ApJ_818_3.pdf", "url": "https://authors.library.caltech.edu/records/6shtm-c3v05/files/Khazov_2016_ApJ_818_3.pdf" } ], "pub_year": "2016", "author_list": "Khazov, D.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/nen28-jak68", "eprint_id": 96126, "eprint_status": "archive", "datestamp": "2023-08-20 10:15:48", "lastmod": "2023-10-20 20:52:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-M", "name": { "family": "Smith", "given": "M." }, "orcid": "0000-0002-3321-1432" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "D'Andrea-C-B", "name": { "family": "D'Andrea", "given": "Chris B." } }, { "id": "Castander-F-J", "name": { "family": "Castander", "given": "Francisco" }, "orcid": "0000-0001-7316-4573" }, { "id": "Casas-R", "name": { "family": "Casas", "given": "R." } } ] }, "title": "DES14X3taz: A Type I Superluminous Supernova Showing a Luminous, Rapidly Cooling Initial Pre-Peak Bump", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2016 The American Astronomical Society.\n\nReceived 2015 December 15; accepted 2016 January 19; published 2016 February 3.\n\nWe acknowledge support from EU/FP7-ERC grants 615929 and 307260, STFC, NSF grant AST-1518052, and a Weizmann-UK Grant. Based on observations made with the Gran Telescopio Canarias (GTC), at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias.\n\nFunding for the DES Projects has been provided by the DOE and NSF (USA), MEC/MICINN/MINECO (Spain), STFC (UK), HEFCE (UK), NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), DFG (Germany), and the Collaborating Institutions in the Dark Energy Survey.\n\nThe Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Z\u00fcrich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU M\u00fcnchen, and the associated Excellence Cluster universe, University of Michigan, NOAO, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, University of Sussex, and Texas A&M University.\n\nThe DES Data Management System is supported by the NSF under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the ERC including grants 240672, 291329, and 306478.\n\nFacilities: Blanco - Cerro Tololo Inter-American Observatory's 4 meter Blanco Telescope, GTC - Gran Telescopio CANARIAS 10.4m telescope (GRANTECAN).\n\nAccepted Version - 1512.06043.pdf
", "abstract": "We present DES14X3taz, a new hydrogen-poor superluminous supernova (SLSN-I) discovered by the Dark Energy Survey (DES) supernova program, with additional photometric data provided by the Survey Using DECam for Superluminous Supernovae. Spectra obtained using Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy on the Gran Telescopio CANARIAS show DES14X3taz is an SLSN-I at z = 0.608. Multi-color photometry reveals a double-peaked light curve: a blue and relatively bright initial peak that fades rapidly prior to the slower rise of the main light curve. Our multi-color photometry allows us, for the first time, to show that the initial peak cools from 22,000 to 8000 K over 15 rest-frame days, and is faster and brighter than any published core-collapse supernova, reaching 30% of the bolometric luminosity of the main peak. No physical 56Ni-powered model can fit this initial peak. We show that a shock-cooling model followed by a magnetar driving the second phase of the light curve can adequately explain the entire light curve of DES14X3taz. Models involving the shock-cooling of extended circumstellar material at a distance of \u2243400 R\u2299 are preferred over the cooling of shock-heated surface layers of a stellar envelope. We compare DES14X3taz to the few double-peaked SLSN-I events in the literature. Although the rise times and characteristics of these initial peaks differ, there exists the tantalizing possibility that they can be explained by one physical interpretation.", "date": "2016-02-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "818", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L8", "id_number": "CaltechAUTHORS:20190604-152202944", "issn": "2041-8213", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190604-152202944", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "corp_creators": { "items": [ "DES Collaboration" ] }, "doi": "10.3847/2041-8205/818/1/l8", "primary_object": { "basename": "1512.06043.pdf", "url": "https://authors.library.caltech.edu/records/nen28-jak68/files/1512.06043.pdf" }, "pub_year": "2016", "author_list": "Smith, M.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/73khy-22c35", "eprint_id": 64287, "eprint_status": "archive", "datestamp": "2023-08-20 09:53:38", "lastmod": "2023-10-17 19:39:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Kaplan-D-L", "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "id": "Breton-R-P", "name": { "family": "Breton", "given": "Rene P." } }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" } }, { "id": "Bhalerao-V-B", "name": { "family": "Bhalerao", "given": "Varun B." }, "orcid": "0000-0002-6112-7609" }, { "id": "Camilo-F", "name": { "family": "Camilo", "given": "Fernando" }, "orcid": "0000-0002-1873-3718" }, { "id": "Dahal-S", "name": { "family": "Dahal", "given": "Sumit" } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Drake-A-J", "name": { "family": "Drake", "given": "Andrew J." } }, { "id": "Hessels-J-W-T", "name": { "family": "Hessels", "given": "J. W. T." }, "orcid": "0000-0003-2317-1446" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David B." } }, { "id": "Lewis-F", "name": { "family": "Lewis", "given": "Fraser" } }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "Ashish A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Ransom-S-M", "name": { "family": "Ransom", "given": "Scott M." } }, { "id": "Roberts-M-S-E", "name": { "family": "Roberts", "given": "Mallory S. E." } }, { "id": "Russell-D-M", "name": { "family": "Russell", "given": "David M." }, "orcid": "0000-0002-3500-631X" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" } ] }, "title": "Properties and Evolution of the Redback Millisecond Pulsar Binary PSR J2129-0429", "ispublished": "pub", "full_text_status": "public", "keywords": "pulsars: individual (PSR J2129\u20130429)", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2015 October 4; accepted 2015 December 1; published 2016 January 14. \n\nT.A.P., E.C.B., and S.T. acknowledge partial support through NASA Grant No. NNX12AO76G. R.P.B. has received funding from the European Union Seventh Framework Programme under grant agreement PIIF-GA-2012-332393. J.W.T.H. acknowledges funding from an NWO Vidi fellowship and ERC Starting Grant \"DRAGNET\" (337062). E.C.B. and T.A.P. thank the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the editing of this paper. \n\nThis paper is based in part on observations obtained with the Palomar 48 inch Oschin telescope and the robotic Palomar 60-inch telescope at the 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 CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182, AST-1313422, and AST-1413600. This work makes use of observations from the Las Cumbres Observatory Global Telescope Network. \n\nFacilities: Hale (Double Beam Spectrograph) - Palomar Observatory's 5.1m Hale Telescope, PO:1.2 m (Palomar Transient Factory) - , PO:1.5 m - , LCOGT - Las Cumbres Observatory Global Telescope.\n\nPublished - Bellm_2016p74.pdf
Submitted - 1510.00721v1.pdf
", "abstract": "PSR J2129\u22120429 is a \"redback\" eclipsing millisecond pulsar binary with an unusually long 15.2 hr orbit. It was discovered by the Green Bank Telescope in a targeted search of unidentified Fermi gamma-ray sources. The pulsar companion is optically bright (mean m_R = 16.6 mag), allowing us to construct the longest baseline photometric data set available for such a system. We present 10 years of archival and new photometry of the companion from the Lincoln Near-Earth Asteroid Research Survey, the Catalina Real-time Transient Survey, the Palomar Transient Factory, the Palomar 60 inch, and the Las Cumbres Observatory Global Telescope. Radial velocity spectroscopy using the Double-Beam Spectrograph on the Palomar 200 inch indicates that the pulsar is massive: 1.74 \u00b1 0.18 M_\u2609. The G-type pulsar companion has mass 0.44 \u00b1 0.04 M_\u2609, one of the heaviest known redback companions. It is currently 95 \u00b1 1% Roche-lobe filling and only mildly irradiated by the pulsar. We identify a clear 13.1 mmag yr^(\u22121) secular decline in the mean magnitude of the companion as well as smaller-scale variations in the optical light curve shape. This behavior may indicate that the companion is cooling. Binary evolution calculations indicate that PSR J2129\u22120429 has an orbital period almost exactly at the bifurcation period between systems that converge into tighter orbits as black widows and redbacks and those that diverge into wider pulsar\u2013white dwarf binaries. Its eventual fate may depend on whether it undergoes future episodes of mass transfer and increased irradiation.", "date": "2016-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "816", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 74", "id_number": "CaltechAUTHORS:20160208-074401021", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160208-074401021", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AO76G" }, { "agency": "Marie Curie Fellowship", "grant_number": "PIIF-GA-2012-332393" }, { "agency": "European Research Council (ERC)", "grant_number": "337062" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "NSF", "grant_number": "AST-1313422" }, { "agency": "NSF", "grant_number": "AST-1413600" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.3847/0004-637X/816/2/74", "primary_object": { "basename": "Bellm_2016p74.pdf", "url": "https://authors.library.caltech.edu/records/73khy-22c35/files/Bellm_2016p74.pdf" }, "related_objects": [ { "basename": "1510.00721v1.pdf", "url": "https://authors.library.caltech.edu/records/73khy-22c35/files/1510.00721v1.pdf" } ], "pub_year": "2016", "author_list": "Bellm, Eric C.; Kaplan, David L.; et el." }, { "id": "https://authors.library.caltech.edu/records/7ngjp-2qg25", "eprint_id": 60582, "eprint_status": "archive", "datestamp": "2023-08-20 09:23:24", "lastmod": "2023-10-24 16:41:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E." }, "orcid": "0000-0002-6786-8774" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P." }, "orcid": "0000-0001-6876-8284" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D." }, "orcid": "0000-0001-8472-1996" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P." }, "orcid": "0000-0002-7572-9088" }, { "id": "Leloudas-G", "name": { "family": "Leloudas", "given": "G." }, "orcid": "0000-0002-8597-0756" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "A." }, "orcid": "0000-0003-2082-1626" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "F." }, "orcid": "0000-0002-8532-9395" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "Umaa D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Wo\u017aniak-P-R", "name": { "family": "Wo\u017aniak", "given": "P. R." }, "orcid": "0000-0002-9919-3310" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" } ] }, "title": "Detection of Broad H\u03b1 Emission Lines in the Late-time Spectra of a Hydrogen-poor Superluminous Supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "Stars: supernova, massive stars", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 August 5; accepted 2015 October 13; published 2015 November 23. \n\nWe thank the anonymous referee for the positive and constructive suggestions, which have helped to improve the paper. We benefited from discussions with Nick Scoville and Orly Gnat on collisional excitations in ISM. We thank Mansi Kasliwal, Thomas Prince, and Howard Bond for helping us obtain the P200 photometry at one epoch. Vicki Toy and John Capone from University of Maryland are acknowledged for taking the photometry observation using LMI on DCT. A.G.Y. is supported by EU/FP7 via ERC grant No. 307260, the Quantum universe I-Core program by the Israeli Committee for planning and budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK \"making connections\" program; and by Kimmel and ARCHES awards. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This paper made use of Lowell Observatory's Discovery Channel Telescope (DCT). Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. The Large Monolithic Imager (LMI) on DCT was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration. US Government support is acknowledged. 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. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. \n\nFacilities: Palomar - , Keck - , SWIFT - , Discovery Channel Telescope - .\n\nPublished - Yan_2015.pdf
Submitted - 1508.04420v1.pdf
", "abstract": "Discovered by the intermediate Palomar Transient Factory (iPTF), iPTF13ehe is a hydrogen-poor\nsuperluminous supernova (SLSN) at z =0.3434, with properties similar to SN2007bi. The early observations show that iPTF13ehe rises within 83 - 148 days (rest-frame) to reach a peak bolometric\nluminosity of L^(peak)_(bol) ~1.3x10^(44) erg s^(-1), then decays very slowly at 0.015 magnitude per day. The measured ejecta velocity is ~13000km s^(-1). The inferred explosion characteristics, such as the ejecta mass\n(67 - 220M\u2299), the total radiative and kinetic energy (E_(rad) ~10^(51) erg, E_(kin) ~2x10^(53) erg), is typical\nof SLSN-R events. However, the late-time spectrum taken at +251 days (rest, post-peak) reveals a\nBalmer H\u03b1 emission feature with broad and narrow components, which has never been detected before\namong other H-poor SLSNe. The broad component has a velocity width of ~4500km s^(-1) and has a\n~300km s^(-1) blue-ward shift relative to the narrow component. We interpret this broad H\u03b1 emission\nline as the interaction between the supernova ejecta and a H-rich circumstellar medium (CSM) shell,\nlocated at a distance of ~4 x 10^(16) cm from the explosion site. This ejecta-CSM interaction can produce the observed H\u03b1 luminosity of ~2x10^(41) erg s^(-1) and causes the rest-frame r-band LC to brighten\nat late times. The fact that the late-time spectra are not completely absorbed by the shock ionized\nCSM shell implies that its Thomson scattering optical depth is likely \u2264 1, thus setting upper limits on\nthe CSM mass \u2264 30M\u2299 and the volume number density \u2264 4 x 10^8 cm ^(-3). The early-time spectra do\nnot show any H emission lines from this CSM shell, indicating that most of the H-atoms are already\nneutral and the shell is optically thin to the visible light. We predict that this shell should produce\nLy\u03b1 absorption in the UV spectra. Of the existing models, a Pulsational Pair Instability Supernova\n(PPISN) model can naturally explain the observed 30M\u2299 H-shell, ejected from a progenitor star with\nan initial mass of (95-150)M\u2299 about 40 years ago. By searching the PTF database for events similar\nto iPTF13ehe, we estimate that about 10% of all SLSNe-I may have late-time Balmer emission lines\nfrom ejecta interactions with H-rich shells.", "date": "2015-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "814", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 108", "id_number": "CaltechAUTHORS:20150928-141615101", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150928-141615101", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "Danish National Research Foundation" }, { "agency": "Discovery Communications" }, { "agency": "NSF", "grant_number": "AST-1005313" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/814/2/108", "primary_object": { "basename": "1508.04420v1.pdf", "url": "https://authors.library.caltech.edu/records/7ngjp-2qg25/files/1508.04420v1.pdf" }, "related_objects": [ { "basename": "Yan_2015.pdf", "url": "https://authors.library.caltech.edu/records/7ngjp-2qg25/files/Yan_2015.pdf" } ], "pub_year": "2015", "author_list": "Yan, Lin; Quimby, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/4hw5n-thr51", "eprint_id": 62943, "eprint_status": "archive", "datestamp": "2023-08-20 09:14:34", "lastmod": "2023-10-25 22:57:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Myers-A-D", "name": { "family": "Myers", "given": "Adam D." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } } ] }, "title": "The SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Quasar Target Selection", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs, cosmology: observations, galaxies: distances and redshifts, galaxies: photometry, methods: data analysis, quasars: general", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 August 19; accepted 2015 October 29; published 2015 December 2. \n\nWe are grateful for insightful discussions about quasar selection statistics with Joe Hennawi, David Hogg, and Gordon Richards. A.D.M. acknowledges a generous research fellowship from the Alexander von Humboldt Foundation at the Max-Planck-Institut f\u00fcr Astronomie and was supported in part by NASA-ADAP awards NNX12AI49G and NNX12AE38G and by NSF awards 1211112 and 1515404. J.P.K. acknowledges support from the ERC advanced grant LIDA. \n\nThis paper includes targets derived from the images of 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 paper represents an effort by both the SDSS-III and SDSS-IV collaborations. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. 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. \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 Astrofi\u00b4sica 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 Observatory 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 Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.\n\nPublished - 405936.pdf
Submitted - 1508.04472v2.pdf
", "abstract": "As part of the Sloan Digital Sky Survey (SDSS) IV the extended Baryon Oscillation Spectroscopic Survey (eBOSS) will improve measurements of the cosmological distance scale by applying the Baryon Acoustic Oscillation (BAO) method to quasar samples. eBOSS will adopt two approaches to target quasars over 7500 deg^2. First, a \"CORE\" quasar sample will combine the optical selection in ugriz using a likelihood-based routine called XDQSOz, with a mid-IR-optical color cut. eBOSS CORE selection (to g < 22 or r < 22) should return ~70 deg^(\u22122) quasars at redshifts 0.9 < z < 2.2 and ~7 deg^(\u22122)z > 2.1 quasars. Second, a selection based on variability in multi-epoch imaging from the Palomar Transient Factory should recover an additional ~3\u20134 deg^(\u22122)z > 2.1 quasars to g < 22.5. A linear model of how imaging systematics affect target density recovers the angular distribution of eBOSS CORE quasars over 96.7% (76.7%) of the SDSS north (south) Galactic Cap area. The eBOSS CORE quasar sample should thus be sufficiently dense and homogeneous over 0.9 < z < 2.2 to yield the first few-percent-level BAO constraint near z bar ~ 1.5. eBOSS quasars at z > 2.1 will be used to improve BAO measurements in the Ly\u03b1 Forest. Beyond its key cosmological goals, eBOSS should be the next-generation quasar survey, comprising >500,000 new quasars and >500,000 uniformly selected spectroscopically confirmed 0.9 < z < 2.2 quasars. At the conclusion of eBOSS, the SDSS will have provided unique spectra for more than 800,000 quasars.", "date": "2015-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "221", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 27", "id_number": "CaltechAUTHORS:20151215-112935949", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151215-112935949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX12AI49G" }, { "agency": "NASA", "grant_number": "NNX12AE38G" }, { "agency": "NSF", "grant_number": "AST-1211112" }, { "agency": "NSF", "grant_number": "AST-1515404" }, { "agency": "European Research Council (ERC)", "grant_number": "LIDA" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "University of Utah" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0067-0049/221/2/27", "primary_object": { "basename": "1508.04472v2.pdf", "url": "https://authors.library.caltech.edu/records/4hw5n-thr51/files/1508.04472v2.pdf" }, "related_objects": [ { "basename": "405936.pdf", "url": "https://authors.library.caltech.edu/records/4hw5n-thr51/files/405936.pdf" } ], "pub_year": "2015", "author_list": "Myers, Adam D.; Kulkarni, Shrinivas R.; et el." }, { "id": "https://authors.library.caltech.edu/records/2ezwm-dmv89", "eprint_id": 63512, "eprint_status": "archive", "datestamp": "2023-08-20 08:37:39", "lastmod": "2023-10-25 23:52:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "P. J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Bloemen-S", "name": { "family": "Bloemen", "given": "S." } }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } }, { "id": "Steeghs-D", "name": { "family": "Steeghs", "given": "D." } }, { "id": "Marsh-T-R", "name": { "family": "Marsh", "given": "T. R." }, "orcid": "0000-0002-2498-7589" }, { "id": "Rutten-R-G-M", "name": { "family": "Rutten", "given": "R. G. M." } }, { "id": "Nelemans-G", "name": { "family": "Nelemans", "given": "G." } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "F\u00fcrst-F", "name": { "family": "F\u00fcrst", "given": "F." }, "orcid": "0000-0003-0388-0560" }, { "id": "Geier-S", "name": { "family": "Geier", "given": "S." }, "orcid": "0000-0002-3948-9339" } ] }, "title": "Phase-resolved spectroscopy and Kepler photometry of the ultracompact AM CVn binary SDSS J190817.07+394036.4", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion discs \u2013 binaries: close \u2013 stars: individual:\nSDSS J190817.07+394036.4", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 July 14. Received 2015 July 9; in original form 2015 May 12. \n\nTK acknowledges support by the Netherlands Research School of Astronomy (NOVA). TRM and DS acknowledge the support from the Science and Technology Facilities Council (STFC) during the course of this work. PJG wishes to thank the California Institute of Technology its hospitality and support during a sabbatical leave.\n\nBased on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, in the island of La Palma. Based on observations with the William Herschel Telescope operated by the Isaac Newton Group at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias on the island of La Palma, Spain. 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. This paper includes data collected by the Kepler mission. The authors gratefully acknowledge the Kepler team and all who have contributed to enabling the mission. The Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Funding for the Kepler Mission is provided by NASAs Science Mission Directorate. This research has made use of NASA's Astrophysics Data System.\n\nPublished - MNRAS-2015-Kupfer-483-96.pdf
", "abstract": "Kepler satellite photometry and phase-resolved spectroscopy of the ultracompact AM CVn type binary SDSS J190817.07+394036.4 are presented. The average spectra reveal a variety of weak metal lines of different species, including silicon, sulphur and magnesium as well as many lines of nitrogen, beside the strong absorption lines of neutral helium. The phase-folded spectra and the Doppler tomograms reveal an S-wave in emission in the core of the He\u2009I 4471 \u00c5 absorption line at a period of P_(orb) = 1085.7 \u00b1 2.8 s identifying this as the orbital period of the system. The Si\u2009II, Mg\u2009II and the core of some He\u2009I lines show an S-wave in absorption with a phase offset of 170\u00b0 \u00b1 15\u00b0 compared to the S-wave in emission. The N\u2009II, Si\u2009III and some helium lines do not show any phase variability at all. The spectroscopic orbital period is in excellent agreement with a period at P_(orb) = 1085.108(9) s detected in the 3 yr Kepler light curve. A Fourier analysis of the Q6\u2013Q17 short-cadence data obtained by Kepler revealed a large number of frequencies above the noise level where the majority shows a large variability in frequency and amplitude. In an Observed-minus-computed analysis, we measured a |P\u02d9| \u223c1.0 |P\u02d9|\u223c1.0\u00d7\u200910^(\u22128)\u2009s s^(\u22121) for some of the strongest variations and set a limit for the orbital period to be |P\u02d9| < 10^(\u221210) |P\u02d9| < 10^(\u221210) s s^(\u22121). The shape of the phase-folded light curve on the orbital period indicates the motion of the bright-spot. Models of the system were constructed to see whether the phases of the radial velocity curves and the light-curve variation can be combined to a coherent picture. However, from the measured phases neither the absorption nor the emission can be explained to originate in the bright-spot.", "date": "2015-10-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "453", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "483-496", "id_number": "CaltechAUTHORS:20160108-124025927", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160108-124025927", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stv1609", "primary_object": { "basename": "MNRAS-2015-Kupfer-483-96.pdf", "url": "https://authors.library.caltech.edu/records/2ezwm-dmv89/files/MNRAS-2015-Kupfer-483-96.pdf" }, "pub_year": "2015", "author_list": "Kupfer, T.; Groot, P. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/zsqn4-dpj73", "eprint_id": 62635, "eprint_status": "archive", "datestamp": "2023-08-22 16:39:33", "lastmod": "2023-10-25 17:17:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yu-Liang", "name": { "family": "Yu", "given": "Liang" }, "orcid": "0000-0003-1667-5427" }, { "id": "Winn-J-N", "name": { "family": "Winn", "given": "Joshua N." }, "orcid": "0000-0002-4265-047X" }, { "id": "Gillon-M", "name": { "family": "Gillon", "given": "Micha\u00ebl" }, "orcid": "0000-0003-1462-7739" }, { "id": "Albrecht-S", "name": { "family": "Albrecht", "given": "Simon" } }, { "id": "Rappaport-S", "name": { "family": "Rappaport", "given": "Saul" }, "orcid": "0000-0003-3182-5569" }, { "id": "Bieryla-A", "name": { "family": "Bieryla", "given": "Allyson" }, "orcid": "0000-0001-6637-5401" }, { "id": "Dai-Fei", "name": { "family": "Dai", "given": "Fei" }, "orcid": "0000-0002-8958-0683" }, { "id": "Delrez-L", "name": { "family": "Delrez", "given": "Laetitia" }, "orcid": "0000-0001-6108-4808" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne" } }, { "id": "Holman-M-J", "name": { "family": "Holman", "given": "Matthew J." }, "orcid": "0000-0002-1139-4880" }, { "id": "Howard-A-W", "name": { "family": "Howard", "given": "Andrew W." }, "orcid": "0000-0001-8638-0320" }, { "id": "Huang-Chelsea-X", "name": { "family": "Huang", "given": "Chelsea X." }, "orcid": "0000-0003-0918-7484" }, { "id": "Isaacson-H-T", "name": { "family": "Isaacson", "given": "Howard T." }, "orcid": "0000-0002-0531-1073" }, { "id": "Jehin-E", "name": { "family": "Jehin", "given": "Emmanuel" } }, { "id": "Lendl-M", "name": { "family": "Lendl", "given": "Monika" } }, { "id": "Montet-B-T", "name": { "family": "Montet", "given": "Benjamin T." }, "orcid": "0000-0001-7516-8308" }, { "id": "Muirhead-P-S", "name": { "family": "Muirhead", "given": "Philip" }, "orcid": "0000-0002-0638-8822" }, { "id": "Sanchis-Ojeda-R", "name": { "family": "Sanchis-Ojeda", "given": "Roberto" }, "orcid": "0000-0002-6193-972X" }, { "id": "Triaud-A-H-M-J", "name": { "family": "Triaud", "given": "Amaury H. M. J." }, "orcid": "0000-0002-5510-8751" } ] }, "title": "Tests of the planetary hypothesis for PTFO 8-8695b", "ispublished": "pub", "full_text_status": "public", "keywords": "planetary systems; stars: individual (PTFO 8-8695); stars: pre-main sequence", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 July 24; accepted 2015 September 4; published 2015 October 7. \n\nWe thank the referee, Jason W. Barnes, for his comments on\nthe manuscript. We are grateful to Geoff Marcy for helping to arrange the Keck observations, to Aur\u00e9lie Fumel for helping with the TRAPPIST observations, and to John Johnson and Jon Swift for attempting to perform photometric observations for this project. We thank Greg Herczeg, Hans Moritz G\u00fcnther, and Nikku Madhusudhan for helpful discussions, and Julian van Eyken for providing the PTF data in a convenient format. Work by JNW was supported by the NASA Origins program (grant NNX11AG85G). M.G. and E.J. are Research Associates at the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, F.R.S-FNRS); L.D. received the support of the F.R.I.A. fund of the FNRS. TRAPPIST is a project funded by the F.R.S-FNRS under grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (SNF). B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. The authors wish to extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. \n\nFacilities: FLWO:1.2 m, Magellan:Baade, Euler1.2 m, Keck:I (HIRES), Spitzer.\n\nPublished - Yu_2015p48.pdf
Submitted - 1509.02176v2.pdf
", "abstract": "The T Tauri star PTFO 8-8695 exhibits periodic fading events that have been interpreted as the transits of a giant planet on a precessing orbit. Here we present three tests of the planet hypothesis. First, we sought evidence for the secular changes in light-curve morphology that are predicted to be a consequence of orbital precession. We observed 28 fading events spread over several years and did not see the expected changes. Instead, we found that the fading events are not strictly periodic. Second, we attempted to detect the planet's radiation, based on infrared observations spanning the predicted times of occultations. We ruled out a signal of the expected amplitude. Third, we attempted to detect the Rossiter\u2013McLaughlin effect by performing high-resolution spectroscopy throughout a fading event. No effect was seen at the expected level, ruling out most (but not all) possible orientations for the hypothetical planetary orbit. Our spectroscopy also revealed strong, time-variable, high-velocity H\u03b1 and Ca H & K emission features. All these observations cast doubt on the planetary hypothesis, and suggest instead that the fading events represent starspots, eclipses by circumstellar dust, or occultations of an accretion hotspot.", "date": "2015-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "812", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 48", "id_number": "CaltechAUTHORS:20151207-092434339", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151207-092434339", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX11AG85G" }, { "agency": "Fond National de la Recherche Scientifique (FNRS)", "grant_number": "FRFC 2.5.594.09.F" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-637X/812/1/48", "primary_object": { "basename": "1509.02176v2.pdf", "url": "https://authors.library.caltech.edu/records/zsqn4-dpj73/files/1509.02176v2.pdf" }, "related_objects": [ { "basename": "Yu_2015p48.pdf", "url": "https://authors.library.caltech.edu/records/zsqn4-dpj73/files/Yu_2015p48.pdf" } ], "pub_year": "2015", "author_list": "Yu, Liang; Winn, Joshua N.; et el." }, { "id": "https://authors.library.caltech.edu/records/r2mfk-b8a55", "eprint_id": 62266, "eprint_status": "archive", "datestamp": "2023-08-22 16:30:35", "lastmod": "2023-10-25 17:00:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Strotjohann-Nora-L", "name": { "family": "Strotjohann", "given": "Nora L." }, "orcid": "0000-0002-4667-6730" }, { "id": "Ofek-Eran-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Gal-Yam-Avishay", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Shaviv-Nir-J", "name": { "family": "Shaviv", "given": "Nir J." }, "orcid": "0000-0003-3894-8422" }, { "id": "Fremling-Christoffer", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Nugent-Peter-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Arcavi-Iair", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Sollerman-Jesper", "name": { "family": "Sollerman", "given": "Jesper" }, "orcid": "0000-0003-1546-6615" }, { "id": "Filippenko-Alexei-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Yaron-Ofer", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-Jason-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Search for precursor eruptions among Type IIb supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (SN2011dh, SN2012P, SN2012cs, SN2013bb)", "note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 June 16; accepted 2015 August 18; published 2015 September 28. \n\nThis paper is based on observations obtained with the Samuel Oschin Telescope as part of the PTF, 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. We are grateful for excellent staff assistance at Palomar and Lick Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus, NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum universe I-Core program by the Israeli Committee for planning and budgeting, and the ISF, Minerva and ISF grants, WIS-UK \"making connections\" and the Kimmel and ARCHES awards. M.S. acknowledges support from the Royal Society and EU/FP7- ERC grant No. [615929]. N.J.S. thanks the IBM Einstein Fellowship support by the Institute for Advanced Study, Princeton. A.V.F's research was made possible by National Science Foundation grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. The Lick Observatory Supernova Search was conducted with the Katzman Automatic Imaging Telescope, made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google.\n\nPublished - Strotjohann_2015p117.pdf
Submitted - 1508.04775v1.pdf
", "abstract": "The progenitor stars of several Type IIb supernovae (SNe) show indications of extended hydrogen envelopes. These envelopes might be the outcome of luminous energetic pre-explosion events, so-called precursor eruptions. We use the Palomar Transient Factory (PTF) pre-explosion observations of a sample of 27 nearby SNe IIb to look for such precursors during the final years prior to the SN explosion. No precursors are found when combining the observations in 15-day bins, and we calculate the absolute-magnitude-dependent upper limit on the precursor rate. At the 90% confidence level, SNe IIb have on average <0.86 precursors as bright as an absolute R-band magnitude of \u221214 in the final 3.5 years before the explosion and <0.56 events over the final year. In contrast, precursors among SNe IIn have a \u2273 5 times higher rate. The kinetic energy required to unbind a low-mass stellar envelope is comparable to the radiated energy of a few-weeks-long precursor that would be detectable for the closest SNe in our sample. Therefore, mass ejections, if they are common in such SNe, are radiatively inefficient or have durations longer than months. Indeed, when using 60-day bins, a faint precursor candidate is detected prior to SN 2012cs (~2% false-alarm probability). We also report the detection of the progenitor of SN 2011dh that does not show detectable variability over the final two years before the explosion. The suggested progenitor of SN 2012P is still present, and hence is likely a compact star cluster or an unrelated object.", "date": "2015-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "811", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 117", "id_number": "CaltechAUTHORS:20151119-145042560", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151119-145042560", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ)" }, { "agency": "Ministry of Science (israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "Israeli Committee for Planning and Budgeting" }, { "agency": "MINERVA (Israel)" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "IBM Einstein Fellowship" }, { "agency": "Institute for Advanced Study" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "Auto-Scope Corporation" }, { "agency": "Lick Observatory" }, { "agency": "University of California" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Google" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/811/2/117", "primary_object": { "basename": "1508.04775v1.pdf", "url": "https://authors.library.caltech.edu/records/r2mfk-b8a55/files/1508.04775v1.pdf" }, "related_objects": [ { "basename": "Strotjohann_2015p117.pdf", "url": "https://authors.library.caltech.edu/records/r2mfk-b8a55/files/Strotjohann_2015p117.pdf" } ], "pub_year": "2015", "author_list": "Strotjohann, Nora L.; Ofek, Eran O.; et el." }, { "id": "https://authors.library.caltech.edu/records/2z4ez-dj042", "eprint_id": 62554, "eprint_status": "archive", "datestamp": "2023-08-22 16:22:24", "lastmod": "2023-10-25 17:14:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aartsen-M-G", "name": { "family": "Aartsen", "given": "M. G." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Barlow-T", "name": { "family": "Barlow", "given": "Tom" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "The Detection of a Type IIn Supernova in Optical Follow-up Observations of IceCube Neutrino Events", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter; galaxies: dwarf; neutrinos; shock waves; supernovae: individual (PTF12csy, SN 2010jl)", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 June 9; accepted 2015 August 15; published 2015 September 18. \n\nWe acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin\u2014Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF). \n\nThis paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O.is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. \n\nP. A. E. Acknowledges support from the UK Space Agency. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. \n\nThe Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). \n\nS.J.S. acknowledges (FP7/2007-2013)/ERC grant agreement no [291222]. \n\nFunding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. \n\nSDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. \n\nWe would like to thank K. Murase and J. Hjorth for helpful discussions.\n\nPublished - Aartsen_2015p52.pdf
Submitted - 1506.03115v2.pdf
", "abstract": "The IceCube neutrino observatory pursues a follow-up program selecting interesting neutrino events in real-time and issuing alerts for electromagnetic follow-up observations. In 2012 March, the most significant neutrino alert during the first three years of operation was issued by IceCube. In the follow-up observations performed by the Palomar Transient Factory (PTF), a Type IIn supernova (SN IIn) PTF12csy was found 0fdg2 away from the neutrino alert direction, with an error radius of 0.\u00ba54. It has a redshift of z = 0.0684, corresponding to a luminosity distance of about 300 Mpc and the Pan-STARRS1 survey shows that its explosion time was at least 158 days (in host galaxy rest frame) before the neutrino alert, so that a causal connection is unlikely. The a posteriori significance of the chance detection of both the neutrinos and the SN at any epoch is 2.2\u03c3 within IceCube's 2011/12 data acquisition season. Also, a complementary neutrino analysis reveals no long-term signal over the course of one year. Therefore, we consider the SN detection coincidental and the neutrinos uncorrelated to the SN. However, the SN is unusual and interesting by itself: it is luminous and energetic, bearing strong resemblance to the SN IIn 2010jl, and shows signs of interaction of the SN ejecta with a dense circumstellar medium. High-energy neutrino emission is expected in models of diffusive shock acceleration, but at a low, non-detectable level for this specific SN. In this paper, we describe the SN PTF12csy and present both the neutrino and electromagnetic data, as well as their analysis.", "date": "2015-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "811", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 52", "id_number": "CaltechAUTHORS:20151202-140807740", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151202-140807740", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Wisconsin Alumni Research Foundation" }, { "agency": "Grid Laboratory of Wisconsin (GLOW)" }, { "agency": "Open Science Grid" }, { "agency": "Department of Energy (DOE)" }, { "agency": "National Energy Research Scientific Computing Center" }, { "agency": "Louisiana Optical Network Initiative (LONI)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Compute/Calcul Canada" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish Polar Research Secretariat" }, { "agency": "Swedish National Infrastructure for Computing (SNIC)" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "Helmholtz Alliance for Astroparticle Physics (HAP)" }, { "agency": "Research Department of Plasmas with Complex Interactions (Bochum), Germany" }, { "agency": "Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO)" }, { "agency": "Flanders Institute to encourage scientific and technological research in industry (IWT)" }, { "agency": "Belgian Federal Science Policy Office (BELSPO)" }, { "agency": "University of Oxford" }, { "agency": "United Kingdom" }, { "agency": "Marsden Fund, New Zealand" }, { "agency": "Australian Research Council" }, { "agency": "Japan Society for Promotion of Science (JSPS)" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "National Research Foundation of Korea (NRF)" }, { "agency": "Danish National Research Foundation" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ)" }, { "agency": "Israeli Ministry of Science" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva and the I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Institute for Astronomy" }, { "agency": "University of Hawaii" }, { "agency": "Pan-STARRS Project Office" }, { "agency": "Max-Planck Society" }, { "agency": "Max Planck Institute for Astronomy" }, { "agency": "Max Planck Institute for Extraterrestrial Physics" }, { "agency": "Johns Hopkins University" }, { "agency": "Durham University" }, { "agency": "University of Edinburgh" }, { "agency": "Queen\u02bcs University Belfast" }, { "agency": "Harvard-Smithsonian Center for Astrophysics" }, { "agency": "Las Cumbres Observatory Global Telescope Network Incorporated" }, { "agency": "National Central University of Taiwan" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" }, { "agency": "Eotvos Lorand University (ELTE)" }, { "agency": "European Research Council (ERC)", "grant_number": "291222" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Fonds de la Recherche Scientifique (FNRS)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "IceCube Collaboration", "PTF Collaboration", "Swift Collaboration", "Pan STARRSi Science Consortium" ] }, "doi": "10.1088/0004-637X/811/1/52", "primary_object": { "basename": "1506.03115v2.pdf", "url": "https://authors.library.caltech.edu/records/2z4ez-dj042/files/1506.03115v2.pdf" }, "related_objects": [ { "basename": "Aartsen_2015p52.pdf", "url": "https://authors.library.caltech.edu/records/2z4ez-dj042/files/Aartsen_2015p52.pdf" } ], "pub_year": "2015", "author_list": "Aartsen, M. G.; Kulkarni, Shrinivas R.; et el." }, { "id": "https://authors.library.caltech.edu/records/95jzn-jhy20", "eprint_id": 60737, "eprint_status": "archive", "datestamp": "2023-08-22 16:20:39", "lastmod": "2023-10-24 21:08:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cano-Z", "name": { "family": "Cano", "given": "Zach" }, "orcid": "0000-0001-9509-3825" }, { "id": "de-Ugarte-Postigo-A", "name": { "family": "de Ugarte Postigo", "given": "A." } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D." }, "orcid": "0000-0001-8472-1996" }, { "id": "Kr\u00fchler-T", "name": { "family": "Kr\u00fchler", "given": "T." } }, { "id": "Margutti-R", "name": { "family": "Margutti", "given": "R." }, "orcid": "0000-0003-4768-7586" }, { "id": "Friis-M", "name": { "family": "Friis", "given": "M." } }, { "id": "Malesani-D", "name": { "family": "Malesani", "given": "D." } }, { "id": "Jakobsson-P", "name": { "family": "Jakobsson", "given": "P." } }, { "id": "Fynbo-J-P-U", "name": { "family": "Fynbo", "given": "J. P. U." }, "orcid": "0000-0002-8149-8298" }, { "id": "Gorosabel-J", "name": { "family": "Gorosabel", "given": "J." } }, { "id": "Hjorth-J", "name": { "family": "Hjorth", "given": "J." }, "orcid": "0000-0002-4571-2306" }, { "id": "S\u00e1nchez-Ram\u00edrez-R", "name": { "family": "S\u00e1nchez-Ram\u00edrez", "given": "R." } }, { "id": "Schulze-S", "name": { "family": "Schulze", "given": "S." }, "orcid": "0000-0001-6797-1889" }, { "id": "Tanvir-N-R", "name": { "family": "Tanvir", "given": "N. R." } }, { "id": "Th\u00f6ne-C-C", "name": { "family": "Th\u00f6ne", "given": "C. C." } }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } } ] }, "title": "GRB 140606B/iPTF14bfu: detection of shock-breakout emission from a cosmological \u03b3-ray burst?", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: general; gamma-ray burst: individual: GRB 140606B; gamma-ray burst: individual: iPTF14bfu; supernovae: general", "note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 June 10. Received 2015 June 10. In original form 2015 May 13. First published online July 23, 2015. \n\nWe thank Giorgos Leloudas for his expertise in analysing the optical spectra of the SN. We also thank Y. Cao for carrying out the Keck observations.\n\nZC is funded by a Project Grant from the Icelandic Research Fund. PJ and MF acknowledge support by the University of Iceland Research fund. JPUF acknowledges support from the ERC-StG grant EGGS-278202. DM acknowledges the Instrument center for Danish Astrophysics (IDA) for support. The Dark Cosmology Centre is funded by the DNRF. SS acknowledges support from CONICYT-Chile FONDECYT 3140534, Basal-CATA PFB-06/2007, and Project IC120009 'Millennium Institute of Astrophysics' (MAS) of Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo.\n\nPublished - 1535.full.pdf
Submitted - 1505.03522v2.pdf
", "abstract": "We present optical and near-infrared photometry of GRB 140606B (z = 0.384), and optical photometry and spectroscopy of its associated supernova (SN). The results of our modelling indicate that the bolometric properties of the SN (M_(Ni) = 0.4 \u00b1 0.2 M_\u2299, M_(ej) = 5 \u00b1 2 M_\u2299, and E_K = 2 \u00b1 1 \u00d7 10^(52) erg) are fully consistent with the statistical averages determined for other \u03b3-ray burst (GRB)-SNe. However, in terms of its \u03b3-ray emission, GRB 140606B is an outlier of the Amati relation, and occupies the same region as low luminosity (ll) and short GRBs. The \u03b3-ray emission in llGRBs is thought to arise in some or all events from a shock breakout (SBO), rather than from a jet. The measured peak photon energy (E_p \u2248 800 keV) is close to that expected for \u03b3-rays created by an SBO (\u2273 1 MeV). Moreover, based on its position in the M_(V, p)-L_(iso, \u03b3) plane and the E_K\u2013\u0393\u03b2 plane, GRB 140606B has properties similar to both SBO-GRBs and jetted-GRBs. Additionally, we searched for correlations between the isotropic \u03b3-ray emission and the bolometric properties of a sample of GRB-SNe, finding that no statistically significant correlation is present. The average kinetic energy of the sample is E\u00af_K = 2.1\u00d710^(52) erg. All of the GRB-SNe in our sample, with the exception of SN 2006aj, are within this range, which has implications for the total energy budget available to power both the relativistic and non-relativistic components in a GRB-SN event.", "date": "2015-09-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "452", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1535-1552", "id_number": "CaltechAUTHORS:20151002-163711324", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151002-163711324", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Icelandic Research Fund" }, { "agency": "University of Iceland Research Fund" }, { "agency": "European Research Council (ERC)", "grant_number": "EGGS-278202" }, { "agency": "Instrument Center for Danish Astrophysics" }, { "agency": "Danish National Research Foundation" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3140534" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "Basal-CATA PFB-06/2007" }, { "agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda, Fomento y Turismo", "grant_number": "IC120009" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stv1327", "primary_object": { "basename": "1505.03522v2.pdf", "url": "https://authors.library.caltech.edu/records/95jzn-jhy20/files/1505.03522v2.pdf" }, "related_objects": [ { "basename": "1535.full.pdf", "url": "https://authors.library.caltech.edu/records/95jzn-jhy20/files/1535.full.pdf" } ], "pub_year": "2015", "author_list": "Cano, Zach; de Ugarte Postigo, A.; et el." }, { "id": "https://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" } ], "pub_year": "2015", "author_list": "Waszczak, Adam; Chang, Chan-Kao; et el." }, { "id": "https://authors.library.caltech.edu/records/evvff-7gd51", "eprint_id": 61321, "eprint_status": "archive", "datestamp": "2023-08-20 07:44:20", "lastmod": "2023-10-25 14:44:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Asteroids in GALEX: Near-ultraviolet Photometry of the Major Taxonomic Groups", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: general \u2013 surveys", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 April 16; accepted 2015 May 6; published 2015 August 13. \n\nA. Waszczak has been supported in part by the W.M. Keck Institute for Space Studies (KISS) at Caltech. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. This work makes use of data products from the GALEX mission, developed and operated with support from JPL/Caltech, the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology, Orbital Sciences, the University of California at Berkeley, and the Laboratoire d'Astrophysique de Marseille. This work also makes use of data derived from the Palomar Transient Factory (PTF) and the Intermediate PTF (iPTF) projects, operated at the 1.2 m Samuel Oschin Telescope at Palomar Observatory. Participating institutions have included Caltech, Columbia University, Las Cumbres Observatory Global Telescope Network, Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, the Kavli Institute for the Physics and Mathematics of the Universe, Los Alamos National Laboratory, the Oskar Klein Centre, the University System of Taiwan, the University of Wisconsin Milwaukee, and the Weizmann Institute of Science. This work also 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 (JPL)/Caltech, funded by NASA. This publication also makes use of data products from NEOWISE, which is a project of JPL/Caltech, funded by the Planetary Science Division of NASA. This work also makes use of data from the Sloan Digital Sky Survey (SDSS), 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.\n\nPublished - Waszczak_2015.pdf
Submitted - 1505.01458v2.pdf
", "abstract": "We present ultraviolet (UV) photometry (near-UV (NUV) band, 180\u2013280 nm) of 405 asteroids observed serendipitously by GALEX from 2003 to 2012. All asteroids in this sample were detected by GALEX at least twice. Unambiguous visible-color-based taxonomic labels (C type versus S type) exist for 315 of these asteroids; of these, thermal-infrared-based diameters are available for 245. We derive NUV \u2212 V color using two independent models to predict the visual magnitude V at each NUV-detection epoch. Both V models produce NUV \u2212 V distributions in which the S types are redder than C types with more than 8\u03c3 confidence. This confirms that the S types' redder spectral slopes in the visible remain redder than the C types' into the NUV, this redness being consistent with absorption by silica-containing rocks. The GALEX asteroid data confirm earlier results from the International Ultraviolet Explorer, which two decades ago produced the only other sizeable set of UV asteroid photometry. The GALEX-derived NUV \u2212 V data also agree with previously published Hubble Space Telescope (HST) UV observations of asteroids 21 Lutetia and 1 Ceres. Both the HST and GALEX data indicate that NUV band is less useful than u band for distinguishing subgroups within the greater population of visible-color-defined C types (notably, M types and G types).", "date": "2015-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "809", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 92", "id_number": "CaltechAUTHORS:20151020-103609257", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151020-103609257", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/809/1/92", "primary_object": { "basename": "1505.01458v2.pdf", "url": "https://authors.library.caltech.edu/records/evvff-7gd51/files/1505.01458v2.pdf" }, "related_objects": [ { "basename": "Waszczak_2015.pdf", "url": "https://authors.library.caltech.edu/records/evvff-7gd51/files/Waszczak_2015.pdf" } ], "pub_year": "2015", "author_list": "Waszczak, Adam; Ofek, Eran O.; et el." }, { "id": "https://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" } ], "pub_year": "2015", "author_list": "Ergon, M.; Jerkstrand, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/zq177-hv449", "eprint_id": 61302, "eprint_status": "archive", "datestamp": "2023-08-20 07:36:15", "lastmod": "2023-10-25 14:43:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "id": "Cheng-Yu-Chi", "name": { "family": "Cheng", "given": "Yu-Chi" } }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Yang-Ting-Chang", "name": { "family": "Yang", "given": "Ting-Chang" } }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" } ] }, "title": "Asteroid Spin-rate Study Using the Intermediate Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids: general \u2013 surveys", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 February 3; accepted 2015 June 27; published 2015 August 11. \n\nThis work is supported in part by the National Science Council of Taiwan under the grants NSC 101-2119-M-008-007-MY3 and NSC 102-2112-M-008-019-MY3. We thank the referees, Petr Pravec and Alan Harris, for their useful suggestions and comments to improve the content of the paper. This publication makes use of data products from 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. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Union\u02bcs Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University.\n\nPublished - Chang_2015.pdf
Submitted - 1506.08493v1.pdf
", "abstract": "Two dedicated asteroid rotation-period surveys have been carried out in the R band with ~20 minute cadence using the intermediate Palomar Transient Factory (iPTF) during 2014 January 6\u20139 and February 20\u201323. The total survey area covered 174 deg^2 in the ecliptic plane. Reliable rotation periods for 1438 asteroids are obtained from a larger data set of 6551 mostly main-belt asteroids, each with \u2a7e 10 detections. Analysis of 1751, PTF-based, reliable rotation periods clearly shows the spin barrier at ~2 hr for rubble-pile asteroids. We found a new large super-fast rotator, 2005 UW163, and another five candidates as well. For asteroids of 3 < D < 15 km, our spin-rate distribution shows a number decrease along with frequency after 5 rev day^(\u22121), which is consistent with the results of the Asteroid Light Curve Database. The discrepancy between our work and that of Pravec et al. (update 2014 April 20) comes mainly from asteroids with \u0394m < 0.2 mag, which could be the result of different survey strategies. For asteroids with D < 3 km, we see a significant number drop at f = 6 rev day^(\u22121). The relatively short YORP effect timescale for small asteroids could have spun up those elongated objects to reach their spin-rate limit resulting in breakup to create such a number deficiency. We also see that the C-type asteroids show a smaller spin-rate limit than the S-type, which agrees with the general impression that C-type asteroids have a lower bulk density than S-type asteroids.", "date": "2015-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "219", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 27", "id_number": "CaltechAUTHORS:20151020-081645580", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151020-081645580", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Council (Taipei)", "grant_number": "NSC 101-2119-M-008-007-MY3" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC 102-2112-M-008-019-MY3" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0067-0049/219/2/27", "primary_object": { "basename": "1506.08493v1.pdf", "url": "https://authors.library.caltech.edu/records/zq177-hv449/files/1506.08493v1.pdf" }, "related_objects": [ { "basename": "Chang_2015.pdf", "url": "https://authors.library.caltech.edu/records/zq177-hv449/files/Chang_2015.pdf" } ], "pub_year": "2015", "author_list": "Chang, Chan-Kao; Ip, Wing-Huen; et el." }, { "id": "https://authors.library.caltech.edu/records/k2n5e-m7y33", "eprint_id": 60535, "eprint_status": "archive", "datestamp": "2023-08-20 07:35:15", "lastmod": "2023-10-24 16:38:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schindewolf-M", "name": { "family": "Schindewolf", "given": "M." } }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } }, { "id": "Heber-U", "name": { "family": "Heber", "given": "U." }, "orcid": "0000-0001-7798-6769" }, { "id": "Drechsel-H", "name": { "family": "Drechsel", "given": "H." } }, { "id": "Schaffenroth-V", "name": { "family": "Schaffenroth", "given": "V." } }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "T." }, "orcid": "0000-0002-6540-1484" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T." }, "orcid": "0000-0002-8850-3627" } ] }, "title": "A new HW Vir binary from the Palomar Transient Factory. PTF1 J072455.75+125300.3: An eclipsing subdwarf B binary with a M-star companion", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing \u2013 stars: early-type \u2013 stars: evolution \u2013 stars: fundamental parameters \u2013 stars: horizontal-branch \u2013subdwarfs", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 23 December 2014; Accepted 10 June 2015; Published online 14 August 2015.\n\nBased on observations collected at the Palomar Observatory with the 200-inch Hale Telescope, operated by the California institute of Technology, its divisions Caltech Optical Observations, the Jet Propulsion Laboratory (operated for NASA) and Cornell University. Based on observations of the Palomar Transient Factory. The Palomar Transient Factory is a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkely National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. T. Kupfer acknowledges support by the Netherlands Research School of Astronomy (NOVA). V. Schaffenroth is supported by the Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (grant 50 OR 1110). This research has made use of ISIS functions provided by ECAP/Remeis Obervatory.\n\nPublished - aa25581-14.pdf
Submitted - 1506.03787v1.pdf
", "abstract": "We report the discovery of an eclipsing binary \u2013 PTF1\u2009J072456+125301\u2013 composed of a subdwarf B (sdB) star (g\u2032 = 17.2^m) with a faint companion. Subdwarf B stars are core helium-burning stars, which can be found on the extreme horizontal branch. About half of them reside in close binary systems, but few are known to be eclipsing, for which fundamental stellar parameters can be derived. We conducted an analysis of photometric data and spectra from the Palomar 60\u2032\u2032 and the 200\u2032\u2032 Hale telescope, respectively. A quantitative spectral analysis found an effective temperature of T_(eff) = 33 900 \u00b1 350 K, log\u2009g = 5.74 \u00b1 0.08, and log\u2009(n_(He)/n_H) = \u22122.02 \u00b1 0.07, typical for an sdB star. The companion does not contribute to the optical light of the system, except through a distinct reflection effect. From the light curve an orbital period of 0.09980(25)\u2009d and a system inclination of 83.56 \u00b1 0.30\u00b0 were derived. The radial velocity curve yielded an orbital semi-amplitude of K_1 = 95.8 \u00b1 8.1 km s^(-1). The mass for the M-type dwarf companion is 0.155 \u00b1 0.020 M\u2299. PTF1\u2009J072456+125301 has similar atmospheric parameters to those of pulsating sdB stars (V346 Hya stars). Therefore it could be a high-priority object for asteroseismology, if pulsations were detected such as in the enigmatic case of NY Vir.", "date": "2015-08", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "580", "publisher": "EDP Sciences", "pagerange": "Art. No. A117", "id_number": "CaltechAUTHORS:20150925-141355852", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150925-141355852", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)", "grant_number": "50 OR 1110" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201425581", "primary_object": { "basename": "1506.03787v1.pdf", "url": "https://authors.library.caltech.edu/records/k2n5e-m7y33/files/1506.03787v1.pdf" }, "related_objects": [ { "basename": "aa25581-14.pdf", "url": "https://authors.library.caltech.edu/records/k2n5e-m7y33/files/aa25581-14.pdf" } ], "pub_year": "2015", "author_list": "Schindewolf, M.; Levitan, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/gayqx-g7b96", "eprint_id": 96193, "eprint_status": "archive", "datestamp": "2023-08-20 07:17:32", "lastmod": "2023-10-20 20:58:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ackermann-M", "name": { "family": "Ackermann", "given": "M." } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Baldini-L", "name": { "family": "Baldini", "given": "L." } }, { "id": "Ballet-J", "name": { "family": "Ballet", "given": "J." } }, { "id": "Barbiellini-G", "name": { "family": "Barbiellini", "given": "G." } } ] }, "title": "Search for early gamma-ray production in supernovae located in dense circumstellar medium with the FERMILAT", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2015. The American Astronomical Society. \n\nReceived 2015 April 10. Accepted 2015 June 2. Published 2015 July 9. \n\nThe Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat \u00e0 l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucl\u00e9aire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'\u00c9tudes Spatiales in France. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We are grateful for excellent staff assistance at the Palomar, Lick, and Keck Observatories. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), the Israeli Ministry of Science, the Israel Science Foundation, Minerva and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for Planning and Budgeting and the ISF, Minerva and ISF grants, WIS-UK \"Making Connections\", and Kimmel and ARCHES awards.", "abstract": "Supernovae (SNe) exploding in a dense circumstellar medium (CSM) are hypothesized to accelerate cosmic rays in collisionless shocks and emit GeV \u03b3-rays and TeV neutrinos on a timescale of several months. We perform the first systematic search for \u03b3-ray emission in Fermi Large Area Telescope data in the energy range from $100\\;\\mathrm{MeV}$ to $300\\;\\mathrm{GeV}$ from the ensemble of 147 SNe Type IIn exploding in a dense CSM. We search for a \u03b3-ray excess at each SNe location in a one-year time window. In order to enhance a possible weak signal, we simultaneously study the closest and optically brightest sources of our sample in a joint-likelihood analysis in three different time windows (1 year, 6 months, and 3 months). For the most promising source of the sample, SN 2010jl (PTF 10aaxf), we repeat the analysis with an extended time window lasting 4.5 years. We do not find a significant excess in \u03b3-rays for any individual source nor for the combined sources and provide model-independent flux upper limits for both cases. In addition, we derive limits on the \u03b3-ray luminosity and the ratio of \u03b3-ray-to-optical luminosity ratio as a function of the index of the proton injection spectrum assuming a generic \u03b3-ray production model. Furthermore, we present detailed flux predictions based on multi-wavelength observations and the corresponding flux upper limit at a 95% confidence level (CL) for the source SN 2010jl (PTF 10aaxf).", "date": "2015-07-09", "date_type": "published", "publication": "Astrophysical Journal", "volume": "807", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. 169", "id_number": "CaltechAUTHORS:20190606-131743652", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190606-131743652", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-637X/807/2/169", "pub_year": "2015", "author_list": "Ackermann, M.; Arcavi, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/7e73t-hnk67", "eprint_id": 58967, "eprint_status": "archive", "datestamp": "2023-08-22 15:41:30", "lastmod": "2023-10-23 19:55:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Singer-L-P", "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan" }, "orcid": "0000-0002-0928-6784" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "The Needle in the 100 deg^2 Haystack: Uncovering Afterglows of Fermi GRBs with the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: individual (GRB 130702A, GRB 140606B); gravitational waves; methods: observational; supernovae: general; surveys", "note": "\u00a9 2015 American Astronomical Society.\n\nReceived 2015 January 2; accepted 2015 February 28; published 2015 June 8.\n\nL.P.S. thanks generous support from the National Science Foundation (NSF) in the form of a Graduate Research Fellowship. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. This paper is based on observations obtained with the Palomar 48 inch Oschin telescope and the Palomar 60 inch telescope at the Palomar Observatory as part of the Intermediate Palomar Transient Factory project, a scientific collaboration among the California Institute of\nTechnology, Los Alamos National Laboratory, the University\nof Wisconsin, Milwaukee, the Oskar Klein Center, the\nWeizmann Institute of Science, the TANGO Program of the\nUniversity System of Taiwan, and the Kavli Institute for the\nPhysics and Mathematics of the Universe. The present work is\npartly funded by Swift Guest Investigator Program Cycle 9\naward 10522 (NASA grant NNX14AC24G) and Cycle 10\naward 10553 (NASA grant NNX14AI99G). Some of the data\npresented herein were obtained at the W. M. Keck Observatory,\nwhich is operated as a scientific partnership among the\nCalifornia Institute of Technology, the University of California,\nand NASA; the Observatory was made possible by the generous\nfinancial support of the W.M. Keck Foundation. We thank\nThomas Kr\u00fchler for reducing the X-shooter spectrum of\nGRB 131011A/iPTF13dsw. We thank the staff of the Mullard\nRadio Astronomy Observatory for their invaluable assistance in\nthe operation of AMI. G.E.A., R.P.F., and T.D.S. acknowledge\nthe support of the European Research Council Advanced Grant\n267697, \"4 Pi Sky: Extreme Astrophysics with Revolutionary\nRadio Telescopes.\" Support for CARMA construction was\nderived from the Gordon and Betty Moore Foundation; the\nKenneth T. and Eileen L. Norris Foundation; the James S.\nMcDonnell Foundation; the Associates of the California Institute\nof Technology; the University of Chicago; the states of\nCalifornia, Illinois, and Maryland; and the NSF. Ongoing\nCARMA development and operations are supported by the NSF\nunder a cooperative agreement and by the CARMA partner\nuniversities. These results made use of Lowell Observatory's\nDCT. Lowell operates the DCT in partnership with Boston\nUniversity, Northern Arizona University, the University of\nMaryland, and the University of Toledo. Partial support of the\nDCT was provided by Discovery Communications. LMI was\nbuilt by Lowell Observatory using funds from the NSF (AST-\n1005313). This work is partly based on observations made with\nGTC, at the Roque de los Muchachos Observatory (La Palma,\nSpain). The research activity of A.d.U.P., C.T., and J.G. is\nsupported by Spanish research project AYA2012-39362-C02-02. A.d.U.P. acknowledges support by the European Commission\nunder the Marie Curie Career Integration Grant programme\n(FP7-PEOPLE-2012-CIG 322307). A portion of this work was\ncarried out at the Jet Propulsion Laboratory under a Research\nand Technology Development Grant, under contract with\nNASA. US Government Support Acknowledged. K.H. acknowledges\nsupport for the IPN under the following NASA grants:\nNNX07AR71G, NNX13AP09G, NNX11AP96G, and\nNNX13AI54G. The Konus-Wind experiment is partially supported\nby a Russian Space Agency contract and RFBR grants\n15-02-00532 and 13-02-12017-ofi-m. IRAF is distributed by the\nNational Optical Astronomy Observatory, which is operated by\nthe Association of Universities for Research in Astronomy\n(AURA) under cooperative agreement with the NSF. This\nresearch has made use of data, software, and/or web tools\nobtained from HEASARC, a service of the Astrophysics Science\nDivision at NASA/GSFC and of the Smithsonian Astrophysical\nObservatory's High Energy Astrophysics Division. This\nresearch has made use of NED, which is operated by the Jet\nPropulsion Laboratory, California Institute of Technology, under\ncontract with NASA. This work made use of data supplied by\nthe UK Swift Science Data Centre at the University of Leicester\nincluding the Swift XRT GRB catalog and light-curve repository\n(Evans et al. 2007, 2009; Goad et al. 2007). This research made\nuse of Astropy49 (Robitaille et al. 2013), a community developed\ncore Python package for Astronomy. Some of the\nresults in this paper have been derived using HEALPix (G\u00f3rski\net al. 2005).\nFacilities: Fermi (GBM, LAT), PO:1.2 m (CFH12k),\nPO:1.5 m, Hale (DBSP), Gemini:Gillett (GMOS), Gemini:\nSouth (GMOS), EVLA, CARMA, Swift (XRT, UVOT),\nKeck:I (LRIS), Keck:II (DEIMOS), NOT (ALFOSC), HCT,\nAMI, VLT: Melipal (X-shooter), INTEGRAL(SPI-ACS),\nOdyssey (HEND), MESSENGER (GRNS), WIND (Konus)\n\nPublished - 0004-637X_806_1_52.pdf
Submitted - 1501.00495v4.pdf
", "abstract": "The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron star mergers that may soon be detected by Advanced LIGO and Virgo.", "date": "2015-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "806", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 52", "id_number": "CaltechAUTHORS:20150721-140335760", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150721-140335760", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA", "grant_number": "NNX14AC24G" }, { "agency": "NASA", "grant_number": "NNX14AI99G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "267697" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Caltech Associates" }, { "agency": "University of Chicago" }, { "agency": "State of California" }, { "agency": "State of Illinois" }, { "agency": "State of Maryland" }, { "agency": "NSF" }, { "agency": "Discovery Communications" }, { "agency": "NSF", "grant_number": "AST-1005313" }, { "agency": "Spanish Research Project", "grant_number": "AYA2012-39362-C02-02" }, { "agency": "Marie Curie Fellowship", "grant_number": "FP7-PEOPLE-2012-CIG 322307" }, { "agency": "U. S. Government" }, { "agency": "NASA", "grant_number": "NNX07AR71G" }, { "agency": "NASA", "grant_number": "NNX13AP09G" }, { "agency": "NASA", "grant_number": "NNX11AP96G" }, { "agency": "NASA", "grant_number": "NNX13AI54G" }, { "agency": "Russian Space Agency" }, { "agency": "Russian Foundation for Basic Research (RFBR)", "grant_number": "15-02-00532" }, { "agency": "Russian Foundation for Basic Research (RFBR)", "grant_number": "13-02-12017-ofi-m" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/806/1/52", "primary_object": { "basename": "0004-637X_806_1_52.pdf", "url": "https://authors.library.caltech.edu/records/7e73t-hnk67/files/0004-637X_806_1_52.pdf" }, "related_objects": [ { "basename": "1501.00495v4.pdf", "url": "https://authors.library.caltech.edu/records/7e73t-hnk67/files/1501.00495v4.pdf" } ], "pub_year": "2015", "author_list": "Singer, Leo P.; Weinstein, Alan; et el." }, { "id": "https://authors.library.caltech.edu/records/5kn8t-vfb32", "eprint_id": 59395, "eprint_status": "archive", "datestamp": "2023-08-20 06:30:33", "lastmod": "2023-10-23 20:32:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "E. Y." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Strong near-infrared carbon in the Type Ia supernova iPTF13ebh", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: general \u2013 supernovae: general \u2013 supernovae: individual: iPTF13ebh", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 7 November 2014; Accepted 7 March 2015; Published online 22 May 2015. \n\nThis paper includes data gathered with the 6.5-m Magellan Telescopes located at Las Campanas Observatory, Chile. \n\nThis paper is based upon work supported by the National Science Foundation under Grant No. AST-1008343. M.S., E.Y.H., C.C, and C.G. acknowledge the generous support provided by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. S.G. acknowledges support from CONICYT through FONDECYT grant 3130680 and from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. The Dark Cosmology Centre is funded by the Danish National Research Foundation. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development program. The bulk of the data presented here was obtained with the 1 m Swope, 2.5 m du Pont, and the 6.5 m Magellan Telescopes at the Las Campanas Observatory. This work also relies on data obtained at the Gemini Observatory, under the long-term program GN-2013B-Q-76. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina). The authors would like to recognize the very significant cultural role and reverence that the summit of Mauna Kea has within the indigenous community of Hawaii. We are grateful for our opportunity to conduct observations from this mountain. We have also made use of the Nordic Optical Telescope, which is 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 William Herschel Telescope and its override programme are 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. This research used resources from the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office Science of the US Department of Energy under Contract No. DEAC02-05CH11231. We have 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 - aa25297-14.pdf
Submitted - 1503.02293v1.pdf
", "abstract": "We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2.3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C\u2009i lines, and the C\u2009i\u03bb1.0693 \u03bcm line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C\u2009ii counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C\u2009i compared to the weaker optical C\u2009ii appears to be general in SNe Ia. iPTF13ebh is a fast decliner with \u0394m15(B) = 1.79 \u00b1 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a \"transitional\" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si\u2009ii\u03bb0.6355 \u03bcm line, implying a long dark phase of ~4 days.", "date": "2015-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "578", "publisher": "EDP Sciences", "pagerange": "Art. No. A9", "id_number": "CaltechAUTHORS:20150811-110635045", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150811-110635045", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1008343" }, { "agency": "Danish Agency for Science and Technology and Innovation" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3130680" }, { "agency": "Iniciativa Cient\u00edfica Milenio del Ministerio de Econom\u00eda", "grant_number": "IC12009" }, { "agency": "Danish National Research Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1051/0004-6361/201425297", "primary_object": { "basename": "1503.02293v1.pdf", "url": "https://authors.library.caltech.edu/records/5kn8t-vfb32/files/1503.02293v1.pdf" }, "related_objects": [ { "basename": "aa25297-14.pdf", "url": "https://authors.library.caltech.edu/records/5kn8t-vfb32/files/aa25297-14.pdf" } ], "pub_year": "2015", "author_list": "Hsiao, E. Y.; Cao, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/4qgkw-9r889", "eprint_id": 55347, "eprint_status": "archive", "datestamp": "2023-08-20 06:21:01", "lastmod": "2023-10-23 15:34:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi Manoj" }, "orcid": "0000-0002-5619-4938" }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "Stefano" }, "orcid": "0000-0001-8818-0795" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." }, "orcid": "0000-0001-5975-290X" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Sagiv-I", "name": { "family": "Sagiv", "given": "Ilan" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "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": "Wo\u017aniak-P-R", "name": { "family": "Wo\u017aniak", "given": "P. R." }, "orcid": "0000-0002-9919-3310" }, { "id": "Moody-D-I", "name": { "family": "Moody", "given": "Daniela I." } }, { "id": "Rebbapragada-U-D", "name": { "family": "Rebbapragada", "given": "Umaa D." }, "orcid": "0000-0002-2560-3495" }, { "id": "Bue-B-D", "name": { "family": "Bue", "given": "Brian D." }, "orcid": "0000-0002-7856-3570" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } } ] }, "title": "A Strong Ultraviolet Pulse From a Newborn Type Ia Supernova", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 Macmillan Publishers Limited. \n\nReceived 14 November 2014; accepted 16 March 2015. \n\nWe thank A. L. Piro, M. Kromer and J. Cohen for discussions. We also thank A. Waszczak, A. Rubin, O. Yaron, A. De Cia, D. A. Perley, G. E. Duggan, O. Smirnova, S. Papadogiannakis, A. Nyholm, Y. F. Martinez and the staff at the Nordic Optical Telescope and Gemini for observation and data reduction. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some data were obtained with the Nordic Optical Telescope, which is operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain. This work also makes use of observations from the Las Cumbres Observatory Global Telescope (LCOGT) network. Research at California Institute of Technology is supported by the National Science Foundation. D.A.H. acknowledges support from the National Science Foundation. A.G.-Y. acknowledges support from the EU/FP7 via an ERC grant, the \"Quantum Universe\" I-Core programme, the ISF, Minerva and Weizmann-UK grants, and the Kimmel Award. M.M.K. acknowledges generous support from the Carnegie-Princeton fellowship. Supernova research at the Oskar Klein Centre is supported by the Swedish Research Council and by the Knut and Alice Wallenberg Foundation. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under contract number DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. The participation of the Los Alamos National Laboratory (LANL) in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development programme. A portion of this work was carried out at the Jet Propulsion Laboratory under a Research and Technology Development Grant, under contract with the National Aeronautics and Space Administration.\n\nSupplemental Material - nature14440-sf1.jpg
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", "abstract": "Type Ia supernovae are destructive explosions of carbon-oxygen white dwarfs. Although they are used empirically to measure cosmological distances, the nature of their progenitors remains mysterious. One of the leading progenitor models, called the single degenerate channel, hypothesizes that a white dwarf accretes matter from a companion star and the resulting increase in its central pressure and temperature ignites thermonuclear explosion. Here we report observations with the Swift Space Telescope of strong but declining ultraviolet emission from a type Ia supernova within four days of its explosion. This emission is consistent with theoretical expectations of collision between material ejected by the supernova and a companion star, and therefore provides evidence that some type Ia supernovae arise from the single degenerate channel.", "date": "2015-05-21", "date_type": "published", "publication": "Nature", "volume": "521", "number": "7552", "publisher": "Nature Publishing Group", "pagerange": "328-331", "id_number": "CaltechAUTHORS:20150227-145859366", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150227-145859366", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF" }, { "agency": "European Research Council (ERC)" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Swedish Research Council" }, { "agency": "Knut and Alice Wallenberg Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature14440", "primary_object": { "basename": "nature14440-sf1.jpg", "url": "https://authors.library.caltech.edu/records/4qgkw-9r889/files/nature14440-sf1.jpg" }, "related_objects": [ { "basename": "nature14440-sf2.jpg", "url": "https://authors.library.caltech.edu/records/4qgkw-9r889/files/nature14440-sf2.jpg" }, { "basename": "nature14440-sf3.jpg", "url": "https://authors.library.caltech.edu/records/4qgkw-9r889/files/nature14440-sf3.jpg" }, { "basename": "nature14440-sf4.jpg", "url": "https://authors.library.caltech.edu/records/4qgkw-9r889/files/nature14440-sf4.jpg" }, { "basename": "nature14440-st1.jpg", "url": "https://authors.library.caltech.edu/records/4qgkw-9r889/files/nature14440-st1.jpg" }, { "basename": "nature14440-st2.jpg", "url": "https://authors.library.caltech.edu/records/4qgkw-9r889/files/nature14440-st2.jpg" } ], "pub_year": "2015", "author_list": "Cao, Yi; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/cp7v3-0tb64", "eprint_id": 58647, "eprint_status": "archive", "datestamp": "2023-08-20 06:15:27", "lastmod": "2023-10-23 19:33:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Mauerhan-J-C", "name": { "family": "Mauerhan", "given": "Jon C." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Clubb-K-I", "name": { "family": "Clubb", "given": "Kelsey I." } }, { "id": "Graham-M-L", "name": { "family": "Graham", "given": "Melissa L." }, "orcid": "0000-0002-9154-3136" }, { "id": "Leonard-D-C", "name": { "family": "Leonard", "given": "Douglas C." } }, { "id": "Horst-J-C", "name": { "family": "Horst", "given": "J. Chuck" } }, { "id": "Williams-G-G", "name": { "family": "Williams", "given": "G. Grant" } }, { "id": "Andrews-J-E", "name": { "family": "Andrews", "given": "Jennifer E." }, "orcid": "0000-0003-0123-0062" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter" }, "orcid": "0000-0002-3389-0586" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "Kate" }, "orcid": "0000-0002-9770-3508" }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "Dong" } }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" } ] }, "title": "PTF11iqb: cool supergiant mass-loss that bridges the gap between Type IIn and normal supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter\n stars: evolution\n supernovae: general\n supernovae: individual: PTF11iqb\n stars: winds, outflows", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 February 16. Received 2015 February 13; in original form 2015 January 8. First published online March 26, 2015. \n\nWe thank Iair Arcavi, Peter Blanchard, Yi Cao, Ori Fox, Paul Groot, Asaf Horesh, Michael Kandrashoff, Pat Kelly, Nick Konidaris, Rubina Kotak, David Levitan, Adam Miller, Yen-Chen Pan, Jarod Parrent, Paul Smith, and Wei Kang Zheng for assistance with some of the observations and data reduction. We thank Eran Ofek for helpful discussions and assistance with the PTF photometric data. We thank the referee, Max Stritzinger, for a careful reading of the\nmanuscript and helpful comments. We thank the staffs at Lick, MMT, LBT, Keck, Palomar, and WHT for their assistance with the observations. Observations using Steward Observatory facilities were obtained as part of the observing program AZTEC: Arizona Transient Exploration and Characterization. Some observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. This\nresearch was based in part on observations made with the LBT. The LBT is an international collaboration among institutions in the United States, Italy and Germany. The LBT Corporation partners are: the University of Arizona on behalf of the Arizona university system; the Istituto Nazionale di Astrofisica, Italy; the LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam and Heidelberg University; the Ohio State University and the Research Corporation, on behalf of the University of Notre Dame, University of Minnesota and University of Virginia. The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00c3sica de Canarias. Some\nof 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. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NS received partial support from NSF grants AST-1210599 and AST-1312221. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva\nand the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. AGY is supported by the EU/FP7 via ERC grant no. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva and ISF grants, WIS-UK 'making connections,' and Kimmel and ARCHES awards. The supernova research of AVF's group at U.C. Berkeley is supported by Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS\nis supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771.KM is supported by a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). MS acknowledges support from the Royal Society. DCL and JCH are grateful for support from NSF grants AST-1009571 and AST-1210311, under which part of this research (photometry collected at MLO) was carried out.\n\nPublished - MNRAS-2015-Smith-1876-96.pdf
Submitted - 1501.02820v1.pdf
", "abstract": "The supernova (SN) PTF11iqb was initially classified as a Type IIn event caught very early after explosion. It showed narrow Wolf\u2013Rayet (WR) spectral features on day 2 (as in SN 1998S and SN 2013cu), but the narrow emission weakened quickly and the spectrum morphed to resemble Types II-L and II-P. At late times, H\u03b1 exhibited a complex, multipeaked profile reminiscent of SN 1998S. In terms of spectroscopic evolution, we find that PTF11iqb was a near twin of SN 1998S, although with somewhat weaker interaction with circumstellar material (CSM) at early times, and stronger interaction at late times. We interpret the spectral changes as caused by early interaction with asymmetric CSM that is quickly (by day 20) enveloped by the expanding SN ejecta photosphere, but then revealed again after the end of the plateau when the photosphere recedes. The light curve can be matched with a simple model for CSM interaction (with a mass-loss rate of roughly 10^(\u22124) M_\u2299 yr^(\u22121)) added to the light curve of a normal SN II-P. The underlying plateau requires a progenitor with an extended hydrogen envelope like a red supergiant at the moment of explosion, consistent with the slow wind speed (<80\u2009km\u2009s^(\u22121)) inferred from narrow H\u03b1 emission. The cool supergiant progenitor is significant because PTF11iqb showed WR features in its early spectrum \u2013 meaning that the presence of such WR features does not necessarily indicate a WR-like progenitor. Overall, PTF11iqb bridges SNe IIn with weaker pre-SN mass-loss seen in SNe II-L and II-P, implying a continuum between these types.", "date": "2015-05-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "449", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1876-1896", "id_number": "CaltechAUTHORS:20150629-064849723", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150629-064849723", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-1210599" }, { "agency": "NSF", "grant_number": "AST-1312221" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Quantum Universe I-Core program" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NSF Postdoctoral Fellowship", "grant_number": "AST-1302771" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Royal Society" }, { "agency": "NSF", "grant_number": "AST-1009571" }, { "agency": "NSF", "grant_number": "AST-1210311" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stv354", "primary_object": { "basename": "1501.02820v1.pdf", "url": "https://authors.library.caltech.edu/records/cp7v3-0tb64/files/1501.02820v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Smith-1876-96.pdf", "url": "https://authors.library.caltech.edu/records/cp7v3-0tb64/files/MNRAS-2015-Smith-1876-96.pdf" } ], "pub_year": "2015", "author_list": "Smith, Nathan; Mauerhan, Jon C.; et el." }, { "id": "https://authors.library.caltech.edu/records/42tv1-xqe83", "eprint_id": 57771, "eprint_status": "archive", "datestamp": "2023-08-22 15:22:53", "lastmod": "2023-10-23 17:44:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "iPTF14yb: The First Discovery of a Gamma-Ray Burst Afterglow Independent of a High-energy Trigger", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: general; stars: flare; supernovae: general", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 February 20; accepted 2015 March 26; published 2015 April 20.\n\nWe thank David Jewitt for executing our Keck/LRIS ToO\nobservations, and Eran Ofek, Leo Singer, and Eric Bellm for\ncomments on this manuscript. A.L.U. was supported by NSF\ngrants PHY-0970074 and PHY-1307429 at the UWM Research\nGrowth Initiative. J.F.G. acknowledges the Sofja Kovalevskaja\naward to P. Schady from the Alexander von Humboldt\nFoundation Germany. D.A.K. thanks TLS Tautenburg for\nfinancial support. The work of A.V.F. was made possible by\nNSF grant AST-1211916, the TABASGO Foundation, Gary\nand Cynthia Bengier, and the Christopher R. Redlich Fund.\nJ.X.P. received funding from NASA grants NNX13AP036 and\nNNX14AI95G.\nThis paper is based in part on observations obtained with the\nP48 Oschin telescope as part of the Intermediate Palomar\nTransient Factory project, a scientific collaboration among the\nCaltech, LANL, UW-Milwaukee, the Oskar Klein Center, the\nWeizmann Institute of Science, the TANGO Program of the\nUniversity System of Taiwan, and the Kavli IPMU. LANL\nparticipation in iPTF is supported by the US Department of\nEnergy as part of the Laboratory of Directed Research and\nDevelopment program. The National Energy Research Scientific\nComputing Center provided staff, computational\nresources, and data storage for this project. Part of the funding\nfor GROND (both hardware and personnel) was generously\ngranted from the Leibniz-Prize to Prof. G. Hasinger (DFG\ngrant HA 1850/28-1). Some of the data presented herein were\nobtained at the W.M. Keck Observatory, which is operated as a\nscientific partnership among the California Institute of\nTechnology, the University of California, and NASA; the\nobservatory was made possible by the generous financial\nsupport of the W.M. Keck Foundation.\nWe thank the RATIR project team and the staff of the\nObservatorio Astron\u00f3mico Nacional on Sierra San Pedro\nM\u00e0rtir. RATIR is a collaboration between the University of\nCalifornia, the Universidad Nacional Auton\u00f3ma de M\u00e9xico,\nNASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector\nand hardware and software support from Teledyne Scientific\nand Imaging. RATIR, the automation of the Harold L. Johnson\nTelescope of the Observatorio Astron\u00f3mico Nacional on Sierra\nSan Pedro M\u00e1rtir, and the operation of both are funded through\nNASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G,\nand NNX12AE66G, CONACyT grants INFR-2009-01-122785\nand CB-2008-101958, UNAM PAPIIT grant IN113810, and UC\nMEXUS-CONACyT grant CN 09-283.\n\nFacilities: PO:1.2m (PTF), Keck:I (LRIS), Magellan: Baade\n(IMACS), Lulin (TRIPOL), Max Planck:2.2m (GROND),\nOANSPM:HJT (RATIR), VLA, CARMA, Swift (XRT)\n\nPublished - 2041-8205_803_2_L24.pdf
Submitted - 1504.00673v1.pdf
", "abstract": "We report here the discovery by the Intermediate Palomar Transient Factory (iPTF) of iPTF14yb, a luminous (M_r \u2248 27.8 mag), cosmological (redshift 1.9733), rapidly fading optical transient. We demonstrate, based on probabilistic arguments and a comparison with the broader population, that iPTF14yb is the optical afterglow of the long-duration gamma-ray burst GRB 140226A. This marks the first unambiguous discovery of a GRB afterglow prior to (and thus entirely independent of) an associated high-energy trigger. We estimate the rate of iPTF14yb-like sources (i.e., cosmologically distant relativistic explosions) based on iPTF observations, inferring an all-sky value of yr^\u22121 (68% confidence interval of 110\u20132000 yr\u22121). Our derived rate is consistent (within the large uncertainty) with the all-sky rate of on-axis GRBs derived by the Swift satellite. Finally, we briefly discuss the implications of the nondetection to date of bona fide \"orphan\" afterglows (i.e., those lacking detectable high-energy emission) on GRB beaming and the degree of baryon loading in these relativistic jets.", "date": "2015-04-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "803", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L24", "id_number": "CaltechAUTHORS:20150522-095957473", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150522-095957473", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0970074" }, { "agency": "NSF", "grant_number": "PHY-1307429" }, { "agency": "Alexander von Humboldt Foundation" }, { "agency": "TLS Tautenburg" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "NASA", "grant_number": "NNX13AP036" }, { "agency": "NASA", "grant_number": "NNX14AI95G" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/803/2/L24", "primary_object": { "basename": "1504.00673v1.pdf", "url": "https://authors.library.caltech.edu/records/42tv1-xqe83/files/1504.00673v1.pdf" }, "related_objects": [ { "basename": "2041-8205_803_2_L24.pdf", "url": "https://authors.library.caltech.edu/records/42tv1-xqe83/files/2041-8205_803_2_L24.pdf" } ], "pub_year": "2015", "author_list": "Cenko, S. Bradley; Perley, Daniel A.; et el." }, { "id": "https://authors.library.caltech.edu/records/5ztyk-d4y09", "eprint_id": 55627, "eprint_status": "archive", "datestamp": "2023-08-22 14:50:20", "lastmod": "2023-10-20 22:26:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yu-Po-Chieh", "name": { "family": "Yu", "given": "P. C." }, "orcid": "0000-0001-8894-0854" }, { "id": "Lin-C-C", "name": { "family": "Lin", "given": "C. C." } }, { "id": "Chen-Wen-Ping", "name": { "family": "Chen", "given": "W. P." }, "orcid": "0000-0003-0262-272X" }, { "id": "Lee-C-D", "name": { "family": "Lee", "given": "C. D." } }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "W. H." }, "orcid": "0000-0002-3140-5014" }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "C. C." }, "orcid": "0000-0001-8771-7554" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Searching for Be Stars in the Open Cluster NGC 663", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: star clusters: individual (NGC 663); stars: emission-line, Be", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2014 August 8; accepted 2014 October 14; published 2015 January 7. \n\nWe thank the referee for constructive comments. We also thank C. K. Chang, M. Kasiliwal, and H. C. Chen for useful discussions and information. This work is supported in part by the National Science Council of Taiwan under grants NSC 101-2119-M-008-007-MY3 (W.-H.I.), NSC 102-2119-M-008-001 (W.-P.C.), and NSC101-2112-M-008-017-MY3 (C.-C.N.). 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 - 1538-3881_149_2_43.pdf
Submitted - 1411.5496v1.pdf
", "abstract": "We present Be star candidates in the open cluster NGC 663, identified by H\u03b1 imaging photometry with the Palomar Transient Factory Survey, as a pilot program to investigate how the Be star phenomena, the emission spectra, extended circumstellar envelopes, and fast rotation, correlate with massive stellar evolution. Stellar membership of the candidates was verified by 2MASS magnitudes and colors and by proper motions (PMs). We discover four new Be stars and exclude one known Be star from being a member due to its inconsistent PMs. The fraction of Be stars to member stars [N(Be)/N(members)] in NGC 663 is 3.5%. The spectral type of the 34 Be stars in NGC 663 shows bimodal peaks at B0\u2013B2 and B5\u2013B7, which is consistent with the statistics in most star clusters. Additionally, we also discover 23 emission-line stars of different types, including non-member Be stars, dwarfs, and giants.", "date": "2015-02", "date_type": "published", "publication": "Astronomical Journal", "volume": "149", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 43", "id_number": "CaltechAUTHORS:20150309-092112610", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150309-092112610", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Council (Taipei)", "grant_number": "NSC 101-2119-M-008-007-MY3" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC 102-2119-M-008-001" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC 101-2112-M-008-017-MY3" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-6256/149/2/43", "primary_object": { "basename": "1411.5496v1.pdf", "url": "https://authors.library.caltech.edu/records/5ztyk-d4y09/files/1411.5496v1.pdf" }, "related_objects": [ { "basename": "1538-3881_149_2_43.pdf", "url": "https://authors.library.caltech.edu/records/5ztyk-d4y09/files/1538-3881_149_2_43.pdf" } ], "pub_year": "2015", "author_list": "Yu, P. C.; Lin, C. C.; et el." }, { "id": "https://authors.library.caltech.edu/records/5wb9b-76935", "eprint_id": 56414, "eprint_status": "archive", "datestamp": "2023-08-20 04:47:28", "lastmod": "2023-10-23 15:23:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Firth-R-E", "name": { "family": "Firth", "given": "R. E." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P." }, "orcid": "0000-0002-3389-0586" }, { "id": "Piro-A-L", "name": { "family": "Piro", "given": "A. L." }, "orcid": "0000-0001-6806-0673" }, { "id": "Baltay-C", "name": { "family": "Baltay", "given": "C." } }, { "id": "Feindt-U", "name": { "family": "Feindt", "given": "U." }, "orcid": "0000-0002-9435-2167" }, { "id": "Hadjiyksta-E", "name": { "family": "Hadjiyksta", "given": "E." } }, { "id": "McKinnon-R", "name": { "family": "McKinnon", "given": "R." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E." }, "orcid": "0000-0002-6786-8774" }, { "id": "Rabinowitz-D-L", "name": { "family": "Rabinowitz", "given": "D." } }, { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E. S." } } ] }, "title": "The rising light curves of Type Ia supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 October 30. Received 2014 October 30. In original form 2014 July 7. First published online December 9, 2014.\n\nWe wish to thank the Reviewer for a careful and considered reading, and thorough and helpful report. MS acknowledges support from the Royal Society and EU/FP7-ERC grant no [615929]. KM is supported by a Marie Curie Intra European Fellowship, within the 7th European Community Framework Programme (FP7). 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. EO is incumbent of the Arye Dissentshik career development\nchair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva, Weizmann-UK and the I-CORE Programme of the Planning and Budgeting Committee and The Israel Science Foundation. Observations obtained with the Samuel Oschin Telescope at the Palomar Observatory 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\nScientific Computing Center, the University of Oxford, and\nthe Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership\namong 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.\nThis research was made possible through the use of the AAVSO\nPhotometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund.\n\nPublished - MNRAS-2015-Firth-3895-910.pdf
Submitted - 1411.1064v1.pdf
Supplemental Material - supplemental_data.txt
", "abstract": "We present an analysis of the early, rising light curves of 18 Type Ia supernovae (SNe Ia) discovered by the Palomar Transient Factory and the La Silla-QUEST variability survey. We fit these early data flux using a simple power law (f(t) = \u03b1 \u00d7 t^n) to determine the time of first light (t_0), and hence the rise time (t_(rise)) from first light to peak luminosity, and the exponent of the power-law rise (n). We find a mean uncorrected rise time of 18.98 \u00b1 0.54 d, with individual supernova (SN) rise times ranging from 15.98 to 24.7 d. The exponent n shows significant departures from the simple 'fireball model' of n = 2 (or f(t)\u2009\u221d\u2009t^2) usually assumed in the literature. With a mean value of n = 2.44 \u00b1 0.13, our data also show significant diversity from event to event. This deviation has implications for the distribution of ^(56)Ni throughout the SN ejecta, with a higher index suggesting a lesser degree of ^(56)Ni mixing. The range of n found also confirms that the ^(56)Ni distribution is not standard throughout the population of SNe Ia, in agreement with earlier work measuring such abundances through spectral modelling. We also show that the duration of the very early light curve, before the luminosity has reached half of its maximal value, does not correlate with the light-curve shape or stretch used to standardize SNe Ia in cosmological applications. This has implications for the cosmological fitting of SN Ia light curves.", "date": "2015-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "446", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3895-3910", "id_number": "CaltechAUTHORS:20150407-085321395", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150407-085321395", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "615929" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK" }, { "agency": "Planning and Budgeting Committee I-CORE Program" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Robert Martin Ayers Sciences Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stu2314", "primary_object": { "basename": "1411.1064v1.pdf", "url": "https://authors.library.caltech.edu/records/5wb9b-76935/files/1411.1064v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Firth-3895-910.pdf", "url": "https://authors.library.caltech.edu/records/5wb9b-76935/files/MNRAS-2015-Firth-3895-910.pdf" }, { "basename": "supplemental_data.txt", "url": "https://authors.library.caltech.edu/records/5wb9b-76935/files/supplemental_data.txt" } ], "pub_year": "2015", "author_list": "Firth, R. E.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/syc3j-n2102", "eprint_id": 62594, "eprint_status": "archive", "datestamp": "2023-08-20 04:38:02", "lastmod": "2023-10-25 17:16:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Kromer-M", "name": { "family": "Kromer", "given": "M." } }, { "id": "Siverd-R", "name": { "family": "Siverd", "given": "R." } }, { "id": "Stassun-K-G", "name": { "family": "Stassun", "given": "K. G." }, "orcid": "0000-0002-3481-9052" }, { "id": "Pepper-J", "name": { "family": "Pepper", "given": "J." }, "orcid": "0000-0002-3827-8417" }, { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" } ] }, "title": "Constraints on the origin of the first light from SN 2014J", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual (SN 2014J)", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2014 October 8; accepted 2014 November 14; published 2015 January 20.\n\nA.G. and R.A. acknowledge support from the Swedish Research Council and the Swedish Space Board.\n\nPublished - Goobar_2015_ApJ_799_106.pdf
Submitted - 1410.1363v2.pdf
", "abstract": "We study the very early light curve of supernova 2014J (SN 2014J) using the high-cadence broad-band imaging data obtained by the Kilodegree Extremely Little Telescope, which fortuitously observed M 82 around the time of the explosion, starting more than 2 months prior to detection, with up to 20 observations per night. These observations are complemented by observations in two narrow-band filters used in an H\u03b1 survey of nearby galaxies by the intermediate Palomar Transient Factory that also captured the first days of the brightening of the supernova. The evolution of the light curves is consistent with the expected signal from the cooling of shock heated material of large scale dimensions, \u22731 R\u2609. This could be due to heated material of the progenitor, a companion star or pre-existing circumstellar environment, e.g., in the form of an accretion disk. Structure seen in the light curves during the first days after explosion could also originate from radioactive material in the outer parts of an exploding white dwarf, as suggested from the early detection of gamma-rays. The model degeneracy translates into a systematic uncertainty of \u00b10.3 days on the estimate of the first light from SN 2014J.", "date": "2015-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "799", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 106", "id_number": "CaltechAUTHORS:20151204-071648290", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151204-071648290", "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)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-637X/799/1/106", "primary_object": { "basename": "1410.1363v2.pdf", "url": "https://authors.library.caltech.edu/records/syc3j-n2102/files/1410.1363v2.pdf" }, "related_objects": [ { "basename": "Goobar_2015_ApJ_799_106.pdf", "url": "https://authors.library.caltech.edu/records/syc3j-n2102/files/Goobar_2015_ApJ_799_106.pdf" } ], "pub_year": "2015", "author_list": "Goobar, A.; Kromer, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/p26qc-rv042", "eprint_id": 55245, "eprint_status": "archive", "datestamp": "2023-08-22 14:45:30", "lastmod": "2023-10-20 22:00:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "White-C-J", "name": { "family": "White", "given": "Christopher J." } }, { "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": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "Ariel" }, "orcid": "0000-0002-4163-4996" }, { "id": "Piro-A-L", "name": { "family": "Piro", "given": "Anthony L." }, "orcid": "0000-0001-6806-0673" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "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": "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": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "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": "Hook-I-M", "name": { "family": "Hook", "given": "Isobel M." }, "orcid": "0000-0002-2960-978X" }, { "id": "J\u00f6nsson-Jakob", "name": { "family": "J\u00f6nsson", "given": "Jakob" } } ] }, "title": "Slow-speed Supernovae from the Palomar Transient Factory: Two Channels", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (iPTF 13an, PTF 09ego, PTF 09eiy, PTF 09eoi, PTF 10xk, PTF 10bvr, PTF 10ujn, PTF 10acdh, PTF 11hyh, SN 2002cx, SN 2002es); surveys; techniques: spectroscopic", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 5 May 201; accepted for publication 6 November 2014; published 15 January 2015.\n\nWe are grateful toM.H. vanKerkwijk and J. M. Silverman for\nvaluable discussions. We thank the referee for useful comments that improved this manuscript, as well as R. J. Foley for a close reading and detailed feedback. We also thank I. Arcavi, C. Badenes, V. Bhalerao, K. Clubb, A. Cucchiara, A. De Cia, O. Fox, A. Horesh, D. Levitan, K. Mooley, D. Perley, S. Tang, S. Tendulkar, P. Vreeswijk, and D. Xu for their contributions to PTF, especially with observations and data reduction. C. J. W. began this research as part of the summer student exchange program between Princeton and Carnegie. M. M. K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A. G.-Y. acknowledges support by the EU/FP7 via ERC grant 307260; ISF, Minerva, and Weizmann-UK grants; as well as the \"Quantum Universe\" I-Core Program of the Planning and Budgeting Committee and the Israel Science Foundation and the Kimmel Award. A. L. P. is supported through NSF grants AST-1205732, PHY-1068881, and PHY-1151197, as well as the Sherman Fairchild Foundation. E. O. O. is incumbent on the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute, Ilan Gluzman\n(Secaucus, NJ), the Israeli Ministry of Science, the Israel\nScience Foundation, Minerva, Weizmann-UK, and the I-CORE\nProgram of the Planning and Budgeting Committee and the\nIsrael Science Foundation. This research made use of the Sloan Digital Sky Survey (SDSS), the NASA/IPAC Extragalactic Database (NED),WISeREP, SIMBAD, and VizieR. The PTF spectra for the slowspeed sample will be made available on WISeREP.\nFacilities. PO:1.2 m, PO:1.5 m, Keck:I (LRIS), Hale (DBSP),\nING:Herschel (ISIS), Keck:II (DEIMOS), Magellan:Baade\n(IMACS)\n\nPublished - 0004-637X_799_1_52.pdf
Submitted - 1405.7409v1.pdf
", "abstract": "Since the discovery of the unusual prototype SN 2002cx, the eponymous class of Type I (hydrogen-poor) supernovae with low ejecta speeds has grown to include approximately two dozen members identified from several heterogeneous surveys, in some cases ambiguously. Here we present the results of a systematic study of 1077 Type\u2009I supernovae discovered by the Palomar Transient Factory, leading to nine new members of this peculiar class. Moreover, we find there are two distinct subclasses based on their spectroscopic, photometric, and host galaxy properties: \"SN 2002cx-like\" supernovae tend to be in later-type or more irregular hosts, have more varied and generally dimmer luminosities, have longer rise times, and lack a Ti\u2009ii trough when compared to \"SN 2002es-like\" supernovae. None of our objects show helium, and we counter a previous claim of two such events. We also find that the occurrence rate of these transients relative to Type Ia supernovae is 5.6^(+22)_(-3.8)% (90% confidence), lower compared to earlier estimates. Combining our objects with the literature sample, we propose that these subclasses have two distinct physical origins.", "date": "2015-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "799", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 52", "id_number": "CaltechAUTHORS:20150226-094929739", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150226-094929739", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Kimmel Award" }, { "agency": "NSF", "grant_number": "AST-1205732" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1151197" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Willner Family Leadership Institute" }, { "agency": "Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/799/1/52", "primary_object": { "basename": "0004-637X_799_1_52.pdf", "url": "https://authors.library.caltech.edu/records/p26qc-rv042/files/0004-637X_799_1_52.pdf" }, "related_objects": [ { "basename": "1405.7409v1.pdf", "url": "https://authors.library.caltech.edu/records/p26qc-rv042/files/1405.7409v1.pdf" } ], "pub_year": "2015", "author_list": "White, Christopher J.; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/ya72q-1ga06", "eprint_id": 55638, "eprint_status": "archive", "datestamp": "2023-08-22 14:38:02", "lastmod": "2023-10-20 22:54:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "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": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Long-term photometric behaviour of outbursting AM CVn systems", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion discs; surveys; binaries: close; novae, cataclysmic variables \u2013white dwarfs", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 October 8. Received 2014 October 7; in original form 2014 July 15.\n\nFirst published online November 11, 2014.\n\nWe thank Lars Bildsten for helpful suggestions related to the recurrence time-orbital period relations. PG and TP thank the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the preparation of this manuscript. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva, Weizmann-UK and the I-CORE Programme of the Planning and Budgeting Committee and The Israel Science Foundation. Observations obtained with the Samuel Oschin Telescope at the Palomar Observatory 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 theWeizmann Institute of Science. The CSS survey is funded by the National Aeronautics and Space Administration under Grant no. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Programme. The CRTS survey is supported by the US National Science Foundation under grants AST-0909182. The LINEAR programme is sponsored by the National Aeronautics and Space Administration (NRA no. NNH09ZDA001N, 09-NEOO09-0010) and the USA Air Force under Air Force Contract FA8721-05-C-0002. This research has made use of NASA's Astrophysics Data System.\n\nPublished - MNRAS-2015-Levitan-391-410.pdf
", "abstract": "The AM CVn systems are a class of He-rich, post-period minimum, semidetached, ultracompact binaries. Their long-term light curves have been poorly understood due to the few systems known and the long (hundreds of days) recurrence times between outbursts. We present combined photometric light curves from the Lincoln Near Earth Asteroid Research, Catalina Real-Time Transient Survey, and Palomar Transient Factory synoptic surveys to study the photometric variability of these systems over an almost 10\u2009yr period. These light curves provide a much clearer picture of the outburst phenomena that these systems undergo. We characterize the photometric behaviour of most known outbursting AM CVn systems and establish a relation between their outburst properties and the systems' orbital periods. We also explore why some systems have only shown a single outburst so far and expand the previously accepted phenomenological states of AM CVn systems. We conclude that the outbursts of these systems show evolution with respect to the orbital period, which can likely be attributed to the decreasing mass transfer rate with increasing period. Finally, we consider the number of AM CVn systems that should be present in modelled synoptic surveys.", "date": "2015-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "446", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "391-410", "id_number": "CaltechAUTHORS:20150309-110150907", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150309-110150907", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "1066293" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "I-CORE Programme of the Planning and Budgeting Committee" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "NASA", "grant_number": "NNH09ZDA001N" }, { "agency": "NASA", "grant_number": "09-NEOO09-0010" }, { "agency": "Air Force", "grant_number": "FA8721-05-C-0002" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stu2105", "primary_object": { "basename": "MNRAS-2015-Levitan-391-410.pdf", "url": "https://authors.library.caltech.edu/records/ya72q-1ga06/files/MNRAS-2015-Levitan-391-410.pdf" }, "pub_year": "2015", "author_list": "Levitan, David; Groot, Paul J.; et el." }, { "id": "https://authors.library.caltech.edu/records/1kdcm-1qh69", "eprint_id": 62595, "eprint_status": "archive", "datestamp": "2023-08-22 14:27:57", "lastmod": "2023-10-25 17:16:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vreeswuk-P-M", "name": { "family": "Vreeswuk", "given": "Paul M." } }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "The hydrogen-poor superluminous supernova iPTF 13ajg and its host galaxy in absorption and emission", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: atoms; supernovae: general; supernovae: individual (iPTF 13ajg)", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 August 15; accepted 2014 September 23; published 2014 November 21. \n\nThis paper is based on observations collected at the Palomar 48 and 60 inch telescopes, the Nordic Optical Telescope (NOT), the Discovery Channel Telescope (DCT), the Very Large Telescope (VLT) under proposal No. 291.D-5009, and the Keck-I and Keck-II telescopes. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA); it was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful to Ori D. Fox, Isaac Shivvers, Patrick L. Kelly, WeiKang Zheng, Sumin Tang, W. Kao, and Joel Johansson for performing part of the Keck observations presented in this paper, and to ESO's User Support Department and Paranal observing staff for arranging and securing the VLT DDT observations. These results made use of Lowell Observatory's Discovery Channel Telescope; Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. The LMI at the DCT was built by Lowell Observatory using funds from the NSF grant AST\u20131005313. We wish to thank Sylvain Veilleux, Antonino Cucchiara, Suvi Gezari, and Eleonora Troja for assistance in obtaining the DCT data. It is a pleasure to thank Daniele Malesani for providing his handy finder-chart routine, and Melina Bersten for interesting discussions. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, GIF, Minerva, and ISF grants, WIS-UK \"making connections,\" and Kimmel and ARCHES awards. A.V.F.'s supernova group at UC Berkeley is supported through NSF grant AST\u20131211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. M.S. acknowledges support from the Royal Society. Support for D.A.P.was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute,which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The Dark Cosmology Centre is funded by the DNRF. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project.\n\nPublished - Vreeswuk,PM_et_al.pdf
Submitted - 1409.8287v1.pdf
", "abstract": "We present imaging and spectroscopy of a hydrogen-poor superluminous supernova (SLSN) discovered by the intermediate Palomar Transient Factory, iPTF 13ajg. At a redshift of z = 0.7403, derived from narrow absorption lines, iPTF 13ajg peaked at an absolute magnitude of M_(u,AB) = \u201322.5, one of the most luminous supernovae to date. The observed bolometric peak luminosity of iPTF 13ajg is 3.2 \u00d7 10^(44) erg s^(\u20131), while the estimated total radiated energy is 1.3 \u00d7 10^(51) erg. We detect narrow absorption lines of Mg I, Mg II, and Fe II, associated with the cold interstellar medium in the host galaxy, at two different epochs with X-shooter at the Very Large Telescope. From Voigt profile fitting, we derive the column densities log N(Mg I) =11.94 \u00b1 0.06, log N(Mg II) =14.7 \u00b1 0.3, and log N(Fe II) =14.25 \u00b1 0.10. These column densities, as well as the Mg I and Mg II equivalent widths of a sample of hydrogen-poor SLSNe taken from the literature, are at the low end of those derived for gamma-ray bursts (GRBs) whose progenitors are also thought to be massive stars. This suggests that the environments of hydrogen-poor SLSNe and GRBs are different. From the nondetection of Fe II fine-structure absorption lines, we derive a lower limit on the distance between the supernova and the narrow-line absorbing gas of 50 pc. The neutral gas responsible for the absorption in iPTF 13ajg exhibits a single narrow component with a low velocity width, \u0394V = 76 km s^(\u20131), indicating a low-mass host galaxy. No host galaxy emission lines are detected, leading to an upper limit on the unobscured star formation rate (SFR) of SFR_([OII]) < 0.07 M_\u2609 yr^(-1). Late-time imaging shows the iPTF 13ajg host galaxy to be faint, with g_(AB) \u2248 27.0 and R_(AB) \u2265 26.0 mag, corresponding to M_(B,Vega) \u2273 \u201317.7 mag.", "date": "2014-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "797", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 24", "id_number": "CaltechAUTHORS:20151204-072412759", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151204-072412759", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Discovery Communications" }, { "agency": "NSF", "grant_number": "AST\u20131005313" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee for planning and funding Quantum Universe I-Core program" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK" }, { "agency": "Kimmel Award" }, { "agency": "NSF", "grant_number": "AST\u20131211916" }, { "agency": "TABASGO Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Royal Society" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51296.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Danish National Research Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "ARCHES Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/797/1/24", "primary_object": { "basename": "1409.8287v1.pdf", "url": "https://authors.library.caltech.edu/records/1kdcm-1qh69/files/1409.8287v1.pdf" }, "related_objects": [ { "basename": "Vreeswuk,PM_et_al.pdf", "url": "https://authors.library.caltech.edu/records/1kdcm-1qh69/files/Vreeswuk,PM_et_al.pdf" } ], "pub_year": "2014", "author_list": "Vreeswuk, Paul M.; Perley, Daniel A.; et el." }, { "id": "https://authors.library.caltech.edu/records/3vrzj-h9b57", "eprint_id": 62587, "eprint_status": "archive", "datestamp": "2023-08-20 03:40:11", "lastmod": "2023-10-25 17:15:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Pan-Y-C", "name": { "family": "Pan", "given": "Y.-C." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P." }, "orcid": "0000-0001-6876-8284" }, { "id": "Chotard-N", "name": { "family": "Chotard", "given": "N." } }, { "id": "Clubb-K-I", "name": { "family": "Clubb", "given": "K. I." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kandrashoff-M-T", "name": { "family": "Kandrashoff", "given": "M. T." } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Saunders-C-M", "name": { "family": "Saunders", "given": "C. M." } }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E." } }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } } ] }, "title": "Exploring the spectral diversity of low-redshift Type Ia supernovae using the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general, galaxies: general, distance scale", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 August 4. Received 2014 August 1; in original form 2014 May 31. Published: 15 September 2014. \n\nKM is supported by a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). MS acknowledges support from the Royal Society. AGY is supported by the EU/FP7-ERC grant no [307260], the Quantum Universe I-Core program by the Israeli Committee for planning and funding, the ISF, GIF, Minerva, and ISF grants, and Kimmel and ARCHES awards. NC acknowledges support from the Lyon Institute of Origins under grant ANR-10-LABX-66. MMK acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. AVF's supernova group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. \n\nThe William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. Based on observations (GN-2010A-Q-20, GN- 2010B-Q-13, GN-2011A-Q-16 and GS-2009B-Q-11) obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina). Observations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, La Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. The authors would like to thank all the observers and data reducers of the collaboration for their hard work throughout the survey (in particular I. Arcavi, S. Ben-Ami, J. Bloom, S. B. Cenko, M. Graham, A. Horesh, E. Hsiao, I. Kleiser, S. Kulkarni, A. Miller, E. Ofek, J. Parrent, D. Perley, R. Quimby, A. Sternberg, N. Suzuki, O. Yaron, D. Xu). This publication has been made possible by the participation of more than 10 000 volunteers in the Galaxy Zoo: Supernova project (http://supernova.galaxyzoo.org/authors). \n\nThe LT 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. This work also makes use of observations from the LCOGT network. 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 (NASA). The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank the dedicated staffs at all the observatories we used for their excellent assistance with the observations. Based on data taken at the European Organization for Astronomical Research in the Southern hemisphere, Chile, under program IDs 084.A-0149(A) and 085.A-0777(A). Observations obtained with the SuperNova Integral Field Spectrograph on the University of Hawaii 2.2-m telescope as part of the Nearby Supernova Factory II project, a scientific collaboration between the Centre de Recherche Astronomique de Lyon, Institut de Physique Nucl\u00e9aire de Lyon, Laboratoire de Physique Nucl\u00e9aire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and Centre de Physique des Particules de Marseille. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.\n\nPublished - stu1607.pdf
Submitted - 1408.1430v1.pdf
Supplemental Material - stu1607_Supplementary_Data.zip
", "abstract": "We present an investigation of the optical spectra of 264 low-redshift (z < 0.2) Type Ia supernovae (SNe Ia) discovered by the Palomar Transient Factory, an untargeted transient survey. We focus on velocity and pseudo-equivalent width measurements of the Si\u2009II 4130, 5972, and 6355\u2009\u00c5 lines, as well those of the Ca\u2009IInear-infrared (NIR) triplet, up to +5\u2009days relative to the SN B-band maximum light. We find that a high-velocity component of the Ca\u2009II NIR triplet is needed to explain the spectrum in \u223c95 per cent of SNe Ia observed before \u22125\u2009days, decreasing to \u223c80 per cent at maximum. The average velocity of the Ca\u2009II high-velocity component is \u223c8500 km\u2009s^(\u22121) higher than the photospheric component. We confirm previous results that SNe Ia around maximum light with a larger contribution from the high-velocity component relative to the photospheric component in their Ca\u2009II NIR feature have, on average, broader light curves and lower Ca\u2009II NIR photospheric velocities. We find that these relations are driven by both a stronger high-velocity component and a weaker contribution from the photospheric Ca\u2009II NIR component in broader light curve SNe Ia. We identify the presence of C\u2009II in very-early-time SN Ia spectra (before \u221210\u2009days), finding that >40 per cent of SNe Ia observed at these phases show signs of unburnt material in their spectra, and that C\u2009II features are more likely to be found in SNe Ia having narrower light curves.", "date": "2014-11-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "444", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3258-3274", "id_number": "CaltechAUTHORS:20151203-143133454", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151203-143133454", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee Quantum Universe I-Core program" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Scientific Research and Development" }, { "agency": "Minerva" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-10-LABX-66" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1302771" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Kimmel Award" }, { "agency": "ARCHES Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stu1607", "primary_object": { "basename": "stu1607_Supplementary_Data.zip", "url": "https://authors.library.caltech.edu/records/3vrzj-h9b57/files/stu1607_Supplementary_Data.zip" }, "related_objects": [ { "basename": "1408.1430v1.pdf", "url": "https://authors.library.caltech.edu/records/3vrzj-h9b57/files/1408.1430v1.pdf" }, { "basename": "stu1607.pdf", "url": "https://authors.library.caltech.edu/records/3vrzj-h9b57/files/stu1607.pdf" } ], "pub_year": "2014", "author_list": "Maguire, K.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/9dt52-2nf98", "eprint_id": 50458, "eprint_status": "archive", "datestamp": "2023-08-22 13:52:47", "lastmod": "2023-10-17 23:49:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Banholzer-S-R", "name": { "family": "Banholzer", "given": "Sophianna R." } }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Martin-N-F", "name": { "family": "Martin", "given": "Nicolas F." }, "orcid": "0000-0002-1349-202X" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "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" }, { "id": "Rix-H-W", "name": { "family": "Rix", "given": "Hans-Walter" }, "orcid": "0000-0003-4996-9069" } ] }, "title": "Stacking the Invisibles: A Guided Search for Low-Luminosity Milky Way Satellites", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; Galaxy: halo; Galaxy: structure; stars: variables: RR Lyrae", "note": "\u00a9 2014 American Astronomical Society. Received 2014 April 24; accepted 2014 August 1; published 2014 September 16.\n\nWe thank \u017deljko Ivezi\u0107, Erik Tollerud, and Colin Slater for\ncomments, suggestions, and useful discussions. B.S. and J.G.C. acknowledge the NSF grant AST-0908139 to J.G.C. for partial support, as do S.R.K. (NSF grant AST-1009987), and C.J.G. (for a NASA grant). B.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC grant agreement No. 321035. S.R.B. thanks the Caltech Summer Undergraduate Research Fellowship (SURF) for support. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva foundation, Weizmann-UK foundation and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. This work has made use of BaSTI web tools. This article is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient\nFactory 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. It is also partially based on observations obtained as part of the Intermediate Palomar Transient Factory project, a scientific\ncollaboration among the California Institute of Technology,\nLos Alamos National Laboratory, the University of Wisconsin,\nMillwakee, the Oskar Klein Center, the Weizmann Institute of\nScience, the TANGO Program of the University System of\nTaiwan, the Kavli Institute for the Physics and Mathematics\nof the Universe, and the Inter-University Centre for Astronomy and Astrophysics. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.\nSDSS-III is managed by the Astrophysical Research Consortium\nfor the Participating Institutions of the SDSS-III\nCollaboration including the University of Arizona, the Brazilian Participation Group, Brook haven 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,\nUniversity of Portsmouth, Princeton University, the\nSpanish Participation Group, University of Tokyo, University\nof Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.\n\nPublished - 0004-637X_793_2_135.pdf
Submitted - 1407.1835v2.pdf
", "abstract": "Almost every known low-luminosity Milky Way dwarf spheroidal (dSph) satellite galaxy contains at least one RR Lyrae star. Assuming that a fraction of distant (60 < d _(helio) < 100 kpc) Galactic halo RR Lyrae stars are members of yet to be discovered low-luminosity dSph galaxies, we perform a guided search for these low-luminosity dSph galaxies. In order to detect the presence of dSph galaxies, we combine stars selected from more than 123 sightlines centered on RR Lyrae stars identified by the Palomar Transient Factory. We find that this method is sensitive enough to detect the presence of Segue 1-like galaxies (M_V= -1.5^(+0.6)_(-0.8), r_h = 30 pc) even if only ~20 sightlines were occupied by such dSph galaxies. Yet, when our method is applied to the Sloan Digital Sky Survey Data Release 10 imaging catalog, no signal is detected. An application of our method to sightlines occupied by pairs of close (<200 pc) horizontal branch stars, also did not yield a detection. Thus, we place upper limits on the number of low-luminosity dSph galaxies with half-light radii from 30 pc to 120 pc, and in the probed volume of the halo. Stronger constraints on the luminosity function may be obtained by applying our method to sightlines centered on RR Lyrae stars selected from the Pan-STARRS1 survey, and eventually, from the Large Synoptic Survey Telescope. In Appendix A, we present spectroscopic observations of an RRab star in the Bo\u00f6tes 3 dSph and a light curve of an RRab star near the Bo\u00f6tes 2 dSph.", "date": "2014-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "793", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 135", "id_number": "CaltechAUTHORS:20141016-152037601", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141016-152037601", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908139" }, { "agency": "NSF", "grant_number": "AST-1009987" }, { "agency": "NASA" }, { "agency": "European Research Council (ERC)", "grant_number": "321035" }, { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" }, { "agency": "Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ)" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva Foundation" }, { "agency": "Weismann-UK foundation" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/793/2/135", "primary_object": { "basename": "0004-637X_793_2_135.pdf", "url": "https://authors.library.caltech.edu/records/9dt52-2nf98/files/0004-637X_793_2_135.pdf" }, "related_objects": [ { "basename": "1407.1835v2.pdf", "url": "https://authors.library.caltech.edu/records/9dt52-2nf98/files/1407.1835v2.pdf" } ], "pub_year": "2014", "author_list": "Sesar, Branimir; Banholzer, Sophianna R.; et el." }, { "id": "https://authors.library.caltech.edu/records/w5ggt-chk46", "eprint_id": 50187, "eprint_status": "archive", "datestamp": "2023-08-22 13:42:26", "lastmod": "2023-10-17 22:50:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339" }, { "id": "Yang-Chen-Wei", "name": { "family": "Yang", "given": "Chen-Wei" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Tendulkar-S-P", "name": { "family": "Tendulkar", "given": "Shriharsh P." }, "orcid": "0000-0003-2548-2926" }, { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "A Continuum of H- to He-Rich Tidal Disruption Candidates With a Preference for E+A Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; galaxies: nuclei; quasars: supermassive black holes", "note": "\u00a9 2014 American Astronomical Society. Received 2014 June 9; accepted 2014 July 25; published 2014 September 3.\n\nWe thank R. Antonucci, L. Bildsten, and C. S. Kochanek for\nhelpful discussions. We appreciate the assistance of V. Bhalerao, A. Cucchiara, D. Levitan, A. Mishra, J. M. Silverman, R. Walters, and O. Yaron in obtaining and reducing observations, and are grateful to the staff at the various observatories where data were obtained. We thank the Swift PI N. Gehrels and the entire Swift team for authorizing, scheduling, and carrying out our requested observations. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project. Additional data 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. This research used resources\nof the National Energy Research Scientific Computing Center,\nwhich is supported by the Office of Science of the U.S. Department of Energy under Contract No.DE-AC02-05CH11231. 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. This research 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\nand Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation\noperated under cooperative agreement by Associated Universities, Inc. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. A.G. and I.A. acknowledge support by the Israeli Science Foundation and an EU/FP7/ERC grant. A.G. further acknowledges grants from the BSF, GIF, and Minerva, as well as the \"Quantum Universe\" I-Core program of the planning and budgeting\ncommittee and the ISF, and a Kimmel Investigator award.\nE.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by a grant from the Israeli Ministry of Science and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant No. 1829/12). M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. J.S.B. and his group were partially supported by NASA/Swift Guest Investigator grants NNX09AQ66G and NNX10AF93G, and NSF/AST-100991. A.A.M. acknowledges support for this work by NASA from a Hubble Fellowship grant ST-HF-51325.01.\n\nPublished - 0004-637X_793_1_38.pdf
Submitted - 1405.1415v2.pdf
", "abstract": "We present the results of a Palomar Transient Factory (PTF) archival search for blue transients that lie in the magnitude range between \"normal\" core-collapse and superluminous supernovae (i.e., with \u201321 \u2264 M_(R (peak)) \u2264 \u2013 19). Of the six events found after excluding all interacting Type IIn and Ia-CSM supernovae, three (PTF09ge, 09axc, and 09djl) are coincident with the centers of their hosts, one (10iam) is offset from the center, and a precise offset cannot be determined for two (10nuj and 11glr). All the central events have similar rise times to the He-rich tidal disruption candidate PS1-10jh, and the event with the best-sampled light curve also has similar colors and power-law decay. Spectroscopically, PTF09ge is He-rich, while PTF09axc and 09djl display broad hydrogen features around peak magnitude. All three central events are in low star formation hosts, two of which are E+A galaxies. Our spectrum of the host of PS1-10jh displays similar properties. PTF10iam, the one offset event, is different photometrically and spectroscopically from the central events, and its host displays a higher star formation rate. Finding no obvious evidence for ongoing galactic nuclei activity or recent star formation, we conclude that the three central transients likely arise from the tidal disruption of a star by a supermassive black hole. We compare the spectra of these events to tidal disruption candidates from the literature and find that all of these objects can be unified on a continuous scale of spectral properties. The accumulated evidence of this expanded sample strongly supports a tidal disruption origin for this class of nuclear transients.", "date": "2014-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "793", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 38", "id_number": "CaltechAUTHORS:20141003-093421671", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141003-093421671", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Israeli Science Foundation" }, { "agency": "European Research Council (ERC)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "MINERVA (Israel)" }, { "agency": "Quantum Universe I-Core Program" }, { "agency": "Kimmel Investigator award" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NASA", "grant_number": "NNX09AQ66G" }, { "agency": "NASA", "grant_number": "NNX10AF93G" }, { "agency": "NSF", "grant_number": "AST-100991" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51325.01" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/793/1/38", "primary_object": { "basename": "0004-637X_793_1_38.pdf", "url": "https://authors.library.caltech.edu/records/w5ggt-chk46/files/0004-637X_793_1_38.pdf" }, "related_objects": [ { "basename": "1405.1415v2.pdf", "url": "https://authors.library.caltech.edu/records/w5ggt-chk46/files/1405.1415v2.pdf" } ], "pub_year": "2014", "author_list": "Arcavi, Iair; Yan, Lin; et el." }, { "id": "https://authors.library.caltech.edu/records/keqa5-x3304", "eprint_id": 49257, "eprint_status": "archive", "datestamp": "2023-08-20 02:50:10", "lastmod": "2023-10-17 21:15:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gorbikov-E", "name": { "family": "Gorbikov", "given": "Evgeny" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "Paul M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Chotard-N", "name": { "family": "Chotard", "given": "Nicolas" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "Annalisa" }, "orcid": "0000-0003-2082-1626" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Tal-David", "name": { "family": "Tal", "given": "David" } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Chen-Juncheng", "name": { "family": "Chen", "given": "Juncheng" } } ] }, "title": "iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general\n supernovae: individual: iPTF13beo\n stars: winds, outflows\n stars: Wolf\u2013Rayet", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 June 9. Received 2014 June 8; in original form 2013 November 28. First published online July 15, 2014. \n\nThis paper is based on observations obtained with the Samuel\nOschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a\nscientific 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. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. EOO is incumbent of the Arye Dissentshik\ncareer development chair and is grateful to support by a\ngrant from the Israeli Ministry of Science and the I-CORE Programme of the Planning and Budgeting Committee and The Israel Science Foundation (grant no. 1829/12). AG-Y acknowledges support by the EU/FP7 via ERC grant no.\n307260, ISF, BSF, Minerva and GIF grants, the 'Quantum Universe' I-Core programme funded by the ISF and the Israeli Planning and Budgeting Committee, and the Kimmel award. Observations obtained with the SuperNova Integral Field Spectrograph on the University of Hawaii 2.2-m telescope as part of the Nearby Supernova Factory II project, a scientific collaboration between the Centre de Recherche Astronomique de Lyon, Institut de Physique Nucl\u00e9aire de Lyon, Laboratoire de Physique Nucl\u00e9aire\net des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and Centre de Physique des Particules de Marseille. NC acknowledges support from the Lyon Institute of Origins under grant ANR-10-LABX-66.\nWe would like to express our gratitude to the anonymous referee for the valuable comments, that helped to improve this paper.\n\nPublished - MNRAS-2014-Gorbikov-671-7.pdf
Submitted - 1312.0012v3.pdf
", "abstract": "We present optical photometric and spectroscopic observations of the Type Ibn (SN 2006jc-like) supernova (SN) iPTF13beo. Detected by the intermediate Palomar Transient Factory \u223c3 h after the estimated first light, iPTF13beo is the youngest and the most distant (\u223c430 Mpc) Type Ibn event ever observed. The iPTF13beo light curve is consistent with light curves of other Type Ibn SNe and with light curves of fast Type Ic events, but with a slightly faster rise-time of two days. In addition, the iPTF13beo R-band light curve exhibits a double-peak structure separated by \u223c9 d, not observed before in any Type Ibn SN. A low-resolution spectrum taken during the iPTF13beo rising stage is featureless, while a late-time spectrum obtained during the declining stage exhibits narrow and intermediate-width He i and Si ii features with full width at half-maximum \u22482000\u20135000 km s^(\u22121) and is remarkably similar to the prototypical SN Ibn 2006jc spectrum. We suggest that our observations support a model of a massive star exploding in a dense He-rich circumstellar medium (CSM). A shock breakout in a CSM model requires an eruption releasing a total mass of \u223c0.1 M_\u2299 over a time-scale of couple of weeks prior to the SN explosion.", "date": "2014-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "443", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "671-677", "id_number": "CaltechAUTHORS:20140904-153832373", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140904-153832373", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Minerva" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Israeli Planning and Budgeting Committee" }, { "agency": "Kimmel Award" }, { "agency": "Lyon Institute of Origins", "grant_number": "ANR-10-LABX-66" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stu1184", "primary_object": { "basename": "1312.0012v3.pdf", "url": "https://authors.library.caltech.edu/records/keqa5-x3304/files/1312.0012v3.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Gorbikov-671-7.pdf", "url": "https://authors.library.caltech.edu/records/keqa5-x3304/files/MNRAS-2014-Gorbikov-671-7.pdf" } ], "pub_year": "2014", "author_list": "Gorbikov, Evgeny; Gal-Yam, Avishay; et el." }, { "id": "https://authors.library.caltech.edu/records/17b64-84f21", "eprint_id": 50175, "eprint_status": "archive", "datestamp": "2023-08-22 13:26:40", "lastmod": "2023-10-17 22:49:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "A New Large Super-fast Rotator: (335433) 2005 UW163", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets; asteroids: individual (335433); surveys", "note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 July 9; accepted 2014 July 25; published 2014 August 6. \n\nThis work is supported in part by the National Science Council of Taiwan under the grants NSC 101-2119-M-008-007-MY3. We are greateful for the indispensable support provided by the staff of the Palomar Observatory. We also thank the referee, Alan Harris, for useful comments that helped to improve the content of the paper.\n\nPublished - 2041-8205_791_2_L35.pdf
Submitted - 1407.8264v1.pdf
", "abstract": "Asteroids of size larger than 150 m generally do not have rotation periods smaller than 2.2 hr. This spin cutoff is believed to be due to the gravitationally bound rubble-pile structures of the asteroids. Rotation with periods exceeding this critical value will cause asteroid breakup. Up until now, only one object, 2001 OE84, has been found to be an exception to this spin cutoff. We report the discovery of a new super-fast rotator, (335433) 2005 UW163, spinning with a period of 1.290 hr and a light curve variation of r' ~ 0.8 mag from the observations made at the P48 telescope and the P200 telescope of the Palomar Observatory. Its H_r' = 17.69 \u00b1 0.27 mag and multi-band colors (i.e., g' \u2013 r' = 0.68 \u00b1 0.03 mag, r' \u2013 i' = 0.19 \u00b1 0.02 mag and SDSS i \u2013 z = \u20130.45 mag) show it is a V-type asteroid with a diameter of 0.6 + 0.3/\u20130.2 km. This indicates (335433) 2005 UW163 is a super-fast rotator beyond the regime of the small monolithic asteroid.", "date": "2014-08-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "791", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L35", "id_number": "CaltechAUTHORS:20141002-133621218", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141002-133621218", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Council (Taipei)", "grant_number": "NSC 101-2119-M-008-007-MY3" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/791/2/L35", "primary_object": { "basename": "2041-8205_791_2_L35.pdf", "url": "https://authors.library.caltech.edu/records/17b64-84f21/files/2041-8205_791_2_L35.pdf" }, "related_objects": [ { "basename": "1407.8264v1.pdf", "url": "https://authors.library.caltech.edu/records/17b64-84f21/files/1407.8264v1.pdf" } ], "pub_year": "2014", "author_list": "Chang, Chan-Kao; Waszczak, Adam; et el." }, { "id": "https://authors.library.caltech.edu/records/m35fe-xj080", "eprint_id": 49013, "eprint_status": "archive", "datestamp": "2023-08-22 13:23:53", "lastmod": "2023-10-17 20:36:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E. S." } }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Pian-E", "name": { "family": "Pian", "given": "E." } }, { "id": "Hurley-K-C", "name": { "family": "Hurley", "given": "K." } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "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": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E." }, "orcid": "0000-0002-6786-8774" }, { "id": "Barthelmy-S-D", "name": { "family": "Barthelmy", "given": "S." } }, { "id": "Boynton-W-V", "name": { "family": "Boynton", "given": "W." } }, { "id": "Goldsten-J-O", "name": { "family": "Goldsten", "given": "J." } }, { "id": "Golenetskii-S-V", "name": { "family": "Golenetskii", "given": "S." } }, { "id": "Ohno-M", "name": { "family": "Ohno", "given": "M." } }, { "id": "Tashiro-M-S", "name": { "family": "Tashiro", "given": "M. S." } }, { "id": "Yamaoka-Kazutaka", "name": { "family": "Yamaoka", "given": "K." } }, { "id": "Zhang-X-L", "name": { "family": "Zhang", "given": "X. L." } } ] }, "title": "Optical follow-up observations of PTF10qts, a luminous broad-lined Type Ic supernova found by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual: PTF10qts", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 May 19. Received 2014 May 19; in original form 2014 March 10.\n\nFirst published online June 27, 2014.\n\nWe acknowledge financial contributions from contract ASI\nI/016/07/0 (COFIS), ASI I/088/06/0, and PRIN INAF 2009 and\n2011. PTF is a collaboration of Caltech, LCOGT, the Weizmann\nInstitute, LBNL, Oxford, Columbia, IPAC, and UC Berkeley. Collaborative work between AG and PAM is supported by a Minerva grant. The Weizmann PTF membership is supported by the ISF via grants to AG. Joint work of AG and SRK is supported by a BSF grant. AG also acknowledges support by grants from the GIF, EU/FP7 via ERC grant 307260, 'The Quantum Universe', I-CORE programme by the Israeli Committee for planning and budgeting, the Kimmel award, and the Lord Sieff of Brimpton Fund. AVF's group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS is supported by an NSF\nAstronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE programme of the Planning and Budgeting Committee and the Israel Science Foundation (grant No 1829/12). We thank the very helpful staffs of the various observatories\n(Palomar, Lick, KNPO, TNG, Keck) at which data were obtained. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of theW. M. Keck Foundation. M. T. Kandrashoff and J. Rex assisted with the Lick observations. We are grateful to the following contributors to the IPN for support and sharing\ntheir data: I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, C. Fellows, K. Harshman, and R. Starr (for the Odyssey team), R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and D. Svinkin (for the Konus-Wind team), A. von Kienlin and A. Rau (for the INTEGRAL team), T. Takahashi, M. Ohno, Y. Hanabata, Y. Fukazawa, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima (for the Suzaku team), T. Cline, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer (for the Swift team), and V. Connaughton, M. S. Briggs, and C. Meegan (for the Fermi GBM team). KH acknowledges NASA support for the IPN under the following grants: NNX10AI23G (Swift), NNX09AV61G (Suzaku), NNX09AU03G (Fermi), and NNX09AR28G (INTEGRAL).\n\nPublished - MNRAS-2014-Walker-2768-79.pdf
Submitted - 1405.5237v1.pdf
", "abstract": "We present optical photometry and spectroscopy of the broad-lined Type Ic supernova (SN Ic-BL) PTF10qts, which was discovered as part of the Palomar Transient Factory. The SN was located in a dwarf galaxy of magnitude r = 21.1 at a redshift z = 0.0907. We find that the R-band light curve is a poor proxy for bolometric data and use photometric and spectroscopic data to construct and constrain the bolometric light curve. The derived bolometric magnitude at maximum light is M_bol = \u221218.51 \u00b1 0.2 mag, comparable to that of SN 1998bw (M_bol = \u221218.7 mag) which was associated with a gamma-ray burst (GRB). PTF10qts is one of the most luminous SNe Ic-BL observed without an accompanying GRB. We estimate the physical parameters of the explosion using data from our programme of follow-up observations, finding that it produced a larger mass of radioactive nickel compared to other SNe Ic-BL with similar inferred ejecta masses and kinetic energies. The progenitor of the event was likely an \u223c20 M_\u2299 star.", "date": "2014-08-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "442", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2768-2779", "id_number": "CaltechAUTHORS:20140828-084958848", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140828-084958848", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/016/07/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/088/06/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "MINERVA (Israel)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Kimmel award" }, { "agency": "Lord Sieff of Brimpton Fund" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1302771" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "NASA", "grant_number": "NNX10AI23G" }, { "agency": "NASA", "grant_number": "NNX09AV61G" }, { "agency": "NASA", "grant_number": "NNX09AU03G" }, { "agency": "NASA", "grant_number": "NNX09AR28G" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stu1017", "primary_object": { "basename": "1405.5237v1.pdf", "url": "https://authors.library.caltech.edu/records/m35fe-xj080/files/1405.5237v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Walker-2768-79.pdf", "url": "https://authors.library.caltech.edu/records/m35fe-xj080/files/MNRAS-2014-Walker-2768-79.pdf" } ], "pub_year": "2014", "author_list": "Walker, E. S.; Mazzali, P. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/sgxzc-5ph25", "eprint_id": 48181, "eprint_status": "archive", "datestamp": "2023-08-22 13:10:44", "lastmod": "2023-10-17 16:42:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Shaviv-N-J", "name": { "family": "Shaviv", "given": "Nir J." } }, { "id": "Steinbok-A", "name": { "family": "Steinbok", "given": "Aviram" } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Tal-David", "name": { "family": "Tal", "given": "David" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" } ] }, "title": "Precursors Prior to Type IIn Supernova Explosions are Common: Precursor Rates, Properties, and Correlations", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (SN 2010mc, PTF 10bjb, SN 2011ht, PTF 10weh, PTF 12cxj, SN 2009ip)", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 January 21; accepted 2014 May 22; published 2014 June 19. \n\nE.O.O. thanks Orly Gnat and Ehud Nakar for many discussions. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California\nInstitute of Technology, Columbia University, Las Cumbres\nObservatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the\nUniversity of Oxford, and the Weizmann Institute of Science.\nSome of the data presented herein were obtained at the W. M.\nKeck 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. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by a grant from the Israeli Ministry of Science, ISF, Minerva, Weizmann-UK and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant no 1829/12). A.V.F.'s group at UC Berkeley has received generous\nfinancial assistance from Gary and Cynthia Bengier, the\nChristopher R. Redlich Fund, the Richard and Rhoda Goldman\nFund, the TABASGO Foundation, and NSF grant AST-1211916.\n\nPublished - 0004-637X_789_2_104.pdf
Submitted - 1401.5468v1.pdf
", "abstract": "There is a growing number of Type IIn supernovae (SNe) which present an outburst prior to their presumably final explosion. These precursors may affect the SN display, and are likely related to poorly charted phenomena in the final stages of stellar evolution. By coadding Palomar Transient Factory (PTF) images taken prior to the explosion, here we present a search for precursors in a sample of 16 Type IIn SNe. We find five SNe IIn that likely have at least one possible precursor event (PTF 10bjb, SN 2010mc, PTF 10weh, SN 2011ht, and PTF 12cxj), three of which are reported here for the first time. For each SN we calculate the control time. We find that precursor events among SNe IIn are common: at the one-sided 99% confidence level, >50% of SNe IIn have at least one pre-explosion outburst that is brighter than 3 \u00d7 10^7 L_\u2609 taking place up to 1/3 yr prior to the SN explosion. The average rate of such precursor events during the year prior to the SN explosion is likely \u2273 1 yr^(\u20131), and fainter precursors are possibly even more common. Ignoring the two weakest precursors in our sample, the precursors rate we find is still on the order of one per year. We also find possible correlations between the integrated luminosity of the precursor and the SN total radiated energy, peak luminosity, and rise time. These correlations are expected if the precursors are mass-ejection events, and the early-time light curve of these SNe is powered by interaction of the SN shock and ejecta with optically thick circumstellar material.", "date": "2014-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "789", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 104", "id_number": "CaltechAUTHORS:20140807-120341972", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140807-120341972", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "MINERVA (Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/789/2/104", "primary_object": { "basename": "0004-637X_789_2_104.pdf", "url": "https://authors.library.caltech.edu/records/sgxzc-5ph25/files/0004-637X_789_2_104.pdf" }, "related_objects": [ { "basename": "1401.5468v1.pdf", "url": "https://authors.library.caltech.edu/records/sgxzc-5ph25/files/1401.5468v1.pdf" } ], "pub_year": "2014", "author_list": "Ofek, Eran O.; Sullivan, Mark; et el." }, { "id": "https://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" } ], "pub_year": "2014", "author_list": "Laher, Russ R.; Surace, Jason; et el." }, { "id": "https://authors.library.caltech.edu/records/8scwv-vsf48", "eprint_id": 47289, "eprint_status": "archive", "datestamp": "2023-08-22 12:58:44", "lastmod": "2023-10-26 20:28:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "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": "Tal-David", "name": { "family": "Tal", "given": "David" } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Bersier-D", "name": { "family": "Bersier", "given": "David" } }, { "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": "De-Cia-A", "name": { "family": "De Cia", "given": "Annalisa" }, "orcid": "0000-0003-2082-1626" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fransson-C", "name": { "family": "Fransson", "given": "Claes" }, "orcid": "0000-0001-8532-3594" }, { "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": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" } ] }, "title": "Interaction-powered Supernovae: Rise-time versus Peak-luminosity Correlation and the Shock-breakout Velocity", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: massive; stars: mass-loss; supernovae: general", "note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 February 27; accepted 2014 April 15; published 2014 June 3. \n\nWe thank Dan Perley for obtaining some spectra. E.O.O.\nthanks Ehud Nakar and Orly Gnat for discussions. This paper\nis based on observations obtained with the Samuel Oschin\nTelescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at theW. 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. We are grateful for excellent staff assistance at Palomar, Lick, and Keck\nObservatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), IsraeliMinistry of Science, Israel Science Foundation, Minerva, Weizmann-UK and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. A.G-Y. acknowledge grants from the ISF, BSF, GIF, Minerva, the EU/FP7 via ERC grant (307260), and the I-CORE program of the Planning and Budgeting Committee and The Israel Science Foundation. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship.\nA.V.F.'s SN group at UC Berkeley has received generous\nfinancial assistance from Gary and CynthiaBengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916.\n\nPublished - 0004-637X_788_2_154.pdf
Submitted - 1404.4085v1.pdf
", "abstract": "Interaction of supernova (SN) ejecta with the optically thick circumstellar medium (CSM) of a progenitor star can result in a bright, long-lived shock-breakout event. Candidates for such SNe include Type IIn and superluminous SNe. If some of these SNe are powered by interaction, then there should be a specific relation between their peak luminosity, bolometric light-curve rise time, and shock-breakout velocity. Given that the shock velocity during shock breakout is not measured, we expect a correlation, with a significant spread, between the rise time and the peak luminosity of these SNe. Here, we present a sample of 15 SNe IIn for which we have good constraints on their rise time and peak luminosity from observations obtained using the Palomar Transient Factory. We report on a possible correlation between the R-band rise time and peak luminosity of these SNe, with a false-alarm probability of 3%. Assuming that these SNe are powered by interaction, combining these observables and theory allows us to deduce lower limits on the shock-breakout velocity. The lower limits on the shock velocity we find are consistent with what is expected for SNe (i.e., ~10^(4) km s^(\u20131)). This supports the suggestion that the early-time light curves of SNe IIn are caused by shock breakout in a dense CSM. We note that such a correlation can arise from other physical mechanisms. Performing such a test on other classes of SNe (e.g., superluminous SNe) can be used to rule out the interaction model for a class of events.", "date": "2014-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "788", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 154", "id_number": "CaltechAUTHORS:20140717-092439857", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140717-092439857", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ)" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "Minerva" }, { "agency": "Weizmann-UK" }, { "agency": "I-CORE Program of the Planning and Budgeting Committee" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/788/2/154", "primary_object": { "basename": "0004-637X_788_2_154.pdf", "url": "https://authors.library.caltech.edu/records/8scwv-vsf48/files/0004-637X_788_2_154.pdf" }, "related_objects": [ { "basename": "1404.4085v1.pdf", "url": "https://authors.library.caltech.edu/records/8scwv-vsf48/files/1404.4085v1.pdf" } ], "pub_year": "2014", "author_list": "Ofek, Eran O.; Arcavi, Iair; et el." }, { "id": "https://authors.library.caltech.edu/records/hf9cb-jhm42", "eprint_id": 47701, "eprint_status": "archive", "datestamp": "2023-08-22 12:59:26", "lastmod": "2023-10-26 21:10:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Amanullah-R", "name": { "family": "Amanullah", "given": "R." }, "orcid": "0000-0002-5559-9351" }, { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Johansson-J", "name": { "family": "Johansson", "given": "J." } }, { "id": "Banerjee-D-P-K", "name": { "family": "Banerjee", "given": "D. P. K." } }, { "id": "Venkataraman-V", "name": { "family": "Venkataraman", "given": "V." } }, { "id": "Joshi-V", "name": { "family": "Joshi", "given": "V." } }, { "id": "Ashok-N-M", "name": { "family": "Ashok", "given": "N. M." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "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" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Petrushevska-T", "name": { "family": "Petrushevska", "given": "T." }, "orcid": "0000-0003-4743-1679" }, { "id": "Stanishev-V", "name": { "family": "Stanishev", "given": "V." } } ] }, "title": "The Peculiar Extinction Law of SN 2014J Measured with the Hubble Space Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (Messier 82); supernovae: individual (SN 2014J)", "note": "\u00a9 2014 American Astronomical Society. Received 2014 April 9; accepted 2014 May 2; published 2014 May 29. We thank Denise Taylor, Claus Leitherer, and John Mackenty\nat the Space Telescope Science Institute for advising and\nassisting us in carrying out this program. R.A. and A.G.\nacknowledge support from the Swedish Research Council and\nthe Swedish Space Board. M.M.K. acknowledges support from\nthe Hubble Fellowship and Carnegie-Princeton Fellowship. Observations were made with the Hubble Space Telescope;\nthe Nordic Optical Telescope, operated by the Nordic Optical\nTelescope Scientific Association at the Observatorio del Roque\nde los Muchachos, La Palma, Spain; and the Mount Abu\n1.2 m Infrared Telescope, India. STSDAS is a product of the\nSpace Telescope Science Institute, which is operated by AURA\nfor NASA. V.S. acknowledges support from Funda\u00e7\u00e3o para a\nCi\u00eancia e a Tecnologia (Ci\u00eancia 2008) and grant PTDC/CTE-AST/112582/2009.\n\nPublished - 2041-8205_788_2_L21.pdf
Submitted - 1404.2595v2.pdf
", "abstract": "The wavelength dependence of the extinction of Type Ia SN 2014J in the nearby galaxy M82 has been measured using UV to near-IR photometry obtained with the Hubble Space Telescope, the Nordic Optical Telescope, and the Mount Abu Infrared Telescope. This is the first time that the reddening of an SN Ia is characterized over the full wavelength range of 0.2-2 \u03bcm. A total-to-selective extinction, R_V \u2265 3.1, is ruled out with high significance. The best fit at maximum using a Galactic type extinction law yields R_V = 1.4 \u00b1 0.1. The observed reddening of SN 2014J is also compatible with a power-law extinction, A _\u03bb/AV = (\u03bb/\u03bb_V )^p as expected from multiple scattering of light, with p = \u20132.1 \u00b1 0.1. After correcting for differences in reddening, SN 2014J appears to be very similar to SN 2011fe over the 14 broadband filter light curves used in our study.", "date": "2014-06-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "788", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L21", "id_number": "CaltechAUTHORS:20140731-094755056", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140731-094755056", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PTDC/CTE-AST", "grant_number": "112582/2009" }, { "agency": "Swedish Research Council" }, { "agency": "Swedish National Space Board (SNSB)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/788/2/L21", "primary_object": { "basename": "1404.2595v2.pdf", "url": "https://authors.library.caltech.edu/records/hf9cb-jhm42/files/1404.2595v2.pdf" }, "related_objects": [ { "basename": "2041-8205_788_2_L21.pdf", "url": "https://authors.library.caltech.edu/records/hf9cb-jhm42/files/2041-8205_788_2_L21.pdf" } ], "pub_year": "2014", "author_list": "Amanullah, R.; Goobar, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/a3918-fpe89", "eprint_id": 47078, "eprint_status": "archive", "datestamp": "2023-08-22 12:56:27", "lastmod": "2023-10-26 20:18:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chang-Chan-Kao", "name": { "family": "Chang", "given": "Chan-Kao" }, "orcid": "0000-0003-1656-4540" }, { "id": "Ip-Wing-Huen", "name": { "family": "Ip", "given": "Wing-Huen" }, "orcid": "0000-0002-3140-5014" }, { "id": "Lin-Hsing-Wen", "name": { "family": "Lin", "given": "Hsing-Wen" }, "orcid": "0000-0001-7737-6784" }, { "id": "Cheng-Yu-Chi", "name": { "family": "Cheng", "given": "Yu-Chi" } }, { "id": "Ngeow-Chow-Choong", "name": { "family": "Ngeow", "given": "Chow-Choong" }, "orcid": "0000-0001-8771-7554" }, { "id": "Yang-Ting-Chang", "name": { "family": "Yang", "given": "Ting-Chang" } }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" } ] }, "title": "313 New Asteroid Rotation Periods from Palomar Transient Factory Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "minor planets, asteroids : general; surveys.", "note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2014 February 14; accepted 2014 April 17; published 2014 May 16. \n\nThis work is supported in part by the National Science Council of Taiwan under the grants NSC 101-2119-M-008-007-MY3 and NSC 102-2112-M-008-019-MY3. We thank Eran Ofek for valuable comments and suggestions that made the manuscript more complete. We also thank the referee, Joseph Masiero, for useful comments that helped to improve the content of the paper. This publication makes use of data products from 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. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. We gratefully acknowledge the extraordinary services specific to NEOWISE contributed by the International Astronomical Unions Minor Planet Center, operated by the Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for Astronomical Telegrams, operated by Harvard University.\n\nPublished - 0004-637X_788_1_17.pdf
Submitted - 1405.1144v1.pdf
", "abstract": "A new asteroid rotation period survey has been carried out by using the Palomar Transient Factory (PTF). Twelve consecutive PTF fields, which covered an area of 87 deg^2 in the ecliptic plane, were observed in the R band with a cadence of ~20 minutes during 2013 February 15-18. We detected 2500 known asteroids with a diameter range of 0.5 km \u2264 D \u2264 200 km. Of these, 313 objects had highly reliable rotation periods and exhibited the \"spin barrier\" at ~2 hr. In contrast to the flat spin-rate distribution of the asteroids with 3 km \u2264 D \u2264 15 km shown by Pravec et al., our results deviated somewhat from a Maxwellian distribution and showed a decrease at the spin rate greater than 5 rev day^(\u20131). One superfast rotator candidate and two possible binary asteroids were also found in this work.", "date": "2014-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "788", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 17", "id_number": "CaltechAUTHORS:20140708-115611973", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140708-115611973", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Council (Taipei)", "grant_number": "NSC101-2119-M-008-007-MY3" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC102-2112-M-008-019-MY3" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "PTF Team" ] }, "doi": "10.1088/0004-637X/788/1/17", "primary_object": { "basename": "0004-637X_788_1_17.pdf", "url": "https://authors.library.caltech.edu/records/a3918-fpe89/files/0004-637X_788_1_17.pdf" }, "related_objects": [ { "basename": "1405.1144v1.pdf", "url": "https://authors.library.caltech.edu/records/a3918-fpe89/files/1405.1144v1.pdf" } ], "pub_year": "2014", "author_list": "Chang, Chan-Kao; Ip, Wing-Huen; et el." }, { "id": "https://authors.library.caltech.edu/records/vszpb-qfx47", "eprint_id": 45864, "eprint_status": "archive", "datestamp": "2023-08-20 01:00:53", "lastmod": "2023-10-26 18:30:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "S." }, "orcid": "0000-0001-6760-3074" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Tal-David", "name": { "family": "Tal", "given": "D." } }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "De-Cia-A", "name": { "family": "De Cia", "given": "A." }, "orcid": "0000-0003-2082-1626" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D." }, "orcid": "0000-0001-8472-1996" }, { "id": "Vreeswijk-P-M", "name": { "family": "Vreeswijk", "given": "P. M." }, "orcid": "0000-0002-7572-9088" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Wheeler-J-C", "name": { "family": "Wheeler", "given": "J. C." } } ] }, "title": "A Wolf\u2013Rayet-like progenitor of SN 2013cu from spectral observations of a stellar wind", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 Macmillan Publishers Limited. All Rights Reserved.\n\nReceived 23 October 2013 Accepted 25 March 2014 Published online 21 May 2014.\n\nThis research was supported by the I-CORE programme 'The Quantum Universe' of the Planning and Budgeting Committee and The Israel Science Foundation. A.G.-Y. acknowledges support by grants from the ISF, BSF, GIF, Minerva and FP7/ERC, and a Kimmel Investigator award. M.M.K. acknowledges support from Hubble and Carnegie-Princeton fellowships. E.O.O. acknowledges the Arye Dissentshik Career Development Chair and a grant from the Israeli MOST. J.C.W. is supported in part by the NSF. J.M.S. is supported by an NSF Postdoctoral Fellowship. A.V.F. acknowledges financial support from the TABASGO Foundation, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund and the NSF. The National Energy Research Scientific Computing Center, supported by the Office of Science of the US Department of Energy, provided staff, computational resources and data storage for this project. The Oskar Klein Centre is funded by the Swedish Research Council. We thank K. Clubb, O. Fox, P. Kelly, S. Tang and B. Sesar for their help with observations, and J. Groh, P. Crowther, M. Bersten, C. Fransson and E. Nakar for advice. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The observatory was made possible by the generous financial support of the W. M. Keck Foundation.\n\nSupplemental Material - nature13304-sf1.jpg
Supplemental Material - nature13304-sf2.jpg
Supplemental Material - nature13304-sf3.jpg
", "abstract": "The explosive fate of massive Wolf\u2013Rayet stars^1 (WRSs) is a key open question in stellar physics. An appealing option is that hydrogen-deficient WRSs are the progenitors of some hydrogen-poor supernova explosions of types\u2009IIb, Ib and Ic (ref. 2). A blue object, having luminosity and colours consistent with those of some WRSs, has recently been identified in pre-explosion images at the location of a supernova of type\u2009Ib (ref. 3), but has not yet been conclusively determined to have been the progenitor. Similar work has so far only resulted in non-detections^4. Comparison of early photometric observations of type\u2009Ic supernovae with theoretical models suggests that the progenitor stars had radii of less than 1012\u2009centimetres, as expected for some WRSs^5. The signature of WRSs, their emission line spectra, cannot be probed by such studies. Here we report the detection of strong emission lines in a spectrum of type\u2009IIb supernova 2013cu (iPTF13ast) obtained approximately 15.5 hours after explosion (by 'flash spectroscopy', which captures the effects of the supernova explosion shock breakout flash on material surrounding the progenitor star). We identify Wolf\u2013Rayet-like wind signatures, suggesting a progenitor of the WN(h) subclass (those WRSs with winds dominated by helium and nitrogen, with traces of hydrogen). The extent of this dense wind may indicate increased mass loss from the progenitor shortly before its explosion, consistent with recent theoretical predictions^6.", "date": "2014-05-22", "date_type": "published", "publication": "Nature", "volume": "509", "number": "7501", "publisher": "Nature Publishing Group", "pagerange": "471-478", "id_number": "CaltechAUTHORS:20140521-090302574", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140521-090302574", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Kimmel Award" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Ministry of Science and Technology (Israel)" }, { "agency": "TABASGO Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Swedish Research Council" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Caltech" }, { "agency": "University of California" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature13304", "primary_object": { "basename": "nature13304-sf1.jpg", "url": "https://authors.library.caltech.edu/records/vszpb-qfx47/files/nature13304-sf1.jpg" }, "related_objects": [ { "basename": "nature13304-sf2.jpg", "url": "https://authors.library.caltech.edu/records/vszpb-qfx47/files/nature13304-sf2.jpg" }, { "basename": "nature13304-sf3.jpg", "url": "https://authors.library.caltech.edu/records/vszpb-qfx47/files/nature13304-sf3.jpg" } ], "pub_year": "2014", "author_list": "Gal-Yam, Avishay; Arcavi, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/zdzvr-10668", "eprint_id": 46319, "eprint_status": "archive", "datestamp": "2023-08-22 12:39:48", "lastmod": "2023-10-26 19:39:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Wolf-W-M", "name": { "family": "Wolf", "given": "William M." }, "orcid": "0000-0002-6828-0630" }, { "id": "Li-Kelin", "name": { "family": "Li", "given": "K. L." } }, { "id": "Kong-Albert-K-H", "name": { "family": "Kong", "given": "Albert K. H." }, "orcid": "0000-0002-5105-344X" }, { "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": "De-Cia-A", "name": { "family": "De Cia", "given": "Annalisa" }, "orcid": "0000-0003-2082-1626" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "An Accreting White Dwarf near the Chandrasekhar Limit in the Andromeda Galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : individual (M31); novae, cataclysmic variables; supernovae : general; white dwarfs; X-rays : binaries", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2014 January 10; accepted 2014 March 11; published 2014 April 16.\n\nThis work was supported by the National Science Foundation\nunder grants PHY 11-25915, AST 11-09174, and\nAST 12-05574. Most of the MESA simulations for this work\nwere made possible by the Triton Resource. The Triton Resource\nis a high-performance research computing system operated by\nthe San Diego Supercomputer Center at UC San Diego. This\nresearch used resources of the National Energy Research Scientific\nComputing Center, which is supported by the Office of\nScience of the U.S. Department of Energy under Contract No.\nDE-AC02-05CH11231. A.K.H.K. is supported by the National\nScience Council of the Republic of China (Taiwan) through\ngrant NSC101-2119-M-008-007-MY3. M.M.K. acknowledges\ngenerous support from the Hubble Fellowship and Carnegie-\nPrinceton Fellowship. We are grateful to the Swift Team for\nthe superb timely scheduling of the observations and providing\ndata and analysis tools, and to Bill Paxton for his development\nof MESA.\nFacilities: PO:1.2m (PTF), PO:1.5m, Keck:I (DEIMOS,\nLRIS), Swift (XRT, UVOT)\n\nPublished - 0004-637X_786_1_61.pdf
Submitted - 1401.2426v2.pdf
", "abstract": "The intermediate Palomar Transient Factory (iPTF) detection of the most recent outburst of the recurrent nova (RN) system RX J0045.4+4154 in the Andromeda galaxy has enabled the unprecedented study of a massive (M > 1.3 M\u2609) accreting white dwarf (WD). We detected this nova as part of the near-daily iPTF monitoring of M31 to a depth of R \u224821 mag and triggered optical photometry, spectroscopy and soft X-ray monitoring of the outburst. Peaking at an absolute magnitude of M_R = \u20136.6 mag, and with a decay time of 1 mag per day, it is a faint and very fast nova. It shows optical emission lines of He/N and expansion velocities of 1900-2600 km s^(\u20131) 1-4 days after the optical peak. The Swift monitoring of the X-ray evolution revealed a supersoft source (SSS) with kT_(eff) \u2248 90-110 eV that appeared within 5 days after the optical peak, and lasted only 12 days. Most remarkably, this is not the first event from this system, rather it is an RN with a time between outbursts of approximately 1 yr, the shortest known. Recurrent X-ray emission from this binary was detected by ROSAT in 1992 and 1993, and the source was well characterized as a M > 1.3 M\u2609 WD SSS. Based on the observed recurrence time between different outbursts, the duration and effective temperature of the SS phase, MESA models of accreting WDs allow us to constrain the accretion rate to M > 1.7 x 10^(-7) M\u2609 yr^(-1) and WD mass >1.30 M\u2609. If the WD keeps 30% of the accreted material, it will take less than a Myr to reach core densities high enough for carbon ignition (if made of C/O) or electron capture (if made of O/Ne) to end the binary evolution.", "date": "2014-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "786", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 61", "id_number": "CaltechAUTHORS:20140618-073932304", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140618-073932304", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 11-25915" }, { "agency": "NSF", "grant_number": "AST 11-09174" }, { "agency": "NSF", "grant_number": "AST 12-05574" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "National Science Council (TaIpei)", "grant_number": "NSC101-2119-M-008-007-MY3" }, { "agency": "NASA" }, { "agency": "Carnegie-Princeton Fellowship" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/786/1/61", "primary_object": { "basename": "0004-637X_786_1_61.pdf", "url": "https://authors.library.caltech.edu/records/zdzvr-10668/files/0004-637X_786_1_61.pdf" }, "related_objects": [ { "basename": "1401.2426v2.pdf", "url": "https://authors.library.caltech.edu/records/zdzvr-10668/files/1401.2426v2.pdf" } ], "pub_year": "2014", "author_list": "Tang, Sumin; Bildsten, Lars; et el." }, { "id": "https://authors.library.caltech.edu/records/e94z0-xtf44", "eprint_id": 46813, "eprint_status": "archive", "datestamp": "2023-08-20 00:48:11", "lastmod": "2023-10-26 19:55:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fremling-C", "name": { "family": "Fremling", "given": "C." }, "orcid": "0000-0002-4223-103X" }, { "id": "Sollerman-J", "name": { "family": "Sollerman", "given": "J." }, "orcid": "0000-0003-1546-6615" }, { "id": "Taddia-F", "name": { "family": "Taddia", "given": "F." }, "orcid": "0000-0002-2387-6801" }, { "id": "Ergon-M", "name": { "family": "Ergon", "given": "M." } }, { "id": "Valenti-S", "name": { "family": "Valenti", "given": "S." }, "orcid": "0000-0001-8818-0795" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "S." }, "orcid": "0000-0001-6760-3074" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" } ] }, "title": "The rise and fall of the Type Ib supernova iPTF13bvn - Not a massive Wolf-Rayet star", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general / supernovae: individual: iPTF13bvn", "note": "\u00a9 2014 ESO. Article published by EDP Sciences. \n\nReceived 26 March 2014; Accepted 16 April 2014. Published online 20 May 2014. \n\nThe Oskar Klein Centre is funded by the Swedish\nResearch Council. This work is partially based on observations made with the\nNordic Optical Telescope, operated by the Nordic Optical Telescope Scientific\nAssociation at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained\nin part with ALFOSC, which is provided by the Instituto de Astrofisica\nde Andalucia (IAA) under a joint agreement with the University of Copenhagen\nand NOTSA. Some of the data presented herein were obtained at theW.M. Keck\nObservatory, which is operated as a scientific partnership among the California\nInstitute of Technology, the University of California, and NASA; the observatory\nwas made possible by the generous financial support of the W. M. Keck\nFoundation. A. G.-Y. is supported by the EU/FP7 via ERC grant 307260, \"The\nQuantum Universe\" I-Core program by the Israeli Committee for planning and\nbudgeting, by ISF, GIF, and Minerva grants, and by the Kimmel award. A.\nV. F.'s group at UC Berkeley has received generous financial assistance from\nthe Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant AST-\n1211916, and NASA grants AR-12623 and AR-12850 from the Space Telescope\nScience Institute (which is operated by AURA, Inc., under NASA contract NAS\n5-26555). We extend our thanks to the following people for their various contributions\nto this work: Shri Kulkarni, Mansi M. Kasliwal, Ofer Yaron, Paul\nVreeswijk, Daniel Perley, Joel Johansson, Anders Jerkstrand, Kelsey Clubb, Ori\nFox, Patrick Kelly, Barak Zackay, Adam Waszczak, Donald O'Sullivan, and\nThomas Augusteijn.\n\nPublished - aa23884-14.pdf
Submitted - 1403.6708v2.pdf
", "abstract": "Context. We investigate iPTF13bvn, a core-collapse (CC) supernova (SN) in the nearby spiral galaxy NGC 5806. This object was discovered by the intermediate Palomar Transient Factory (iPTF) very close to the estimated explosion date and was classified as a stripped-envelope CC SN, likely of Type Ib. Furthermore, a possible progenitor detection in pre-explosion Hubble Space Telescope (HST) images was reported, making this the only SN Ib with such an identification. Based on the luminosity and color of the progenitor candidate, as well as on early-time spectra and photometry of the SN, it was argued that the progenitor candidate is consistent with a single, massive Wolf-Rayet (WR) star.\n\nAims. We aim to confirm the progenitor detection, to robustly classify the SN using additional spectroscopy, and to investigate if our follow-up photometric and spectroscopic data on iPTF13bvn are consistent with a single-star WR progenitor scenario.\n\nMethods. We present a large set of observational data, consisting of multi-band light curves (UBVRI, g\u2032r\u2032i\u2032z\u2032) and optical spectra. We perform standard spectral line analysis to track the evolution of the SN ejecta. We also construct a bolometric light curve and perform hydrodynamical calculations to model this light curve to constrain the synthesized radioactive nickel mass and the total ejecta mass of the SN. Late-time photometry is analyzed to constrain the amount of oxygen. Furthermore, image registration of pre- and post-explosion HST images is performed.\n\nResults. Our HST astrometry confirms the location of the progenitor candidate of iPTF13bvn, and follow-up spectra securely classify this as a SN Ib. We use our hydrodynamical model to fit the observed bolometric light curve, estimating the total ejecta mass to be 1.9 M\u2299 and the radioactive nickel mass to be 0.05 M\u2299. The model fit requires the nickel synthesized in the explosion to be highly mixed out in the ejecta. We also find that the late-time nebular r\u2032-band luminosity is not consistent with predictions based on the expected oxygen nucleosynthesis in very massive stars.\n\nConclusions. We find that our bolometric light curve of iPTF13bvn is not consistent with the previously proposed single massive WR-star progenitor scenario. The total ejecta mass and, in particular, the late-time oxygen emission are both significantly lower than what would be expected from a single WR progenitor with a main-sequence mass of at least 30 M\u2299.", "date": "2014-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "565", "publisher": "EDP Sciences", "pagerange": "Art. No. A114", "id_number": "CaltechAUTHORS:20140703-105004666", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-105004666", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "W. M. Keck Foundation" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "Israeli Committee I-Core Program" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "MINERVA (Israel)" }, { "agency": "Kimmel Award" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NASA", "grant_number": "AR-12623" }, { "agency": "NASA", "grant_number": "AR-12850" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1051/0004-6361/201423884", "primary_object": { "basename": "1403.6708v2.pdf", "url": "https://authors.library.caltech.edu/records/e94z0-xtf44/files/1403.6708v2.pdf" }, "related_objects": [ { "basename": "aa23884-14.pdf", "url": "https://authors.library.caltech.edu/records/e94z0-xtf44/files/aa23884-14.pdf" } ], "pub_year": "2014", "author_list": "Fremling, C.; Sollerman, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/24ext-p0c44", "eprint_id": 46284, "eprint_status": "archive", "datestamp": "2023-08-22 12:30:33", "lastmod": "2023-10-26 19:38:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Margon-B", "name": { "family": "Margon", "given": "Bruce" }, "orcid": "0000-0002-7837-3363" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "Gregg" }, "orcid": "0000-0002-7083-4049" }, { "id": "Harding-L-K", "name": { "family": "Harding", "given": "Leon K." } }, { "id": "Kyne-G", "name": { "family": "Kyne", "given": "Gillian" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Rutten-R-G-M", "name": { "family": "Rutten", "given": "Ren\u00e9 G. M." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "PTF1 J191905.19+481506.2--A Partially Eclipsing AM CVn System Discovered in the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; binaries: close; novae, cataclysmic variables; stars: individual (PTF1J191905.19+481506.2); white dwarfs", "note": "\u00a9 2014 The American Astronomical Society.\n\nReceived 2013 September 28; accepted 2014 February 27; published 2014 April 2.\n\nT.K. acknowledges support by the Netherlands Research\nSchool of Astronomy (NOVA).We thank Dong Xu for reducing\nthe initial classification spectra.\nObservations obtained with the Samuel Oschin Telescope at\nthe Palomar Observatory as part of the Palomar Transient Factory\nproject, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory,\nthe Lawrence Berkeley National Laboratory, the National\nEnergy Research Scientific Computing Center, the University\nof Oxford, and the Weizmann Institute of Science. Some\nof the data presented herein were obtained at the W. M. Keck\nObservatory, which is operated as a scientific partnership among\nthe California Institute of Technology, the University of California\nand the National Aeronautics and Space Administration.\nThe Observatory was made possible by the generous financial\nsupport of the W. M. Keck Foundation. The authors wish to\nrecognize and acknowledge the very significant cultural role\nand reverence that the summit of Mauna Kea has always had\nwithin the indigenous Hawaiian community. We are most fortunate\nto have the opportunity to conduct observations from this\nmountain. Based in part on observations obtained at the Gemini\nObservatory, which is operated by the Association of Universities\nfor Research in Astronomy, Inc., under a cooperative\nagreement with the NSF on behalf of the Gemini partnership:\nthe National Science Foundation (United States), the National\nResearch Council (Canada), CONICYT (Chile), the Australian\nResearch Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia\ne Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e\nInnovaci\u00f3n Productiva (Argentina). The Gemini data were obtained\nunder Program ID GN-2012B-Q-110. Based in part on\nobservations made with the Gran Telescopio Canarias (GTC)\ninstalled in the Spanish Observatorio del Roque de los Muchachos\nof the Instituto de Astrof\u00edsica de Canarias, on the island of\nLa Palma.\n\nFacilities: PO:1.2m, PO:1.5m, Gemini:Gillett (GMOS-N),\nGTC (OSIRIS), Hale (CHIMERA, DBSP), Keck:I (LRIS),\nShane (Kast Double spectrograph)\n\nPublished - 0004-637X_785_2_114.pdf
Submitted - 1402.7129v1.pdf
", "abstract": "We report on PTF1 J191905.19+481506.2, a newly discovered, partially eclipsing, outbursting AM CVn system found in the Palomar Transient Factory synoptic survey. This is only the second known eclipsing AM CVn system. We use high-speed photometric observations and phase-resolved spectroscopy to establish an orbital period of 22.4559(3) minutes. We also present a long-term light curve and report on the normal and super-outbursts regularly seen in this system, including a super-outburst recurrence time of 36.8(4) days. We use the presence of the eclipse to place upper and lower limits on the inclination of the system and discuss the number of known eclipsing AM CVn systems versus what would be expected.", "date": "2014-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "785", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 114", "id_number": "CaltechAUTHORS:20140616-132349713", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140616-132349713", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Nederlandse Onderzoekschool voor de Astronomie (NOVA)" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Radiation-Laboratory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/785/2/114", "primary_object": { "basename": "0004-637X_785_2_114.pdf", "url": "https://authors.library.caltech.edu/records/24ext-p0c44/files/0004-637X_785_2_114.pdf" }, "related_objects": [ { "basename": "1402.7129v1.pdf", "url": "https://authors.library.caltech.edu/records/24ext-p0c44/files/1402.7129v1.pdf" } ], "pub_year": "2014", "author_list": "Levitan, David; Kupfer, Thomas; et el." }, { "id": "https://authors.library.caltech.edu/records/wn086-17w48", "eprint_id": 46139, "eprint_status": "archive", "datestamp": "2023-08-22 12:28:32", "lastmod": "2023-10-26 18:42:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "Paolo A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Gnat-O", "name": { "family": "Gnat", "given": "Orly" } }, { "id": "Modjaz-M", "name": { "family": "Modjaz", "given": "Maryam" }, "orcid": "0000-0001-7132-0333" }, { "id": "Rabinak-I", "name": { "family": "Rabinak", "given": "Itay" } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel" }, "orcid": "0000-0001-8472-1996" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "Dong" } } ] }, "title": "SN 2010mb: Direct Evidence for a Supernova Interacting with a Large Amount of Hydrogen-free Circumstellar Material", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; stars: Population III; supernovae: general", "note": "\u00a9 2014 American Astronomical Society. Received 2013 September 17; accepted 2014 February 16; published 2014 March 24. The authors thank C. Franson, S.E. Woosley and K. Maeda for useful discussions on the theoretical aspects of SN 2010mb. S.B. acknowledges support by a Ramon Fellowship from ISA. A.G. acknowledges support by grants from the ISF, BSF, GIF, Minerva, the FP7/ERC grant no 307260, the \"Quantum-Universe\" I-core program of the planning and budgeting committee and the ISF, and a Kimmel Investigator award. P.A.M. acknowledges financial support from INAF/PRIN 2011 and ASI. D.P. is supported by the Alon fellowship for outstanding young researchers, and the Raymond and Beverly Sackler Chair for young scientists. M.S. acknowledges support from the Royal Society. J.S.B. was partially supported by an NSF-CDI grant. M.M.K. acknowledges generous support from the Hubble and Carnegie-Princeton Fellowships. E.O.O. acknowledges the Arye Dissentshik career development chair and a grant from the Israeli MOST. The National Energy Research Scientific Computing Center, supported by the Office of Science of the U.S. Department of Energy, provided staff, computational resources, and data storage for this project. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation\nGroup, Brookhaven National Laboratory, Carnegie Mellon\nUniversity, University of Florida, the French Participation\nGroup, the German Participation Group, Harvard University,\nthe 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\nPublished - 0004-637X_785_1_37.pdf
Submitted - 1309.6496v1.pdf
", "abstract": "We present our observations of SN 2010mb, a Type Ic supernova (SN) lacking spectroscopic signatures of H and He. SN 2010mb has a slowly declining light curve (LC) (~600 days) that cannot be powered by ^(56)Ni/^(56)Co radioactivity, the common energy source for Type Ic SNe. We detect signatures of interaction with hydrogen-free circumstellar material including a blue quasi-continuum and, uniquely, narrow oxygen emission lines that require high densities (~10^9 cm^(\u20133)). From the observed spectra and LC, we estimate that the amount of material involved in the interaction was ~3 M_\u2609. Our observations are in agreement with models of pulsational pair-instability SNe described in the literature.", "date": "2014-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "785", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 37", "id_number": "CaltechAUTHORS:20140609-074647824", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140609-074647824", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ISA Ramon Fellowship" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Minerva" }, { "agency": "European Research Council (ERC)", "grant_number": "307260" }, { "agency": "\"Quantum-Universe\" I-Core Program" }, { "agency": "Kimmel Award" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Alon Fellowship" }, { "agency": "Raymond and Beverly Sackler Chair for young scientists" }, { "agency": "Royal Society" }, { "agency": "NSF" }, { "agency": "NASA" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Ministry of Science and Technology (Israel)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/785/1/37", "primary_object": { "basename": "0004-637X_785_1_37.pdf", "url": "https://authors.library.caltech.edu/records/wn086-17w48/files/0004-637X_785_1_37.pdf" }, "related_objects": [ { "basename": "1309.6496v1.pdf", "url": "https://authors.library.caltech.edu/records/wn086-17w48/files/1309.6496v1.pdf" } ], "pub_year": "2014", "author_list": "Ben-Ami, Sagi; Gal-Yam, Avishay; et el." }, { "id": "https://authors.library.caltech.edu/records/t9e00-gkf53", "eprint_id": 45316, "eprint_status": "archive", "datestamp": "2023-08-20 00:03:00", "lastmod": "2023-10-26 17:56:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hovatta-T", "name": { "family": "Hovatta", "given": "T." }, "orcid": "0000-0002-2024-8199" }, { "id": "Pavlidou-V", "name": { "family": "Pavlidou", "given": "V." } }, { "id": "King-O-G", "name": { "family": "King", "given": "O. G." } }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "id": "Dancikova-R", "name": { "family": "Dancikova", "given": "R." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Drake-A", "name": { "family": "Drake", "given": "A." } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } }, { "id": "Max-Moerbeck-W", "name": { "family": "Max-Moerbeck", "given": "W." }, "orcid": "0000-0002-5491-5244" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "T. A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "A. C. S." }, "orcid": "0000-0001-9152-961X" }, { "id": "Richards-J-L", "name": { "family": "Richards", "given": "J. L." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Connection between optical and \u03b3-ray variability in blazars", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active\n BL Lacertae objects: general\n galaxies: jets\n quasars: general", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 December 27. Received 2013 December 27; in original form 2013 September 16. First published online: January 30, 2014. \n\nWe thank the referee, Tigran Arshakian, for useful comments that helped to improve the paper. TH thanks Elina Lindfors for useful discussions. TH was supported in part by the Jenny and Antti Wihuri foundation. VP acknowledges support by the European Comission Seventh Framework Programme (FP7) through the Marie Curie Career Integration Grant PCIG10-GA-2011-304001 'JetPop' and the EU FP7 Grant PIRSES-GA-2012-31578 'EuroCal'. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative\nagreement by Associated Universities, Inc. The CSS survey is\nfunded 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 US National Science Foundation under grant AST-0909182. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California\nInstitute 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. It is also partially based on observations obtained as part of the Intermediate Palomar Transient Factory project, a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Millwakee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the\nUniversity System of Taiwan, the Kavli Institute for the Physics and Mathematics of the Universe and the Inter-University Centre for Astronomy and Astrophysics. 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\nAdministration.\n\nPublished - MNRAS-2014-Hovatta-690-702.pdf
Submitted - 1401.0538v1.pdf
Supplemental Material - CRTS_data_table.txt
Supplemental Material - PTF_data_table.txt
", "abstract": "We use optical data from the Palomar Transient Factory (PTF) and the Catalina Real-Time Transient Survey (CRTS) to study the variability of \u03b3-ray-detected and non-detected objects in a large population of active galactic nuclei selected from the Candidate Gamma-Ray Blazar Survey and Fermi Gamma-Ray Space Telescope catalogues. Our samples include 714 sources with PTF data and 1244 sources with CRTS data. We calculate the intrinsic modulation index to quantify the optical variability amplitude in these samples. We find the \u03b3-ray-detected objects to be more variable than the non-detected ones. The flat spectrum radio quasars (FSRQs) are more variable than the BL Lac objects in our sample, but the significance of the difference depends on the sample used. When dividing the objects based on their synchrotron peak frequency, we find the low synchrotron peaked (LSP) objects to be significantly more variable than the high synchrotron peaked (HSP) ones, explaining the difference between the FSRQs and BL Lacs. This could be due to the LSPs being observed near their electron energy peak, while in the HSPs the emission is caused by lower energy electrons, which cool more slowly. We also find a significant correlation between the optical and \u03b3-ray fluxes that is stronger in the HSP BL Lacs than in the FSRQs. The FSRQs in our sample are also more Compton dominated than the HSP BL Lacs. These findings are consistent with models where the \u03b3-ray emission of HSP objects is produced by the synchrotron self-Compton mechanism, while the LSP objects need an additional external Compton component that increases the scatter in the flux\u2013flux correlation.", "date": "2014-03-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "439", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "690-702", "id_number": "CaltechAUTHORS:20140429-133204484", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-133204484", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Jenny and Antti Wihuri Foundation" }, { "agency": "Marie Curie Fellowship", "grant_number": "PCIG10-GA-2011-304001" }, { "agency": "European Research Council (ERC)", "grant_number": "PIRSES-GA-2012-31578" }, { "agency": "NASA", "grant_number": "NNX08AW31G" }, { "agency": "NASA", "grant_number": "NNX11A043G" }, { "agency": "NSF", "grant_number": "AST-0808050" }, { "agency": "NSF", "grant_number": "AST-1109911" }, { "agency": "NASA", "grant_number": "NNG05GF22G" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stt2494", "primary_object": { "basename": "1401.0538v1.pdf", "url": "https://authors.library.caltech.edu/records/t9e00-gkf53/files/1401.0538v1.pdf" }, "related_objects": [ { "basename": "CRTS_data_table.txt", "url": "https://authors.library.caltech.edu/records/t9e00-gkf53/files/CRTS_data_table.txt" }, { "basename": "MNRAS-2014-Hovatta-690-702.pdf", "url": "https://authors.library.caltech.edu/records/t9e00-gkf53/files/MNRAS-2014-Hovatta-690-702.pdf" }, { "basename": "PTF_data_table.txt", "url": "https://authors.library.caltech.edu/records/t9e00-gkf53/files/PTF_data_table.txt" } ], "pub_year": "2014", "author_list": "Hovatta, T.; Pavlidou, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/me9kh-snt66", "eprint_id": 45217, "eprint_status": "archive", "datestamp": "2023-08-22 11:59:05", "lastmod": "2023-10-26 17:52:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Goobar-A", "name": { "family": "Goobar", "given": "A." }, "orcid": "0000-0002-4163-4996" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "D. A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Tendulkar-S-P", "name": { "family": "Tendulkar", "given": "S. P." }, "orcid": "0000-0003-2548-2926" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "The Rise of SN 2014J in the Nearby Galaxy M82", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: individual (Messier 82); supernovae: individual (SN 2014J)", "note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2014 February 7; accepted 2014 February 21; published 2014 March 7.\n\nWe thank S. Fossey for making the discovery R-band image\nof SN 2014J available to us. We are grateful to S. Fossey\nand M. Phillips for helpful comments on the manuscript. We\nacknowledge A. McKay, A. Bradley, N. Scoville, P. L. Capak,\nC. M. Carollo, S. Lilly, H. Sheth, V. Bhalerao, P. Donati, S. Geier, F. Saturni, G. Nowak, and A. Finoguenov for cooperating with ToO observations. A.G. and R.A. acknowledge support from the Swedish Research Council and the Swedish Space Board and A.G.-Y. an ERC grant. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. 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, Faulkes Telescope North image observed by Gain Lee, the Mount Abu 1.2 m Infrared telescope, India, and the 1.93 m telescope of Haute-Provence Observatory, CNRS, France. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.\n\nPublished - 2041-8205_784_1_L12.pdf
Submitted - 1402.0849v3.pdf
", "abstract": "We report on the discovery of SN 2014J in the nearby galaxy M82. Given its proximity, it offers the best opportunity to date to study a thermonuclear supernova (SN) over a wide range of the electromagnetic spectrum. Optical, near-IR, and mid-IR observations on the rising light curve, orchestrated by the intermediate Palomar Transient Factory, show that SN 2014J is a spectroscopically normal Type Ia supernova (SN Ia), albeit exhibiting high-velocity features in its spectrum and heavily reddened by dust in the host galaxy. Our earliest detections start just hours after the fitted time of explosion. We use high-resolution optical spectroscopy to analyze the dense intervening material and do not detect any evolution in the resolved absorption features during the light curve rise. Similar to other highly reddened SNe Ia, a low value of total-to-selective extinction, R_V \u2272 2, provides the best match to our observations. We also study pre-explosion optical and near-IR images from Hubble Space Telescope with special emphasis on the sources nearest to the SN location.", "date": "2014-03-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "784", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L12", "id_number": "CaltechAUTHORS:20140425-092110085", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140425-092110085", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Swedish Research Council" }, { "agency": "Swedish Space Board" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "European Research Council (ERC)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/784/1/L12", "primary_object": { "basename": "1402.0849v3.pdf", "url": "https://authors.library.caltech.edu/records/me9kh-snt66/files/1402.0849v3.pdf" }, "related_objects": [ { "basename": "2041-8205_784_1_L12.pdf", "url": "https://authors.library.caltech.edu/records/me9kh-snt66/files/2041-8205_784_1_L12.pdf" } ], "pub_year": "2014", "author_list": "Goobar, A.; Cao, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/q3py1-z5n73", "eprint_id": 44724, "eprint_status": "archive", "datestamp": "2023-08-22 11:50:15", "lastmod": "2023-10-26 14:54:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aasi-J", "name": { "family": "Aasi", "given": "J." } }, { "id": "Abadie-J", "name": { "family": "Abadie", "given": "J." } }, { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Abernathy-M-R", "name": { "family": "Abernathy", "given": "M. R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Ajith-P", "name": { "family": "Ajith", "given": "P." }, "orcid": "0000-0001-7519-2439" }, { "id": "Anderson-R-A", "name": { "family": "Anderson", "given": "R. A." } }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Austin-L", "name": { "family": "Austin", "given": "L." } }, { "id": "Barayoga-J-C", "name": { "family": "Barayoga", "given": "J. C." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Black-E", "name": { "family": "Black", "given": "E." } }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Cepeda-C", "name": { "family": "Cepeda", "given": "C." } }, { "id": "Chakraborty-R", "name": { "family": "Chakraborty", "given": "R." } }, { "id": "Chalermsongsak-T", "name": { "family": "Chalermsongsak", "given": "T." } }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Daudert-B", "name": { "family": "Daudert", "given": "B." } }, { "id": "Dergachev-V", "name": { "family": "Dergachev", "given": "V." } }, { "id": "Driggers-J-C", "name": { "family": "Driggers", "given": "J. C." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Fotopoulos-N", "name": { "family": "Fotopoulos", "given": "N." } }, { "id": "Gushwa-K-E", "name": { "family": "Gushwa", "given": "K. E." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hall-E", "name": { "family": "Hall", "given": "E." } }, { "id": "Harms-J", "name": { "family": "Harms", "given": "J." }, "orcid": "0000-0002-7332-9806" }, { "id": "Heefner-J", "name": { "family": "Heefner", "given": "J." } }, { "id": "Lewis-J-B", "name": { "family": "Lewis", "given": "J. B." } }, { "id": "Litvine-V", "name": { "family": "Litvine", "given": "V." } }, { "id": "Lloyd-D", "name": { "family": "Lloyd", "given": "D." } }, { "id": "Mageswaran-M", "name": { "family": "Mageswaran", "given": "M." } }, { "id": "Mailand-K", "name": { "family": "Mailand", "given": "K." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Martynov-D", "name": { "family": "Martynov", "given": "D." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Nash-T", "name": { "family": "Nash", "given": "T." } }, { "id": "Ogin-G-H", "name": { "family": "Ogin", "given": "G. H." } }, { "id": "Osthelder-C", "name": { "family": "Osthelder", "given": "C." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Phelps-M", "name": { "family": "Phelps", "given": "M." } }, { "id": "Poux-C", "name": { "family": "Poux", "given": "C." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Privitera-S", "name": { "family": "Privitera", "given": "S." } }, { "id": "Quintero-E-A", "name": { "family": "Quintero", "given": "E." } }, { "id": "Raymond-V", "name": { "family": "Raymond", "given": "V." } }, { "id": "Reitze-D-H", "name": { "family": "Reitze", "given": "D. H." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sannibale-V", "name": { "family": "Sannibale", "given": "V." } }, { "id": "Seifert-F", "name": { "family": "Seifert", "given": "F." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Singer-L", "name": { "family": "Singer", "given": "L." } }, { "id": "Smith-M-R", "name": { "family": "Smith", "given": "M. R." } }, { "id": "Smith-Lefebvre-N-D", "name": { "family": "Smith-Lefebvre", "given": "N. D." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thirugnanasambandam-M-P", "name": { "family": "Thirugnanasambandam", "given": "M. P." } }, { "id": "Thrane-E", "name": { "family": "Thrane", "given": "E." }, "orcid": "0000-0002-4418-3895" }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "A. J." }, "orcid": "0000-0002-0928-6784" }, { "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "S. E." } }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R." }, "orcid": "0000-0002-9145-8580" }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Yeaton-Massey-D", "name": { "family": "Yeaton-Massey", "given": "D." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Gossan-S", "name": { "family": "Gossan", "given": "S." } }, { "id": "Hong-T", "name": { "family": "Hong", "given": "T." } }, { "id": "Kaufman-K", "name": { "family": "Kaufman", "given": "K." } }, { "id": "Luan-Jing", "name": { "family": "Luan", "given": "J." }, "orcid": "0000-0001-6048-1959" }, { "id": "Miao-Haixing", "name": { "family": "Miao", "given": "H." }, "orcid": "0000-0003-2879-5821" }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Vallisneri-M", "name": { "family": "Vallisneri", "given": "M." }, "orcid": "0000-0002-4162-0033" }, { "id": "Yang-H", "name": { "family": "Yang", "given": "H." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Nissanke-S", "name": { "family": "Nissanke", "given": "S." } }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Hodge-K-A", "name": { "family": "Hodge", "given": "K. A." } }, { "id": "Jacobson-M", "name": { "family": "Jacobson", "given": "M." } }, { "id": "James-E", "name": { "family": "James", "given": "E." } }, { "id": "Kalmus-P", "name": { "family": "Kalmus", "given": "P." } }, { "id": "Kells-W", "name": { "family": "Kells", "given": "W." } }, { "id": "King-P-J", "name": { "family": "King", "given": "P. J." } }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "First Searches for Optical Counterparts to Gravitational-Wave Candidate Events", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; catalogs; gravitational waves; stars: neutron; surveys", "note": "\u00a9 2014 American Astronomical Society. Received 2013 October 30; accepted 2014 January 18; published 2014 February 11. We thank J. Barnes, D. Kasen, B. Metzger, and E. Nakar for\nproviding the kilonova model light curves that we have used in our Figures 4\u20137. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully\nacknowledge the support of the research by these agencies\nand by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National\nResearch Foundation of Korea, Industry Canada and the\nProvince of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, FIRB 2012 Project RBFR12PM1F (Italian Ministry of Education, University and Research), and the Alfred P. Sloan Foundation. This work is based on results partially obtained at the ESO observatory, La Silla. 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. This document has been assigned the identifier LIGO-P1200171-v19.\n\nPublished - 0067-0049_211_1_7.pdf
Submitted - 1310.2314v2.pdf
", "abstract": "During the Laser Interferometer Gravitational-wave Observatory and Virgo joint science runs in 2009-2010, gravitational wave (GW) data from three interferometer detectors were analyzed within minutes to select GW candidate events and infer their apparent sky positions. Target coordinates were transmitted to several telescopes for follow-up observations aimed at the detection of an associated optical transient. Images were obtained for eight such GW candidates. We present the methods used to analyze the image data as well as the transient search results. No optical transient was identified with a convincing association with any of these candidates, and none of the GW triggers showed strong evidence for being astrophysical in nature. We compare the sensitivities of these observations to several model light curves from possible sources of interest, and discuss prospects for future joint GW-optical observations of this type.", "date": "2014-03", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "211", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 7", "id_number": "CaltechAUTHORS:20140408-071345962", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140408-071345962", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max-Planck-Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Australian Research Council" }, { "agency": "International Science Linkages program of the Commonwealth of Australia" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)" }, { "agency": "Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears" }, { "agency": "Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research" }, { "agency": "Ministry of Science and Higher Education (Poland)" }, { "agency": "FOCUS Programme of Foundation for Polish Science" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "NASA" }, { "agency": "Hungarian Scientific Research Fund (OTKA)" }, { "agency": "Lyon Institute of Origins (LIO)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Industry Canada" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Carnegie Trust" }, { "agency": "Leverhulme Trust" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Research Corporation" }, { "agency": "FIRB 2012 Project", "grant_number": "RBFR12PM1F" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ontario Ministry of Economic Development and Innovation" } ] }, "other_numbering_system": { "items": [ { "id": "P1200171-v19", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "LIGO" }, { "id": "Palomar-Transient-Factory" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1088/0067-0049/211/1/7", "primary_object": { "basename": "0067-0049_211_1_7.pdf", "url": "https://authors.library.caltech.edu/records/q3py1-z5n73/files/0067-0049_211_1_7.pdf" }, "related_objects": [ { "basename": "1310.2314v2.pdf", "url": "https://authors.library.caltech.edu/records/q3py1-z5n73/files/1310.2314v2.pdf" } ], "pub_year": "2014", "author_list": "Aasi, J.; Abadie, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/rmyde-ccx18", "eprint_id": 44217, "eprint_status": "archive", "datestamp": "2023-08-22 11:47:04", "lastmod": "2023-10-26 00:18:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pan-Y-C", "name": { "family": "Pan", "given": "Y.-C." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Botyanszki-J", "name": { "family": "Botyanszki", "given": "J." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "DeRose-J", "name": { "family": "DeRose", "given": "J." } }, { "id": "Fakhouri-H-K", "name": { "family": "Fakhouri", "given": "H. K." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Hsiao-Eric-Y-Astro", "name": { "family": "Hsiao", "given": "E. Y." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "C." }, "orcid": "0000-0003-1731-0497" }, { "id": "Nordin-J", "name": { "family": "Nordin", "given": "J." } }, { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E. S." } }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } } ] }, "title": "The host galaxies of Type Ia supernovae discovered by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general cosmology: observations; distance scale", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 November 22; Received 2013 November 11; in original form 2013 September 23.\n\nFirst published online: December 20, 2013.\nMS acknowledges support from the Royal Society. AG acknowledges support from the EU/FP7 via and ERC grant, funding from the ISF and BSF, and the Minerva ARCHES and Kimmel awards. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT\n(Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina). Based on Gemini progammes GN-2010B-Q-111, GS-2010B-Q-82, GN-2011A-Q-82, GN-2011B-Q-108, GN-2012A-Q-91, GS-2012A-Q-3, GN-2012B-Q-122 and GS-2012B-Q-83 for the host galaxy observations, and GN-2010A-Q-20, GN-2010B-Q-13, GN-2011AQ-16 and GS-2009B-Q-11 for the SN observations. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. Observations obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the PTF project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory,\nthe National Energy Research Scientific Computing Center,\nthe University of Oxford and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of 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. Based on observations collected at the\nEuropean Organization for Astronomical Research in the Southern hemisphere, Chile, under programme IDs 084.A-0149 and 085.A-0777. Observations obtained with the SuperNova Integral Field Spectrograph on the University of Hawaii 2.2m telescope as part of the Nearby Supernova Factory II project, a scientific collaboration between the Centre de Recherche Astronomique de Lyon, Institut de Physique Nucl\u00e9aire de Lyon, Laboratoire de Physique Nucl\u00e9aire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute\nfor Astrophysics, Tsinghua Center for Astrophysics and Centre de Physique des Particules de Marseille. This research hasmade 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 publication has been made possible by the participation of more than 10 000 volunteers in the Galaxy Zoo: Supernovae project (http://supernova.galaxyzoo.org/authors).\n\nPublished - MNRAS-2014-Pan-1391-416.pdf
Submitted - 1311.6344v1.pdf
", "abstract": "We present spectroscopic observations of the host galaxies of 82 low-redshift Type Ia supernovae (SNe Ia) discovered by the Palomar Transient Factory. We determine star formation rates, gas-phase/stellar metallicities, and stellar masses and ages of these objects. As expected, strong correlations between the SN Ia light-curve width (stretch) and the host age/mass/metallicity are found: fainter, faster declining events tend to be hosted by older/massive/metal-rich galaxies. There is some evidence that redder SNe Ia explode in higher metallicity galaxies, but we found no relation between the SN colour and host galaxy extinction based on the Balmer decrement, suggesting that the colour variation of these SNe does not primarily arise from this source. SNe Ia in higher mass/metallicity galaxies also appear brighter after stretch/colour corrections than their counterparts in lower mass hosts, and the stronger correlation is with gas-phase metallicity suggesting this may be the more important variable. We also compared the host stellar mass distribution to that in galaxy-targeted SN surveys and the high-redshift untargeted Supernova Legacy Survey (SNLS). SNLS has many more low-mass galaxies, while the targeted searches have fewer. This can be explained by an evolution in the galaxy stellar mass function, coupled with an SN delay-time distribution proportional to t^\u22121. Finally, we found no significant difference in the mass\u2013metallicity relation of our SN Ia hosts compared to field galaxies, suggesting any metallicity effect on the SN Ia rate is small.", "date": "2014-02-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "438", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1391-1416", "id_number": "CaltechAUTHORS:20140310-100817835", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140310-100817835", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Minerva ARCHES Award" }, { "agency": "Kimmel Award" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stt2287", "primary_object": { "basename": "1311.6344v1.pdf", "url": "https://authors.library.caltech.edu/records/rmyde-ccx18/files/1311.6344v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Pan-1391-416.pdf", "url": "https://authors.library.caltech.edu/records/rmyde-ccx18/files/MNRAS-2014-Pan-1391-416.pdf" } ], "pub_year": "2014", "author_list": "Pan, Y.-C.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/9fmes-98y43", "eprint_id": 45001, "eprint_status": "archive", "datestamp": "2023-08-22 11:42:36", "lastmod": "2023-10-26 17:29:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D. B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "J." }, "orcid": "0000-0003-2251-0602" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "K." }, "orcid": "0000-0002-2557-5180" }, { "id": "Pan-Yen-Chen", "name": { "family": "Pan", "given": "Y.-C." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "id": "Sternberg-A", "name": { "family": "Sternberg", "given": "A." } }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } }, { "id": "Bersier-D", "name": { "family": "Bersier", "given": "D." } }, { "id": "James-P", "name": { "family": "James", "given": "P." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" } ] }, "title": "A Multi-wavelength Investigation of the Radio-loud Supernova PTF11qcj and its Circumstellar Environment", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (PTF11qcj)", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 13 August 2013, accepted for publication 12 December 2013; Published 24 January 2014.\n\nPTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and Berkeley. Staff and computational resources were provided by NERSC, supported by the DOE Office of Science. HET/LRS are supported by UT/Austin, the Pennsylvania State University, Stanford, Ludwig-Maximilians-Universitat Munchen, Georg-August-Universitat Gottingen, and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The K. Jansky Very Large Array is operated by NRAO, for the NSF under cooperative agreement by Associated Universities, Inc. The\nW. M. Keck Observatory, is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The 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. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. A.G. and S.R.K. acknowledge support from the BSF; A.G. further acknowledges support from the ISF, EU/FP7 via an ERC grant, GIF, Minerva, and a Kimmel Award; E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science\nFoundation (grant No 1829/12); J.S.B. acknowledges support of an NSF-CDI Grant 0941742, \"Real- time Classification of Massive Time-series Data Streams\"; M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship; M.S. acknowledges support from the Royal Society; S.B.C. acknowledges generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. A.C. thanks the VLA staff for their support, and in particular:Miriam Krauss for very useful discussions on many aspects of the data reduction procedures; Heidi Medlin for support with the scheduling of the observations; and Drew Medlin for useful discussions on the VLA data reduction pipeline. A.C. also thanks E. Nakar for useful discussions. We thank the anonymous referee for useful comments.\n\nPublished - 0004-637X_782_1_42.pdf
Submitted - 1307.2366v3.pdf
", "abstract": "We present the discovery, classification, and extensive panchromatic (from radio to X-ray) follow-up observations of PTF11qcj, a supernova (SN) discovered by the Palomar Transient Factory (PTF). Our observations with the Karl G. Jansky Very Large Array show that this event is radio-loud: PTF11qcj reached a radio peak luminosity comparable to that of the famous gamma-ray-burst-associated SN 1998bw (L_(5\u2009GHz) \u2248 10^(29) erg s^(\u22121) Hz^(\u22121)). PTF11qcj is also detected in X-rays with the Chandra Observatory, and in the infrared band with Spitzer. Our multi-wavelength analysis probes the SN interaction with circumstellar material. The radio observations suggest a progenitor mass-loss rate of ~10^(\u22124) M_\u2609 yr^(\u22121) \u00d7 (v_w/1000 km s^(\u22121)), and a velocity of \u22480.3\u20130.5\u2009c for the fastest moving ejecta (at \u224810 days after explosion). However, these estimates are derived assuming the simplest model of SN ejecta interacting with a smooth circumstellar wind, and do not account for possible inhomogeneities in the medium and asphericity of the explosion. The radio data show deviations from such a simple model, as well as a late-time re-brightening. The X-ray flux from PTF11qcj is compatible with the high-frequency extrapolation of the radio synchrotron emission (within the large uncertainties). A light echo from pre-existing dust is in agreement with our infrared data. Our pre-explosion data from the PTF suggest that a precursor eruption of absolute magnitude M_r \u2248 \u221213 mag may have occurred \u22482.5 yr prior to the SN explosion. Overall, PTF11qcj fits the expectations from the explosion of a Wolf\u2013Rayet star. Precursor eruptions may be a feature characterizing the final pre-explosion evolution of such stars.", "date": "2014-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "782", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 42", "id_number": "CaltechAUTHORS:20140417-091838062", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-091838062", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "European Research Council (ERC)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "MINERVA (Israel)" }, { "agency": "Kimmel Award" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "I-CORE Program Planning and Budgeting Committee" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Royal Society" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/782/1/42", "primary_object": { "basename": "0004-637X_782_1_42.pdf", "url": "https://authors.library.caltech.edu/records/9fmes-98y43/files/0004-637X_782_1_42.pdf" }, "related_objects": [ { "basename": "1307.2366v3.pdf", "url": "https://authors.library.caltech.edu/records/9fmes-98y43/files/1307.2366v3.pdf" } ], "pub_year": "2014", "author_list": "Corsi, A.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/6msvy-cef50", "eprint_id": 43782, "eprint_status": "archive", "datestamp": "2023-08-22 11:30:56", "lastmod": "2023-10-25 23:52:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Grefenstette-B-W", "name": { "family": "Grefenstette", "given": "Brian" }, "orcid": "0000-0002-1984-2932" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Madsen-K-K", "name": { "family": "Madsen", "given": "Kristin" }, "orcid": "0000-0003-1252-4891" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "SN 2010jl: Optical to Hard X-Ray Observations Reveal an Explosion Embedded in a Ten Solar Mass Cocoon", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (SN 2010jl)", "note": "\u00a9 2014 American Astronomical Society.\n\nReceived 2013 July 2; accepted 2013 November 25; published 2014 January 6.\n\nWe thank an anonymous referee for a constructive report.\nE.O.O. thanks Roni Waldman, Nir Sapir, and Orly Gnat for\ndiscussions. This work was supported under NASA Contract\nNo. NNG08FD60C and made use of data from the NuSTAR\nmission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of\nTechnology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science, Israel Science Foundation, Minerva, and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant No 1829/12). A.V.F.'s SN group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916.\n\nPublished - 0004-637X_781_1_42.pdf
Submitted - 1307.2247v1.pdf
", "abstract": "Some supernovae (SNe) may be powered by the interaction of the SN ejecta with a large amount of circumstellar matter (CSM). However, quantitative estimates of the CSM mass around such SNe are missing when the CSM material is optically thick. Specifically, current estimators are sensitive to uncertainties regarding the CSM density profile and the ejecta velocity. Here we outline a method to measure the mass of the optically thick CSM around such SNe. We present new visible-light and X-ray observations of SN 2010jl (PTF 10aaxf), including the first detection of an SN in the hard X-ray band using NuSTAR. The total radiated luminosity of SN 2010jl is extreme\u2014at least 9 \u00d7 10^50 erg. By modeling the visible-light data, we robustly show that the mass of the circumstellar material within ~10^16 cm of the progenitor of SN 2010jl was in excess of 10 M_\u2609. This mass was likely ejected tens of years prior to the SN explosion. Our modeling suggests that the shock velocity during shock breakout was ~6000 km s^\u20131, decelerating to ~2600 km s^\u20131 about 2 yr after maximum light. Furthermore, our late-time NuSTAR and XMM spectra of the SN presumably provide the first direct measurement of SN shock velocity 2 yr after the SN maximum light\u2014measured to be in the range of 2000-4500 km s^\u20131 if the ions and electrons are in equilibrium, and \u2273 2000 km s^\u20131 if they are not in equilibrium. This measurement is in agreement with the shock velocity predicted by our modeling of the visible-light data. Our observations also show that the average radial density distribution of the CSM roughly follows an r^\u20132 law. A possible explanation for the \u2273 10 M_\u2609 of CSM and the wind-like profile is that they are the result of multiple pulsational pair instability events prior to the SN explosion, separated from each other by years.", "date": "2014-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "781", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 42", "id_number": "CaltechAUTHORS:20140211-134538316", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140211-134538316", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG08FD60C" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Minerva" }, { "agency": "Planning and Budgeting Committee I-CORE Program" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" } ] }, "local_group": { "items": [ { "id": "NuSTAR" }, { "id": "Space-Radiation-Laboratory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/781/1/42", "primary_object": { "basename": "0004-637X_781_1_42.pdf", "url": "https://authors.library.caltech.edu/records/6msvy-cef50/files/0004-637X_781_1_42.pdf" }, "related_objects": [ { "basename": "1307.2247v1.pdf", "url": "https://authors.library.caltech.edu/records/6msvy-cef50/files/1307.2247v1.pdf" } ], "pub_year": "2014", "author_list": "Ofek, Eran O.; Harrison, Fiona A.; et el." }, { "id": "https://authors.library.caltech.edu/records/k50rx-3z327", "eprint_id": 43784, "eprint_status": "archive", "datestamp": "2023-08-22 11:31:09", "lastmod": "2023-10-25 23:52:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Price-Whelan-A", "name": { "family": "Price-Whelan", "given": "Adrian M." }, "orcid": "0000-0003-0872-7098" }, { "id": "Ag\u00fceros-M-A", "name": { "family": "Ag\u00fceros", "given": "Marcel A." }, "orcid": "0000-0001-7077-3664" }, { "id": "Fournier-A-P", "name": { "family": "Fournier", "given": "Amanda P." } }, { "id": "Street-R-A", "name": { "family": "Street", "given": "Rachel" }, "orcid": "0000-0001-6279-0552" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Covey-K-R", "name": { "family": "Covey", "given": "Kevin R." }, "orcid": "0000-0001-6914-7797" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Statistical Searches for Microlensing Events in Large, Non-uniformly Sampled Time-Domain Surveys: A Test Using Palomar Transient Factory Data", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: micro; methods: statistical; surveys", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 June 21; accepted 2013 November 13; published 2014 January 6. \n\nWe thank E. Bowsher, S. Douglas, and S. Tang for their\nassistance in obtaining spectra for our candidates and M. Modjaz for help in interpreting several of these spectra. We are grateful to the anonymous referee and to our editor, E. Feigelson, for comments that improved the paper. This paper is based upon work supported by a National Science\nFoundation Graduate Research Fellowship under grant No.\n11-44155 and on observations obtained with the Samuel Oschin\nTelescope 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.\nFunding for SDSS-III has been provided by the Alfred P.\nSloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation\nGroup, Harvard University, the Instituto de Astrofisica\nde 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\nUniversity, New York University, Ohio State University, Pennsylvania\nState University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of\nTokyo, University of Utah, Vanderbilt University, University\nof Virginia, University of Washington, and Yale University.\nThis publication makes use of data products from the Widefield\nInfrared Survey Explorer, which is a joint project of the\nUniversity of California, Los Angeles, and the Jet Propulsion\nLaboratory/California Institute of Technology, funded by the\nNational Aeronautics and Space Administration.\nThis research made use of Astropy, a community-developed\ncore Python package for astronomy (Astropy Collaboration\n2013).\n\nPublished - 0004-637X_781_1_35.pdf
Submitted - 1311.3683v2.pdf
", "abstract": "Many photometric time-domain surveys are driven by specific goals, such as searches for supernovae or transiting exoplanets, which set the cadence with which fields are re-imaged. In the case of the Palomar Transient Factory (PTF), several sub-surveys are conducted in parallel, leading to non-uniform sampling over its ~20,000 deg^2 footprint. While the median 7.26 deg^2 PTF field has been imaged ~40 times in the R band, ~2300 deg^2 have been observed >100 times. We use PTF data to study the trade off between searching for microlensing events in a survey whose footprint is much larger than that of typical microlensing searches, but with far-from-optimal time sampling. To examine the probability that microlensing events can be recovered in these data, we test statistics used on uniformly sampled data to identify variables and transients. We find that the von Neumann ratio performs best for identifying simulated microlensing events in our data. We develop a selection method using this statistic and apply it to data from fields with >10 R-band observations, 1.1 \u00d7 10^9 light curves, uncovering three candidate microlensing events. We lack simultaneous, multi-color photometry to confirm these as microlensing events. However, their number is consistent with predictions for the event rate in the PTF footprint over the survey's three years of operations, as estimated from near-field microlensing models. This work can help constrain all-sky event rate predictions and tests microlensing signal recovery in large data sets, which will be useful to future time-domain surveys, such as that planned with the Large Synoptic Survey Telescope.", "date": "2014-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "781", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 35", "id_number": "CaltechAUTHORS:20140211-143531840", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140211-143531840", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "11-44155" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-637X/781/1/35", "primary_object": { "basename": "0004-637X_781_1_35.pdf", "url": "https://authors.library.caltech.edu/records/k50rx-3z327/files/0004-637X_781_1_35.pdf" }, "related_objects": [ { "basename": "1311.3683v2.pdf", "url": "https://authors.library.caltech.edu/records/k50rx-3z327/files/1311.3683v2.pdf" } ], "pub_year": "2014", "author_list": "Price-Whelan, Adrian M.; Ag\u00fceros, Marcel A.; et el." }, { "id": "https://authors.library.caltech.edu/records/a30ns-tt409", "eprint_id": 96194, "eprint_status": "archive", "datestamp": "2023-08-19 23:04:50", "lastmod": "2023-10-20 20:58:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mulchaey-J-S", "name": { "family": "Mulchaey", "given": "John S." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kollmeier-J-A", "name": { "family": "Kollmeier", "given": "Juna" }, "orcid": "0000-0001-9852-1610" } ] }, "title": "Calcium-rich gap transients: solving the calcium conundrum in the intracluster medium", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014. The American Astronomical Society. \n\nReceived 2013 October 21. Accepted 2013 December 7. Published 2013 December 19. \n\nWe are grateful to Jelle de Plaa and Esra Bulbul for providing additional insight on their previous work and we thank Avishay Gal-Yam, Melissa Graham, and Paolo Mazzali for helpful discussions. This work was inspired by presentations at the conference Energetic Astronomy: Richard Mushotzky at 65. We thank Chris Reynolds for his help organizing the conference.\n\nPublished - Mulchaey_2014_ApJL_780_L34.pdf
", "abstract": "X-ray measurements suggest that the abundance of calcium in the intracluster medium is higher than can be explained using favored models for core-collapse and Type Ia supernovae alone. We investigate whether the \"calcium conundrum\" in the intracluster medium can be alleviated by including a contribution from the recently discovered subclass of supernovae known as calcium-rich gap transients. Although the calcium-rich gap transients make up only a small fraction of all supernovae events, we find that their high calcium yields are sufficient to reproduce the X-ray measurements found for nearby rich clusters. We find the \u03c72 goodness-of-fit metric improves from 84 to 2 by including this new class. Moreover, calcium-rich supernovae preferentially occur in the outskirts of galaxies making it easier for the nucleosynthesis products of these events to be incorporated in the intracluster medium via ram-pressure stripping. The discovery of calcium-rich gap transients in clusters and groups far from any individual galaxy suggests that supernovae associated with intracluster stars may play an important role in enriching the intracluster medium. Calcium-rich gap transients may also help explain anomalous calcium abundances in many other astrophysical systems including individual stars in the Milky Way, the halos of nearby galaxies, and the circumgalactic medium. Our work highlights the importance of considering the diversity of supernovae types and corresponding yields when modeling the abundance of the intracluster medium and other gas reservoirs.", "date": "2014-01-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "780", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L34", "id_number": "CaltechAUTHORS:20190606-145147947", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190606-145147947", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/2041-8205/780/2/L34", "primary_object": { "basename": "Mulchaey_2014_ApJL_780_L34.pdf", "url": "https://authors.library.caltech.edu/records/a30ns-tt409/files/Mulchaey_2014_ApJL_780_L34.pdf" }, "pub_year": "2014", "author_list": "Mulchaey, John S.; Kasliwal, M. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/yk5g5-5f655", "eprint_id": 42975, "eprint_status": "archive", "datestamp": "2023-08-19 22:28:19", "lastmod": "2023-10-25 23:11:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John" }, "orcid": "0000-0003-2251-0602" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" } ] }, "title": "An early and comprehensive millimetre and centimetre wave and X-ray study of SN 2011dh: a non-equipartition blast wave expanding into a massive stellar wind", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general \u2013 supernovae: individual: SN 2011dh \u2013 radio continuum: general \u2013 X-rays: general", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 August 30. Received 2013 August 30; in original form 2013 June 5. Published: 26 September 2013.\n\nWe thank the EVLA and CARMA staff for promptly scheduling this target of opportunity. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. This work made use of data supplied by the UK SSDC. PTF is a fully automated, wide-field survey aimed at a systematic exploration of explosions and variable phenomena in optical wavelengths. The participating institutions are Caltech, Columbia University, Weizmann Institute of Science, Lawrence Berkeley Laboratory, Oxford and University of California at Berkeley. The programme is centred on a 12K \u00d7 8K, 7.8 deg2 CCD array (CFH12K) re-engineered for the 1.2-m Oschin Telescope at the Palomar Observatory by Caltech Optical Observatories. Photometric follow-up is undertaken by the automated Palomar 1.5-m telescope. Research at Caltech is supported by grants from NSF and NASA. The Weizmann PTF partnership is supported in part by the Israeli Science Foundation via grants to AG. The Weizmann\u2013Caltech collaboration is supported by a grant from the BSF to AG and SRK. AG further acknowledges the Lord Sieff of Brimpton Foundation. CS is supported by the NASA Wisconsin Space Grant Consortium. FB acknowledges support from CONICYT, Chile, under grants FONDECYT 1101024 and FONDAP-CATA 15010003, Programa de Financiamiento Basal, the Iniciativa Cientifica Milenio through the Millennium Center for Supernova Science grant P10-064-F, and Chandra X-ray Center grants SAO GO9-0086D and GO0-11095A. MMK acknowledges support from the Hubble Fellowship and the Carnegie\u2013Princeton Fellowship. NP acknowledges partial support by STScI-DDRF grant D0001.82435. Research at the Naval Research Laboratory is supported by funding from the Office of Naval Research. SBC acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Sylvia & Jim Katzman Foundation, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916. We thank the anonymous referee for his constructive comments.\n\nPublished - stt1645.pdf
Submitted - 1209.1102v1.pdf
", "abstract": "Only a handful of supernovae (SNe) have been studied in multiwavelengths from the radio to X-rays, starting a few days after the explosion. The early detection and classification of the nearby Type IIb SN 2011dh/PTF 11eon in M51 provides a unique opportunity to conduct such observations. We present detailed data obtained at one of the youngest phase ever of a core-collapse SN (days 3\u201312 after the explosion) in the radio, millimetre and X-rays; when combined with optical data, this allows us to explore the early evolution of the SN blast wave and its surroundings. Our analysis shows that the expanding SN shock wave does not exhibit equipartition (\u03f5_e/\u03f5_B \u223c 1000), and is expanding into circumstellar material that is consistent with a density profile falling like R^(\u22122). Within modelling uncertainties we find an average velocity of the fast parts of the ejecta of 15\u2009000 \u00b1 1800\u2009km\u2009s^(\u22121), contrary to previous analysis. This velocity places SN 2011dh in an intermediate blast wave regime between the previously defined compact and extended SN Type IIb subtypes. Our results highlight the importance of early (\u223c1\u2009d) high-frequency observations of future events. Moreover, we show the importance of combined radio/X-ray observations for determining the microphysics ratio \u03f5_e/\u03f5_B.", "date": "2013-12-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "436", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1258-1267", "id_number": "CaltechAUTHORS:20131212-093147751", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131212-093147751", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Associates of the California Institute of Technology" }, { "agency": "University of Chicago" }, { "agency": "State of California" }, { "agency": "State of Illinois" }, { "agency": "State of Maryland" }, { "agency": "NSF" }, { "agency": "Israeli Science Foundation (ISF)" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Lord Sieff of Brimpton Foundation" }, { "agency": "NASA Wisconsin Space Grant Consortium" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1101024" }, { "agency": "Fondo de Financiamiento de Centros de Investigaci\u00f3n en \u00c1reas Prioritarias (FONDAP)", "grant_number": "15010003" }, { "agency": "Programa de Financiamiento Basal" }, { "agency": "Iniciativa Cientifica Milenio", "grant_number": "P10-064-F" }, { "agency": "NASA", "grant_number": "SAO GO9-0086D" }, { "agency": "NASA", "grant_number": "GO0-11095A" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Space Telescope Science Institute", "grant_number": "D0001.82435" }, { "agency": "Office of Naval Research (ONR)" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NSF", "grant_number": "AST-1211916" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stt1645", "primary_object": { "basename": "1209.1102v1.pdf", "url": "https://authors.library.caltech.edu/records/yk5g5-5f655/files/1209.1102v1.pdf" }, "related_objects": [ { "basename": "stt1645.pdf", "url": "https://authors.library.caltech.edu/records/yk5g5-5f655/files/stt1645.pdf" } ], "pub_year": "2013", "author_list": "Horesh, Assaf; Carpenter, John; et el." }, { "id": "https://authors.library.caltech.edu/records/1fsg2-3qs18", "eprint_id": 43639, "eprint_status": "archive", "datestamp": "2023-08-19 22:23:13", "lastmod": "2023-10-25 23:44:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-Jeffrey-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Vink\u00f3-J", "name": { "family": "Vinko", "given": "Jozsef" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Fox-Ori-D", "name": { "family": "Fox", "given": "Ori D." }, "orcid": "0000-0003-2238-1572" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Johansson-Joel", "name": { "family": "Johansson", "given": "Joel" }, "orcid": "0000-0001-5975-290X" }, { "id": "Perley-Daniel-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Tal-David", "name": { "family": "Tal", "given": "David" } }, { "id": "Wheeler-J-Craig", "name": { "family": "Wheeler", "given": "J. Craig" } }, { "id": "Amanullah-Rahman", "name": { "family": "Amanullah", "given": "Rahman" }, "orcid": "0000-0002-5559-9351" }, { "id": "Arcavi-Iair", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Bloom-Joshua-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Gal-Yam-Avishay", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Goobar-Ariel", "name": { "family": "Goobar", "given": "Ariel" }, "orcid": "0000-0002-4163-4996" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-Russ-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Lee-William-H", "name": { "family": "Lee", "given": "William H." } }, { "id": "Marion-G-H", "name": { "family": "Marion", "given": "G. H." } }, { "id": "Nugent-Peter-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Shivvers-Isaac", "name": { "family": "Shivvers", "given": "Isaac" }, "orcid": "0000-0003-3373-8047" } ] }, "title": "SN 2000cx and SN 2013bh: extremely rare, nearly twin Type Ia supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general\n supernovae: individual: SN 2000cx\n supernovae: individual: SN 2013bh", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nFirst published online: September 24, 2013. Accepted 2013 August 29. Received 2013 August 8; in original form 2013 July 12. \n\nWe would like to thank M. Ganeshalingam, P. Kelly and E. Ofek\nfor helpful discussions, J. Caldwell, S. Odewahn and S. Rostopchin for their assistance with some of the observations, as well as the PESSTO and CRTS collaborations for making some of their data on SN 2013bh publicly available. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universit\u00e4t\nM\u00fcnchen and Georg-August-Universit\u00e4t G\u00f6ttingen. The HET is\nnamed in honour of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics who fabricated several optics for the instrument but died before its completion. The LRS is a joint project of the HET partnership and the Instituto de Astronom\u00eda de la Universidad Nacional Aut\u03ccnoma de M\u00e9xico. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership\namong the California Institute of Technology, the University\nof California and the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the\nopportunity to conduct observations from this mountain. This work is partially based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We thank the RATIR instrument team and the staff of the\nObservatorio Astron\u03ccmico Nacional on Sierra San Pedro M\u00e1rtir. RATIR is a collaboration between the University of California, the Universidad Nacional Auton\u03ccma de M\u00e9xico, NASA Goddard Space Flight Center and Arizona State University, benefiting from the loan of an H2RG detector from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio\nAstron\u03ccmico Nacional on Sierra San Pedro M\u00e1rtir and the\noperation of both are funded by the partner institutions and through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G and NNX12AE66G, CONACyT grants INFR-2009-01-122785, UNAM\nPAPIIT grant IN113810 and a UC MEXUS-CONACyT grant. The\nNational Energy Research Scientific Computing Center, supported by the Office of Science of the US Department of Energy, provided staff, computational resources and data storage for this project. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the\nParticipating Institutions, the NSF and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. JV is supported by Hungarian OTKA Grant NN 107637. MMK acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. JCW's supernova group at UT Austin is supported by NSF Grant AST 11-09801. Some work on this paper by JCW was done in the hospitable clime of the Aspen Center for Physics that\nis supported by NSF Grant PHY-1066293. JSB acknowledges the\ngenerous support of a CDI grant (#0941742) from the National\nScience Foundation.\n\nPublished - MNRAS-2013-Silverman-1225-37.pdf
Submitted - 1307.3555v2.pdf
", "abstract": "The Type Ia supernova (SN Ia) SN 2000cx was one of the most peculiar transients ever discovered, with a rise to maximum brightness typical of a SN Ia, but a slower decline and a higher photospheric temperature. 13\u2009yr later SN 2013bh (also known as iPTF13abc), a near identical twin, was discovered and we obtained optical and near-infrared photometry and low-resolution optical spectroscopy from discovery until about 1 month past r-band maximum brightness. The spectra of both objects show iron-group elements [Co\u2009II, Ni II, Fe\u2009 II, Fe\u2009 III and high-velocity features (HVFs) of Ti\u2009 II], intermediate-mass elements (Si\u2009II, Si\u2009III and S\u2009 II) and separate normal velocity features (\u223c12 000\u2009km\u2009s^(\u22121)) and HVFs (\u223c24 000\u2009km\u2009s^(\u22121)) of Ca\u2009II. Persistent absorption from Fe\u2009III and Si\u2009III, along with the colour evolution, implies high blackbody temperatures for SNe 2013bh and 2000cx (\u223c12 000\u2009K). Both objects lack narrow Na\u2009I D absorption and exploded in the outskirts of their hosts, indicating that the SN environments were relatively free of interstellar or circumstellar material and may imply that the progenitors came from a relatively old and low-metallicity stellar population. Models of SN 2000cx, seemingly applicable to SN 2013bh, imply the production of up to \u223c1 M_\u2299 of ^(56)Ni and (4.3\u20135.5) \u00d7 10^(\u22123) M_\u2299 of fast-moving Ca ejecta.", "date": "2013-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "436", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1225-1237", "id_number": "CaltechAUTHORS:20140204-093249647", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140204-093249647", "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": "NNX09AH71G" }, { "agency": "NASA", "grant_number": "NNX09AT02G" }, { "agency": "NASA", "grant_number": "NNX10AI27G" }, { "agency": "NASA", "grant_number": "NNX12AE66G" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "INFR-2009-01-122785" }, { "agency": "UNAM-PAPIIT", "grant_number": "IN113810" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-1302771" }, { "agency": "Hungarian Scientific Research Fund (OTKA)", "grant_number": "NN 107637" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NSF", "grant_number": "AST-1109801" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "NSF", "grant_number": "CDI-0941742" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/stt1647", "primary_object": { "basename": "1307.3555v2.pdf", "url": "https://authors.library.caltech.edu/records/1fsg2-3qs18/files/1307.3555v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Silverman-1225-37.pdf", "url": "https://authors.library.caltech.edu/records/1fsg2-3qs18/files/MNRAS-2013-Silverman-1225-37.pdf" } ], "pub_year": "2013", "author_list": "Silverman, Jeffrey M.; Vinko, Jozsef; et el." }, { "id": "https://authors.library.caltech.edu/records/0dsb4-y5z45", "eprint_id": 42981, "eprint_status": "archive", "datestamp": "2023-08-19 22:17:16", "lastmod": "2023-10-25 23:11:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "Alessandra" }, "orcid": "0000-0001-8104-3536" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "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" } ] }, "title": "PTF 12gzk\u2014A Rapidly Declining, High-velocity Type Ic Radio Supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "radio continuum: general \u2013 radio continuum: stars \u2013 supernovae: general \u2013 supernovae: individual:\n(PTF12gzk) \u2013 X-rays: general", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2013 June 17; accepted 2013 September 15; published 2013 November 6.\n\nWe thank the VLA, Swift, and CARMA staff for promptly\nscheduling this target of opportunity. The National Radio Astronomy\nObservatory is a facility of the National Science Foundation\noperated under cooperative agreement by Associated\nUniversities, Inc. This work made use of data supplied by the\nUK Swift Science Data Centre at the University of Leicester.\nPTF is a fully automated, wide-field survey aimed at a systematic\nexploration of explosions and variable phenomena in\noptical wavelengths. The participating institutions are Caltech,\nColumbia University, Weizmann Institute of Science, Lawrence\nBerkeley Laboratory, Oxford, and University of California at\nBerkeley. The program is centered on a 12K\u00d78K, 7.8 deg2 CCD\narray (CFH12K) re-engineered for the 1.2 m Oschin Telescope\nat the Palomar Observatory by Caltech Optical Observatories.\nPhotometric follow-up is undertaken by the automated Palomar 1.5 m telescope. The research of A.G. is supported by grants\nfrom the ISF, BSF, GIF, and Minerva, the EU/FP7 via an ERC\ngrant, and the Kimmel award for innovative investigation.\n\nPublished - 0004-637X_778_1_63.pdf
Submitted - 1306.5755.pdf
", "abstract": "Only a few cases of Type Ic supernovae (SNe) with high-velocity ejecta (\u22650.2 c) have been discovered and studied. Here, we present our analysis of radio and X-ray observations of the Type Ic SN PTF 12gzk. The radio emission declined less than 10 days after explosion, suggesting SN ejecta expanding at high velocity (~0.3 c). The radio data also indicate that the density of the circumstellar material (CSM) around the supernova is lower by a factor of ~10 than the CSM around normal Type Ic SNe. PTF 12gzk may therefore be an intermediate event between a \"normal\" SN Ic and a gamma-ray-burst-SN-like event. Our observations of this rapidly declining radio SN at a distance of 58 Mpc demonstrates the potential to detect many additional radio SNe, given the new capabilities of the Very Large Array (improved sensitivity and dynamic scheduling), which are currently missed, leading to a biased view of radio SNe Ic. Early optical discovery followed by rapid radio observations would provide a full description of the ejecta velocity distribution and CSM densities around stripped massive star explosions as well as strong clues about the nature of their progenitor stars.", "date": "2013-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 63", "id_number": "CaltechAUTHORS:20131212-101237448", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131212-101237448", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Minerva" }, { "agency": "European Research Council (ERC)" }, { "agency": "Kimmel Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/778/1/63", "primary_object": { "basename": "0004-637X_778_1_63.pdf", "url": "https://authors.library.caltech.edu/records/0dsb4-y5z45/files/0004-637X_778_1_63.pdf" }, "related_objects": [ { "basename": "1306.5755.pdf", "url": "https://authors.library.caltech.edu/records/0dsb4-y5z45/files/1306.5755.pdf" } ], "pub_year": "2013", "author_list": "Horesh, Assaf; Kulkarni, Shrinivas R.; et el." }, { "id": "https://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" } ], "pub_year": "2013", "author_list": "Helou, George; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/y4sxj-rw633", "eprint_id": 42910, "eprint_status": "archive", "datestamp": "2023-08-19 22:04:54", "lastmod": "2023-10-25 23:08:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" } ] }, "title": "A statistical analysis of circumstellar material in Type Ia supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar, matter\n supernovae: general,\n distance scale", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 August 16. Received 2013 August 15; in original form 2013 July 12. First published online: September 26, 2013.\n\nMS acknowledges support from the Royal Society. Research leading to these results has received funding from the European Research Council (ERC) under the European Union's Seventh Framework Programme (FP7/2007- 2013)/ERC Grant agreement no [291222] (PI: Smartt). AG is supported by the EU/FP7 via an ERC grant, and by Minerva/ARCHES and Kimmel awards. SH is supported by a Minerva/ARCHES award. GL is supported by the Swedish Research Council through grant No. 623-2011-7117. Based on observations collected at the European Organisation for Astronomical Research in the Southern hemisphere, Chile, as part of PESSTO (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programme ID 188.D-3003, as well as observations\nmade with ESO Telescopes at the La Silla Paranal Observatory\nunder programme ID 090.D-0828(A) and 089.D-0647(A).\nBased on observations (GS-2012B-Q-86) 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 (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva\n(Argentina). Based in part on data from the 1.3 m telescope\noperated by the SMARTS consortium. 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\nFacilities Council. Observations were obtained with the\nSamuel Oschin Telescope at the Palomar Observatory as part of the Palomar Transient factory project, a scientific collaboration between the California Institute of Technology, Columbia Unversity, La Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford and the Weizmann Institute of Science. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de\nCanarias. This paper uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been\nprovided 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\nHigher Education Funding Council for England. The SDSS Web\nSite is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced\nStudy, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.\n\nPublished - MNRAS-2013-Maguire-222-40.pdf
Submitted - 1308.3899v1.pdf
", "abstract": "A key tracer of the elusive progenitor systems of Type Ia supernovae (SNe Ia) is the detection of narrow blueshifted time-varying Na\u2009i D absorption lines, interpreted as evidence of circumstellar material surrounding the progenitor system. The origin of this material is controversial, but the simplest explanation is that it results from previous mass-loss in a system containing a white dwarf and a non-degenerate companion star. We present new single-epoch intermediate-resolution spectra of 17 low-redshift SNe Ia taken with XShooter on the European Southern Observatory Very Large Telescope. Combining this sample with events from the literature, we confirm an excess (\u223c20 per\u2009cent) of SNe Ia displaying blueshifted narrow Na\u2009i D absorption features compared to redshifted Na\u2009i D features. The host galaxies of SNe Ia displaying blueshifted absorption profiles are skewed towards later-type galaxies, compared to SNe Ia that show no Na\u2009i D absorption and SNe Ia displaying blueshifted narrow Na\u2009i D absorption features have broader light curves. The strength of the Na\u2009i D absorption is stronger in SNe Ia displaying blueshifted Na\u2009i D absorption features than those without blueshifted features, and the strength of the blueshifted Na\u2009i D is correlated with the B \u2212 V colour of the SN at maximum light. This strongly suggests the absorbing material is local to the SN. In the context of the progenitor systems of SNe Ia, we discuss the significance of these findings and other recent observational evidence on the nature of SN Ia progenitors. We present a summary that suggests that there are at least two distinct populations of normal, cosmologically useful SNe Ia.", "date": "2013-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "436", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "222-240", "id_number": "CaltechAUTHORS:20131209-141742638", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131209-141742638", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "291222" }, { "agency": "MINERVA (Israel)" }, { "agency": "Kimmel Award" }, { "agency": "Swedish Research Council", "grant_number": "623-2011-7117" }, { "agency": "ARCHES Award" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1093/mnras/stt1586", "primary_object": { "basename": "1308.3899v1.pdf", "url": "https://authors.library.caltech.edu/records/y4sxj-rw633/files/1308.3899v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Maguire-222-40.pdf", "url": "https://authors.library.caltech.edu/records/y4sxj-rw633/files/MNRAS-2013-Maguire-222-40.pdf" } ], "pub_year": "2013", "author_list": "Maguire, K.; Nugent, P. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/q1d9v-1t250", "eprint_id": 42224, "eprint_status": "archive", "datestamp": "2023-08-19 21:57:38", "lastmod": "2023-10-25 15:45:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Singer-L-P", "name": { "family": "Singer", "given": "Leo P." }, "orcid": "0000-0001-9898-5597" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Brown-D-A", "name": { "family": "Brown", "given": "Duncan A." }, "orcid": "0000-0002-9180-5765" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "Alessandra" }, "orcid": "0000-0001-8104-3536" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." } }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Mulchaey-J-S", "name": { "family": "Mulchaey", "given": "John" } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom" } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "McEnery-J-E", "name": { "family": "McEnery", "given": "Julie" } }, { "id": "Rau-A", "name": { "family": "Rau", "given": "A." }, "orcid": "0000-0001-5990-6243" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" } ] }, "title": "Discovery and redshift of an optical afterglow in 71 deg^2: iPTF13bxl and GRB 130702A", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: individual (GRB 130702A)", "note": "\u00a9 2013 American Astronomical Society. Received 2013 July 20; accepted 2013 September 9; published 2013 October 7. We acknowledge A. Weinstein, A. Gal-Yam, R. Quimby, V.\nConnaughton, and the Fermi-GBM team for valuable discussions, S. Caudill, S. Tinyanont, D. Khatami for P200 observing, and the developers of the COSMOS package for Magellan data reduction. This research is supported by the National Science Foundation through a Graduate Research Fellowship for L.P.S., award PHY-0847611 for D.A.B., and NSF-CDI grant for J.S.B. M.M.K. acknowledges generous support from the Carnegie-Princeton Fellowship. M.M.K. and D.A.P. are supported by NASA through the Hubble Fellowship grants HST-HF-51293.01 and HST-HF-51296.01-A, awarded by the\nSpace Telescope Science Institute, which is operated by the\nAssociation of Universities for Research in Astronomy, Inc.,\nfor NASA, under contract NAS 5-26555. E.O.O. is the incumbent of the Arye Dissentshik career development chair and is supported by grants from the Israeli Ministry of Science and the I-CORE Program. D.A.B. is further supported by an RCSA Cottrell Scholar award. This research made use of Astropy (Robitaille et al. 2013, http://www.astropy.org), a community-developed core Python\npackage for Astronomy. The National Radio Astronomy\nObservatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - 2041-8205_776_2_L34.pdf
Submitted - 1307.5851v4.pdf
", "abstract": "We report the discovery of the optical afterglow of the \u03b3-ray burst (GRB) 130702A, identified upon searching 71 deg^2 surrounding the Fermi Gamma-ray Burst Monitor (GBM) localization. Discovered and characterized by the intermediate Palomar Transient Factory, iPTF13bxl is the first afterglow discovered solely based on a GBM localization. Real-time image subtraction, machine learning, human vetting, and rapid response multi-wavelength follow-up enabled us to quickly narrow a list of 27,004 optical transient candidates to a single afterglow-like source. Detection of a new, fading X-ray source by Swift and a radio counterpart by CARMA and the Very Large Array confirmed the association between iPTF13bxl and GRB 130702A. Spectroscopy with the Magellan and Palomar 200 inch telescopes showed the afterglow to be at a redshift of z = 0.145, placing GRB 130702A among the lowest redshift GRBs detected to date. The prompt \u03b3-ray energy release and afterglow luminosity are intermediate between typical cosmological GRBs and nearby sub-luminous events such as GRB 980425 and GRB 060218. The bright afterglow and emerging supernova offer an opportunity for extensive panchromatic follow-up. Our discovery of iPTF13bxl demonstrates the first observational proof-of-principle for ~10 Fermi-iPTF localizations annually. Furthermore, it represents an important step toward overcoming the challenges inherent in uncovering faint optical counterparts to comparably localized gravitational wave events in the Advanced LIGO and Virgo era.", "date": "2013-10-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "776", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L34", "id_number": "CaltechAUTHORS:20131104-131232227", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131104-131232227", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "PHY-0847611" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51293.01" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51296.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "I-CORE Program" }, { "agency": "Cottrell Scholar of Research Corporation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/776/2/L34", "primary_object": { "basename": "1307.5851v4.pdf", "url": "https://authors.library.caltech.edu/records/q1d9v-1t250/files/1307.5851v4.pdf" }, "related_objects": [ { "basename": "2041-8205_776_2_L34.pdf", "url": "https://authors.library.caltech.edu/records/q1d9v-1t250/files/2041-8205_776_2_L34.pdf" } ], "pub_year": "2013", "author_list": "Singer, Leo P.; Cenko, S. Bradley; et el." }, { "id": "https://authors.library.caltech.edu/records/cz9cf-jhx34", "eprint_id": 99423, "eprint_status": "archive", "datestamp": "2023-08-22 10:35:52", "lastmod": "2023-10-18 18:17:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric C." }, "orcid": "0000-0001-8018-5348" }, { "id": "Bhalerao-V-B", "name": { "family": "Bhalerao", "given": "Varun B." }, "orcid": "0000-0002-6112-7609" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "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": "Tracing the Orphan Stream to 55 kpc with RR Lyrae Stars", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure; stars: variables: RR Lyrae", "note": "\u00a9 2013 American Astronomical Society. Received 2013 June 30; accepted 2013 August 8; published 2013 September 23. B.S and J.G.C thank NSF grant AST-0908139 to\nJ.G.C for partial support, as do S.R.K (to NSF grant\nAST-1009987), and C.J.G (for a NASA grant). E.O.O\nis incumbent of the Arye Dissentshik career development\nchair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE Program of\nthe Planning and Budgeting Committee and The Israel\nScience Foundation (grant No 1829/12). We thank the\nstaff at the Palomar Hale telescope for help and support\nwith observations. We thank the anonymous referee for\nthe careful reading of our manuscript and the valuable\ncomments.\nThis article is based on observations obtained with the\nSamuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between\nthe California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley\nNational Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and\nthe Weizmann Institute of Science. It is also partially\nbased on observations obtained as part of the Intermediate Palomar Transient Factory project, a scientific collaboration among the California Institute of Technology,\nLos Alamos National Laboratory, the University of Wisconsin, Millwakee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the\nUniversity System of Taiwan, the Kavli Institute for the\nPhysics and Mathematics of the Universe, and the Inter-University Centre for Astronomy and Astrophysics.\n\nPublished - 0004-637X_776_1_26.pdf
Submitted - 1308.0857v1.pdf
", "abstract": "We report positions, velocities and metallicities of 50 ab-type RR Lyrae (RRab) stars observed in the\nvicinity of the Orphan stellar stream. Using about 30 RRab stars classified as being likely members\nof the Orphan stream, we study the metallicity and the spatial extent of the stream. We find that\nRRab stars in the Orphan stream have a wide range of metallicities, from -1.5 dex to -2.7 dex. The\naverage metallicity of the stream is -2.1 dex, identical to the value obtained by Newberg et al. (2010)\nusing blue horizontal branch stars. We find that the most distant parts of the stream (40-50 kpc from\nthe Sun) are about 0.3 dex more metal-poor than the closer parts (within ~ 30 kpc), suggesting a\npossible metallicity gradient along the stream's length. We have extended the previous studies and\nhave mapped the stream up to 55 kpc from the Sun. Even after a careful search, we did not identify\nany more distant RRab stars that could plausibly be members of the Orphan stream. If confirmed\nwith other tracers, this result would indicate a detection of the end of the leading arm of the stream.\nWe have compared the distances of Orphan stream RRab stars with the best-fit orbits obtained by\nNewberg et al. (2010). We find that model 6 of Newberg et al. (2010) cannot explain the distances\nof the most remote Orphan stream RRab stars, and conclude that the best fit to distances of Orphan\nstream RRab stars and to the local circular velocity is provided by potentials where the total mass\nof the Galaxy within 60 kpc is M_(60) ~ 2.7 x 10^(11) M_\u2299, or about 60% of the mass found by previous\nstudies. More extensive modelling that would consider non-spherical potentials and the possibility of\nmisalignment between the stream and the orbit, is highly encouraged.", "date": "2013-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "776", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 26", "id_number": "CaltechAUTHORS:20191023-154321407", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191023-154321407", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908139" }, { "agency": "NSF", "grant_number": "AST-1009987" }, { "agency": "NASA" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Planning and Budgeting Committee I-CORE Program" }, { "agency": "Israel Science Foundation", "grant_number": "1829/12" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/776/1/26", "primary_object": { "basename": "0004-637X_776_1_26.pdf", "url": "https://authors.library.caltech.edu/records/cz9cf-jhx34/files/0004-637X_776_1_26.pdf" }, "related_objects": [ { "basename": "1308.0857v1.pdf", "url": "https://authors.library.caltech.edu/records/cz9cf-jhx34/files/1308.0857v1.pdf" } ], "pub_year": "2013", "author_list": "Sesar, Branimir; Grillmair, Carl J.; et el." }, { "id": "https://authors.library.caltech.edu/records/mcrhe-btw70", "eprint_id": 41955, "eprint_status": "archive", "datestamp": "2023-08-19 21:30:10", "lastmod": "2023-10-25 14:57:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John" }, "orcid": "0000-0003-2251-0602" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Gelino-C-R", "name": { "family": "Gelino", "given": "Christopher R." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Discovery, Progenitor and Early Evolution of a Stripped Envelope Supernova iPTF13bvn", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: adaptive optics \u2013 shock waves \u2013 stars: Wolf\u2013Rayet \u2013 supernovae: individual\n(iPTF13bvn) \u2013 surveys", "note": "\u00a9 2013 The American Astronomical Society.\nReceived 4 July 2013, accepted for publication 15 August 2013. Published 30 August 2013.\n\nWe thank A. L. Piro for valuable discussions. We thank the\nfollowing people for co-operating with our target of opportunity\nor queue observations: M. Roth (Magellan), A. Hartuynan\n(TNG), J. Johnson (Keck), and J. Caldwell (HET). We thank A.\nHoward and H. Isaacson for HIRES data reduction. We thank R.\nCampbell, Hien Tran, and S. Tendulkar for helping with OSIRIS\nLGS-AO observation and data reduction. We thank P. Vreeswijk\nfor assisting with HST image registration. We thank J. Vinko,\nR. Foley, B. Kirshner, D. Perley, A. Corsi, and K. Mooley as\nproposal co-Is. We thank J. Swift, B. Montet, M. Bryan, R.\nJensen-Clem, D. Polishook, and S. Tinyanont for assisting with\nobservations.\nM.M.K. acknowledges generous support from the Hubble\nFellowship and Carnegie-Princeton Fellowship. J.M.S. is supported\nby an NSF Astronomy and Astrophysics Postdoctoral\nFellowship under award AST-1302771. N.D. acknowledges the\nHubble Fellowship. Research by A.G.Y. and his group was supported\nby grants from the ISF, BSF, GIF, Minerva, the EU/FP7\nvia an ERC grant and the Kimmel award. The research of J.C.W.\nis supported by NSF Grant AST 11-09801.\nThe National Energy Research Scientific Computing Center,\nsupported by the Office of Science of the U.S. Department of\nEnergy, provided staff, computational resources, and data storage\nfor this project. The Australia Telescope is funded by the\nCommonwealth of Australia for operation as a National Facility\nmanaged by CSIRO. This research has been supported by the\nAustralian Research Council through Super Science Fellowship\ngrant FS100100033. The Centre for All-sky Astrophysics is an\nAustralian Research Council Centre of Excellence, funded by\ngrant CE110001020. The National Radio Astronomy Observatory\nis a facility of the National Science Foundation operated\nunder cooperative agreement by Associated Universities, Inc.\nOngoing CARMA development and operations are supported\nby the National Science Foundation under a cooperative agreement,\nand by the CARMA partner universities.\n\nPublished - 2041-8205_775_1_L7.pdf
Submitted - 1307.1470v2.pdf
", "abstract": "The intermediate Palomar Transient Factory reports our discovery of a young supernova, iPTF13bvn, in the nearby galaxy, NGC 5806 (22.5 Mpc). Our spectral sequence in the optical and infrared suggests a Type Ib classification. We identify a blue progenitor candidate in deep pre-explosion imaging within a 2\u03c3 error circle of 80 mas (8.7 pc). The candidate has an M_B luminosity of \u22125.52 \u00b1 0.39 mag and a B\u2009\u2212\u2009I color of 0.25 \u00b1 0.25 mag. If confirmed by future observations, this would be the first direct detection for a progenitor of a Type Ib. Fitting a power law to the early light curve, we find an extrapolated explosion date around 0.6 days before our first detection. We see no evidence of shock cooling. The pre-explosion detection limits constrain the radius of the progenitor to be smaller than a few solar radii. iPTF13bvn is also detected in centimeter and millimeter wavelengths. Fitting a synchrotron self-absorption model to our radio data, we find a mass-loading parameter of 1.3\u00d710^(12) g cm^(\u22121). Assuming a wind velocity of 10^3 km s^(\u22121), we derive a progenitor mass-loss rate of 3 \u00d7 10^(\u22125)\u2009M\u2609 yr^(\u22121). Our observations, taken as a whole, are consistent with a Wolf\u2013Rayet progenitor of the supernova iPTF13bvn.", "date": "2013-09-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "775", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L7", "id_number": "CaltechAUTHORS:20131016-140041272", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131016-140041272", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NSF", "grant_number": "AST-1302771" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "MINERVA" }, { "agency": "European Research Council (ERC)" }, { "agency": "Kimmel Award" }, { "agency": "NSF", "grant_number": "AST 11-09801" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Commonwealth of Australia" }, { "agency": "Australian Research Council", "grant_number": "FS100100033" }, { "agency": "Australian Research Council", "grant_number": "CE110001020" }, { "agency": "CARMA Partner Universities" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/775/1/L7", "primary_object": { "basename": "1307.1470v2.pdf", "url": "https://authors.library.caltech.edu/records/mcrhe-btw70/files/1307.1470v2.pdf" }, "related_objects": [ { "basename": "2041-8205_775_1_L7.pdf", "url": "https://authors.library.caltech.edu/records/mcrhe-btw70/files/2041-8205_775_1_L7.pdf" } ], "pub_year": "2013", "author_list": "Cao, Yi; Horesh, Assaf; et el." }, { "id": "https://authors.library.caltech.edu/records/khv1s-xxr63", "eprint_id": 41215, "eprint_status": "archive", "datestamp": "2023-08-22 10:05:33", "lastmod": "2023-10-24 23:32:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bauer-J-M", "name": { "family": "Bauer", "given": "James M." } }, { "id": "Grav-T", "name": { "family": "Grav", "given": "Tommy" }, "orcid": "0000-0002-3379-0534" }, { "id": "Blauvelt-E-K", "name": { "family": "Blauvelt", "given": "Erin" } }, { "id": "Mainzer-A-K", "name": { "family": "Mainzer", "given": "A. K." } }, { "id": "Masiero-J-R", "name": { "family": "Masiero", "given": "Joseph R." }, "orcid": "0000-0003-2638-720X" }, { "id": "Stevenson-R-A", "name": { "family": "Stevenson", "given": "Rachel" } }, { "id": "Kramer-Emily-A", "name": { "family": "Kramer", "given": "Emily" }, "orcid": "0000-0003-0457-2519" }, { "id": "Fern\u00e1ndez-Y-R", "name": { "family": "Fernandez", "given": "Yan R." }, "orcid": "0000-0003-1156-9721" }, { "id": "Lisse-C-M", "name": { "family": "Lisse", "given": "C. M." }, "orcid": "0000-0002-9548-1526" }, { "id": "Cutri-R-M", "name": { "family": "Cutri", "given": "Roc M." }, "orcid": "0000-0002-0077-2305" }, { "id": "Weissman-P-R", "name": { "family": "Weissman", "given": "Paul R." } }, { "id": "Dailey-J-W", "name": { "family": "Dailey", "given": "John W." } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank J." }, "orcid": "0000-0002-8532-9395" }, { "id": "Walker-R-G", "name": { "family": "Walker", "given": "Russell" } }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "Adam" } }, { "id": "Nugent-C-R", "name": { "family": "Nugent", "given": "Carrie R." } }, { "id": "Meech-K-J", "name": { "family": "Meech", "given": "Karen J." }, "orcid": "0000-0002-2058-5670" }, { "id": "Lucas-A", "name": { "family": "Lucas", "given": "Andrew" } }, { "id": "Pearman-G", "name": { "family": "Pearman", "given": "George" } }, { "id": "Wilkins-A-N", "name": { "family": "Wilkins", "given": "Ashlee" } }, { "id": "Watkins-J-A", "name": { "family": "Watkins", "given": "Jessica" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "Edward L." }, "orcid": "0000-0001-5058-1593" } ] }, "title": "Centaurs and Scattered Disk Objects in the Thermal Infrared: Analysis of WISE/NEOWISE Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "comets: general; minor planets, asteroids: general", "note": "\u00a9 2013 American Astronomical Society. Received 2013 February 23; accepted 2013 June 5; published 2013 July 22. This publication makes use of data products from the\nWide-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 publication also makes use of data products from NEOWISE, which is a project of JPL/Caltech, funded by the Planetary Science Division of NASA. This material is based in part upon work supported by NASA through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. R. Stevenson is supported by the NASA Postdoctoral Program, and E. Kramer acknowledges her support through the JPL graduate internship program. Data were based in part on observations obtained at the Hale Telescope, Palomar Observatory, as part of a collaborative agreement between the California Institute of Technology, its divisions Caltech Optical Observatories, and the Jet Propulsion\nLaboratory (operated for NASA). Also, this work is based\nin part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Minist\u00e9rio da Ci\u00eancia, Tecnologia, e Inova\u00e7\u00e3o (MCTI) da Rep\u00fablica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU), with time allocated through NOAO. We thank the anonymous reviewer for the very helpful comments of manuscript drafts.\n\nPublished - 0004-637X_773_1_22.pdf
Submitted - 1306.1862.pdf
", "abstract": "The Wide-field Infrared Survey Explorer (WISE) observed 52 Centaurs and scattered disk objects (SDOs) in the thermal infrared, including 15 new discoveries. We present analyses of these observations to estimate sizes and mean optical albedos. We find mean albedos of 0.08 \u00b1 0.04 for the entire data set. Thermal fits yield average beaming parameters of 0.9 \u00b1 0.2 that are similar for both SDO and Centaur sub-classes. Biased cumulative size distributions yield size-frequency distribution power law indices of ~\u20131.7 \u00b1 0.3. The data also reveal a relation between albedo and color at the 3\u03c3 level. No significant relation between diameter and albedos is found.", "date": "2013-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "773", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 22", "id_number": "CaltechAUTHORS:20130910-135805155", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130910-135805155", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNA09DA77A" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "JPL Graduate Fellowship" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "WISE Team", "PTF Team" ] }, "doi": "10.1088/0004-637X/773/1/22", "primary_object": { "basename": "0004-637X_773_1_22.pdf", "url": "https://authors.library.caltech.edu/records/khv1s-xxr63/files/0004-637X_773_1_22.pdf" }, "related_objects": [ { "basename": "1306.1862.pdf", "url": "https://authors.library.caltech.edu/records/khv1s-xxr63/files/1306.1862.pdf" } ], "pub_year": "2013", "author_list": "Bauer, James M.; Grav, Tommy; et el." }, { "id": "https://authors.library.caltech.edu/records/x0m37-91v58", "eprint_id": 41072, "eprint_status": "archive", "datestamp": "2023-08-19 20:55:03", "lastmod": "2023-10-24 23:26:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "A." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Aharonson-O", "name": { "family": "Aharonson", "given": "O." }, "orcid": "0000-0001-9930-2495" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Polishook-D", "name": { "family": "Polishook", "given": "D." } }, { "id": "Bauer-J-M", "name": { "family": "Bauer", "given": "J. M." } }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "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" } ] }, "title": "Main-belt comets in the Palomar Transient Factory survey \u2013 I. The search for extendedness", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys \u2013 comets: general \u2013minor planets, asteroids: general", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 May 30. Received 2013 May 26; in original form 2013 January 8. First published online: June 24, 2013.\n\nWe thank the referee for useful comments. This work is based on data obtained with the 1.2-m Samuel Oschin Telescope at Palomar\nObservatory as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology,\nColumbia University, Las Cumbres Observatory, Lawrence Berkeley National Laboratory, the National Energy Research Scientific\nComputing Center, the University of Oxford and the Weizmann Institute of Science (WIS). EOO is incumbent of the Arye Dissentshik\ncareer development chair and is grateful for support via a grant from the Israeli Ministry of Science. OA and EOO wish to\nthank the Helen Kimmel Center for Planetary Science at WIS. SRK and his group are partially supported by NSF grant AST-0507734.\nDP is grateful to the AXA research fund.\n\nPublished - MNRAS-2013-Waszczak-3115-32.pdf
Submitted - 1305.7176v1.pdf
", "abstract": "Cometary activity in main-belt asteroids probes the ice content of these objects and provides clues to the history of volatiles in the inner Solar system. We search the Palomar Transient Factory survey to derive upper limits on the population size of active main-belt comets (MBCs). From data collected from 2009 March through 2012 July, we extracted \u223c2 million observations of \u223c220 thousand known main-belt objects (40 per cent of the known population, down to \u223c1-km diameter) and discovered 626 new objects in multinight linked detections. We formally quantify the 'extendedness' of a small-body observation, account for systematic variation in this metric (e.g. due to on-sky motion) and evaluate this method's robustness in identifying cometary activity using observations of 115 comets, including two known candidate MBCs and six newly discovered non-MBCs (two of which were originally designated as asteroids by other surveys). We demonstrate a 66 per cent detection efficiency with respect to the extendedness distribution of the 115 sampled comets, and a 100 per cent detection efficiency with respect to extendedness levels greater than or equal to those we observed in the known candidate MBCs P/2010 R2 (La Sagra) and P/2006 VW_(139). Using a log-constant prior, we infer 95 per cent confidence upper limits of 33 and 22 active MBCs (per million main-belt asteroids down to \u223c1-km diameter), for detection efficiencies of 66 and 100 per cent, respectively. In a follow-up to this morphological search, we will perform a photometric (disc-integrated brightening) search for MBCs.", "date": "2013-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "433", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3115-3132", "id_number": "CaltechAUTHORS:20130903-160604685", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130903-160604685", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science (Israel)" }, { "agency": "NSF", "grant_number": "AST-0507734" }, { "agency": "AXA Research Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "corp_creators": { "items": [ "PTF Team" ] }, "doi": "10.1093/mnras/stt951", "primary_object": { "basename": "1305.7176v1.pdf", "url": "https://authors.library.caltech.edu/records/x0m37-91v58/files/1305.7176v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Waszczak-3115-32.pdf", "url": "https://authors.library.caltech.edu/records/x0m37-91v58/files/MNRAS-2013-Waszczak-3115-32.pdf" } ], "pub_year": "2013", "author_list": "Waszczak, A.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/sernk-jkj94", "eprint_id": 96329, "eprint_status": "archive", "datestamp": "2023-08-19 20:59:16", "lastmod": "2023-10-20 21:04:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Pan-Yen-Chen", "name": { "family": "Pan", "given": "Yen-Chen" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "Isobel M." }, "orcid": "0000-0002-2960-978X" } ] }, "title": "Late-time Spectral Observations of the Strongly Interacting Type Ia Supernova PTF11kx", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2013. The American Astronomical Society.", "abstract": "PTF11kx was a Type Ia supernova (SN Ia) that showed time-variable absorption features, including saturated Ca II H and K lines that weakened and eventually went into emission. The strength of the emission component of H\u03b1 gradually increased, implying that the SN was undergoing significant interaction with its circumstellar medium (CSM). These features, and many others, were blueshifted slightly and showed a P-Cygni profile, likely indicating that the CSM was directly related to, and probably previously ejected by, the progenitor system itself. These and other observations led Dilday et al. to conclude that PTF11kx came from a symbiotic nova progenitor like RS Oph. In this work we extend the spectral coverage of PTF11kx to 124-680 rest-frame days past maximum brightness. The late-time spectra of PTF11kx are dominated by H\u03b1 emission (with widths of full width at half-maximum intensity \u22482000 km s-1), strong Ca II emission features (~10,000 km s-1 wide), and a blue \"quasi-continuum\" due to many overlapping narrow lines of Fe II. Emission from oxygen, He I, and Balmer lines higher than H\u03b1 is weak or completely absent at all epochs, leading to large observed H\u03b1/H\u03b2 intensity ratios. The H\u03b1 emission appears to increase in strength with time for ~1 yr, but it subsequently decreases significantly along with the Ca II emission. Our latest spectrum also indicates the possibility of newly formed dust in the system as evidenced by a slight decrease in the red wing of H\u03b1. During the same epochs, multiple narrow emission features from the CSM temporally vary in strength. The weakening of the H\u03b1 and Ca II emission at late times is possible evidence that the SN ejecta have overtaken the majority of the CSM and agrees with models of other strongly interacting SNe Ia. The varying narrow emission features, on the other hand, may indicate that the CSM is clumpy or consists of multiple thin shells.", "date": "2013-08", "date_type": "published", "publication": "Astrophysical Journal", "volume": "772", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. 125", "id_number": "CaltechAUTHORS:20190612-132447529", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190612-132447529", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-637X/772/2/125", "pub_year": "2013", "author_list": "Silverman, Jeffrey M.; Nugent, Peter E.; et el." }, { "id": "https://authors.library.caltech.edu/records/0jf53-19459", "eprint_id": 41144, "eprint_status": "archive", "datestamp": "2023-08-22 09:45:35", "lastmod": "2023-10-24 23:29:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter; supernovae: general; supernovae: individual (SN 1997cy, SN 1999E, SN 2002ic, SN 2005gj, SN 2008J, SN 2008cg, SN 2011jb, CSS120327:110520-015205, PTF11kx, PTF10htz, PTF10iuf, PTF10yni, PTF11dsb, PTF11hzx, PTF12efc)", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2013 March 29; accepted 2013 April 26; published 2013 June 14.\n\nWe thank K. Alatalo, T. Barlow, E. Bellm, B. Cobb, A.\nCucchiara, M. Ganeshalingam, Y. Green, M. Hidas, L. Kewley,\nN. Konidaris, S. Lazarevic, N. Lee, D. Levitan, M. McCourt,\nK. Mooley, R. Mostardi, D. Perley, A. G. Riess, B. Sesar, R.\nStreet, T. Treu, V. Viscomi, and X. Wang for their assistance\nwith some of the observations and data reduction; B. Dilday,\nO. Fox, and L. Wang for helpful discussions; and D. Balam,\nM. Stritzinger, J. Vinko, and J. C. Wheeler for providing\nunpublished spectra of possible SNe Ia-CSM. We are grateful\nto the staffs at the Isaac Newton Group of Telescopes and the\nLick, Keck, Palomar, and Kitt Peak National Observatories for\ntheir support. Some of the data presented herein were obtained\nat the W.M. Keck Observatory, which is operated as a scientific\npartnership among the California Institute of Technology, the\nUniversity of California, and the National Aeronautics and\nSpace Administration (NASA); the observatory was made\npossible by the generous financial support of the W. M. Keck\nFoundation. The authors recognize and acknowledge the very\nsignificant cultural role and reverence that the summit of Mauna\nKea has always had within the indigenous Hawaiian community;\nwe are most fortunate to have the opportunity to conduct\nobservations from this mountain. 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 NASA. Funding for SDSSIII\nhas been provided by the Alfred P. Sloan Foundation, the\nParticipating Institutions, the National Science Foundation, and\nthe U.S. Department of Energy Office of Science. The SDSSIII\nWeb site is http://www.sdss3.org/. Supernova research by\nA.V.F.'s group at UC Berkeley is supported by Gary and Cynthia\nBengier, the Richard and Rhoda Goldman Fund, the Christopher\nR. Redlich Fund, the TABASGO Foundation, and NSF grants\nAST-0908886 and AST-1211916. Work by A.G.-Y. and his\ngroup is supported by grants from the ISF, BSF, GIF, Minerva,\nan FP7/ERC grant, and the Helen and Martin Kimmel Award\nfor Innovative Investigation. M.M.K. acknowledges generous\nsupport from a Hubble Fellowship and a Carnegie-Princeton\nFellowship.\n\nPublished - 0067-0049_207_1_3.pdf
Submitted - 1304.0763v1.pdf
", "abstract": "Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the best-studied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogen-rich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by H\u03b1 emission (with widths of ~2000 km s^(\u20131)) and exhibit large H\u03b1/H\u03b2 intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He I emission. They also show possible evidence of dust formation through a decrease in the red wing of H\u03b1 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na I D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be \u201321.3 mag \u2264 M_R \u2264 \u201319 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.", "date": "2013-07", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "207", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 3", "id_number": "CaltechAUTHORS:20130906-132112928", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130906-132112928", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Minerva" }, { "agency": "European Research Council (ERC)" }, { "agency": "Kimmel Award" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0067-0049/207/1/3", "primary_object": { "basename": "0067-0049_207_1_3.pdf", "url": "https://authors.library.caltech.edu/records/0jf53-19459/files/0067-0049_207_1_3.pdf" }, "related_objects": [ { "basename": "1304.0763v1.pdf", "url": "https://authors.library.caltech.edu/records/0jf53-19459/files/1304.0763v1.pdf" } ], "pub_year": "2013", "author_list": "Silverman, Jeffrey M.; Cao, Yi; et el." }, { "id": "https://authors.library.caltech.edu/records/e5k1f-7hq76", "eprint_id": 39449, "eprint_status": "archive", "datestamp": "2023-08-22 09:36:06", "lastmod": "2023-10-24 16:49:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "Alessandra" }, "orcid": "0000-0001-8104-3536" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John" }, "orcid": "0000-0003-2251-0602" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "G." }, "orcid": "0000-0002-7083-4049" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Discovery of a Cosmological, Relativistic Outburst via its Rapidly Fading Optical Emission", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: general; stars: flare; supernovae: general", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2013 January 20; accepted 2013 April 15; published 2013 May 14. \n\nWe thank David Levitan and Kunal Mooley for obtaining observations used in this work, and John Tomsick for valuable comments on the manuscript. We are grateful to the following IPN team members for sharing their data: K. Hurley, I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin,W. Boynton, C. Fellows, K. Harshman, R. Starr, S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, D. Svinkin, A. von Kienlin, X. Zhang, K. Yamaoka, T. Takahashi, M. Ohno, Y. Hanabata, Y. Fukazawa,M. Tashiro, Y. Terada, T. Murakami, K. Makishima, T. Cline, S. Barthelmy, J.Cummings,N.Gehrels, H. Krimm, D. Palmer, J. Goldsten, V. Connaughton, M. S. Briggs, and C. Meegan. \n\nA.V.F. and his group acknowledge generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, NASA/Swift grants NNX10AI21G and NNX12AD73G, the TABASGO Foundation, and NSF grant AST-1211916. A.C. acknowledges support from LIGO, which was constructed by the California Institute of Technology and theMassachusetts Institute of Technology with funding from the NSF and operates under cooperative agreement PHY-0757058. D.A.P. is supported by NASA through Hubble Fellowship grantHST-HF-51296.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Research by A.G.Y. and his team is supported by grants from the ISF, BSF, GIF, the EU/FP7 via an ERC grant, and a Kimmel Award. P.J.G. acknowledges support from Caltech during his 2011 sabbatical stay. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science. A.A.M. is supported by the NSF Graduate Research Fellowship Program. J.S.B. acknowledges NSF grant CDI-0941742. D.P. is grateful for the AXA research fund. A.S. is supported by a Minerva Fellowship. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. Observations were obtained with the Samuel Oschin telescope and the Hale telescope at Palomar Observatory 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 theWeizmann Institute of Science. The National Energy Research Scientific Computing Center, supported by the Office of Science of the U.S. Department of Energy, provided staff, computational resources, and data storage for this project. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the NSF. Ongoing CARMA development and operations are supported by the NSF under a cooperative agreement, and by the CARMA partner universities. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck\nFoundation. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project is further supported by NASA/Swift Guest Investigator grant NNX08AN84G. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. It 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 NASA. In addition, we have utilized the SIMBAD database, operated at CDS, Strasbourg, France. \n\nFacilities: PO:1.2m (PTF), Hale (WIRC), Keck:I (LRIS), Magellan:Baade (IMACS), FLWO:2MASS (PAIRITEL), VLA, CARMA, Fermi (GBM), Swift (BAT, XRT)\n\nPublished - 0004-637X_769_2_130.pdf
Submitted - 1304.4236.pdf
", "abstract": "We report the discovery by the Palomar Transient Factory (PTF) of the transient source PTF11agg, which is distinguished by three primary characteristics: (1) bright (R_peak = 18.3 mag), rapidly fading (\u0394R = 4 mag in \u0394t = 2 days) optical transient emission; (2) a faint (R = 26.2 \u00b1 0.2 mag), blue (g' \u2013 R = 0.17 \u00b1 0.29 mag) quiescent optical counterpart; and (3) an associated year-long, scintillating radio transient. We argue that these observed properties are inconsistent with any known class of Galactic transients (flare stars, X-ray binaries, dwarf novae), and instead suggest a cosmological origin. The detection of incoherent radio emission at such distances implies a large emitting region, from which we infer the presence of relativistic ejecta. The observed properties are all consistent with the population of long-duration gamma-ray bursts (GRBs), marking the first time such an outburst has been discovered in the distant universe independent of a high-energy trigger. We searched for possible high-energy counterparts to PTF11agg, but found no evidence for associated prompt emission. We therefore consider three possible scenarios to account for a GRB-like afterglow without a high-energy counterpart: an \"untriggered\" GRB (lack of satellite coverage), an \"orphan\" afterglow (viewing-angle effects), and a \"dirty fireball\" (suppressed high-energy emission). The observed optical and radio light curves appear inconsistent with even the most basic predictions for off-axis afterglow models. The simplest explanation, then, is that PTF11agg is a normal, on-axis long-duration GRB for which the associated high-energy emission was simply missed. However, we have calculated the likelihood of such a serendipitous discovery by PTF and find that it is quite small (\u22482.6%). While not definitive, we nonetheless speculate that PTF11agg may represent a new, more common (>4 times the on-axis GRB rate at 90% confidence) class of relativistic outbursts lacking associated high-energy emission. If so, such sources will be uncovered in large numbers by future wide-field optical and radio transient surveys.", "date": "2013-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "769", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 130", "id_number": "CaltechAUTHORS:20130718-112522810", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130718-112522810", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX12AD73G" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "LIGO" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51296.01-A" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "European Research Council (ERC)" }, { "agency": "Kimmel Award" }, { "agency": "Caltech" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "AXA research fund" }, { "agency": "Minerva Fellowship" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "LIGO" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/769/2/130", "primary_object": { "basename": "0004-637X_769_2_130.pdf", "url": "https://authors.library.caltech.edu/records/e5k1f-7hq76/files/0004-637X_769_2_130.pdf" }, "related_objects": [ { "basename": "1304.4236.pdf", "url": "https://authors.library.caltech.edu/records/e5k1f-7hq76/files/1304.4236.pdf" } ], "pub_year": "2013", "author_list": "Cenko, S. Bradley; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/s8740-5xz03", "eprint_id": 42334, "eprint_status": "archive", "datestamp": "2023-08-22 09:33:28", "lastmod": "2023-10-25 15:50:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Terziev-E", "name": { "family": "Terziev", "given": "Emil" } }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Baranec-C", "name": { "family": "Baranec", "given": "Christoph" }, "orcid": "0000-0002-1917-9157" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "Burse-M-P", "name": { "family": "Burse", "given": "Mahesh P." } }, { "id": "Chorida-P", "name": { "family": "Chorida", "given": "Pravin" } }, { "id": "Das-H-K", "name": { "family": "Das", "given": "H. K." } }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." } }, { "id": "Kraus-A-L", "name": { "family": "Kraus", "given": "Adam L." }, "orcid": "0000-0001-9811-568X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran" }, "orcid": "0000-0002-6786-8774" }, { "id": "Punnadi-S", "name": { "family": "Punnadi", "given": "Sujit" } }, { "id": "Ramaprakash-A-N", "name": { "family": "Ramaprakash", "given": "A. N." } }, { "id": "Riddle-R-L", "name": { "family": "Riddle", "given": "Reed L." }, "orcid": "0000-0002-0387-370X" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Tendulkar-S-P", "name": { "family": "Tendullkar", "given": "Shriharsh P." }, "orcid": "0000-0003-2548-2926" } ] }, "title": "Millions of Multiples: Detecting and Characterizing Close-separation Binary Systems in Synoptic Sky Surveys", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; methods: data analysis; stars: statistics; surveys; techniques: image processing", "note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2012 October 15; accepted 2013 April 16; published 2013 May 30.\n\nWe thank Yanqin Wu for very useful discussions, and the\nPalomar Observatory staff for their superb support of Robo-\nAO and PTF operations. E.T. participated in the Summer Undergraduate Research Program (SURP) at the Dunlap Institute for Astronomy & Astrophysics, University of Toronto. N.M.L. is a Dunlap Fellow at the Dunlap Institute for Astronomy & Astrophysics, University of Toronto. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and by the National Science Foundation under Grant Nos. AST-0906060 and AST-0960343, by a grant from the Mt. Cuba Astronomical Foundation, and by a gift from Samuel Oschin. Observations were obtained with the Samuel Oschin Telescope at the Palomar Observatory 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. A.L.K. was supported by NASA through Hubble Fellowship grant 51257.01 awarded by STScI, which is operated by AURA, Inc., for ANSA, under contract NAS 5-26555.\n\nPublished - 0067-0049_206_2_18.pdf
Submitted - 1210.4550v1.pdf
", "abstract": "The direct detection of binary systems in wide-field surveys is limited by the size of the stars' point-spread functions (PSFs). A search for elongated objects can find closer companions, but is limited by the precision to which the PSF shape can be calibrated for individual stars. Based on a technique from weak-lensing analysis, we have developed the BinaryFinder algorithm to search for close binaries by using precision measurements of PSF ellipticity across wide-field survey images. We show that the algorithm is capable of reliably detecting binary systems down to \u22481/5 of the seeing limit, and can directly measure the systems' position angles, separations, and contrast ratios. To verify the algorithm's performance we evaluated 100,000 objects in Palomar Transient Factory (PTF) wide-field-survey data for signs of binarity, and then used the Robo-AO robotic laser adaptive optics system to verify the parameters of 44 high-confidence targets. We show that BinaryFinder correctly predicts the presence of close companions with a <11% false-positive rate, measures the detected binaries' position angles within 1\u00b0 to 4\u00b0 (depending on signal-to-noise ratio and separation), and separations within 25%, and weakly constrains their contrast ratios. When applied to the full PTF data set, we estimate that BinaryFinder will discover and characterize ~450,000 physically associated binary systems with separations <2 arcsec and magnitudes brighter than m_R = 18. New wide-field synoptic surveys with high sensitivity and sub-arcsecond angular resolution, such as LSST, will allow BinaryFinder to reliably detect millions of very faint binary systems with separations as small as 0.1 arcsec.", "date": "2013-06", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "206", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 18", "id_number": "CaltechAUTHORS:20131108-093537237", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131108-093537237", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0906060" }, { "agency": "NSF", "grant_number": "AST-0960343" }, { "agency": "Mt. Cuba Astronomical Foundation" }, { "agency": "Samuel Oschin" }, { "agency": "NASA Hubble Fellowship", "grant_number": "51257.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0067-0049/206/2/18", "primary_object": { "basename": "0067-0049_206_2_18.pdf", "url": "https://authors.library.caltech.edu/records/s8740-5xz03/files/0067-0049_206_2_18.pdf" }, "related_objects": [ { "basename": "1210.4550v1.pdf", "url": "https://authors.library.caltech.edu/records/s8740-5xz03/files/1210.4550v1.pdf" } ], "pub_year": "2013", "author_list": "Terziev, Emil; Law, Nicholas M.; et el." }, { "id": "https://authors.library.caltech.edu/records/xwad2-0t183", "eprint_id": 38784, "eprint_status": "archive", "datestamp": "2023-08-22 09:18:22", "lastmod": "2023-10-23 23:28:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Findeisen-K", "name": { "family": "Findeisen", "given": "Krzysztof" } }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne" } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran" }, "orcid": "0000-0002-6786-8774" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Disk-related Bursts and Fades in Young Stars", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: late-type; stars: pre-main sequence; stars: solar-type; stars: variables: T Tauri, Herbig Ae/Be", "note": "\u00a9 2013 American Astronomical Society. Received 2012 December 21; accepted 2013 March 13; published 2013 April 17. We thank Asaaf Horesh, Kunal Mooley, and Yi Cao for\nacquiring a spectrum of FHO 7 for us, Gregory Herczeg for\nreducing the HYDRA and Norris spectroscopic data, Susan\nTokarz for reducing the Hectospec data, and Evan Kirby for\nhelping us with the DEIMOS pipeline. We thank the anonymous\nreferee for several comments that improved our presentation. We also thank John Carpenter and Nairn Baliber for much helpful discussion and suggestions for tests to run, and Luisa Rebull for providing us with a copy of the Spitzer data. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific\npartnership among the California Institute of Technology,\nthe 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.\nFacilities: PO:1.2m (P48 Survey Camera), Keck:II\n(DEIMOS), MMT (Hectospec), WIYN (HYDRA), Hale\n(Norris)\n\nPublished - 0004-637X_768_1_93.pdf
", "abstract": "We present first results from a new, multiyear, time domain survey of young stars in the North America Nebula complex using the Palomar Transient Factory. Our survey is providing an unprecedented view of aperiodic variability in young stars on timescales of days to years. The analyzed sample covers R_(PTF) \u2248 13.5-18 and spans a range of mid-infrared color, with larger-amplitude optical variables (exceeding 0.4 mag root mean squared) more likely to have mid-infrared evidence for circumstellar material. This paper characterizes infrared excess stars with distinct bursts above or fades below a baseline of lower-level variability, identifying 41 examples. The light curves exhibit a remarkable diversity of amplitudes, timescales, and morphologies, with a continuum of behaviors that cannot be classified into distinct groups. Among the bursters, we identify three particularly promising sources that may represent theoretically predicted short-timescale accretion instabilities. Finally, we find that fading behavior is approximately twice as common as bursting behavior on timescales of days to years, although the bursting and fading duty cycle for individual objects often varies from year to year.", "date": "2013-05-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "768", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 93", "id_number": "CaltechAUTHORS:20130604-132233198", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130604-132233198", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Smithsonian Astrophysical Observatory" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/768/1/93", "primary_object": { "basename": "0004-637X_768_1_93.pdf", "url": "https://authors.library.caltech.edu/records/xwad2-0t183/files/0004-637X_768_1_93.pdf" }, "pub_year": "2013", "author_list": "Findeisen, Krzysztof; Hillenbrand, Lynne; et el." }, { "id": "https://authors.library.caltech.edu/records/qkhy8-1n769", "eprint_id": 38545, "eprint_status": "archive", "datestamp": "2023-08-22 09:08:42", "lastmod": "2023-10-23 20:33:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tang-Sumin", "name": { "family": "Tang", "given": "Sumin" }, "orcid": "0000-0002-6225-8918" }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter" }, "orcid": "0000-0002-3389-0586" }, { "id": "Bellm-E-C", "name": { "family": "Bellm", "given": "Eric" }, "orcid": "0000-0001-8018-5348" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Masci-F-J", "name": { "family": "Masci", "given": "Frank" }, "orcid": "0000-0002-8532-9395" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "R Coronae Borealis Stars in M31 from the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (M31); stars: AGB and post-AGB; stars: carbon; stars: variables: general; supergiants", "note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2013 March 7; accepted 2013 March 15; published 2013 April 1.\n\nWe thank Geoff Clayton for pointing out the similarities between PTF-M31-RCB-1 (2) and RY Sgr (V854 Cen), providing\nspectra of RY Sgr and V854 Cen, and many helpful discussions. We thank the anonymous referee for comments that have helped to improve this Letter. We thank Sagi Ben-Ami and Dong Xu for reducing two candidate spectra, and Adam Miller for helpful discussion. This work was supported by the National Science Foundation under grants PHY 11-25915 and AST 11-09174. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science.\nFacilities: PO:1.2m (PTF), Hale (DBSP), Keck:II (DEIMOS)\n\nPublished - 2041-8205_767_2_L23.pdf
", "abstract": "We report the discovery of R Coronae Borealis (RCB) stars in the Andromeda galaxy (M31) using the Palomar Transient Factory (PTF). RCB stars are rare hydrogen-deficient, carbon-rich supergiant variables, most likely the merger products of two white dwarfs. These new RCBs, including two confirmed ones and two candidates, are the first to be found beyond the Milky Way and the Magellanic Clouds. All of M31 RCBs showed >1.5 mag irregular declines over timescales of weeks to months. Due to the limiting magnitude of our data (R \u2248 21-22 mag), these RCB stars have R \u2248 19.5-20.5 mag at maximum light, corresponding to M_R = \u20134 to \u20135, making them some of the most luminous RCBs known. Spectra of two objects show that they are warm RCBs, similar to the Milky Way RCBs RY Sgr and V854 Cen. We consider these results, derived from a pilot study of M31 variables, as an important proof-of-concept for the study of rare bright variables in nearby galaxies with the PTF or other synoptic surveys.", "date": "2013-04-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "767", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L23", "id_number": "CaltechAUTHORS:20130516-133502401", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130516-133502401", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY 11-25915" }, { "agency": "NSF", "grant_number": "AST 11-09174" }, { "agency": "Ministry of Science (Israel)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/767/2/L23", "primary_object": { "basename": "2041-8205_767_2_L23.pdf", "url": "https://authors.library.caltech.edu/records/qkhy8-1n769/files/2041-8205_767_2_L23.pdf" }, "pub_year": "2013", "author_list": "Tang, Sumin; Cao, Yi; et el." }, { "id": "https://authors.library.caltech.edu/records/ca835-ttb11", "eprint_id": 38921, "eprint_status": "archive", "datestamp": "2023-08-22 09:04:42", "lastmod": "2023-10-24 14:51:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } }, { "id": "Kupfer-T", "name": { "family": "Kupfer", "given": "Thomas" }, "orcid": "0000-0002-6540-1484" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "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" }, { "id": "Simonian-G-V", "name": { "family": "Simonian", "given": "Gregory V." } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "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": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason" }, "orcid": "0000-0001-7291-0087" } ] }, "title": "Five new outbursting AM CVn systems discovered by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion discs; binaries: close; stars: individual: PTF1 J043517.73+ 002940.7; stars: individual: PTF1 J094329.59+102957.6; novae, cataclysmic variables; white dwarfs", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2012 December 18. Received 2012 December 14; in original form 2012 September 18.\n\nFirst published online: February 1, 2013.\nWe thank Sagi Ben-Ami, Yi Cao, Brad Cenko, Avishay Gal-Yam,\nAssaf Horesh, Mansi Kasliwal, Thomas Matheson, Kunal Mooley\nand Robert Quimby for help in obtaining observations and reducing data. We thank Kevin Rykoski and Carolyn Heffner at the Palomar Observatory for developing the fast cadence mode on the LFC instrument. Part of this work was performed by TAP while at the Aspen Center for Physics, which is supported by NSF Grant #1066293. PJG thanks the California Institute of Technology for its hospitality during his sabbatical stay. Observations obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory,\nthe Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics\nand Space Administration. The Observatory was made possible\nby the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Based in part on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by\nDenmark, Finland, Iceland, Norway and Sweden, in the Spanish\nObservatorio del Roque de los Muchachos 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 research has made use of NASA's Astrophysics Data System.\n\nPublished - MNRAS-2013-Levitan-996-1007.pdf
", "abstract": "We present five new outbursting AM CVn systems and one candidate discovered as part of an ongoing search for such systems using the Palomar Transient Factory (PTF). This is the first large-area, systematic search for AM CVn systems using only large-amplitude photometric variability to select candidates. Three of the confirmed systems and the candidate system were discovered as part of the PTF transient search. Two systems were found as part of a search for outbursts through the PTF photometric data base. We discuss the observed characteristics of each of these systems, including the orbital periods of two systems. We also consider the position of these systems, selected in a colour-independent survey, in colour\u2013colour space and compare to systems selected solely by their colours. We find that the colours of our newly discovered systems do not differ significantly from those of previously known systems, but significant errors preclude a definitive answer.", "date": "2013-04-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "430", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "996-1007", "id_number": "CaltechAUTHORS:20130612-134000701", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-134000701", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/sts672", "primary_object": { "basename": "MNRAS-2013-Levitan-996-1007.pdf", "url": "https://authors.library.caltech.edu/records/ca835-ttb11/files/MNRAS-2013-Levitan-996-1007.pdf" }, "pub_year": "2013", "author_list": "Levitan, David; Kupfer, Thomas; et el." }, { "id": "https://authors.library.caltech.edu/records/d235g-3dp97", "eprint_id": 39067, "eprint_status": "archive", "datestamp": "2023-08-19 18:56:55", "lastmod": "2023-10-24 16:21:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hachinger-S", "name": { "family": "Hachinger", "given": "S." } }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Baron-E", "name": { "family": "Baron", "given": "E." } }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "J." }, "orcid": "0000-0001-5703-2108" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Bersier-D", "name": { "family": "Bersier", "given": "D." } }, { "id": "Dilday-B", "name": { "family": "Dilday", "given": "B." } }, { "id": "James-P-A", "name": { "family": "James", "given": "P. A." } }, { "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" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Parrent-J-T", "name": { "family": "Parrent", "given": "J." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Walker-E-S", "name": { "family": "Walker", "given": "E. S." } } ] }, "title": "The UV/optical spectra of the Type Ia supernova SN 2010jn: a bright supernova with outer layers rich in iron-group elements", "ispublished": "pub", "full_text_status": "public", "keywords": "radiative transfer\n techniques: spectroscopic\n supernovae: general\n super-novae: individual: SN\u20092010jn", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: January 9, 2013. Accepted 2012 November 26. Received 2012 November 26; in original form 2012 August 6. This work has been made possible by the participation of more than 10 000 volunteers in the 'Galaxy Zoo Supernovae' project, http://supernova.galaxyzoo.org/authors. It is based on observations made with the NASA/ESA HST, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The observations are associated with programme 12298. PAM and SH acknowledge support by the programme ASI-INAF\nI/009/10/0. MS acknowledges support from the Royal Society, and AG acknowledges support by the ISF, a Minerva ARCHES award, and the Lord Sieff of Brimpton Fund. MMK acknowledges generous support from the Hubble Fellowship and the Carnegie-Princeton Fellowship. We have used observations from the LT, operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto\nde Astrof\u00edsica de Canarias with financial support from the\nUK Science and Technology Facilities Council. Spectroscopic observations in the optical have been taken at the Gemini Observatory under programme ID GN-2010B-Q-13, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnolog\u00eda e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva (Argentina). Finally, an optical\nspectrum has been taken at the WHT, 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\u00b4\u0131sica de Canarias. We have used data from the NASA/IPAC Extragalactic Database (NED; http://nedwww.ipac.caltech.edu, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration). For data handling, we have made use of various software (as mentioned in the text) including IRAF. IRAF \u2013 Image Reduction and Analysis Facility\n(http://iraf.noao.edu) \u2013 is an astronomical data reduction software distributed by the National Optical Astronomy Observatory (NOAO; operated by AURA, Inc., under contract with the National Science Foundation).\n\nPublished - MNRAS-2013-Hachinger-2228-48.pdf
", "abstract": "Radiative transfer studies of Type Ia supernovae (SNe\u2009Ia) hold the promise of constraining both the density profile of the SN ejecta and its stratification by element abundance which, in turn, may discriminate between different explosion mechanisms and progenitor classes. Here we analyse the Type Ia SN\u20092010jn (PTF10ygu) in detail, presenting and evaluating near-ultraviolet (near-UV) spectra from the Hubble Space Telescope and ground-based optical spectra and light curves. SN\u20092010jn was discovered by the Palomar Transient Factory (PTF) 15\u2009d before maximum light, allowing us to secure a time series of four near-UV spectra at epochs from \u221210.5 to +4.8\u2009d relative to B-band maximum. The photospheric near-UV spectra are excellent diagnostics of the iron-group abundances in the outer layers of the ejecta, particularly those at very early times. Using the method of 'Abundance Tomography' we derive iron-group abundances in SN\u20092010jn with a precision better than in any previously studied SN\u2009Ia. Optimum fits to the data can be obtained if burned material is present even at high velocities, including significant mass fractions of iron-group elements. This is consistent with the slow decline rate (or high 'stretch') of the light curve of SN\u20092010jn, and consistent with the results of delayed-detonation models. Early-phase UV spectra and detailed time-dependent series of further SNe\u2009Ia offer a promising probe of the nature of the SN\u2009Ia mechanism.", "date": "2013-03-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "429", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2228-2248", "id_number": "CaltechAUTHORS:20130625-091333437", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130625-091333437", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Royal Society" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "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": "Minist\u00e9rio da Ci\u00eancia,Tecnolog\u00eda e Inova\u00e7\u00e3o" }, { "agency": "Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF" }, { "agency": "Israel Science Foundation" }, { "agency": "MINERVA (Israel)" }, { "agency": "Lord Sieff of Brimpton Fund" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "ARCHES Award" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1093/mnras/sts492", "primary_object": { "basename": "MNRAS-2013-Hachinger-2228-48.pdf", "url": "https://authors.library.caltech.edu/records/d235g-3dp97/files/MNRAS-2013-Hachinger-2228-48.pdf" }, "pub_year": "2013", "author_list": "Hachinger, S.; Mazzali, P. A.; et el." }, { "id": "https://authors.library.caltech.edu/records/y0y6s-5g358", "eprint_id": 33541, "eprint_status": "archive", "datestamp": "2023-08-22 08:44:55", "lastmod": "2023-10-18 20:24:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Covey-K-R", "name": { "family": "Covey", "given": "Kevin R." }, "orcid": "0000-0001-6914-7797" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Muirhead-P-S", "name": { "family": "Muirhead", "given": "Philip" }, "orcid": "0000-0002-0638-8822" }, { "id": "Fischer-W-J", "name": { "family": "Fischer", "given": "William" }, "orcid": "0000-0002-3747-2496" }, { "id": "Crepp-J-R", "name": { "family": "Crepp", "given": "Justin R." }, "orcid": "0000-0003-0800-0593" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" } ] }, "title": "Highly Variable Extinction and Accretion in the Jet-driving Class I Type Young Star PTF 10nvg (V2492 Cyg, IRAS 20496+4354)", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: formation; stars: individual (V2492 Cyg, PTF 10nvg, IRAS 20496+4354); stars: pre-main sequence", "note": "\u00a9 2013 American Astronomical Society. Received 2012 July 31; accepted 2012 December 7; published 2013 January 30. We commend PTF and PAIRITEL critical personnel Peter Nugent, Eran Ofek, and Dan Starr, and Cullen Blake for effective facility operation and data distribution. Mark Sullivan ran his PTF-specific PSF fitting code for us. In addition, we thank Joey Richards for helpful conversations and advice about the light curve analysis. We are also grateful to the many observers who kindly helped with the acquisition and/or reduction of spectra that are reported either in this paper or in Covey et al. (2011), including Katie Hamren, Everett Schlwain, Aaron Barth, Evan Kirby, Melissa Graham, Eric Hsiao, Peter Blanchard, Antonio Cucchiara, Adam Morgan, Daniel Perley, Christopher Griffith, Michael Kandrashoff, Luisa Rebull, Wilson Liu, John Angione, Shriharsh Tendulkar, Aaron Ofer, Kelsey Clubb, Greg Herczeg, Adam Kraus, Nick Law, Andrew Howard, Dan DeFelippis, Kunal Mooley, Trevor David, Geoff Marcy, and Howard Isaacson. CARMA Summer School students Isaac Shivvers, Che-Yu Chen, and Aaron Juarez participated in some of the CARMA observations and data reduction described herein. We are also very grateful for the assistance of staff members at the observatories where data were obtained. Funding acknowledgements are as follows. (1) K.R.C. acknowledges support for this work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51253.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555, and support for publication charges generously provided by Dr. William Tifft. (2) A.V.F.'s group at UC Berkeley acknowledges generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and US National Science Foundation (NSF) grant AST-0908886. (3) PAIRITEL has been supported by a Swift Guest Investigator grant NASA/NNX12AE67G. (4) Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. (5) The Infrared Telescope Facility is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. (6) Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement (grant number AST-0838260) and by the CARMA partner universities. Facilities: PO:1.2m, FLWO:2MASS, Shane, Hale (two instruments), ARC,Keck:I,Keck:II, IRTF,CARMA,WIYN:0.9m, UKIRT, Spitzer, WISE.\n\nPublished - 1538-3881_145_3_59.pdf
Submitted - 1208.2066v1.pdf
", "abstract": "We report extensive new photometry and spectroscopy of the highly variable young stellar object PTF 10nvg (also known as IRAS 20496+4354 and V2492 Cyg), including optical and near-infrared time-series data as well as mid-infrared and millimeter data. Following the previously reported 2010 rise to R_(PTF)\u227e13^m.5 and subsequent fade, during 2011 and 2012 the source underwent additional episodes of brightening, followed by several magnitude dimming events including prolonged faint states at R_(PTF)\u227320^m. The observed high-amplitude variations are largely consistent with extinction changes (\u0394A_V up to 30 mag) having a ~220 day quasi-periodic signal. However, photometry measured when the source was near maximum brightness in mid-2010 as well as in late-2012 does not phase well to this period. Spectral evolution includes not only changes in the spectral slope but also correlated variation in the prominence of TiO/VO/CO bands and atomic line emission, as well as anti-correlated variation in forbidden line emission which, along with H_2, dominates optical and infrared spectra at faint epochs. Notably, night-to-night variations in several forbidden doublet strengths and ratios are observed. High-dispersion spectra were obtained in a variety of photometric states and reveal time-variable line profiles. Neutral and singly ionized atomic species are likely formed in an accretion flow and/or impact while the origin of zero-velocity atomic Li I \u03bb6707 in emission is unknown. Forbidden lines, including several rare species, exhibit blueshifted emission profiles and likely arise from an outflow/jet. Several of these lines are also seen spatially offset from the continuum source position, presumably in a shocked region of an extended jet. Blueshifted absorption components of the Na I D doublet, K I \u03bb\u03bb7665, 7669 doublet, and the O I 7774 triplet, as well as blueshifted absorption components seen against the broad H\u03b1 and Ca II triplet emission lines, similarly are formed in the outflow. CARMA maps resolve on larger scales a spatially extended outflow in millimeter-wavelength CO. We attribute the recently observed photometric and spectroscopic behavior to rotating circumstellar disk material located at separation \u0251 \u2248 0.7(M_*/M_\u2609)^(1/3) AU from the continuum source, causing the semi-periodic dimming. Occultation of the central star as well as the bright inner disk and the accretion/outflow zones renders shocked gas in the inner part of the jet amenable to observation at the faint epochs. We discuss PTF 10nvg as a source exhibiting both accretion-driven (perhaps analogous to V1647 Ori) and extinction-driven (perhaps analogous to UX Ori or GM Cep) high-amplitude variability phenomena.", "date": "2013-03", "date_type": "published", "publication": "Astronomical Journal", "volume": "145", "number": "3", "publisher": "American Astronomical Society", "pagerange": "Art. No. 59", "id_number": "CaltechAUTHORS:20120827-074754766", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120827-074754766", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51253.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA", "grant_number": "NNX12AE67G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NNX-08AE38A" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Caltech Associates" }, { "agency": "University of Chicago" }, { "agency": "State of California" }, { "agency": "State of Illinois" }, { "agency": "State of Maryland" }, { "agency": "NSF", "grant_number": "AST-0838260" }, { "agency": "CARMA Partner Universities" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-6256/145/3/59", "primary_object": { "basename": "1208.2066v1.pdf", "url": "https://authors.library.caltech.edu/records/y0y6s-5g358/files/1208.2066v1.pdf" }, "related_objects": [ { "basename": "1538-3881_145_3_59.pdf", "url": "https://authors.library.caltech.edu/records/y0y6s-5g358/files/1538-3881_145_3_59.pdf" } ], "pub_year": "2013", "author_list": "Hillenbrand, Lynne A.; Miller, Adam A.; et el." }, { "id": "https://authors.library.caltech.edu/records/p1anw-kxf86", "eprint_id": 37378, "eprint_status": "archive", "datestamp": "2023-08-22 08:40:26", "lastmod": "2023-10-23 17:24:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "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. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Murray-D", "name": { "family": "Murray", "given": "D." } }, { "id": "Nakar-E", "name": { "family": "Nakar", "given": "E." }, "orcid": "0000-0002-4534-7089" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Shaviv-N-J", "name": { "family": "Shaviv", "given": "N. J." } }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" } ] }, "title": "An outburst from a massive star 40 days before a supernova explosion", "ispublished": "pub", "full_text_status": "public", "keywords": "High-energy astrophysics; Stars", "note": "\u00a9 2013 Macmillan Publishers Limited.\n\nReceived 14 October; accepted 18 December 2012.\n\nWe thank E. Quataert and M. Cantiello for discussions. The VLA is operated by the National Radio Astronomy Observatory, a facility of the US National Science Foundation (NSF) operated under cooperative agreement by Associated Universities, Inc. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project. We are grateful for the assistance of the staff at the various observatories where data were obtained. We acknowledge support from the Arye Dissentshik career development chair, the Helen Kimmel Center for Planetary Science, the Israeli Ministry of Science, the Royal Society, the NSF, the Israeli Science Foundation, the German-Israeli Foundation, ERC, the US Department of Energy, Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, and the TABASGO Foundation.\n\nAuthor Contributions: E.O.O. initiated the search for precursor outbursts and wrote the\npaper, M.S. wrote the image-subtraction pipeline, S.B.C. reduced the Swift-UVOT\nobservations,M.M.K. reduced the P60 observations, A.G.-Y. helped with the spectroscopic\nanalysis, L.B., E.N. and N.J.S. contributed to the theoretical interpretation, A.V.F. assisted\nwith the spectroscopy and edited the paper, D.A.H., D.M. and J.M.S. conducted the\nspectroscopic observations or reductions, O.Y. helped write the paper, and S.R.K., I.A.,\nJ.S.B., R.L., P.E.N. and J.S. built the PTF hardware and software infrastructure.\n\nSubmitted - 1302.2633.pdf
Supplemental Material - nature11877-s1.pdf
", "abstract": "Some observations suggest that very massive stars experience extreme mass-loss episodes shortly before they explode as supernovae, as do several models. Establishing a causal connection between these mass-loss episodes and the final explosion would provide a novel way to study pre-supernova massive-star evolution. Here we report observations of a mass-loss event detected 40\u2009days before the explosion of the type\u2009IIn supernova SN\u20092010mc (also known as PTF\u200910tel). Our photometric and spectroscopic data suggest that this event is a result of an energetic outburst, radiating at least 6\u2009\u00d7\u200910^(47)\u2009erg of energy and releasing about 10^(\u22122) solar masses of material at typical velocities of 2,000\u2009km\u2009s^(\u22121). The temporal proximity of the mass-loss outburst and the supernova explosion implies a causal connection between them. Moreover, we find that the outburst luminosity and velocity are consistent with the predictions of the wave-driven pulsation model, and disfavour alternative suggestions.", "date": "2013-02-07", "date_type": "published", "publication": "Nature", "volume": "494", "number": "7435", "publisher": "Nature Publishing Group", "pagerange": "65-67", "id_number": "CaltechAUTHORS:20130307-133705176", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130307-133705176", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Arye Dissentshik career development chair" }, { "agency": "Helen Kimmel Center for Planetary Science" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Royal Society" }, { "agency": "NSF" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "European Research Council (ERC)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature11877", "primary_object": { "basename": "1302.2633.pdf", "url": "https://authors.library.caltech.edu/records/p1anw-kxf86/files/1302.2633.pdf" }, "related_objects": [ { "basename": "nature11877-s1.pdf", "url": "https://authors.library.caltech.edu/records/p1anw-kxf86/files/nature11877-s1.pdf" } ], "pub_year": "2013", "author_list": "Ofek, E. O.; Sullivan, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/wgexg-ds014", "eprint_id": 36964, "eprint_status": "archive", "datestamp": "2023-08-22 08:24:04", "lastmod": "2023-10-23 15:59:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D." }, "orcid": "0000-0002-3714-672X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Gnat-O", "name": { "family": "Gnat", "given": "O." } }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "N." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "O." }, "orcid": "0000-0002-0301-8017" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "L." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "D." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "B." }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "X-Ray Emission from Supernovae in Dense Circumstellar Matter Environments: A Search for Collisionless Shocks", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (SN 2006jc, SN 2010jl)", "note": "\u00a9 2013 American Astronomical Society. Received 2012 May 30; accepted 2012 October 18; published 2013 January 4. We thank Ehud Nakar, Boaz Katz, and Nir Sapir for many\ndiscussions, and the anonymous referee for constructive comments. This paper is based on observations obtained with\nthe Samuel Oschin Telescope as part of the Palomar Transient\nFactory project, a scientific collaboration between the\nCalifornia Institute of Technology, Columbia University, Las\nCumbres 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 incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science. M.S. acknowledges support from the Royal Society. A.C. acknowledges support from LIGO, which was constructed by the California Institute of Technology and the Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. S.R.K. and his group are partially supported by the NSF grant AST-0507734. A.G. acknowledges support by the Israeli, German\u2013Israeli, and the U.S.\u2013Israel Binational Science Foundations, a Minerva grant, and the Lord Sieff of Brimpton fund. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under\nContract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for the PTF project. P.E.N. acknowledges support from the U.S. Department of Energy Scientific Discovery through Advanced Computing program under contract DE-FG02-06ER06-04. J.S.B.'s work on PTF was supported by NSF/OIA award AST-0941742 (\"Real-Time Classification of Massive Time-Series Data Streams\"). L.B. is supported by the NSF under grants PHY 05-51164 and AST 07-07633. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A.V.F.'s supernova group at UC Berkeley is supported by Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, Auto-Scope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation.\n\nPublished - 0004-637X_763_1_42.pdf
", "abstract": "The optical light curve of some supernovae (SNe) may be powered by the outward diffusion of the energy deposited by the explosion shock (the so-called shock breakout) in optically thick (\u03c4 \u2273 30) circumstellar matter (CSM). Recently, it was shown that the radiation-mediated and radiation-dominated shock in an optically thick wind must transform into a collisionless shock and can produce hard X-rays. The X-rays are expected to peak at late times, relative to maximum visible light. Here we report on a search, using Swift/XRT and Chandra, for X-ray emission from 28 SNe that belong to classes whose progenitors are suspected to be embedded in dense CSM. Our sample includes 19 Type IIn SNe, one Type Ibn SN, and eight hydrogen-poor superluminous SNe (SLSN-I such as SN 2005ap). Two SNe (SN 2006jc and SN 2010jl) have X-ray properties that are roughly consistent with the expectation for X-rays from a collisionless shock in optically thick CSM. However, the X-ray emission from SN 2006jc can also be explained as originating in an optically thin region. Thus, we propose that the optical light curve of SN 2010jl is powered by shock breakout in CSM. We suggest that two other events (SN 2010al and SN 2011ht) were too X-ray bright during the SN maximum optical light to be explained by the shock-breakout model. We conclude that the light curves of some, but not all, SNe IIn/Ibn are powered by shock breakout in CSM. For the rest of the SNe in our sample, including all of the SLSN-I events, our X-ray limits are not deep enough and were typically obtained too early (i.e., near the SN maximum light) for definitive conclusions about their nature. Late-time X-ray observations are required in order to further test whether these SNe are indeed embedded in dense CSM. We review the conditions required for a shock breakout in a wind profile. We argue that the timescale, relative to maximum light, for the SN to peak in X-rays is a probe of the column density and the density profile above the shock region. In SNe whose X-ray emission slowly rises, and peaks at late times, the optical light curve is likely powered by the diffusion of shock energy in a dense CSM. We note that if the CSM density profile falls faster than a constant-rate wind-density profile, then X-rays may escape at earlier times than estimated for the wind-profile case. Furthermore, if the CSM has a region in which the density profile is very steep relative to a steady wind-density profile, or if the CSM is neutral, then the radio free-free absorption may be sufficiently low for radio emission to be detected.", "date": "2013-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "763", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 42", "id_number": "CaltechAUTHORS:20130215-140729372", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130215-140729372", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science (Israel)" }, { "agency": "Royal Society" }, { "agency": "LIGO" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "NSF", "grant_number": "AST-0507734" }, { "agency": "Israel Science Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "MINERVA (Israel)" }, { "agency": "Lord Sieff of Brimpton Fund" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "NSF", "grant_number": "AST-0941742" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "Auto-Scope Corporation" }, { "agency": "Lick Observatory" }, { "agency": "University of California" }, { "agency": "Sylvia and Jim Katzman Foundation" } ] }, "other_numbering_system": { "items": [ { "id": "2009-65", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "LIGO" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/763/1/42", "primary_object": { "basename": "0004-637X_763_1_42.pdf", "url": "https://authors.library.caltech.edu/records/wgexg-ds014/files/0004-637X_763_1_42.pdf" }, "pub_year": "2013", "author_list": "Ofek, E. O.; Fox, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/h6rsn-4f551", "eprint_id": 36406, "eprint_status": "archive", "datestamp": "2023-08-19 13:45:52", "lastmod": "2023-10-20 23:07:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Perley-D-A", "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Becker-J-C", "name": { "family": "Becker", "given": "Juliette C." }, "orcid": "0000-0002-7733-4522" }, { "id": "Bottom-M", "name": { "family": "Bottom", "given": "Michael" }, "orcid": "0000-0003-1341-5531" }, { "id": "Muirhead-P-S", "name": { "family": "Muirhead", "given": "Philip S." }, "orcid": "0000-0002-0638-8822" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" } ] }, "title": "Discovery and Early Multi-wavelength Measurements of the Energetic Type Ic Supernova PTF12gzk: A Massive-star Explosion in a Dwarf Host Galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general supernovae: individual (PTF12gzk)", "note": "\u00a9 2012 American Astronomical Society. Received 2012 August 28; accepted 2012 October 23; published 2012 November 9. S.B. is supported by a Ramon Fellowship from ISA. A.G.\nacknowledges support by grants from the ISF, BSF, GIF,\nMinerva, and the EU FP7/ERC. A.V.F. and his group benefit\nfrom financial assistance from Gary & Cynthia Bengier, the\nRichard & Rhoda Goldman Fund, the Sylvia & Jim Katzman\nFoundation, the Christopher R. Redlich Fund, the TABASGO\nFoundation, NSF grants AST-0908886 and AST-1211916, and\nNASA/HST grant GO-12530 from STScI (which is operated\nby the AURA, Inc., under NASA contract NAS 05-26555).\nP.A.M. and E.P. acknowledge financial support from grants\nINAF PRIN 2011 and ASI/INAF I/088/06/0. M.I. and Y.J.\nwere supported by the Creative Initiative program of the NRFK. M.M.K. acknowledges Hubble and Carnegie-Princeton\nFellowships. D.C.L. is supported by NSF grant AST-1009571.\nE.O.O. acknowledges the Arye Dissentshik career development\nchair and a grant from the Israeli MOST.\nPTF is a collaboration of Caltech, LCOGT, the Weizmann\nInstitute, LBNL/NERSC, Oxford, Columbia, IPAC, and UC\nBerkeley. We are grateful for the assistance of the staff at the\nvarious observatories used to obtain data. This research has\nmade use of the NASA/IPAC Extragalactic Database (NED)\nwhich is operated by JPL, Caltech, under contract with NASA.\n\nPublished - 2041-8205_760_2_L33.pdf
", "abstract": "We present the discovery and extensive early-time observations of the Type Ic supernova (SN) PTF12gzk. Our light curves show a rise of 0.8 mag within 2.5 hr. Power-law fits (f(t)\u03b1(t \u2013 t_0)^n ) to these data constrain the explosion date to within one day. We cannot rule out a quadratic fireball model, but higher values of n are possible as well for larger areas in the fit parameter space. Our bolometric light curve and a dense spectral sequence are used to estimate the physical parameters of the exploding star and of the explosion. We show that the photometric evolution of PTF12gzk is slower than that of most SNe Ic. The high ejecta expansion velocities we measure (~30, 000 km s^(\u20131) derived from line minima four days after explosion) are similar to the observed velocities of broad-lined SNe Ic associated with gamma-ray bursts (GRBs) rather than to normal SN Ic velocities. Yet, this SN does not show the persistent broad lines that are typical of broad-lined SNe Ic. The host-galaxy characteristics are also consistent with GRB-SN hosts, and not with normal SN Ic hosts. By comparison with the spectroscopically similar SN 2004aw, we suggest that the observed properties of PTF12gzk indicate an initial progenitor mass of 25-35 M_\u2609 and a large ((5-10) \u00d7 10^(51) erg) kinetic energy, the later being close to the regime of GRB-SN properties.", "date": "2012-12-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "760", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L33", "id_number": "CaltechAUTHORS:20130115-153632924", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-153632924", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ISA Ramon Fellowship" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Minerva" }, { "agency": "European Research Council (ERC)" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Christopher R. Redlich Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA", "grant_number": "GO-12530" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "I/088/06/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "National Research Foundation of Korea" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NSF", "grant_number": "AST-1009571" }, { "agency": "Ministry of Science and Technology (Israel)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "AST-1211916" }, { "agency": "NASA Hubble Fellowship" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/760/2/L33", "primary_object": { "basename": "2041-8205_760_2_L33.pdf", "url": "https://authors.library.caltech.edu/records/h6rsn-4f551/files/2041-8205_760_2_L33.pdf" }, "pub_year": "2012", "author_list": "Ben-Ami, Sagi; Horesh, Assaf; et el." }, { "id": "https://authors.library.caltech.edu/records/gnfd9-45283", "eprint_id": 35969, "eprint_status": "archive", "datestamp": "2023-08-22 07:45:45", "lastmod": "2023-10-20 22:00:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abadie-J", "name": { "family": "Abadie", "given": "J." } }, { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. P." } }, { "id": "Abbott-R", "name": { "family": "Abbott", "given": "R." } }, { "id": "Adhikari-R-X", "name": { "family": "Adhikari", "given": "R. X." }, "orcid": "0000-0002-5731-5076" }, { "id": "Ajith-P", "name": { "family": "Ajith", "given": "P." }, "orcid": "0000-0001-7519-2439" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "S. B." } }, { "id": "Arai-Koji", "name": { "family": "Arai", "given": "K." }, "orcid": "0000-0001-8916-8915" }, { "id": "Araya-M-C", "name": { "family": "Araya", "given": "M. C." } }, { "id": "Barayoga-J-C-B", "name": { "family": "Barayoga", "given": "J. C. B." } }, { "id": "Betzwieser-J", "name": { "family": "Betzwieser", "given": "J." } }, { "id": "Billingsley-G", "name": { "family": "Billingsley", "given": "G." }, "orcid": "0000-0002-4141-2744" }, { "id": "Black-E", "name": { "family": "Black", "given": "E." } }, { "id": "Blackburn-J-K", "name": { "family": "Blackburn", "given": "J. K." }, "orcid": "0000-0002-3838-2986" }, { "id": "Bork-R", "name": { "family": "Bork", "given": "R." } }, { "id": "Brooks-A-F", "name": { "family": "Brooks", "given": "A. F." }, "orcid": "0000-0003-4295-792X" }, { "id": "Cepeda-C", "name": { "family": "Cepeda", "given": "C." } }, { "id": "Chalermsongsak-T", "name": { "family": "Chalermsongsak", "given": "T." } }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Coyne-D-C", "name": { "family": "Coyne", "given": "D. C." }, "orcid": "0000-0002-6427-3222" }, { "id": "Dannenberg-R", "name": { "family": "Dannenberg", "given": "R." } }, { "id": "Daudert-B", "name": { "family": "Daudert", "given": "B." } }, { "id": "Dergachev-V", "name": { "family": "Dergachev", "given": "V." } }, { "id": "DeSalvo-R", "name": { "family": "DeSalvo", "given": "R." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Driggers-J-C", "name": { "family": "Driggers", "given": "J. C." } }, { "id": "Ehrens-P", "name": { "family": "Ehrens", "given": "P." } }, { "id": "Engel-R", "name": { "family": "Engel", "given": "R." } }, { "id": "Etzel-T", "name": { "family": "Etzel", "given": "T." } }, { "id": "Fotopoulos-N", "name": { "family": "Fotopoulos", "given": "N." } }, { "id": "Gustafson-E-K", "name": { "family": "Gustafson", "given": "E. K." } }, { "id": "Hanna-C", "name": { "family": "Hanna", "given": "C." } }, { "id": "Harms-J", "name": { "family": "Harms", "given": "J." }, "orcid": "0000-0002-7332-9806" }, { "id": "Heefner-J", "name": { "family": "Heefner", "given": "J." } }, { "id": "Heptonstall-A-W", "name": { "family": "Heptonstall", "given": "A. W." } }, { "id": "Hodge-K-A", "name": { "family": "Hodge", "given": "K. A." } }, { "id": "Hong-T", "name": { "family": "Hong", "given": "T." } }, { "id": "Ivanov-A", "name": { "family": "Ivanov", "given": "A." } }, { "id": "Jacobson-M", "name": { "family": "Jacobson", "given": "M." } }, { "id": "James-E", "name": { "family": "James", "given": "E." } }, { "id": "Kalmus-P", "name": { "family": "Kalmus", "given": "P." } }, { "id": "Kells-W", "name": { "family": "Kells", "given": "W." } }, { "id": "Keppel-D-G", "name": { "family": "Keppel", "given": "D. G." } }, { "id": "King-P-J", "name": { "family": "King", "given": "P. J." } }, { "id": "Kondrashov-V", "name": { "family": "Kondrashov", "given": "V." } }, { "id": "Korth-W-Z", "name": { "family": "Korth", "given": "W. Z." }, "orcid": "0000-0003-3527-1348" }, { "id": "Kozak-D-B", "name": { "family": "Kozak", "given": "D." }, "orcid": "0000-0003-3118-8950" }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "A." } }, { "id": "Lindquist-P-E", "name": { "family": "Lindquist", "given": "P. E." } }, { "id": "Luan-J", "name": { "family": "Luan", "given": "J." } }, { "id": "Mageswaran-M", "name": { "family": "Mageswaran", "given": "M." } }, { "id": "Mailand-K", "name": { "family": "Mailand", "given": "K." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Miao-Haixing", "name": { "family": "Miao", "given": "H." }, "orcid": "0000-0003-2879-5821" }, { "id": "Nash-T", "name": { "family": "Nash", "given": "T." } }, { "id": "Ogin-G-H", "name": { "family": "Ogin", "given": "G. H." } }, { "id": "Osthelder-C", "name": { "family": "Osthelder", "given": "C." } }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "C. D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Patel-P", "name": { "family": "Patel", "given": "P." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Phelps-M", "name": { "family": "Phelps", "given": "M." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Privitera-S", "name": { "family": "Privitera", "given": "S." } }, { "id": "Reitze-D-H", "name": { "family": "Reitze", "given": "D. H." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Rollins-J-G", "name": { "family": "Rollins", "given": "J. G." } }, { "id": "Sannibale-V", "name": { "family": "Sannibale", "given": "V." } }, { "id": "Santamar\u00eda-L", "name": { "family": "Santamar\u00eda", "given": "L." } }, { "id": "Seifert-F", "name": { "family": "Seifert", "given": "F." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Singer-L", "name": { "family": "Singer", "given": "L." } }, { "id": "Smith-M-R", "name": { "family": "Smith", "given": "M. R." } }, { "id": "Somiya-Kentaro", "name": { "family": "Somiya", "given": "K." } }, { "id": "Stochino-A", "name": { "family": "Stochino", "given": "A." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Villar-A-E", "name": { "family": "Villar", "given": "A. E." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Wen-L", "name": { "family": "Wen", "given": "L." } }, { "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "S. E." } }, { "id": "Willems-P-A", "name": { "family": "Willems", "given": "P. A." } }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "R." }, "orcid": "0000-0002-9145-8580" }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Yang-H", "name": { "family": "Yang", "given": "H." } }, { "id": "Yeaton-Massey-D", "name": { "family": "Yeaton-Massey", "given": "D." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan J." }, "orcid": "0000-0002-0928-6784" } ] }, "title": "Search for Gravitational Waves Associated with Gamma-Ray Bursts during LIGO Science Run 6 and Virgo Science Runs 2 and 3", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; gamma-ray burst: general; gravitational waves", "note": "\u00a9 2012 American Astronomical Society. Received 2012 May 29; accepted 2012 September 22; published 2012 October 30. We are indebted to the observers of the electromagnetic events\nand the Gamma-ray burst Coordinates Network for providing\nus with valuable data. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian\nResearch Council, the International Science Linkages program\nof the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Econom\u00eda y Competitividad, the Conselleria d'Economia Hisenda i Innovaci\u03cc of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics\nand Space Administration, the Carnegie Trust, the Leverhulme\nTrust, the David and Lucile Packard Foundation, the Research\nCorporation, and the Alfred P. Sloan Foundation. This document has been assigned LIGO Laboratory document number\nLIGO-P1000121-v10.\n\nPublished - 0004-637X_760_1_12.pdf
", "abstract": "We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole, and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10^(\u20132) M_\u2609 c^2 at 150 Hz, with a median limit of 17 Mpc. For short-hard GRBs we place exclusion distances on binary neutron star and neutron-star-black-hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16 Mpc and 28 Mpc, respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. However, projecting these exclusions to the sensitivities of Advanced LIGO and Virgo, which should begin operation in 2015, we find that the detection of gravitational waves associated with GRBs will become quite possible.", "date": "2012-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "760", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 12", "id_number": "CaltechAUTHORS:20121213-075343117", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121213-075343117", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Max Planck Society" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Australian Research Council" }, { "agency": "International Science Linkages program of the Commonwealth of Australia" }, { "agency": "Council of Scientific and Industrial Research (India)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Ministerio de Economia y Competividad (MEC)" }, { "agency": "Conselleria d'Economia Hisenda i Innovaci\u03cc of the Govern de les Illes Balears" }, { "agency": "Stichting voor Fundamenteel Onderzoek der Materie (FOM)" }, { "agency": "Ministry of Science and Higher Education (Poland)" }, { "agency": "FOCUS Programme of Foundation for Polish Science" }, { "agency": "Royal Society" }, { "agency": "Scottish Funding Council" }, { "agency": "Scottish Universities Physics Alliance" }, { "agency": "NASA" }, { "agency": "Carnegie Trust" }, { "agency": "Leverhulme Trust" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Research Corporation" }, { "agency": "Alfred P. Sloan Foundation" } ] }, "other_numbering_system": { "items": [ { "id": "LIGO-P1000121-v10", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "LIGO" }, { "id": "Palomar-Transient-Factory" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1088/0004-637X/760/1/12", "primary_object": { "basename": "0004-637X_760_1_12.pdf", "url": "https://authors.library.caltech.edu/records/gnfd9-45283/files/0004-637X_760_1_12.pdf" }, "pub_year": "2012", "author_list": "Abadie, J.; Abbott, B. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/60stx-5mg27", "eprint_id": 35759, "eprint_status": "archive", "datestamp": "2023-08-22 07:41:36", "lastmod": "2023-10-20 20:37:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "R. R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "J." }, "orcid": "0000-0001-7291-0087" }, { "id": "Fulton-B-J", "name": { "family": "Fulton", "given": "B. J." }, "orcid": "0000-0003-3504-5316" } ] }, "title": "Hubble Space Telescope studies of low-redshift Type Ia supernovae: evolution with redshift and ultraviolet spectral trends", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; galaxies: general; distance scale; cosmological parameters", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society. \n\nAccepted 2012 August 10; Received 2012 August 10; in original form 2012 May 29. Article first published online: 10 Oct. 2012. \n\nMS acknowledges support from the Royal Society. AG-Y and MS\nacknowledge support from the Weizmann-UK 'making connections' programme. AG-Y further acknowledges support by the ISF, BSF, a Minerva grant, the ARCHES award and the Lord Sieff of Brompton Fund. DAH and BD are supported by the Las Cumbres Observatory Global Telescope Network. MMK acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science.\nThis paper is based on observations made with the NASA/ESA\nHST, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programmes 11721 and 12298. 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. \n\nObservations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, La Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford and the Weizmann Institute of Science. The William Herschel Telescope\nis operated on the island of La Palma by the Isaac Newton\nGroup in the Spanish Observatorio del Roque de los Muchachos\nof the Instituto de Astrof\u00edsica de Canarias. Some of the data were obtained with 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. These observations were made possible by\nthe generous financial support of the W. M. Keck Foundation. This paper uses observations obtained with facilities of the LCOGT. The BOS is operated by the Las Cumbres Observatory Global Telescope Network and is located at the Sedgwick Reserve, a part of the University of California Natural Reserve System. This research has\nmade use of the NASA/IPAC Extragalactic Database (NED) which\nis operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication has been made possible by the participation of more than 10 000 volunteers in the Galaxy Zoo: Supernovae project (http://supernova.galaxyzoo.org/authors).\n\nPublished - mnr21909.pdf
Accepted Version - 1205.7040.pdf
", "abstract": "We present an analysis of the maximum light, near-ultraviolet (NUV; 2900 < \u03bb < 5500\u2009\u00c5) spectra of 32 low-redshift (0.001 < z < 0.08) Type Ia supernovae (SNe Ia), obtained with the Hubble Space Telescope (HST) using the Space Telescope Imaging Spectrograph. We combine this spectroscopic sample with high-quality gri light curves obtained with robotic telescopes to measure SN Ia photometric parameters, such as stretch (light-curve width), optical colour and brightness (Hubble residual). By comparing our new data to a comparable sample of SNe Ia at intermediate redshift (0.4 < z < 0.9), we detect modest spectral evolution (3\u03c3), in the sense that our mean low-redshift NUV spectrum has a depressed flux compared to its intermediate-redshift counterpart. We also see a strongly increased dispersion about the mean with decreasing wavelength, confirming the results of earlier surveys. We show that these trends are consistent with changes in metallicity as predicted by contemporary SN Ia spectral models. We also examine the properties of various NUV spectral diagnostics in the individual SN spectra. We find a general correlation between SN stretch and the velocity (or position) of many NUV spectral features. In particular, we observe that higher stretch SNe have larger Ca\u2009ii H&K velocities, which also correlate with host galaxy stellar mass. This latter trend is probably driven by the well-established correlation between stretch and host galaxy stellar mass. We find no significant trends between UV spectral features and optical colour. Mean spectra constructed according to whether the SN has a positive or negative Hubble residual show very little difference at NUV wavelengths, indicating that the NUV evolution and variation we identify does not directly correlate with Hubble diagram residuals. Our work confirms and strengthens earlier conclusions regarding the complex behaviour of SNe Ia in the NUV spectral region, but suggests the correlations we find are more useful in constraining progenitor models rather than improving the use of SNe\u2009Ia as cosmological probes.", "date": "2012-11-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "426", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2359-2379", "id_number": "CaltechAUTHORS:20121203-103035154", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121203-103035154", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Las Cumbres Observatory Global Telescope Network" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Ministry of Science (Israel)" }, { "agency": "Minerva Grant" }, { "agency": "ARCHES Award" }, { "agency": "Lord Sieff of Brompton Fund" }, { "agency": "Weizmann-UK Making Connections Programme" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2012.21909.x", "primary_object": { "basename": "1205.7040.pdf", "url": "https://authors.library.caltech.edu/records/60stx-5mg27/files/1205.7040.pdf" }, "related_objects": [ { "basename": "mnr21909.pdf", "url": "https://authors.library.caltech.edu/records/60stx-5mg27/files/mnr21909.pdf" } ], "pub_year": "2012", "author_list": "Maguire, K.; Ellis, R. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/00g8e-vwy56", "eprint_id": 35872, "eprint_status": "archive", "datestamp": "2023-08-19 13:18:13", "lastmod": "2023-10-20 21:52:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Richards-J-W", "name": { "family": "Richards", "given": "J. W." } }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Starr-D-L", "name": { "family": "Starr", "given": "D. L." } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Butler-N-R", "name": { "family": "Butler", "given": "N. R." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" } ] }, "title": "Automating Discovery and Classification of Transients and Variable Stars in the Synoptic Survey Era", "ispublished": "pub", "full_text_status": "public", "keywords": "Data Analysis and Techniques", "note": "\u00a9 2012 Astronomical Society of the Pacific.\n\nReceived 2011 June 27; accepted 2012 September 12; published 2012 October 29.\n\nThe authors acknowledge the generous support of a CDI grant (#0941742) from the National Science Foundation. J.S.B. and D.L.S. also thank the Las Cumbres Observatory for support during the early stages of this work. S.B.C. wishes to acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, National Aeronautics and Space Administration (NASA)/Swift grant NNX10AI21G, NASA/Fermi grant NNX1OA057G, and National Science Foundation (NSF) grant AST-0908886. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract #DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project.\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 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 has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (Ochsenbein et al. 2000).\n\nPublished - 668468.pdf
", "abstract": "The rate of image acquisition in modern synoptic imaging surveys has already begun to outpace the feasibility of keeping astronomers in the real-time discovery and classification loop. Here we present the inner workings of a framework, based on machine-learning algorithms, that captures expert training and ground-truth knowledge about the variable and transient sky to automate (1) the process of discovery on image differences, and (2) the generation of preliminary science-type classifications of discovered sources. Since follow-up resources for extracting novel science from fast-changing transients are precious, self-calibrating classification probabilities must be couched in terms of efficiencies for discovery and purity of the samples generated. We estimate the purity and efficiency in identifying real sources with a two-epoch image-difference discovery algorithm for the Palomar Transient Factory (PTF) survey. Once given a source discovery, using machine-learned classification trained on PTF data, we distinguish between transients and variable stars with a 3.8% overall error rate (with 1.7% errors for imaging within the Sloan Digital Sky Survey footprint). At >96% classification efficiency, the samples achieve 90% purity. Initial classifications are shown to rely primarily on context-based features, determined from the data itself and external archival databases. In the first year of autonomous operations of PTF, this discovery and classification framework led to several significant science results, from outbursting young stars to subluminous Type IIP supernovae to candidate tidal disruption events. We discuss future directions of this approach, including the possible roles of crowdsourcing and the scalability of machine learning to future surveys such as the Large Synoptic Survey Telescope (LSST).", "date": "2012-11", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "124", "number": "921", "publisher": "Astronomical Society of the Pacific", "pagerange": "1175-1196", "id_number": "CaltechAUTHORS:20121207-095356939", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121207-095356939", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "Las Cumbres Observatory" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1086/668468", "primary_object": { "basename": "668468.pdf", "url": "https://authors.library.caltech.edu/records/00g8e-vwy56/files/668468.pdf" }, "pub_year": "2012", "author_list": "Bloom, J. S.; Richards, J. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/em3ap-hg748", "eprint_id": 35314, "eprint_status": "archive", "datestamp": "2023-08-22 07:06:53", "lastmod": "2023-10-20 15:57:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Baranec-C", "name": { "family": "Baranec", "given": "Christoph" }, "orcid": "0000-0002-1917-9157" }, { "id": "Davis-J-T-C", "name": { "family": "Davis", "given": "Jack T. C." } }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Riddle-R-L", "name": { "family": "Riddle", "given": "Reed" }, "orcid": "0000-0002-0387-370X" }, { "id": "Tendulkar-S-P", "name": { "family": "Tendulkar", "given": "Shriharsh P." }, "orcid": "0000-0003-2548-2926" }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "Fulton-B-J", "name": { "family": "Fulton", "given": "Benjamin J." }, "orcid": "0000-0003-3504-5316" } ] }, "title": "Three New Eclipsing White-dwarf-M-dwarf Binaries Discovered in a Search for Transiting Planets around M-dwarfs", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: eclipsing; methods: data analysis; planets and satellites: detection; stars: low-mass; techniques: photometric; white dwarfs", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 December 2; accepted 2012 July 30; published 2012 September 11. \n\nWe thank Michael Kandrashoff, Jieun Choi, and Peter Blanchard for observations at Lick Observatory, and thank the anonymous referee for their constructive suggestions and swift report. Observations were obtained with the Samuel Oschin Telescope and the 60 inch telescope at the Palomar Observatory 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\nComputing Center, the University of Oxford, and the Weizmann\nInstitute of Science. Some of the data presented herein were obtained at the W.M.Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations\nfrom this mountain. The Byrne Observatory at Sedgwick\n(BOS) is operated by the Las Cumbres Observatory Global Telescope Network and is located at the Sedgwick Reserve, a part of the University of California Natural Reserve System. The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology, and the Inter-University Centre for Astronomy and Astrophysics, and by the National Science Foundation under Grant Nos. AST-0906060 and AST-0960343. This paper uses observations obtained with the FTN observatory of the Las Cumbres Observatory Global Telescope. This research has also made use of the SIMBAD database, operated at CDS, Strasbourg, France. The radial velocity analysis in this paper used two existing data analysis pipelines,\nMAKEE by Tom Barlow and BFall by Slavek Rucinski; we\ngratefully acknowledge their contribution to the field in developing and supporting this software. N.M.L. is supported by a Dunlap Fellowship at University of Toronto. A.L.K. was supported by NASA through Hubble Fellowship Grant 51257.01 awarded by STScI, which is operated by AURA, Inc., for ANSA, under contract NAS 5-26555. M.M.K. acknowledges support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A.V.F. and his group at UC Berkeley acknowledge generous financial assistance from Gary and Cynthia Bengier, the Richard & Rhoda Goldman Fund, the TABASGO Foundation, and NSF Grant AST-0908886.\nFacilities: PO:1.2m, Keck:I, LCOGT\n\nPublished - 0004-637X_757_2_133.pdf
", "abstract": "We present three new eclipsing white-dwarf/M-dwarf binary systems discovered during a search for transiting planets around M-dwarfs. Unlike most known eclipsing systems of this type, the optical and infrared emission is dominated by the M-dwarf components, and the systems have optical colors and discovery light curves consistent with being Jupiter-radius transiting planets around early M-dwarfs. We detail the PTF/M-dwarf transiting planet survey, part of the Palomar Transient Factory (PTF). We present a graphics processing unit (GPU)-based box-least-squares search for transits that runs approximately 8 \u00d7 faster than similar algorithms implemented on general purpose systems. For the discovered systems, we decompose low-resolution spectra of the systems into white-dwarf and M-dwarf components, and use radial velocity measurements and cooling models to estimate masses and radii for the white dwarfs. The systems are compact, with periods between 0.35 and 0.45 days and semimajor axes of approximately 2 R_\u2609 (0.01 AU). The M-dwarfs have masses of approximately 0.35 M_\u2609, and the white dwarfs have hydrogen-rich atmospheres with temperatures of around 8000 K and have masses of approximately 0.5 M_\u2609. We use the Robo-AO laser guide star adaptive optics system to tentatively identify one of the objects as a triple system. We also use high-cadence photometry to put an upper limit on the white-dwarf radius of 0.025 R_\u2609 (95% confidence) in one of the systems. Accounting for our detection efficiency and geometric factors, we estimate that 0.08%^(+0.10%)_(-0.05%) (90% confidence) of M-dwarfs are in these short-period, post-common-envelope white-dwarf/M-dwarf binaries where the optical light is dominated by the M-dwarf. The lack of detections at shorter periods, despite near-100% detection efficiency for such systems, suggests that binaries including these relatively low-temperature white dwarfs are preferentially found at relatively large orbital radii. Similar eclipsing binary systems can have arbitrarily small eclipse depths in red bands and generate plausible small-planet-transit light curves. As such, these systems are a source of false positives for M-dwarf transiting planet searches. We present several ways to rapidly distinguish these binaries from transiting planet systems.", "date": "2012-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "757", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 133", "id_number": "CaltechAUTHORS:20121106-153848418", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121106-153848418", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Toronto Dunlap Fellowship" }, { "agency": "NASA Hubble Fellowship", "grant_number": "51257.01" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/757/2/133", "primary_object": { "basename": "0004-637X_757_2_133.pdf", "url": "https://authors.library.caltech.edu/records/em3ap-hg748/files/0004-637X_757_2_133.pdf" }, "pub_year": "2012", "author_list": "Law, Nicholas M.; Hillenbrand, Lynne A.; et el." }, { "id": "https://authors.library.caltech.edu/records/z26pp-jr993", "eprint_id": 96334, "eprint_status": "archive", "datestamp": "2023-08-19 12:41:18", "lastmod": "2023-10-20 21:05:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Barone-Nugent-R-L", "name": { "family": "Barone-Nugent", "given": "R. L." } }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "C." }, "orcid": "0000-0003-1731-0497" }, { "id": "Wyithe-J-S-B", "name": { "family": "Wyithe", "given": "J. S. B." } }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "J." }, "orcid": "0000-0003-3820-1740" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "J." }, "orcid": "0000-0001-5703-2108" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Hsiao-Eric-Y", "name": { "family": "Hsiao", "given": "E. Y." }, "orcid": "0000-0003-1039-2928" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E." }, "orcid": "0000-0002-6786-8774" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } } ] }, "title": "Near-infrared observations of type Ia supernovae: The best known\n standard candle for cosmology", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 The Authors. \n\nAccepted 2012 May 29. Received 2012 May 28; in original form 2012 April 5. \n\nThis work is based on data collected at the ESO VLT (programme\nnumber 083.A-0480) and observations obtained at the Gemini Observatory (programme numbers GN2010A-Q-16, GN2010B-Q17, GN2011A-Q-11 and GN-2011B-Q-21), which is operated by\nthe Association of Universities for Research in Astronomy, Inc.,\nunder a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States),\nthe Science and Technology Facilities Council (United Kingdom),\nthe National Research Council (Canada), CONICYT (Chile), the\nAustralian Research Council (Australia), Ministrio da Cincia, Tecnologia e Inovao (Brazil) and Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina). CL is the recipient of an Australian\nResearch Council Future Fellowship (project number FT0992259).\nThis research was conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (project number\nCE110001020). MS acknowledges support from the Royal Society.\nThe Liverpool Telescope is operated on the island of La Palma by\nLiverpool John Moores University in the Spanish Observatorio del\nRoque de los Muchachos of the Instituto de Astrofisica de Canarias\nwith financial support from the UK Science and Technology Facilities Council. This publication has been made possible by the\nparticipation of more than 10 000 volunteers in the Galaxy Zoo\nSupernovae project, http://supernova.galaxyzoo.org/authors. AG-Y\nacknowledges support by ISF, BSF, GIF and Minerva grants, an\nARCHES award and the Lord Sieff of Brimpton Fund. SBC acknowledges generous financial assistance from Gary & Cynthia\nBengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants\nNNX10AI21G and GO-7100028, the TABASGO Foundation and\nNSF grant AST-0908886. MMK acknowledges generous support\nfrom the Hubble Fellowship and Carnegie-Princeton Fellowship.\n\nPublished - 425-2-1007.pdf
", "abstract": "We present an analysis of the Hubble diagram for 12 Type Ia supernovae (SNe Ia) observed in the near-infrared J and H bands. We select SNe exclusively from the redshift range 0.03 < z < 0.09 to reduce uncertainties coming from peculiar velocities while remaining in a cosmologically well-understood region. All of the SNe in our sample exhibit no spectral or B-band light-curve peculiarities\nand lie in the B-band stretch range of 0.8-1.15. Our results suggest that SNe Ia observed in the near-infrared (NIR) are the best known standard candles. We fit previously determined NIR light-curve templates to new high-precision data to derive peak magnitudes and to determine the scatter about the Hubble line. Photometry of the 12 SNe is presented in the natural system. Using a standard cosmology of (H_0, Omega_m, Lambda) = (70,0.27,0.73) we find a median J-band absolute magnitude of M_J = -18.39 with a scatter of 0.116 and a median H-band absolute magnitude of M_H = -18.36 with a scatter of 0.085. The scatter in the H band is the smallest yet measured. We search for correlations between residuals in the J- and H-band Hubble diagrams and SN properties, such as SN\ncolour, B-band stretch and the projected distance from host-galaxy centre. The only significant correlation is between the J-band Hubble residual and the J-H pseudo-colour. We also examine how the scatter changes when fewer points in the near-infrared are used to constrain the light curve. With a single point in the H band taken anywhere from 10 days before to 15 days after B-band maximum light and a prior on the date of H-band maximum set from the date of B-band maximum, we find that we can measure distances to an accuracy of 6%. The precision of SNe Ia in the NIR provides new opportunities for precision measurements of both the expansion history of the universe and peculiar velocities of nearby galaxies.", "date": "2012-09-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "425", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1007-1012", "id_number": "CaltechAUTHORS:20190612-134001545", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190612-134001545", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1111/j.1365-2966.2012.21412.x", "primary_object": { "basename": "425-2-1007.pdf", "url": "https://authors.library.caltech.edu/records/z26pp-jr993/files/425-2-1007.pdf" }, "pub_year": "2012", "author_list": "Barone-Nugent, R. L.; Lidman, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/3gh03-6cw64", "eprint_id": 35179, "eprint_status": "archive", "datestamp": "2023-08-22 06:51:29", "lastmod": "2023-10-20 15:48:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Silverio-K", "name": { "family": "Silverio", "given": "Kathryn" } }, { "id": "Stockton-A", "name": { "family": "Stockton", "given": "Alan" } }, { "id": "Cuillandre-J-C", "name": { "family": "Cuillandre", "given": "Jean-Charles" } }, { "id": "Marcy-G-W", "name": { "family": "Marcy", "given": "Geoffrey W." }, "orcid": "0000-0002-2909-0113" }, { "id": "Howard-A-W", "name": { "family": "Howard", "given": "Andrew W." }, "orcid": "0000-0001-8638-0320" }, { "id": "Isaacson-H-T", "name": { "family": "Isaacson", "given": "Howard" }, "orcid": "0000-0002-0531-1073" } ] }, "title": "The Red Supergiant Progenitor of Supernova 2012aw (PTF12bvh) in Messier 95", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (Messier 95, NGC 3351); stars: evolution; stars: fundamental parameters; stars: late-type; supernovae: general; supernovae: individual (SN 2012aw)", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2012 May 27; accepted 2012 July 11; published 2012 August 22.\n\nWe thank the referee for useful comments that helped improve\nthis manuscript. This work is based in part on observations\nwith the NASA/ESA Hubble Space Telescope, obtained at the\nSpace Telescope Science Institute (STScI), which is operated\nby AURA, Inc., under NASA contract NAS5-26555. We thank\nNancy Elias-Rosa for initial analysis of the HST and CFHT\nimages, and Mark Sullivan for information about the upper\nlimit to the SN 2012aw/PTF12bvh detection by PTF. Some\nof the data presented herein were obtained at the W. M.\nKeck 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. A.G. is supported by grants from the ISF, BSF, and GIF foundations, a Weizmann Minerva grant, and the Lord Sieff of Brimpton Fund. The research of A.V.F. and his group at UC Berkeley is funded by Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NSF grant AST-0908886, the TABASGO Foundation, and NASA/HST grant AR-12623 from STScI. This work was supported in part by the NSF grant PHY-1066293 and the hospitality of the Aspen Center for Physics. We dedicate this paper to the memory of our dear friend and colleague, Weidong Li, with whom two of us (A.V.F. and S.D.V.) spent many fun years identifying the progenitor stars of SNe; his tragic passing deeply saddened those who knew him.\n\nPublished - 0004-637X_756_2_131.pdf
", "abstract": "We report on the direct detection and characterization of the probable red supergiant (RSG) progenitor of the intermediate-luminosity Type II-Plateau (II-P) supernova (SN) 2012aw in the nearby (10.0 Mpc) spiral galaxy Messier 95 (M95; NGC 3351). We have identified the star in both Hubble Space Telescope images of the host galaxy, obtained 17-18 yr prior to the explosion, and near-infrared ground-based images, obtained 6-12 yr prior to the SN. The luminous supergiant showed evidence for substantial circumstellar dust, manifested as excess line-of-sight extinction. The effective total-to-selective ratio of extinction to the star was R'_V \u2248 4.35, which is significantly different from that of diffuse interstellar dust (i.e., R_V = 3.1), and the total extinction to the star was therefore, on average, A_V \u2248 3.1 mag. We find that the observed spectral energy distribution for the progenitor star is consistent with an effective temperature of 3600 K (spectral type M3), and that the star therefore had a bolometric magnitude of \u20138.29. Through comparison with recent theoretical massive-star evolutionary tracks we can infer that the RSG progenitor had an initial mass 15 \u2272 M_(ini)(M_\u2609) < 20. Interpolating by eye between the available tracks, we surmise that the star had initial mass ~17-18 M_\u2609. The circumstellar dust around the progenitor must have been destroyed in the explosion, as the visual extinction to the SN is found to be low (AV = 0.24 mag with R_V = 3.1).", "date": "2012-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "756", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 131", "id_number": "CaltechAUTHORS:20121030-134132487", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121030-134132487", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Weizmann Minerva" }, { "agency": "Lord Sieff of Brimpton Fund" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "TABASGO Foundation" }, { "agency": "NASA", "grant_number": "AR-12623" }, { "agency": "NSF", "grant_number": "PHY-1066293" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Palomar-Transient-Factory" } ] }, "doi": "10.1088/0004-637X/756/2/131", "primary_object": { "basename": "0004-637X_756_2_131.pdf", "url": "https://authors.library.caltech.edu/records/3gh03-6cw64/files/0004-637X_756_2_131.pdf" }, "pub_year": "2012", "author_list": "Van Dyk, Schuyler D.; Cenko, S. Bradley; et el." }, { "id": "https://authors.library.caltech.edu/records/h85cp-epj24", "eprint_id": 34066, "eprint_status": "archive", "datestamp": "2023-08-19 12:23:05", "lastmod": "2023-10-18 21:49:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dilday-B", "name": { "family": "Dilday", "given": "B." } }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "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" } ] }, "title": "PTF 11kx: A Type Ia Supernova with a Symbiotic Nova Progenitor", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Association for the Advancement of Science.\n\nReceived for publication 16 January 2012; accepted for publication 5 July 2012.\n\nThe Palomar Transient Factory project is a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory,\nthe Lawrence Berkeley National Laboratory, the National\nEnergy Research Scientific Computing Center, the University\nof Oxford, and the Weizmann Institute of Science. The\nNational Energy Research Scientific Computing Center,\nsupported by the Office of Science of the U.S. Department of\nEnergy, provided staff, computational resources, and data\nstorage for this project. Some of the data presented herein\nwere obtained at the W. M. Keck Observatory, which is\noperated as a scientific partnership among the California\nInstitute of Technology, the University of California, and NASA; 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 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. We are grateful to the staffs of the Lick, Keck, and other observatories for their assistance. We thank D. Kasen for insightful discussions on the analysis presented here, and we thank M. Auger for assistance in using his spectroscopic reduction pipeline. The research of A.V.F.'s group was supported by grants from the NSF, the TABASGO Foundation, Gary and Cynthia Bengier, and the Richard and Rhoda Goldman Fund. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A.G.-Y. is supported by grants from the Israel Science Foundation and the U.S.-Israel Binational Foundation, an Award for Research Cooperation and\nHigh Excellence in Science from the Bundesministerium f\u00fcr Bildung und Forschung, and the Lord Seiff of Brimpton Fund. The data presented in this paper are available from the Weizmann Interactive Supernova Data Repository (www.weizmann.ac.il/astrophysics/wiserep).\n\nSubmitted - 1207.1306v1.pdf
Supplemental Material - Dilday.SM.pdf
", "abstract": "There is a consensus that type Ia supernovae (SNe Ia) arise from the thermonuclear explosion of white dwarf stars that accrete matter from a binary companion. However, direct observation of SN Ia progenitors is lacking, and the precise nature of the binary companion remains uncertain. A temporal series of high-resolution optical spectra of the SN Ia PTF 11kx reveals a complex circumstellar environment that provides an unprecedentedly detailed view of the progenitor system. Multiple shells of circumstellar material are detected, and the SN ejecta are seen to interact with circumstellar material starting 59 days after the explosion. These features are best described by a symbiotic nova progenitor, similar to RS Ophiuchi.", "date": "2012-08-24", "date_type": "published", "publication": "Science", "volume": "337", "number": "6097", "publisher": "American Association for the Advancement of Science", "pagerange": "942-945", "id_number": "CaltechAUTHORS:20120913-113255775", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120913-113255775", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Energy Research Scientific Computing Center" }, { "agency": "NSF" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)" }, { "agency": "Brimpton Fund" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1126/science.1219164", "primary_object": { "basename": "1207.1306v1.pdf", "url": "https://authors.library.caltech.edu/records/h85cp-epj24/files/1207.1306v1.pdf" }, "related_objects": [ { "basename": "Dilday.SM.pdf", "url": "https://authors.library.caltech.edu/records/h85cp-epj24/files/Dilday.SM.pdf" } ], "pub_year": "2012", "author_list": "Dilday, B.; Horesh, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/n8rm5-8zf04", "eprint_id": 28493, "eprint_status": "archive", "datestamp": "2023-09-14 19:23:27", "lastmod": "2023-10-23 20:50:11", "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": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Bhalerao-V-B", "name": { "family": "Bhalerao", "given": "Varun B." }, "orcid": "0000-0002-6112-7609" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "Calcium-rich gap transients in the remote outskirts of galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general; Galaxy: halo; novae, cataclysmic variables; supernovae: individual (SN2005E, SN2007ke, PTF09dav, PTF10iuv, PTF11bij); surveys; white dwarfs", "note": "\u00a9 2012 American Astronomical Society. Received 2011 November 28; accepted 2012 June 19; published 2012 August 7. We thank Chuck Steidel and Ryan Trainor for target of\nopportunity observations of PTF 11bij with Keck I. We are\ngrateful to the staff of the Expanded Very Large Array for\nefficiently executing target of opportunity triggers. Excellent assistance was provided by the staffs of the various observatories where we obtained data (Lick, Keck, Palomar, WHT, and EVLA). M.M.K. acknowledges support from the Hubble Fellowship and Carnegie-Princeton Fellowship. E.O.O. is supported by an Einstein Fellowship. H.B.P. is a CfA and Bikura prize fellow. The Weizmann Institute's participation in PTF is supported by grants to AGY from the Israel Science Foundation, the US-Israel Binational Science Foundation and the Minerva/ARCHES Prize. A.V.F. and his group at UC Berkeley acknowledge generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and National Science Foundation (NSF) grant AST-0908886. KAIT was constructed and supported by donations from Sun Microsystems, Inc., the Hewlett-Packard Company,\nAutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. Computational resources and data storage were contributed by NERSC, supported by U.S, DOE contract DE-AC02-05CH11231. P.E.N. acknowledges support from the U.S. DOE contract DE-FG02-06ER06-04. J.S.B. acknowledges support of an NSF-CDI grant 0941742, \"Real-time Classification of Massive Time-series Data Streams.\" M.S. acknowledges support from the Royal Society. L.B. acknowledges NSF grants PHY-11-25915 and AST-11-09174. D.C.L. acknowledges NSF grant AST-1009571. 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; it was made possible by the generous financial support of the W. M. Keck Foundation. 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. The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All spectra are available in digital form at WISEREP (Yaron & Gal-Yam 2012; http:www.weizmann.ac.il/astrophysics/wiserep/).\n\nPublished - 0004-637X_755_2_161.pdf
Submitted - 1111.6109v1.pdf
", "abstract": "From the first two seasons of the Palomar Transient Factory, we identify three peculiar transients (PTF09dav, PTF10iuv, PTF11bij) with five distinguishing characteristics: peak luminosity in the gap between novae and supernovae (M_R \u2248 - 15.5 to -16.5), rapid photometric evolution (t_(rise) \u224812-15 days), large photospheric velocities (\u22486000 to 11000 km s^(-1)), early spectroscopic evolution into nebular phase (\u22481 to 3 months) and peculiar nebular spectra dominated by Calcium. We also culled the extensive decade-long Lick Observatory Supernova Search database and identified an additional member of this group, SN 2007ke. Our choice of photometric and spectroscopic properties was motivated by SN 2005E (Perets et al. 2010). To our surprise, as in the case of SN 2005E, all four members of this group are also clearly offset from the bulk of their host galaxy. Given the well-sampled early and late-time light curves, we derive ejecta masses in the range of 0.4--0.7 M_\u2299. Spectroscopically, we find that there may be a diversity in the photospheric phase, but the commonality is in the unusual nebular spectra. Our extensive follow-up observations rule out standard thermonuclear and standard core-collapse explosions for this class of \"Calcium-rich gap\" transients. If the progenitor is a white dwarf, we are likely seeing a detonation of the white dwarf core and perhaps, even shock-front interaction with a previously ejected nova shell. In the less likely scenario of a massive star progenitor, a very non-standard channel specific to a low-metallicity environment needs to be invoked (e.g., ejecta fallback leading to black hole formation). Detection (or lack thereof) of a faint underlying host (dwarf galaxy, cluster) will provide a crucial and decisive diagnostic to choose between these alternatives.", "date": "2012-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "755", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 161", "id_number": "CaltechAUTHORS:20111216-133850759", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111216-133850759", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Einstein Fellowship" }, { "agency": "Israeli Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "AutoScope Corporation" }, { "agency": "Lick Observatory" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "Royal Society" }, { "agency": "NSF", "grant_number": "PHY-11-25915" }, { "agency": "NSF", "grant_number": "AST-11-09174" }, { "agency": "NSF", "grant_number": "AST-1009571" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/755/2/161", "primary_object": { "basename": "0004-637X_755_2_161.pdf", "url": "https://authors.library.caltech.edu/records/n8rm5-8zf04/files/0004-637X_755_2_161.pdf" }, "related_objects": [ { "basename": "1111.6109v1.pdf", "url": "https://authors.library.caltech.edu/records/n8rm5-8zf04/files/1111.6109v1.pdf" } ], "pub_year": "2012", "author_list": "Kasliwal, Mansi M.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/zzbg1-te088", "eprint_id": 31938, "eprint_status": "archive", "datestamp": "2023-09-14 19:26:49", "lastmod": "2023-10-23 20:50:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "David" } }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Juri\u0107-M", "name": { "family": "Juri\u0107", "given": "Mario" } }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ R." }, "orcid": "0000-0003-2451-5482" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "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": "Two Distant Halo Velocity Groups Discovered by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: halo \u2013 Galaxy: kinematics and dynamics \u2013 Galaxy: structure \u2013 stars: variables: RR Lyrae", "note": "\u00a9 2012 The American Astronomical Society.\nReceived 2012 March 7; accepted 2012 June 26; published 2012 August 2.\n\nJ.G.C. and B.S. thank NSF grant AST-0908139 to J.G.C for partial support, as do\nS.R.K (to NSF grant AST-1009987), and C.J.G (for a NASA grant). Support for this work\nwas provided by NASA through Hubble Fellowship grant 51256.01 awarded to E.N.K by the\nSpace Telescope Science Institute, which is operated by the Association of Universities for\nResearch in Astronomy, Inc., for NASA, under contract NAS 5-26555.\nWe thank the referee for a thorough review and suggestions which led to an improved\nmanuscript. B.S. would like to thank \u0179. Ivezi\u0107, B. Willman, and K. Vivas for useful discussions.\nWe thank I. Arcavi, A. Gal-Yam, P. Groot, A. Horesh, and D. Perley for observing at\nKeck and Palomar. We thank the staff at the Palomar Hale telescope for help and support\nwith observations. We are grateful to the many people who have worked to make the Keck\nTelescope and its instruments a reality and to operate and maintain the Keck Observatory.\nThe authors wish to extend special thanks to those of Hawaiian ancestry on whose sacred\nmountain we are privileged to be guests. Without their generous hospitality, none of the\nobservations presented herein would have been possible.\nThis article is based on observations obtained with the Samuel Oschin Telescope as part\nof the Palomar Transient Factory project, a scientific collaboration between the California\nInstitute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence\nBerkeley National Laboratory, the National Energy Research Scientific Computing Center,\nthe University of Oxford, and the Weizmann Institute of Science.\n\nPublished - 0004-637X_755_2_134.pdf
Submitted - 1206.0269v1.pdf
", "abstract": "We report the discovery of two new halo velocity groups (Cancer groups A and B) traced by 8 distant RR Lyrae stars and observed by the Palomar Transient Factory (PTF) survey at R.A.~129\u00b0, Dec~20\u00b0 (l~205\u00b0, b~32\u00b0). Located at 92 kpc from the Galactic center (86 kpc from the Sun), these are some of the most distant substructures in the Galactic halo known to date. Follow-up spectroscopic observations with the Palomar Observatory 5.1-m Hale telescope and W. M. Keck Observatory 10-m Keck I telescope indicate that the two groups are moving away from the Galaxy at v_(gsr) = 78.0+-5.6 km s^(-1) (Cancer group A) and v_(gsr) = 16.3+-7.1 km s^(-1) (Cancer group B). The groups have velocity dispersions of \u03c3_(v_)gsr))=12.4+-5.0 km s^(-1) and \u03c3 _(v_(gsr))=14.9+-6.2 km s^(-1), and are spatially extended (about several kpc) making it very unlikely that they are bound systems, and are more likely to be debris of tidally disrupted dwarf galaxies or globular clusters. Both groups are metal-poor (median metallicities of [Fe/H]^A = -1.6 dex and [Fe/H]^B =-2.1 dex), and have a somewhat uncertain (due to small sample size) metallicity dispersion of ~0.4 dex, suggesting dwarf galaxies as progenitors. Two additional RR Lyrae stars with velocities consistent with those of the Cancer groups have been observed ~25 \u00b0 east, suggesting possible extension of the groups in that direction.", "date": "2012-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "755", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 134", "id_number": "CaltechAUTHORS:20120618-134946055", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120618-134946055", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0908139" }, { "agency": "NSF", "grant_number": "AST-1009987" }, { "agency": "NASA Hubble Fellowship", "grant_number": "51256.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "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": "10.1088/0004-637X/755/2/134", "primary_object": { "basename": "0004-637X_755_2_134.pdf", "url": "https://authors.library.caltech.edu/records/zzbg1-te088/files/0004-637X_755_2_134.pdf" }, "related_objects": [ { "basename": "1206.0269v1.pdf", "url": "https://authors.library.caltech.edu/records/zzbg1-te088/files/1206.0269v1.pdf" } ], "pub_year": "2012", "author_list": "Sesar, Branimir; Cohen, Judith G.; et el." }, { "id": "https://authors.library.caltech.edu/records/d3km1-snz87", "eprint_id": 42977, "eprint_status": "archive", "datestamp": "2023-09-15 04:36:16", "lastmod": "2023-10-23 21:07:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "Julian C." }, "orcid": "0000-0003-2192-5371" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David R." }, "orcid": "0000-0002-5741-3047" }, { "id": "von-Braun-K", "name": { "family": "von Braun", "given": "Kaspar" }, "orcid": "0000-0002-5823-4630" }, { "id": "Kane-S-R", "name": { "family": "Kane", "given": "Stephen R." }, "orcid": "0000-0002-7084-0529" }, { "id": "Plavchan-P", "name": { "family": "Plavchan", "given": "Peter" }, "orcid": "0000-0002-8864-1667" }, { "id": "Crepp-J-R", "name": { "family": "Crepp", "given": "Justin R." }, "orcid": "0000-0003-0800-0593" }, { "id": "Howard-A-W", "name": { "family": "Howard", "given": "Andrew W." }, "orcid": "0000-0001-8638-0320" }, { "id": "Akeson-R-L", "name": { "family": "Akeson", "given": "Rachel L." }, "orcid": "0000-0001-9674-1564" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles A." }, "orcid": "0000-0002-5627-5471" }, { "id": "Boden-A-F", "name": { "family": "Boden", "given": "Andrew F." } }, { "id": "Gelino-D-M", "name": { "family": "Gelino", "given": "Dawn M." }, "orcid": "0000-0003-1274-2784" }, { "id": "Hoard-D-W", "name": { "family": "Hoard", "given": "D. W." }, "orcid": "0000-0002-6800-6519" }, { "id": "Ram\u00edrez-S-V", "name": { "family": "Ram\u00edrez", "given": "Solange V." } }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "John R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David B." } }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" }, { "id": "Fulton-B-J", "name": { "family": "Fulton", "given": "Benjamin J." }, "orcid": "0000-0003-3504-5316" } ] }, "title": "The PTF Orion Project: A Possible Planet Transiting a T-Tauri Star", "ispublished": "pub", "full_text_status": "public", "keywords": "open clusters and associations: individual (25 Ori); planets and satellites: detection; stars: individual (2MASS J05250755+0134243, CVSO 30, PTFO 8-8695, PTF1 J052507.55+013424.3); stars: pre-main sequence", "note": "\u00a9 2012 The American Astronomical Society. \n\nReceived 2011 October 24; accepted 2012 June 6; published 2012 July 25. \n\nThe authors acknowledge Tim Morton and Dimitri Veras for\ntheir helpful input. S.B.C. wishes to acknowledge generous support\nfrom Gary and Cynthia Bengier, the Richard and Rhoda\nGoldman Fund, National Aeronautics and Space Administration\n(NASA)/Swift grant NNX10AI21G, NASA/Fermi grant\nNNX1OA057G, and National Science Foundation (NSF) grant\nAST\u20130908886. S.M. acknowledges support from NSF awards\nAST-1006676, AST-1126413, PSARC, and the NASA Astrobiology\nInstitute.\nObservations obtained with the Samuel Oschin Telescope\nat the Palomar Observatory as part of the Palomar Transient\nFactory project, 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.\nThe Hobby\u2013Eberly Telescope (HET) is a joint project of\nthe University of Texas at Austin, the Pennsylvania State University,\nStanford University, Ludwig-Maximilians-Universit\u00e4t\nM\u00fcnchen, and Georg-August-Universit\u00e4t G\u00f6ttingen. The HET\nis named in honor of its principal benefactors, William P. Hobby\nand Robert E. Eberly.\nSome of the data presented herein were obtained at the\nW. M. Keck Observatory, which is operated as a scientific\npartnership among the California Institute of Technology, the\nUniversity of California and the National Aeronautics and\nSpace Administration. The Observatory was made possible by\nthe generous financial support of the W. M. Keck Foundation.\nThe authors wish to recognize and acknowledge the very\nsignificant cultural role and reverence that the summit of Mauna\nKea has always had within the indigenous Hawaiian community.\nWe are most fortunate to have the opportunity to conduct\nobservations from this mountain.\nThe Byrne Observatory at Sedgwick (BOS) is operated by\nthe Las Cumbres Observatory Global Telescope Network and\nis located at the Sedgwick Reserve, a part of the University of\nCalifornia Natural Reserve System.\nThis research has made use of the NASA Exoplanet Archive,\nwhich is operated by the California Institute of Technology,\nunder contract with the National Aeronautics and Space Administration\nunder the Exoplanet Exploration Program.\nThis publication makes use of data products from the Two\nMicron All Sky Survey, which is a joint project of the University\nof Massachusetts and the Infrared Processing and Analysis\nCenter/California Institute of Technology, funded by the National\nAeronautics and Space Administration and the National\nScience Foundation.\nThis research has made use of the VizieR catalog access\ntool, CDS, Strasbourg, France, and of the software package Uncertainties: a Python package for calculations with uncertainties,\nEric O. Lebigot.28\nThis work was partially supported by funding from the Center\nfor Exoplanets and Habitable Worlds. The Center for Exoplanets\nand Habitable Worlds is supported by the Pennsylvania State\nUniversity, the Eberly College of Science, and the Pennsylvania\nSpace Grant Consortium.\nSupport for this work was provided by an award issued by\nJPL/Caltech.\nFacilities: PO:1.2m (PTF), HET (HRS), Keck:I (HIRES),\nKeck:II (NIRC2), LCOGT (BOS), FTN, FTS, Mayall, Hale\n\nPublished - 0004-637X_755_1_42.pdf
Submitted - 1206.1510v2.pdf
", "abstract": "We report observations of a possible young transiting planet orbiting a previously known weak-lined T-Tauri star in the 7\u201310\u2009Myr old Orion-OB1a/25-Ori region. The candidate was found as part of the Palomar Transient Factory (PTF) Orion project. It has a photometric transit period of 0.448413 \u00b1 0.000040 days, and appears in both 2009 and 2010 PTF data. Follow-up low-precision radial velocity (RV) observations and adaptive optics imaging suggest that the star is not an eclipsing binary, and that it is unlikely that a background source is blended with the target and mimicking the observed transit. RV observations with the Hobby\u2013Eberly and Keck telescopes yield an RV that has the same period as the photometric event, but is offset in phase from the transit center by \u2248 \u2212 0.22 periods. The amplitude (half range) of the RV variations is 2.4\u2009km\u2009s^(\u22121) and is comparable with the expected RV amplitude that stellar spots could induce. The RV curve is likely dominated by stellar spot modulation and provides an upper limit to the projected companion mass of M_psin\u2009i_(orb) \u227e4.8 \u00b1 1.2\u2009M_(Jup); when combined with the orbital inclination, i_(orb), of the candidate planet from modeling of the transit light curve, we find an upper limit on the mass of the planetary candidate of M_p \u227e5.5 \u00b1 1.4\u2009M_(Jup). This limit implies that the planet is orbiting close to, if not inside, its Roche limiting orbital radius, so that it may be undergoing active mass loss and evaporation.", "date": "2012-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "755", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 42", "id_number": "CaltechAUTHORS:20131212-095046259", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131212-095046259", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NSF", "grant_number": "AST-1006676" }, { "agency": "NSF", "grant_number": "AST-1126413" }, { "agency": "Penn State Astrobiology Research Center (PSARC)" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Center for Exoplanets and Habitable Worlds" }, { "agency": "Pennsylvania State University" }, { "agency": "Eberly College of Science" }, { "agency": "Pennsylvania Space Grant Consortium" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/755/1/42", "primary_object": { "basename": "0004-637X_755_1_42.pdf", "url": "https://authors.library.caltech.edu/records/d3km1-snz87/files/0004-637X_755_1_42.pdf" }, "related_objects": [ { "basename": "1206.1510v2.pdf", "url": "https://authors.library.caltech.edu/records/d3km1-snz87/files/1206.1510v2.pdf" } ], "pub_year": "2012", "author_list": "van Eyken, Julian C.; Ciardi, David R.; et el." }, { "id": "https://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" }, "pub_year": "2012", "author_list": "Ofek, E. O.; Laher, R.; et el." }, { "id": "https://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" }, "pub_year": "2012", "author_list": "Laher, Russ R.; Rebull, Luisa M.; et el." }, { "id": "https://authors.library.caltech.edu/records/98ebq-gcb58", "eprint_id": 32666, "eprint_status": "archive", "datestamp": "2023-08-22 05:59:02", "lastmod": "2023-10-18 15:58:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Lou-Yu-Qing", "name": { "family": "Lou", "given": "Yu-Qing" } }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "Classical Novae in Andromeda: Light Curves from the Palomar Transient Factory and GALEX", "ispublished": "pub", "full_text_status": "public", "keywords": "globular clusters: general; novae, cataclysmic variables; surveys", "note": "\u00a9 2012 The American Astronomical Society.\nReceived 2012 January 12; accepted 2012 April 16; published 2012 June 5.\nWe thank the referee, Dr. Massimo Della Valle, for very helpful comments and suggestions to improve the manuscript. We thank Marina Orio and Sumin Tang for valuable discussions. We thank the Weizmann Monitoring Team (A. Gal-Yam, I. Arcavi, D. Polishook, A. Sternberg, O. Yaron, D. Xu) for daily monitoring of transient candidates from the PTF discovery stream. M.M.K. acknowledges support from the Hubble Fellowship and the Carnegie-Princeton Fellowship. S.B.C wishes to acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, National Aeronautics and Space Administration (NASA)/Swift grant NNX10AI21G, NASA/Fermi grant NNX1OA057G, and National Science Foundation (NSF) grant AST\u20130908886. This research was supported in part by Tsinghua Center for Astrophysics (THCA), by the National Natural Science Foundation of China (NSFC) grants 10373009, 10533020, and 11073014 at Tsinghua University, by the Ministry of Science and Technology (MOST) under State Key Development Program for Basic Research grant 2012CB821800, by the Tsinghua University Initiative Scientific Research Program, by the SRFDP 20050003088, 200800030071, and 20110002110008, and by the Yangtze Endowment from the Ministry of Education at Tsinghua University. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources and data storage for PTF. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - Cao2012p18931Astrophys_J.pdf
", "abstract": "We present optical light curves of 29 novae in M31 during the 2009 and 2010 observing seasons of the Palomar Transient Factory (PTF). The dynamic and rapid cadences in PTF monitoring of M31, from one day to ten minutes, provide excellent temporal coverage of nova light curves, enabling us to record the photometric evolution of M31 novae in unprecedented detail. We also detect eight of these novae in the near-ultraviolet (UV) band with the Galaxy Evolution Explorer (GALEX) satellite. Novae M31N 2009-10b and M31N 2010-11a show prominent UV emission peaking a few days prior to their optical maxima, possibly implying aspherical outbursts. Additionally, our blueshifted spectrum of the recent outburst of PT And (M31N 2010-12a) indicates that it is a recurrent nova in M31 and not a dwarf nova in the Milky Way as was previously assumed. Finally, we systematically searched for novae in all confirmed globular clusters (GCs) of M31 and found only M31N 2010-10f associated with Bol 126. The specific nova rate in the M31 GC system is thus about one per year, which is not enhanced relative to the rate outside the GC system.", "date": "2012-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "752", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No 133", "id_number": "CaltechAUTHORS:20120724-100019191", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120724-100019191", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10373009" }, { "agency": "National Natural Science Foundation of China", "grant_number": "10533020" }, { "agency": "National Natural Science Foundation of China", "grant_number": "11073014" }, { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "2012CB821800" }, { "agency": "Tsinghua University Initiative Scientific Research Program" }, { "agency": "SRFDP", "grant_number": "20050003088" }, { "agency": "SRFDP", "grant_number": "200800030071" }, { "agency": "SRFDP", "grant_number": "20110002110008" }, { "agency": "Ministry of Education Yangtze Endowment" }, { "agency": "Tsinghua Center for Astrophysics (THCA)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/752/2/133", "primary_object": { "basename": "Cao2012p18931Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/98ebq-gcb58/files/Cao2012p18931Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Cao, Yi; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/tytq9-xm811", "eprint_id": 32481, "eprint_status": "archive", "datestamp": "2023-08-22 05:58:10", "lastmod": "2023-10-18 14:27:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Parrent-J-T", "name": { "family": "Parrent", "given": "J. T." } }, { "id": "Cao-Yi", "name": { "family": "Cao", "given": "Y." }, "orcid": "0000-0002-8036-8491" }, { "id": "Konidaris-N-P", "name": { "family": "Konidaris", "given": "N." }, "orcid": "0000-0003-1905-2815" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } } ] }, "title": "Analysis of the Early-time Optical Spectra of SN 2011fe in M101", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (SN 2011fe)", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2012 April 18; accepted 2012 May 15; published 2012 May 31.\n\nThis work was supported by the Las Cumbres Observatory\nGlobal Telescope Network. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under contract no. DE-AC02-05CH11231.\nObservations were obtained as part of the Palomar Transient\nFactory project. The TNG is operated by the Fundacion Galileo Galilei\u2014INAF (Istituto Nazionale di Astrofisica). The LT and WHT are operated by the Isaac Newton Group. The three telescopes are located in the Spanish Observatorio of the Roque de Los Muchachos of the Instituto de Astrofisica de Canarias. Some observations were obtained at the Gemini\nObservatory (GN-2011B-Q-215), which is operated by the\nAssociation of Universities for Research in Astronomy, Inc.,\nunder a cooperative agreement with the NSF on behalf of the\nGemini partnership. Other observations were obtained with the 200 inch telescope at Palomar Observatory, the UH 2.2 m\ntelescope, which is part of the Nearby Supernova Factory II\nproject, and the Lick 3 m telescope, which is operated by the University of California. Some of the data presented herein were obtained at the W. M. Keck Observatory.\n\nPublished - Parrent2012p18828Astrophys_J_Lett.pdf
", "abstract": "The nearby Type Ia supernova (SN Ia) SN 2011fe in M101 (cz = 241 km s^(\u20131)) provides a unique opportunity to study the early evolution of a \"normal\" SN Ia, its compositional structure, and its elusive progenitor system. We present 18 high signal-to-noise spectra of SN 2011fe during its first month beginning 1.2 days post-explosion and with an average cadence of 1.8 days. This gives a clear picture of how various line-forming species are distributed within the outer layers of the ejecta, including that of unburned material (C+O). We follow the evolution of C II absorption features until they diminish near maximum light, showing overlapping regions of burned and unburned material between ejection velocities of 10,000 and 16,000 km s^(\u20131). This supports the notion that incomplete burning, in addition to progenitor scenarios, is a relevant source of spectroscopic diversity among SNe Ia. The observed evolution of the highly Doppler-shifted O I \u03bb7774 absorption features detected within 5 days post-explosion indicates the presence of O I with expansion velocities from 11,500 to 21,000 km s^(\u20131). The fact that some O I is present above C II suggests that SN 2011fe may have had an appreciable amount of unburned oxygen within the outer layers of the ejecta.", "date": "2012-06-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "752", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L26", "id_number": "CaltechAUTHORS:20120716-133338149", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120716-133338149", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Las Cumbres Observatory Global Telescope Network" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/752/2/L26", "primary_object": { "basename": "Parrent2012p18828Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/tytq9-xm811/files/Parrent2012p18828Astrophys_J_Lett.pdf" }, "pub_year": "2012", "author_list": "Parrent, J. T.; Cao, Y.; et el." }, { "id": "https://authors.library.caltech.edu/records/kt83c-bpc04", "eprint_id": 31451, "eprint_status": "archive", "datestamp": "2023-08-22 05:19:25", "lastmod": "2023-10-17 16:36:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Polishook-D", "name": { "family": "Polishook", "given": "D." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Waszczak-A", "name": { "family": "Waszczak", "given": "A." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Aharonson-O", "name": { "family": "Aharonson", "given": "O." }, "orcid": "0000-0001-9930-2495" }, { "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": "Klein-C", "name": { "family": "Klein", "given": "C." } }, { "id": "Bloom-J", "name": { "family": "Bloom", "given": "J." } }, { "id": "Brosch-N", "name": { "family": "Brosch", "given": "N." } }, { "id": "Prialnik-D", "name": { "family": "Prialnik", "given": "D." } }, { "id": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "C." }, "orcid": "0000-0003-4072-169X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P." }, "orcid": "0000-0002-3389-0586" }, { "id": "Poznanksi-D", "name": { "family": "Poznanksi", "given": "D." } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "Asteroid rotation periods from the Palomar Transient Factory survey", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; minor planets; asteroids: general", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS.\n\nIssue published online: 4 Apr. 2012; Article first published online: 28 Feb. 2012; Accepted 2011 December 23. Received 2011 December 22; in original form 2011 October 17.\n\nWe thank the referee for useful comments. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford and theWeizmann Institute of Science.\nThe Weizmann PTF partnership is funded in part by grants\nfrom the Israeli Science Foundation (ISF) to AG-Y. PTF Collaborative work between the Weizmann and Caltech groups is supported by the Binational Science Foundation (BSF) via grants to SRK and AG-Y. DPol further acknowledges support from the Benoziyo Center for Astrophysics and the Yeda-Sela Center at WIS. SRK and his group are partially supported by the NSF grant AST\u20130507734. SBC wishes to acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NASA/Swift grant NNX10AI21G, NASA/Fermi grant NNX1OA057G and National Science Foundation (NSF) grant AST\u20130908886.\n\nPublished - Polishook2012p18072Mon_Not_R_Astron_Soc.pdf
Supplemental Material - MNR_20462_sm_supmat.zip
", "abstract": "The Palomar Transient Factory (PTF) is a synoptic survey designed to explore the transient and variable sky in a wide variety of cadences. We use PTF observations of fields that were observed multiple times (\u227310) per night, for several nights, to find asteroids, construct their light curves and measure their rotation periods. Here we describe the pipeline we use to achieve these goals and present the results from the first four (overlapping) PTF fields analysed as part of this programme. These fields, which cover an area of 21 deg^2, were observed on four nights with a cadence of \u223c20 min. Our pipeline was able to detect 624 asteroids, of which 145 (\u224820 per cent) were previously unknown. We present high-quality rotation periods for 88 main-belt asteroids and possible period or lower limit on the period for an additional 85 asteroids. For the remaining 451 asteroids, we present lower limits on their photometric amplitudes. Three of the asteroids have light curves that are characteristic of binary asteroids. We estimate that implementing our search for all existing high-cadence PTF data will provide rotation periods for about 10 000 asteroids mainly in the magnitude range \u224814 to \u224820.", "date": "2012-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "421", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2094-2108", "id_number": "CaltechAUTHORS:20120514-102852818", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120514-102852818", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Benoziyo Center for Astrophysics and the Yeda-Sela Center at WIS" }, { "agency": "NSF", "grant_number": "AST\u20130507734" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST\u20130908886" } ] }, "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": "10.1111/j.1365-2966.2012.20462.x", "primary_object": { "basename": "MNR_20462_sm_supmat.zip", "url": "https://authors.library.caltech.edu/records/kt83c-bpc04/files/MNR_20462_sm_supmat.zip" }, "related_objects": [ { "basename": "Polishook2012p18072Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/kt83c-bpc04/files/Polishook2012p18072Mon_Not_R_Astron_Soc.pdf" } ], "pub_year": "2012", "author_list": "Polishook, D.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/tf8nz-mgj59", "eprint_id": 29930, "eprint_status": "archive", "datestamp": "2023-08-22 05:08:19", "lastmod": "2023-10-24 22:35:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P. A." }, "orcid": "0000-0001-6876-8284" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "S." }, "orcid": "0000-0001-6760-3074" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "A. V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D. B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "A." }, "orcid": "0000-0002-5936-1156" }, { "id": "Howell-J-L", "name": { "family": "Howell", "given": "J. L." } }, { "id": "Keliser-I-K-W", "name": { "family": "Kleiser", "given": "I. K. W." } }, { "id": "Nakar-E", "name": { "family": "Nakar", "given": "E." }, "orcid": "0000-0002-4534-7089" }, { "id": "Rabinak-I", "name": { "family": "Rabinak", "given": "I." } }, { "id": "Sari-R", "name": { "family": "Sari", "given": "R." }, "orcid": "0000-0002-1084-3656" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "J. M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "D." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N. M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "Evidence for a Compact Wolf-Rayet Progenitor for the Type Ic Supernova PTF 10vgv", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (PTF 10vgv)", "note": "\u00a9 2012 American Astronomical Society. Received 2011 October 25; accepted 2012 January 4; published 2012 February 8. We thank Boaz Katz and Eli Waxman for useful comments.\nPTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and UC Berkeley. Staff and computational resources were provided by NERSC, supported by the DOE Office of Science. Lick Observatory and\nthe Kast spectrograph are operated by the University of California. HET and its LRS are supported by UT Austin, the\nPennsylvania State University, Stanford, Ludwig-Maximilians-\nUniversit\u00e4t M\u00fcnchen, Georg-August-Universit\u00e4t G\u00f6ttingen, and\nthe Instituto de Astronomia de la Universidad Nacional Autonoma\nde Mexico. The EVLA is operated by NRAO for the NSF, under cooperative agreement by Associated Universities,\nInc. We thank the staffs of the above observatories\nfor their assistance. A.G. and S.R.K. acknowledge support\nfrom the BSF; A.G. further acknowledges support from\nthe ISF, FP7/IRG, Minerva, the Sieff Foundation, and the\nGerman\u2013Israeli Fund (GIF). A.V.F. and his group at UC Berkeley\nacknowledge generous financial assistance from Gary &\nCynthia Bengier, the Richard & Rhoda Goldman Fund, the\nTABASGO Foundation, and NSF grant AST-0908886. A.C.\nacknowledges support from LIGO, which was constructed by\nCaltech and MIT with funding from the NSF under cooperative\nagreementPHY-0757058, and partial support from NASA/Swift\ngrant NNH10ZDA001N.\n\nPublished - Corsi2012p17629Astrophys_J_Lett.pdf
", "abstract": "We present the discovery of PTF 10vgv, a Type Ic supernova (SN) detected by the Palomar Transient Factory, using the Palomar 48 inch telescope (P48). R-band observations of the PTF 10vgv field with P48 probe the SN emission from its very early phases (about two weeks before R-band maximum) and set limits on its flux in the week prior to the discovery. Our sensitive upper limits and early detections constrain the post-shock-breakout luminosity of this event. Via comparison to numerical (analytical) models, we derive an upper-limit of R \u227e 4.5 R_\u2609 (R \u227e 1 R_\u2609) on the radius of the progenitor star, a direct indication in favor of a compact Wolf-Rayet star. Applying a similar analysis to the historical observations of SN 1994I yields R \u227e 1/4 R_\u2609 for the progenitor radius of this SN.", "date": "2012-03-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "747", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L5", "id_number": "CaltechAUTHORS:20120402-091946766", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120402-091946766", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)" }, { "agency": "University of Texas" }, { "agency": "Pennsylvania State University" }, { "agency": "Stanford University" }, { "agency": "Ludwig-Maximilians-Universit\u00e4t M\u00fcnchen" }, { "agency": "Georg-August-Universit\u00e4t G\u00f6ttingen" }, { "agency": "Instituto de Astronomy de la Universidad Nacional Autonoma de Mexico" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Israel Science Foundation" }, { "agency": "European Research Council (ERC)" }, { "agency": "Minerva" }, { "agency": "Sieff Foundation" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "LIGO" }, { "agency": "NSF", "grant_number": "PHY-0757058" }, { "agency": "NASA", "grant_number": "NNH10ZDA001N" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Palomar-Transient-Factory" }, { "id": "LIGO" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/747/1/L5", "primary_object": { "basename": "Corsi2012p17629Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/tf8nz-mgj59/files/Corsi2012p17629Astrophys_J_Lett.pdf" }, "pub_year": "2012", "author_list": "Corsi, A.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/khwe2-rts76", "eprint_id": 29840, "eprint_status": "archive", "datestamp": "2023-08-22 05:01:22", "lastmod": "2023-10-24 22:29:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Tendulkar-S-P", "name": { "family": "Tendulkar", "given": "Shriharsh P." }, "orcid": "0000-0003-2548-2926" } ] }, "title": "PTF10iya: a short-lived, luminous flare from the nuclear region of a star-forming galaxy", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion discs; black hole physics; galaxies: active; galaxies: nuclei", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS. Accepted 2011 November 18. Received 2011 October 16; in original form 2011 March 3. Article first published online: 18 Jan 2012. We wish to thank S.A. Wright, K. Bundy and the anonymous referee for valuable comments and discussions regarding this manuscript. Follow-up data were obtained by the Palomar Transient Factory TDF Key Project.\nSBC and AVF wish to acknowledge generous support from\nGary and Cynthia Bengier, the Richard and Rhoda Goldman\nFund, NASA/Swift grant NNX10AI21G, NASA/Fermi grant\nNNX1OA057G, and NSF grant AST-0908886. NRB is supported\nthrough the Einstein Fellowship Program (NASA Cooperative\nAgreement NNG06DO90A). JSB and his group were partially supported\nby NASA/Swift Guest Investigator grants NNX09AQ66G\nand NNX10AF93G, and a SciDAC grant from the US Department\nof Energy. The Weizmann Institute PTF partnership is supported\nin part by grants from the Israeli Science Foundation to AG. Joint work by the Weizmann and Caltech groups is supported by a grant from the Binational Science Foundation toAGand SRK, and AG acknowledges further support from a EU/FP7 MarieCurie IRG fellowship. LB is supported by the NSF under grants PHY-0551164 and AST-0707633. P60 operations are funded in part by NASA through the Swift Guest Investigator Program (grant NNG06GH61G).\nWe acknowledge the use of public data from the Swift data\narchive. Some of the data presented herein were obtained at the\nW. 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. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPublished - Cenko2012p17529Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present the discovery and characterization of PTF10iya, a short-lived (\u0394t\u2248 10 d, with an optical decay rate of \u223c0.3 mag d^(\u22121)), luminous (M_(g') \u2248 -21) transient source found by the Palomar Transient Factory. The ultraviolet/optical spectral energy distribution is reasonably well fitted by a blackbody with T\u2248 (1\u20132) \u00d7 10^4 K and peak bolometric luminosity LBB\u2248 (1\u20135) \u00d7 10^(44) erg s^(\u22121) (depending on the details of the extinction correction). A comparable amount of energy is radiated in the X-ray band that appears to result from a distinct physical process. The location of PTF10iya is consistent with the nucleus of a star-forming galaxy (z= 0.224 05 \u00b1 0.000 06) to within 350 mas (99.7 per cent confidence radius), or a projected distance of less than 1.2 kpc. At first glance, these properties appear reminiscent of the characteristic 'big blue bump' seen in the near-ultraviolet spectra of many active galactic nuclei (AGNs). However, emission-line diagnostics of the host galaxy, along with a historical light curve extending back to 2007, show no evidence for AGN-like activity. We therefore consider whether the tidal disruption of a star by an otherwise quiescent supermassive black hole may account for our observations. Though with limited temporal information, PTF10iya appears broadly consistent with the predictions for the early 'super-Eddington' phase of a solar-type star being disrupted by a \u223c10^7 M_\u2299 black hole. Regardless of the precise physical origin of the accreting material, the large luminosity and short duration suggest that otherwise quiescent galaxies can transition extremely rapidly to radiate near the Eddington limit; many such outbursts may have been missed by previous surveys lacking sufficient cadence.", "date": "2012-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "420", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2684-2699", "id_number": "CaltechAUTHORS:20120326-093254516", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120326-093254516", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA Einstein Fellowship", "grant_number": "NNG06DO90A" }, { "agency": "NASA", "grant_number": "NNX09AQ66G" }, { "agency": "NASA", "grant_number": "NNX10AF93G" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Israeli Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "NSF", "grant_number": "PHY-0551164" }, { "agency": "NSF", "grant_number": "AST-0707633" }, { "agency": "NASA", "grant_number": "NNG06GH61G" }, { "agency": "W. M. Keck Foundation" }, { "agency": "SciDAC" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1111/j.1365-2966.2011.20240.x", "primary_object": { "basename": "Cenko2012p17529Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/khwe2-rts76/files/Cenko2012p17529Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2012", "author_list": "Cenko, S. Bradley; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/ax7wj-78a15", "eprint_id": 31945, "eprint_status": "archive", "datestamp": "2023-08-22 05:05:55", "lastmod": "2023-10-17 21:43:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abadie-J", "name": { "family": "Abadie", "given": "J." } }, { "id": "Abbott-B-P", "name": { "family": "Abbott", "given": "B. 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E." } }, { "id": "Mageswaran-M", "name": { "family": "Mageswaran", "given": "M." } }, { "id": "Mailand-K", "name": { "family": "Mailand", "given": "K." } }, { "id": "Maros-E", "name": { "family": "Maros", "given": "E." } }, { "id": "Marx-J-N", "name": { "family": "Marx", "given": "J. N." } }, { "id": "McIntyre-G", "name": { "family": "McIntyre", "given": "G." } }, { "id": "Meshkov-S", "name": { "family": "Meshkov", "given": "S." } }, { "id": "Nash-T", "name": { "family": "Nash", "given": "T." } }, { "id": "Ogin-G-H", "name": { "family": "Ogin", "given": "G. H." } }, { "id": "Osthelder-C", "name": { "family": "Osthelder", "given": "C." } }, { "id": "Patel-P", "name": { "family": "Patel", "given": "P." } }, { "id": "Pedraza-M", "name": { "family": "Pedraza", "given": "M." } }, { "id": "Phelps-M", "name": { "family": "Phelps", "given": "M." } }, { "id": "Price-L-R", "name": { "family": "Price", "given": "L. R." } }, { "id": "Privitera-S", "name": { "family": "Privitera", "given": "S." } }, { "id": "Robertson-N-A", "name": { "family": "Robertson", "given": "N. A." } }, { "id": "Sannibale-V", "name": { "family": "Sannibale", "given": "V." } }, { "id": "Santamar\u00eda-L", "name": { "family": "Santamar\u00eda", "given": "L." } }, { "id": "Searle-A-C", "name": { "family": "Searle", "given": "A. C." } }, { "id": "Seifert-F", "name": { "family": "Seifert", "given": "F." } }, { "id": "Sengupta-A-S", "name": { "family": "Sengupta", "given": "A. S." } }, { "id": "Singer-A", "name": { "family": "Singer", "given": "A." } }, { "id": "Singer-L", "name": { "family": "Singer", "given": "L." } }, { "id": "Smith-M-R", "name": { "family": "Smith", "given": "M. R." } }, { "id": "Stochino-A", "name": { "family": "Stochino", "given": "A." } }, { "id": "Taylor-R", "name": { "family": "Taylor", "given": "R." } }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Torrie-C-I", "name": { "family": "Torrie", "given": "C. I." } }, { "id": "Vass-S", "name": { "family": "Vass", "given": "S." } }, { "id": "Villar-A-E", "name": { "family": "Villar", "given": "A. E." } }, { "id": "Wallace-L", "name": { "family": "Wallace", "given": "L." } }, { "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "S. E." } }, { "id": "Willems-P-A", "name": { "family": "Willems", "given": "P. A." } }, { "id": "Yamamoto-Hiroaki", "name": { "family": "Yamamoto", "given": "H." } }, { "id": "Yeaton-Massey-D", "name": { "family": "Yeaton-Massey", "given": "D." } }, { "id": "Zhang-Liyuan", "name": { "family": "Zhang", "given": "L." }, "orcid": "0000-0002-0898-787X" }, { "id": "Zweizig-J", "name": { "family": "Zweizig", "given": "J." }, "orcid": "0000-0002-1521-3397" }, { "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Y." }, "orcid": "0000-0002-9730-9463" }, { "id": "Hong-T", "name": { "family": "Hong", "given": "T." } }, { "id": "Luan-J", "name": { "family": "Luan", "given": "J." } }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "C. D." }, "orcid": "0000-0003-4993-2055" }, { "id": "Somiya-Kentaro", "name": { "family": "Somiya", "given": "K." } }, { "id": "Vallisneri-M", "name": { "family": "Vallisneri", "given": "M." }, "orcid": "0000-0002-4162-0033" }, { "id": "Wen-L", "name": { "family": "Wen", "given": "L." } }, { "id": "Yang-H", "name": { "family": "Yang", "given": "H." } }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "R. W. P." } }, { "id": "Harms-J", "name": { "family": "Harms", "given": "J." }, "orcid": "0000-0002-7332-9806" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "K. S." } }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan J." }, "orcid": "0000-0002-0928-6784" } ] }, "title": "Implementation and testing of the first prompt search\n for gravitational wave transients with electromagnetic counterparts", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational waves; methods: observational", "note": "\u00a9 2012 ESO. Received: 6 October 2011. Accepted: 22 December 2011. Published online:\t29 March 2012. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of\nNiedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge\nthe support of gravitational wave research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educaci\u00f3n y Ciencia, the Conselleria d'Economia Hisenda i Innovaci\u00f3 of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by The Netherlands Organisation for Scientific Research, the\nPolish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space\nAdministration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. The authors acknowledge support for TAROT from the French Minist\u00e8re des Affaires \u00c9trang\u00e8res and Minist\u00e8re de l'Enseignement Sup\u00e9rieur et\nde la Recherche. The observations by ROTSE-III were supported by NASA grant NNX08AV63G and NSF grant PHY-0801007. The work with Swift was partially supported through a NASA grant/cooperative agreement number NNX09AL61G to the Massachusetts Institute of Technology. The contribution from the \"Pi of the Sky\" group was financed by the Polish Ministry of Science in 2008-2011 as a research project. We thank Joshua S. Bloom for useful discussions on the rates of PTF transients and their classification. This document has been assigned\nLIGO Laboratory document number LIGO-P1000061-v19.\n\nPublished - Abadie2012p18477Astron_Astrophys.pdf
", "abstract": "Aims. A transient astrophysical event observed in both gravitational wave (GW) and electromagnetic (EM) channels would yield rich scientific rewards. A first program initiating EM follow-ups to possible transient GW events has been developed and exercised by the LIGO and Virgo community in association with several partners. In this paper, we describe and evaluate the methods used to promptly identify and localize GW event candidates and to request images of targeted sky locations.\n\nMethods. During two observing periods (Dec. 17, 2009 to Jan. 8, 2010 and Sep. 2 to Oct. 20, 2010), a low-latency analysis pipeline was used to identify GW event candidates and to reconstruct maps of possible sky locations. A catalog of nearby galaxies and Milky Way globular clusters was used to select the most promising sky positions to be imaged, and this directional information was delivered to EM observatories with time lags of about thirty minutes. A Monte Carlo simulation has been used to evaluate the low-latency GW pipeline's ability to reconstruct source positions correctly.\n\nResults. For signals near the detection threshold, our low-latency algorithms often localized simulated GW burst signals to tens of square degrees, while neutron star/neutron star inspirals and neutron star/black hole inspirals were localized to a few hundred square degrees. Localization precision improves for moderately stronger signals. The correct sky location of signals well above threshold and originating from nearby galaxies may be observed with ~50% or better probability with a few pointings of wide-field telescopes.", "date": "2012-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "539", "publisher": "EDP Sciences", "pagerange": "Art. No. A124", "id_number": "CaltechAUTHORS:20120619-081035905", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120619-081035905", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "State of Niedersachsen/Germany" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Minist\u00e8re des Affaires Etrang\u00e8res" }, { "agency": "Minist\u00e8re de'l Enseignement Sup\u00e9rieur et de la Recherche" }, { "agency": "NASA", "grant_number": "NNX08AV63G" }, { "agency": "NSF", "grant_number": "PHY-0801007" }, { "agency": "NASA", "grant_number": "NNX09AL61G" }, { "agency": "Ministry of Science (Poland)" }, { "agency": "Max-Planck-Society" } ] }, "other_numbering_system": { "items": [ { "id": "P1000061-v19", "name": "LIGO Document" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Palomar-Transient-Factory" }, { "id": "LIGO" } ] }, "corp_creators": { "items": [ "LIGO Scientific Collaboration", "Virgo Collaboration" ] }, "doi": "10.1051/0004-6361/201118219", "primary_object": { "basename": "Abadie2012p18477Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/ax7wj-78a15/files/Abadie2012p18477Astron_Astrophys.pdf" }, "pub_year": "2012", "author_list": "Abadie, J.; Abbott, B. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/7b0bh-5ya23", "eprint_id": 31603, "eprint_status": "archive", "datestamp": "2023-08-22 04:56:24", "lastmod": "2023-10-17 18:42:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "Derek B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John" }, "orcid": "0000-0003-2251-0602" }, { "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": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "de-Bruyn-A-G", "name": { "family": "de Bruyn", "given": "A. G." } }, { "id": "Kamble-A", "name": { "family": "Kamble", "given": "Atish" }, "orcid": "0000-0003-0861-5168" }, { "id": "Wijers-R-A-M-J", "name": { "family": "Wijers", "given": "Ralph A. M. J." } }, { "id": "van-der-Horst-A-J", "name": { "family": "van der Horst", "given": "Alexander J." }, "orcid": "0000-0001-9149-6707" }, { "id": "Kouveliotou-C", "name": { "family": "Kouveliotou", "given": "Chryssa" }, "orcid": "0000-0003-1443-593X" }, { "id": "Podsiadlowski-P", "name": { "family": "Podsiadlowski", "given": "Philipp" } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Maguire-K", "name": { "family": "Maguire", "given": "Kate" }, "orcid": "0000-0002-9770-3508" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Shara-M-M", "name": { "family": "Shara", "given": "Michael" } } ] }, "title": "Early Radio and X-Ray Observations of the Youngest Nearby Type Ia Supernova PTF 11kly (SN 2011fe)", "ispublished": "pub", "full_text_status": "public", "keywords": "radio continuum: general; supernovae: general; X-rays: general", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 September 13; accepted 2011 October 25; published 2012 January 20. \n\nWe thank the CARMA and EVLA staff for promptly scheduling this target of opportunity. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We thank the ASTRON Radio Observatory for the generous and swift allocation of observing time. PTF is a fully automated, wide-field survey aimed at a systematic exploration of explosions and variable phenomena in optical wavelengths. The participating institutions are Caltech, Columbia University, Weizmann Institute of Science, Lawrence Berkeley Laboratory, University of Oxford, and University of California at Berkeley. The program is centered on a 12K \u00d7 8K, 7.8 square degree CCD array (CFH12K) re-engineered for the 1.2mOschin Telescope at the Palomar Observatory by Caltech Optical Observatories. Photometric follow-up is undertaken by the automated Palomar 1.5 m telescope. Research at Caltech is supported by grants from NSF and NASA. The Weizmann PTF partnership is supported in part by the Israeli Science Foundation via grants to A.G. Weizmann\u2013Caltech Collaboration is supported by a grant from the BSF to A.G. and S.R.K. A.G. further acknowledges the Lord Sieff of Brimpton Foundation. M.M.K. acknowledges support from a Hubble Fellowship and Carnegie\u2013Princeton Fellowship. We thank the ASTRON Radio Observatory for the generous and swift allocation of observing time. The Westerbork Synthesis Radio Telescope is operated by ASTRON (Netherlands Foundation for Radio Astronomy) with support from the Netherlands Organization for Scientific Research (NWO). A.J.v.d.H. was supported by NASA grant NNH07ZDA001-GLAST. S. B. C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. A.K. is partially supported by NSF award AST-1008353.\n\nPublished - Horesh2012p18198Astrophys_J.pdf
", "abstract": "On 2011 August 24 (UT) the Palomar Transient Factory (PTF) discovered PTF11kly (SN 2011fe), the youngest\nand most nearby Type Ia supernova (SN Ia) in decades. We followed this event up in the radio (centimeter and\nmillimeter bands) and X-ray bands, starting about a day after the estimated explosion time.We present our analysis\nof the radio and X-ray observations, yielding the tightest constraints yet placed on the pre-explosion mass-loss rate\nfrom the progenitor system of this supernova. We find a robust limit of \u1e40 \u227e 10^(\u22128)(w/100 km s^(\u22121))M_\u2609 yr^(\u22121) from\nsensitive X-ray non-detections, as well as a similar limit from radio data, which depends, however, on assumptions\nabout microphysical parameters. We discuss our results in the context of single-degenerate models for SNe Ia and\nfind that our observations modestly disfavor symbiotic progenitor models involving a red giant donor, but cannot\nconstrain systems accreting from main-sequence or sub-giant stars, including the popular supersoft channel. In\nview of the proximity of PTF11kly and the sensitivity of our prompt observations, we would have to wait for a long\ntime (a decade or longer) in order to more meaningfully probe the circumstellar matter of SNe Ia.", "date": "2012-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "746", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 21", "id_number": "CaltechAUTHORS:20120523-080543419", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120523-080543419", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Leicester Swift Science Data Centre" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Lord Sieff of Brimpton Foundation" }, { "agency": "NASA Hubble Fellowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "NASA", "grant_number": "NNH07ZDA001-GLAST" }, { "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" }, { "agency": "NSF", "grant_number": "AST-1008353" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/746/1/21", "primary_object": { "basename": "Horesh2012p18198Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7b0bh-5ya23/files/Horesh2012p18198Astrophys_J.pdf" }, "pub_year": "2012", "author_list": "Horesh, Assaf; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/eg4pc-jnf95", "eprint_id": 29470, "eprint_status": "archive", "datestamp": "2023-08-22 04:47:56", "lastmod": "2023-10-24 22:13:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-Nathan", "name": { "family": "Smith", "given": "Nathan" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Butler-N-R", "name": { "family": "Butler", "given": "Nat" } }, { "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": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "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": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Sesar-B", "name": { "family": "Sesar", "given": "Branimir" }, "orcid": "0000-0002-0834-3978" }, { "id": "Ben-Ami-S", "name": { "family": "Ben-Ami", "given": "Sagi" }, "orcid": "0000-0001-6760-3074" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Polishook-D", "name": { "family": "Polishook", "given": "David" } }, { "id": "Xu-Dong", "name": { "family": "Xu", "given": "Dong" } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" } ] }, "title": "SN 2010jp (PTF10aaxi): a jet in a Type II supernova", "ispublished": "pub", "full_text_status": "public", "keywords": "circumstellar matter; supernovae: general; supernovae: individual: SN 2010jp; ISM: jets and outflows", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS. \n\nAccepted 2011 October 28. Received 2011 October 27; in original form 2011 August 8. Article first published online: 13 Jan 2012. \n\nWe thank P. Challis and R. Kirshner for assistance with the MMT observations in 2010 November, and for providing the reduced spectrum from that night. SBC acknowledges generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. DP and EOO are supported by Einstein fellowships from NASA. The National Energy Research Scientific Computing Center, which\nis supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231, provided staff,\ncomputational resources and data storage for this project. The\nWeizmann\u2013PTF partnership is supported in part by grants from\nthe Israeli Science Foundation to AG. Collaborative Caltech\u2013WIS\nwork is supported by a grant from the Binational Science Foundation to AG and SRK. The work of AG is further supported by an FP7 Marie Curie IRG Fellowship and the Benoziyo Center for Astrophysics, and by the Lord Sieff of Brimpton Memorial Fund. JSB was partially supported by a grant from the National Science Foundation (NSF-CDI # 0941742). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The observatory was made possible by the generous financial support of the W. M. Keck Foundation.\nThe authors wish to recognize and acknowledge the very\nsignificant 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - Smith2012p17269Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present photometry and spectroscopy of the peculiar Type II supernova (SN) SN 2010jp, also named PTF10aaxi. The light curve exhibits a linear decline with a relatively low peak absolute magnitude of only \u221215.9 (unfiltered), and a low radioactive decay luminosity at late times, which suggests a low synthesized nickel mass of M (^(56) Ni) \u2272 0.003 M_\u2299. Spectra of SN 2010jp display an unprecedented triple-peaked H\u03b1 line profile, showing (1) a narrow (full width at half-maximum \u2273800 km s\u22121) central component that suggests shock interaction with dense circumstellar material (CSM); (2) high-velocity blue and red emission features centred at \u221212 600 and +15 400 km s^(\u22121), respectively; and (3) very broad wings extending from \u221222 000 to +25 000 km s\u22121. These features persist over multiple epochs during the \u223c100 d after explosion. We propose that this line profile indicates a bipolar jet-driven explosion, with the central component produced by normal SN ejecta and CSM interaction at mid and low latitudes, while the high-velocity bumps and broad-line wings arise in a non-relativistic bipolar jet. Two variations of the jet interpretation seem plausible: (1) a fast jet mixes ^(56)Ni to high velocities in polar zones of the H-rich envelope; or (2) the reverse shock in the jet produces blue and red bumps in Balmer lines when a jet interacts with dense CSM. Jet-driven Type II SNe are predicted for collapsars resulting from a wide range of initial masses above 25 M_\u2299, especially at subsolar metallicity. This seems consistent with the SN host environment, which is either an extremely low-luminosity dwarf galaxy or the very remote parts of an interacting pair of star-forming galaxies. It also seems consistent with the apparently low ^(56)Ni mass that may accompany black hole formation. We speculate that the jet survives to produce observable signatures because the star's H envelope was very low mass, having been mostly stripped away by the previous eruptive mass-loss indicated by the Type IIn features in the spectrum.", "date": "2012-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "420", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1135-1144", "id_number": "CaltechAUTHORS:20120224-154245659", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120224-154245659", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "GO-7100028" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Lord Sieff of Brimpton Memorial Fund" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1111/j.1365-2966.2011.20104.x", "primary_object": { "basename": "Smith2012p17269Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/eg4pc-jnf95/files/Smith2012p17269Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2012", "author_list": "Smith, Nathan; Cenko, S. Bradley; et el." }, { "id": "https://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" } ], "pub_year": "2012", "author_list": "Ofek, E. O.; Laher, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/cqxqe-s8c87", "eprint_id": 28661, "eprint_status": "archive", "datestamp": "2023-08-19 08:57:35", "lastmod": "2023-10-24 18:03:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Li-Weidong", "name": { "family": "Li", "given": "Weidong" } }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Exclusion of a luminous red giant as a companion star\n to the progenitor of supernova SN 2011fe", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 Macmillan Publishers Limited. \n\nReceived 07 September 2011. Accepted 14 October 2011. Published online 14 December 2011. \n\nWe thank D. Maoz and S. Starrfield for comments, and the staff of the W. M. Keck Observatory, especially J. Lyke and R. Campbell, for their assistance in obtaining the NIRC adaptive optics imaging. P.P. acknowledges discussions on symbiotic binaries with J. Mikolajewska. M.M.K. acknowledges support by NASA's\nHubble Fellowship and the Carnegie-Princeton Fellowship. J.S.B.'s group was partially supported by NASA. J.S.B., A.V.F., L.B. and S.W.J. acknowledge support from the US National Science Foundation. A.V.F.'s group at UC Berkeley, and the Katzman Automatic Imaging Telescope (KAIT) and its ongoing operation, have received financial assistance from NASA, Gary and Cynthia Bengier, the Richard &Rhoda Goldman Fund, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. E.O.O. is\nsupported by an Einstein Fellowship from NASA. M.M.S. and J.B. acknowledge the support of Hilary Lipsitz and the American Museum of Natural History for essential funding. M.S. acknowledges support from the Royal Society. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial\nsupport of the W. M. Keck Foundation. Observations were obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, La Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. The National Energy Research Scientific Computing Center, provided staff, computational resources, and data storage\nfor this project.\nAuthor Contributions: W.L., J.S.B., S.W.J., C.M. and B.P. analysed the Hubble Space\nTelescope photometry in the context of progenitor limits. P.P. contributed the analysis\nof progenitor models. A.A.M., J.W.R. and S.B.C. analysed historical imaging from the\nPalomar Transient Factory (PTF) and KAIT in the context of nova limits. M.M.K. and\nK.J.S. provided the analysis of Spitzer observations. M.M.S. and J.B. provided analysis of\nthe Hubble Space Telescope imaging. M.M.S. also contributed interpretation of the\nprogenitor limits. N.R.B., E.O.O. and L.B. contributed analysis and interpretation of the\nhistorical X-ray imaging. D.P., R.M.Q., S.R.K., N.M.L., E.O.O., S.B.C., M.S., D.A.H., J.S.B.,\nP.E.N., M.M.K., L.B. and K.M.were responsible for obtaining, reducing, and analysing the\nPTF observations. A.S. and H.-Y.S.obtained the Keck adaptive optics imaging and S.B.C.\nreduced and analysed those images. A.V.F., M.G., W.L. and J.M.S. were responsible for\nthe KAIT imaging and analysis.\n\nSupplemental Material - nature10646-s1.pdf
", "abstract": "Type Ia supernovae are thought to result from a thermonuclear explosion of an accreting white dwarf in a binary system, but little is known of the precise nature of the companion star and the physical properties of the progenitor system. There are two classes of models: double-degenerate (involving two white dwarfs in a close binary system) and single-degenerate models. In the latter, the primary white dwarf accretes material from a secondary companion until conditions are such that carbon ignites, at a mass of 1.38 times the mass of the Sun. The type Ia supernova SN 2011fe was recently detected in a nearby galaxy. Here we report an analysis of archival images of the location of SN 2011fe. The luminosity of the progenitor system (especially the companion star) is 10\u2013100 times fainter than previous limits on other type Ia supernova progenitor systems, allowing us to rule out luminous red giants and almost all helium stars as the mass-donating companion to the exploding white dwarf.", "date": "2011-12-15", "date_type": "published", "publication": "Nature", "volume": "480", "number": "7377", "publisher": "Nature Publishing Group", "pagerange": "348-350", "id_number": "CaltechAUTHORS:20120105-073059365", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120105-073059365", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Felllowship" }, { "agency": "Carnegie-Princeton Fellowship" }, { "agency": "NSF" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "TABASGO Foundation" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "Hilary Lipsitz" }, { "agency": "Royal Society" }, { "agency": "W. M. Keck Foundation" }, { "agency": "American Museum of Natural History" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature10646", "primary_object": { "basename": "nature10646-s1.pdf", "url": "https://authors.library.caltech.edu/records/cqxqe-s8c87/files/nature10646-s1.pdf" }, "pub_year": "2011", "author_list": "Li, Weidong; Ofek, Eran O.; et el." }, { "id": "https://authors.library.caltech.edu/records/qvazd-c1n68", "eprint_id": 28647, "eprint_status": "archive", "datestamp": "2023-08-22 04:22:43", "lastmod": "2023-10-24 18:03:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Howard-A-W", "name": { "family": "Howard", "given": "Andrew W." }, "orcid": "0000-0001-8638-0320" }, { "id": "Isaacson-H-T", "name": { "family": "Isaacson", "given": "Howard T." }, "orcid": "0000-0002-0531-1073" }, { "id": "Fulton-B-J", "name": { "family": "Fulton", "given": "Benjamin J." }, "orcid": "0000-0003-3504-5316" } ] }, "title": "Supernova SN 2011fe from an exploding carbon\u2013oxygen white dwarf star", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy; physics", "note": "\u00a9 2011 Nature Publishing Group, a division of Macmillan Publishers Limited.\n\nReceived 8 September; accepted 14 October 2011.\n\nThe PTF project 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. The National Energy Research Scientific Computing Center, supported by the Office of Science of the US Department of Energy (DOE), provided staff, computational resources and data storage for this project. P.E.N. acknowledges support from the US DOE Scientific Discovery through Advanced Computing programme. M.S. acknowledges support from the Royal Society. J.S.B. and L.B. were supported by the National Science\nFoundation (NSF). The work of A.V.F. is funded by the NSF, the TABASGO Foundation, Gary and Cynthia Bengier, and the Richard and Rhoda Goldman Fund. A.G. thanks the ISF and BSF. The Liverpool Telescope is operated 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 of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the staffs of\nthe many observatories at which data were obtained for their assistance.\n\nAuthor Contributions: P.E.N., M.S. and D.A.H. oversee the PTF programme on type Ia\nsupernovae. P.E.N. oversaw the preparation of the manuscript. M.S., D.B., K.M., Y.-C.P.,\nJ.L. and P.J. performed and reduced the FRODOSpec observations. S.B.C., M.T.K., A.V.F.\nand J.M.S. obtained and reduced the Lick spectrum. G.W.M., A.W.H. and H.T.I. obtained\nthe HIRES observations. S.B.C., J.S.B., S.R.K., M.M.K., N.M.L., E.O.O., R.M.Q. and D.P.\nassisted in the operation of the Palomar 48-inch telescope as part of the PTF\ncollaboration. R.C.T. and J.E.T. performed the SYNAPPS analysis. D.K., L.B. and P.P.\nassisted with the theoretical interpretation of our observations. N.S., B.J.F., J.T.P., D.S.,\nF.B.B., B.D., M.L.G., I.M.H., P.M., E.P., E.S.W. and A.G. assisted in follow-up observations of\nSN 2011fe.\n\nSubmitted - 1110.6201.pdf
Supplemental Material - nature10644-s1.pdf
", "abstract": "Type Ia supernovae have been used empirically as 'standard candles' to demonstrate the acceleration of the expansion of the Universe even though fundamental details, such as the nature of their progenitor systems and how the stars explode, remain a mystery. There is consensus that a white dwarf star explodes after accreting matter in a binary system, but the secondary body could be anything from a main-sequence star to a red giant, or even another white dwarf. This uncertainty stems from the fact that no recent type Ia supernova has been discovered close enough to Earth to detect the stars before explosion. Here we report early observations of supernova SN 2011fe in the galaxy M101 at a distance from Earth of 6.4 megaparsecs. We find that the exploding star was probably a carbon\u2013oxygen white dwarf, and from the lack of an early shock we conclude that the companion was probably a main-sequence star. Early spectroscopy shows high-velocity oxygen that slows rapidly, on a timescale of hours, and extensive mixing of newly synthesized intermediate-mass elements in the outermost layers of the supernova. A companion paper uses pre-explosion images to rule out luminous red giants and most helium stars as companions to the progenitor.", "date": "2011-12-15", "date_type": "published", "publication": "Nature", "volume": "480", "number": "7377", "publisher": "Nature Publishing Group", "pagerange": "344-347", "id_number": "CaltechAUTHORS:20120104-113414677", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120104-113414677", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)" }, { "agency": "Royal Society" }, { "agency": "NSF" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature10644", "primary_object": { "basename": "nature10644-s1.pdf", "url": "https://authors.library.caltech.edu/records/qvazd-c1n68/files/nature10644-s1.pdf" }, "related_objects": [ { "basename": "1110.6201.pdf", "url": "https://authors.library.caltech.edu/records/qvazd-c1n68/files/1110.6201.pdf" } ], "pub_year": "2011", "author_list": "Nugent, Peter E.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/tdwy8-saa24", "eprint_id": 28391, "eprint_status": "archive", "datestamp": "2023-08-19 08:52:21", "lastmod": "2023-10-24 17:51:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "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": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673" }, { "id": "Fulton-B-J", "name": { "family": "Fulton", "given": "Benjamin J." }, "orcid": "0000-0003-3504-5316" } ] }, "title": "SN 2011dh: Discovery of a Type IIb Supernova from a Compact Progenitor in the Nearby Galaxy M51", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: individual (PTF11eon/SN2011dh)", "note": "\u00a9 2011 American Astronomical Society. \n\nReceived 2011 June 19; accepted 2011 October 4; published 2011 November 4. \n\nThe Weizmann Institute PTF partnership is supported by the\nIsraeli Science Foundation via grants to A.G. Collaborative work between A.G. and S.R.K. is supported by the US-Israel Binational Science Foundation. A.G. further acknowledges support from the EU FP7 Marie Curie program via an IRG fellowship and a Minerva grant. P.E.N. is supported by the US Department of Energy Scientific Discovery through Advanced Computing program under contract DE-FG02-06ER06-04. M.S. acknowledges support from the Royal Society; M.S. and A.G. are also grateful for a Weizmann-UK Making Connections grant. A.V.F.'s supernova group at U.C. Berkeley acknowledges generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, US National Science Foundation grant AST-0908886, and the TABASGO Foundation. J.S.B. acknowledges support of an NSF-CDI grant 0941742 and NSF/AAG grant NSF/AST-100991. P.M., E.P., and E.S.W. acknowledge financial support from INAF through PRIN INAF 2009. Instrumentation at Wise Observatory was funded in part by the Israel Space Agency (ISA), the Max Planck Institute for Astronomy (MPA) in Heidelberg, Germany, the German Israeli Science Foundation for Research and Development, and the Israel Science Foundation. The WHT is operated by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Byrne Observatory at Sedgwick (BOS) is operated by the Las Cumbres Observatory Global Telescope Network. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of the W. M. Keck Foundation. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and supported by the Harvard University Milton Fund, the University of Virginia, SAO, UC Berkeley, and NASA via Swift Guest Investigator programs NNX09AQ66Q and NNX10A128G. We are grateful to the dedicated staffs at all of the observatories where we obtained data. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project.\n\nPublished - Arcavi2011p16472Astrophys_J_Lett.pdf
Submitted - 1106.3551.pdf
", "abstract": "On 2011 May 31 UT a supernova (SN) exploded in the nearby galaxy M51 (the Whirlpool Galaxy). We discovered this event using small telescopes equipped with CCD cameras and also detected it with the Palomar Transient Factory survey, rapidly confirming it to be a Type II SN. Here, we present multi-color ultraviolet through infrared photometry which is used to calculate the bolometric luminosity and a series of spectra. Our early-time observations indicate that SN 2011dh resulted from the explosion of a relatively compact progenitor star. Rapid shock-breakout cooling leads to relatively low temperatures in early-time spectra, compared to explosions of red supergiant stars, as well as a rapid early light curve decline. Optical spectra of SN 2011dh are dominated by H lines out to day 10 after explosion, after which He I lines develop. This SN is likely a member of the cIIb (compact IIb) class, with progenitor radius larger than that of SN 2008ax and smaller than the eIIb (extended IIb) SN 1993J progenitor. Our data imply that the object identified in pre-explosion Hubble Space Telescope images at the SN location is possibly a companion to the progenitor or a blended source, and not the progenitor star itself, as its radius (~10^(13) cm) would be highly inconsistent with constraints from our post-explosion spectra.", "date": "2011-12-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "742", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L18", "id_number": "CaltechAUTHORS:20111209-094859011", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111209-094859011", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "Royal Society" }, { "agency": "Weizmann-UK" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "NSF", "grant_number": "AST-100991" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN INAF 2009" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/742/2/L18", "primary_object": { "basename": "1106.3551.pdf", "url": "https://authors.library.caltech.edu/records/tdwy8-saa24/files/1106.3551.pdf" }, "related_objects": [ { "basename": "Arcavi2011p16472Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/tdwy8-saa24/files/Arcavi2011p16472Astrophys_J_Lett.pdf" } ], "pub_year": "2011", "author_list": "Arcavi, Iair; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/fj9vn-cdz11", "eprint_id": 29401, "eprint_status": "archive", "datestamp": "2023-08-22 04:18:10", "lastmod": "2023-10-24 22:09:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maguire-K", "name": { "family": "Maguire", "given": "K." }, "orcid": "0000-0002-9770-3508" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "R. S." }, "orcid": "0000-0001-7782-7071" }, { "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" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "PTF10ops \u2013 a subluminous, normal-width light curve Type Ia supernova in the middle of nowhere", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual: PTF10ops", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 July 27. Received 2011 July 27; in original form 2011 July 13. Article first published online: 26 Sep. 2011. MS acknowledges support from the Royal Society. AG-Y and MS\nacknowledge support from theWeizmann-UK 'making connection'\nprogramme. The Weizmann Institute\u2013PTF partnership is funded in\npart by the Israeli Science Foundation (ISF) via a grant to AG-Y.\nThe joint WIS\u2013Caltech activity is funded by a Binational Science\nFoundation (BSF) grant to AG-Y and SRK. AG-Y further acknowledges\nsupport from the EU/FP7 via a Marie Curie IRG fellowship\nand an ARCHES prize from the German BMBF. This work\nwas supported by the Science and Technology Facilities Council.\nEOO is supported by NASA grants. EOO and DP are both\nsupported by Einstein fellowships. SBC acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard &\nRhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-\n7100028, the TABASGOFoundation, andNSF grantAST-0908886.\nThis publication has been made possible by the participation of\nmore than 10 000 volunteers in the Galaxy Zoo Supernovae project,\nhttp://supernova.galaxyzoo.org/authors.\nThe WHT is operated on the island of La Palma by the Isaac Newton\nGroup in the Spanish Observatorio del Roque de losMuchachos\nof the Instituto de Astrof\u00b4\u0131sica de Canarias. The Liverpool Telescope\nis operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of\nthe Instituto de Astrofisica de Canarias with financial support from\nthe UK Science and Technology Facilities Council. Observations\nwere obtained with the Samuel Oschin Telescope at the Palomar\nObservatory as part of the Palomar Transient factory project, a\nscientific collaboration between the California Institute of Technology, Columbia Unversity, La Cumbres Observatory, the Lawrence\nBerkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data were obtained with 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. These observations were made possible by the generous financial support of the W. M. Keck Foundation. SNIFS on the UH2.2-m telescope is part of the Nearby Supernova Factory II project, a scientific collaboration among the Centre de Recherche Astronomique de Lyon, Institut de Physique Nucl\u00e9aire de Lyon, Laboratoire de Physique Nucl\u00e9aire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and the Centre de Physique des Particules de Marseille. Based on observations made with the NASA/ESA Hubble Space Telescope, data were 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\nNASA contract NAS 5-26555.\" This research has made use of the NASA/IPAC Extragalactic Data base (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - Maguire2011p17140Mon_Not_R_Astron_Soc.pdf
", "abstract": "PTF10ops is a Type Ia supernova (SN Ia), whose light curve and spectral properties place it outside the current SN Ia subtype classifications. Its spectra display the characteristic lines of subluminous SNe Ia, but it has a normal-width light curve with a long rise time, typical of normal-luminosity SNe Ia. The early-time optical spectra of PTF10ops were modelled using a spectral fitting code and found to have all the lines typically seen in subluminous SNe Ia, without the need to invoke more uncommon elements. The host galaxy environment of PTF10ops is also unusual with no galaxy detected at the position of the SN down to an absolute limiting magnitude of r\u2265\u221212.0 mag, but a very massive galaxy is present at a separation of \u223c148 kpc and at the same redshift as suggested by the SN spectral features. The progenitor of PTF10ops is most likely a very old star, possibly in a low-metallicity environment, which affects its explosion mechanism and observational characteristics. PTF10ops does not easily fit into any of the current models of either subluminous or normal SN Ia progenitor channels.", "date": "2011-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "418", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "747-758", "id_number": "CaltechAUTHORS:20120222-073817268", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120222-073817268", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "Weizmann-UK" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA Einstein Fellowship" }, { "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" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NAS5-26555" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1111/j.1365-2966.2011.19526.x", "primary_object": { "basename": "Maguire2011p17140Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/fj9vn-cdz11/files/Maguire2011p17140Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Maguire, K.; Ellis, R. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/pfn3z-qhy02", "eprint_id": 28463, "eprint_status": "archive", "datestamp": "2023-08-22 04:08:39", "lastmod": "2023-10-24 17:55:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Van-Dyk-S-D", "name": { "family": "Van Dyk", "given": "Schuyler D." }, "orcid": "0000-0001-9038-9950" }, { "id": "Li-Weidong", "name": { "family": "Li", "given": "Weidong" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Kraus-A-L", "name": { "family": "Kraus", "given": "Adam L." }, "orcid": "0000-0001-9811-568X" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Polishook-D", "name": { "family": "Polishook", "given": "David" } } ] }, "title": "The Progenitor of Supernova 2011dh/PTF11eon In Messier 51", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 5194); stars: evolution; supernovae: general; supernovae: individual (SN 2011dh)", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 June 15; accepted 2011 October 5; published 2011 October 18. \n\nThis work was based in part on observations made with the\nNASA/ESA Hubble Space Telescope, obtained from the Data\nArchive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS 05-26555;\nthe W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, with generous financial support from the W. M. Keck Foundation; and the Lick Observatory, operated by the University of California. KAIT and its ongoing research were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, Auto-Scope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. We thank the staffs of the Lick and\nKeck Observatories for their assistance with the observations. We thank Peter Nugent for useful comments, and the referee for helpful suggestions which improved this manuscript. Support for this research was provided by NASA through grants GO-11575, AR-11248, and AR-12126 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. A.V.F. and his group at UC Berkeley also acknowledge generous support from\nGary and Cynthia Bengier, the Richard and Rhoda Goldman\nFund, NASA/Swift grant NNX10AI21G, NASA/Fermi grant\nNNX1OA057G, NSF grant AST\u20130908886, and the TABASGO\nFoundation. A.G. is supported by the ISF. E.O.O. is supported by an Einstein Fellowship and NASA grants. J.M.S. thanks Marc J. Staley for a graduate fellowship.\nFacilities: Keck:II, Keck:I, HST (ACS), Spitzer (IRAC),\nGALEX, KAIT\n\nPublished - VanDyk2011p16476Astrophys_J_Lett.pdf
", "abstract": "We have identified a luminous star at the position of supernova (SN) 2011dh/PTF11eon, in pre-SN archival, multi-band images of the nearby, nearly face-on galaxy Messier 51 (M51) obtained by the Hubble Space Telescope with the Advanced Camera for Surveys. This identification has been confirmed, to the highest available astrometric precision, using a Keck-II adaptive-optics image. The available early-time spectra and photometry indicate that the SN is a stripped-envelope, core-collapse Type IIb, with a more compact progenitor (radius ~ 10^(11) cm) than was the case for the well-studied SN IIb 1993J. We infer that the extinction to SN 2011dh and its progenitor arises from a low Galactic foreground contribution, and that the SN environment is of roughly solar metallicity. The detected object has absolute magnitude M^0_V \u2248 \u20137.7 and effective temperature ~6000 K. The star's radius, ~10^(13) cm, is more extended than what has been inferred for the SN progenitor. We speculate that the detected star is either an unrelated star very near the position of the actual progenitor, or, more likely, the progenitor's companion in a mass-transfer binary system. The position of the detected star in a Hertzsprung-Russell diagram is consistent with an initial mass of 17-19 M_\u2609. The light of this star could easily conceal, even in the ultraviolet, the presence of a stripped, compact, very hot (~10^5 K), nitrogen-rich Wolf-Rayet star progenitor.", "date": "2011-11-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "741", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L28", "id_number": "CaltechAUTHORS:20111214-095212608", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111214-095212608", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Caltech" }, { "agency": "University of California" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Lick Observatory" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "AutoScope Corporation" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "TABASGO Foundation" }, { "agency": "NASA", "grant_number": "GO-11575" }, { "agency": "NASA", "grant_number": "AR-11248" }, { "agency": "NASA", "grant_number": "AR-12126" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "Israel Science Foundation" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "Marc J. Staley" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/741/2/L28", "primary_object": { "basename": "VanDyk2011p16476Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/pfn3z-qhy02/files/VanDyk2011p16476Astrophys_J_Lett.pdf" }, "pub_year": "2011", "author_list": "Van Dyk, Schuyler D.; Li, Weidong; et el." }, { "id": "https://authors.library.caltech.edu/records/m1ejz-pvg60", "eprint_id": 28919, "eprint_status": "archive", "datestamp": "2023-08-22 04:09:16", "lastmod": "2023-10-24 18:14:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Corsi-A", "name": { "family": "Corsi", "given": "A." }, "orcid": "0000-0001-8104-3536" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "PTF 10bzf (SN 2010ah): A Broad-Line Ic Supernova Discovered by the Palomar Transient Factory", "ispublished": "pub", "full_text_status": "public", "keywords": "gamma-ray burst: general; radiation mechanisms: non-thermal; supernovae: general; supernovae: individual (PTF 10bzf)", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 January 21; accepted 2011 August 7; published 2011 October 19. \nPTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and Berkeley. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. E.O.O. is supported by an Einstein Fellowship and NASA grants. D.P. is supported by an Einstein fellowship. The Weizmann Institute PTF partnership is supported in part by grants from the Israeli Science Foundation (ISF) to A.G. Joint work by the Weizmann and Caltech groups is supported by a grant from the Binational Science Foundation (BSF) to A.G. and S.R.K. A.G. acknowledges further support from an EU/FP7 Marie Curie IRG fellowship and a research grant from the Peter and Patricia Gruber Awards. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva (Argentina). The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. LAIWO, a wide-angle camera operating on the 1 m telescope at the Wise Observatory, Israel, was built at the Max Planck Institute for Astronomy (MPIA) in Heidelberg, Germany, with financial support from the MPIA, and grants from the German Israeli Science Foundation for Research and Development, and from the Israel Science Foundation. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation. We are grateful to IPN collaborators S. Golenetskii, R. Aptekar, E. Mazets, D. Frederiks, and T. Cline for the Konus data; to M. Briggs and C. Meegan for the Fermi data; to T. Takahashi, Y. Terada, M. Tashiro, Y. Fukazawa, T. Murakami, M. Ohno, and K. Makishima for the Suzaku data; to S. Barthelmy, N. Gehrels, H. Krimm, and D. Palmer for the Swift data; to D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, C. Fellows, K. Harshman, and R. Starr for the Odyssey data; and to A. von Kienlin and X. Zhang for the INTEGRAL data. K.H. acknowledges support from the following NASA sources: NNX09AV61G (Suzaku), NNX10AI23G (Swift), NNX10AU34G (Fermi), and NNX07AR71G (MESSENGER). S.B.C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. A.C. and S.R.K. acknowledge partial support from NASA/Swift Guest Investigator Program Cycle 7 (NNH10ZDA001N).\n\nPublished - Corsi2011p16858Astrophys_J.pdf
", "abstract": "We present the discovery and follow-up observations of a broad-line Type Ic supernova (SN), PTF 10bzf (SN 2010ah), detected by the Palomar Transient Factory (PTF) on 2010 February 23. The SN distance is \u2245218 Mpc, greater than GRB 980425/SN 1998bw and GRB 060218/SN 2006aj, but smaller than the other SNe firmly associated with gamma-ray bursts (GRBs). We conducted a multi-wavelength follow-up campaign with Palomar 48 inch, Palomar 60 inch, Gemini-N, Keck, Wise, Swift, the Allen Telescope Array, Combined Array for Research in Millimeter-wave Astronomy, Westerbork Synthesis Radio Telescope, and Expanded Very Large Array. Here we compare the properties of PTF 10bzf with those of SN 1998bw and other broad-line SNe. The optical luminosity and spectral properties of PTF 10bzf suggest that this SN is intermediate, in kinetic energy and amount of ^(56)Ni, between non-GRB-associated SNe like 2002ap or 1997ef, and GRB-associated SNe like 1998bw. No X-ray or radio counterpart to PTF 10bzf was detected. X-ray upper limits allow us to exclude the presence of an underlying X-ray afterglow as luminous as that of other SN-associated GRBs such as GRB 030329 or GRB 031203. Early-time radio upper limits do not show evidence for mildly relativistic ejecta. Late-time radio upper limits rule out the presence of an underlying off-axis GRB, with energy and wind density similar to the SN-associated GRB 030329 and GRB 031203. Finally, by performing a search for a GRB in the time window and at the position of PTF 10bzf, we find that no GRB in the interplanetary network catalog could be associated with this SN.", "date": "2011-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "741", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 76", "id_number": "CaltechAUTHORS:20120123-115808955", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120123-115808955", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "Gemini partnership" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "National Research Council of Canada" }, { "agency": "CONICYT (Chile)" }, { "agency": "Australian Research Council" }, { "agency": "Minist\u00e9rio da Ci\u00eancia e Tecnologia (Brazil)" }, { "agency": "Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva (Argentina)" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Max Planck Institute for Astronomy (MPIA)" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "NASA", "grant_number": "NNX09AV61G" }, { "agency": "NASA", "grant_number": "NNX10AI23G" }, { "agency": "NASA", "grant_number": "NNX10AU34G" }, { "agency": "NASA", "grant_number": "NNX07AR71G" }, { "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" }, { "agency": "NASA", "grant_number": "NNH10ZDA001N" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/741/2/76", "primary_object": { "basename": "Corsi2011p16858Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/m1ejz-pvg60/files/Corsi2011p16858Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Corsi, A.; Ofek, E. O.; et el." }, { "id": "https://authors.library.caltech.edu/records/pq1kn-m6g40", "eprint_id": 28293, "eprint_status": "archive", "datestamp": "2023-08-22 03:58:07", "lastmod": "2023-10-24 17:47:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ag\u00fceros-M-A", "name": { "family": "Ag\u00fceros", "given": "Marcel A." }, "orcid": "0000-0001-7077-3664" }, { "id": "Covey-K-R", "name": { "family": "Covey", "given": "Kevin R." }, "orcid": "0000-0001-6914-7797" }, { "id": "Lemonias-J-J", "name": { "family": "Lemonias", "given": "Jenna J." } }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Kraus-A-L", "name": { "family": "Kraus", "given": "Adam" }, "orcid": "0000-0001-9811-568X" }, { "id": "Batalha-N-M", "name": { "family": "Batalha", "given": "Natasha" } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "The Factory and the Beehive. I. Rotation Periods for Low-Mass Stars in Praesepe", "ispublished": "pub", "full_text_status": "public", "keywords": "open clusters and associations: individual (Praesepe); stars: rotation; surveys; techniques: photometric", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 June 23; accepted 2011 July 19; published 2011 October 4. We thank Sydney Barnes for detailed discussions of his models, and Mark Giampapa, Joel Hartman, Jonathan Irwin, Steve Saar, and Aleks Scholz for their useful comments on a draft of the paper. We are grateful to Janet Jacobsen for her\ncontributions to the PTF infrastructure; without her efforts, this work would not have been possible. Finally, we thank the referee for a very prompt review of this manuscript, and for several helpful suggestions that improved it. K.R.C. and A.L.K. acknowledge support provided by NASA\nthrough Hubble Fellowship grants HST-HF-51253.01 and 51257.01 awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science.\nThis research has made use of NASA's Astrophysics Data System Bibliographic Services, the SIMBAD database, operated at CDS, Strasbourg, France, the NASA/IPAC Extragalactic Database, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and the VizieR database of astronomical catalogs (Ochsenbein et al. 2000). IRAF (Image\nReduction and Analysis Facility) 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. The Two Micron All Sky Survey was a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (California Institute of Technology). The\nUniversity of Massachusetts was responsible for the overall management of the project, the observing facilities, and the data acquisition. The Infrared Processing and Analysis Center was responsible for data processing, data distribution, and data archiving.\n\nPublished - Agueeros2011p16389Astrophys_J.pdf
", "abstract": "Stellar rotation periods measured from single-age populations are critical for investigating how stellar angular momentum content evolves over time, how that evolution depends on mass, and how rotation influences the stellar dynamo and the magnetically heated chromosphere and corona. We report rotation periods for 40 late-K to mid-M star members of the nearby, rich, intermediate-age (~600 Myr) open cluster Praesepe. These rotation periods were derived from ~200 observations taken by the Palomar Transient Factory of four cluster fields from 2010 February to May. Our measurements indicate that Praesepe's mass-period relation transitions from a well-defined singular relation to a more scattered distribution of both fast and slow rotators at ~0.6 M_\u2609. The location of this transition is broadly consistent with expectations based on observations of younger clusters and the assumption that stellar spin-down is the dominant mechanism influencing angular momentum evolution at 600 Myr. However, a comparison to data recently published for the Hyades, assumed to be coeval to Praesepe, indicates that the divergence from a singular mass-period relation occurs at different characteristic masses, strengthening the finding that Praesepe is the younger of the two clusters. We also use previously published relations describing the evolution of rotation periods as a function of color and mass to evolve the sample of Praesepe periods in time. Comparing the resulting predictions to periods measured in M35 and NGC 2516 (~150 Myr) and for kinematically selected young and old field star populations suggests that stellar spin-down may progress more slowly than described by these relations.", "date": "2011-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "740", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 110", "id_number": "CaltechAUTHORS:20111205-105516419", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111205-105516419", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51235.01" }, { "agency": "NASA", "grant_number": "51257.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/740/2/110", "primary_object": { "basename": "Agueeros2011p16389Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/pq1kn-m6g40/files/Agueeros2011p16389Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Ag\u00fceros, Marcel A.; Covey, Kevin R.; et el." }, { "id": "https://authors.library.caltech.edu/records/vkyzq-w2f49", "eprint_id": 42914, "eprint_status": "archive", "datestamp": "2023-08-22 03:54:13", "lastmod": "2023-10-25 23:08:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levitan-D-B", "name": { "family": "Levitan", "given": "David" } }, { "id": "Fulton-B-J", "name": { "family": "Fulton", "given": "Benjamin J." }, "orcid": "0000-0003-3504-5316" }, { "id": "Groot-P-J", "name": { "family": "Groot", "given": "Paul J." }, "orcid": "0000-0002-4488-726X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Shporer-A", "name": { "family": "Shporer", "given": "Avi" }, "orcid": "0000-0002-1836-3120" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Horesh-A", "name": { "family": "Horesh", "given": "Assaf" }, "orcid": "0000-0002-5936-1156" } ] }, "title": "PTF1 J071912.13+485834.0: An Outbursting AM CVn System Discovered by a Synoptic Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "accretion, accretion disks; binaries: close; novae, cataclysmic variables; stars: individual (PTF1 J071912.13+485834.0); white dwarfs", "note": "\u00a9 2011 The American Astronomical Society.\n\nReceived 2011 May 9; accepted 2011 July 6; published 2011 September 7.\n\nObservations obtained with the Samuel Oschin Telescope\nat the Palomar Observatory as part of the Palomar Transient\nFactory project, a scientific collaboration between the California\nInstitute of Technology, Columbia University, Las Cumbres\nObservatory, the Lawrence Berkeley National Laboratory,\nthe National Energy Research Scientific Computing Center, the\nUniversity of Oxford, and the Weizmann Institute of Science.\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. The William\nHerschel Telescope is operated on the island of La Palma by the\nIsaac Newton Group in the Spanish Observatorio del Roque de\nlos Muchachos of the Instituto de Astrof\u00edsica de Canarias. This\npaper uses observations obtained with facilities of the Las Cumbres\nObservatory Global Telescope. The Byrne Observatory at\nSedgwick (BOS) is operated by the Las Cumbres Observatory\nGlobal Telescope Network and is located at the Sedgwick Reserve,\na part of the University of California Natural Reserve\nSystem.\nS.B.C. acknowledges generous support from Gary and\nCynthia Bengier, the Richard and Rhoda Goldman Fund, National\nAeronautics and Space Administration (NASA)/Swift\ngrant NNX10AI21G, NASA/Fermi grant NNX1OA057G, and\nNational Science Foundation (NSF) grant AST\u20130908886.\nFacilities: PO:1.2m, PO:1.5m, LCOGT, FTN (Spectral),\nHale (DBSP), ING:Herschel (ACAM), Keck:I (LRIS)\n\nPublished - 0004-637X_739_2_68.pdf
Submitted - 1107.1209v1.pdf
", "abstract": "We present extensive photometric and spectroscopic observations of PTF1 J071912.13+485834.0, an outbursting AM CVn system discovered by the Palomar Transient Factory (PTF). AM CVn systems are stellar binaries with some of the smallest separations known and orbital periods ranging from 5 to 65 minutes. They are believed to be composed of a white dwarf accretor and a (semi-)degenerate He-rich donor and are considered to be the helium equivalents of cataclysmic variables (CVs). We have spectroscopically and photometrically identified an orbital period of 26.77 \u00b1 0.02 minutes for PTF1 J071912.13+485834.0 and found a super-outburst recurrence time of greater than 65 days along with the presence of \"normal\" outbursts\u2014rarely seen in AM CVn systems but well known in super-outbursting CVs. We present a long-term light curve over two super-cycles as well as high-cadence photometry of both outburst and quiescent stages, both of which show clear variability. We also compare both the outburst and quiescent spectra of PTF1 J071912.13+485834.0 to other known AM CVn systems, and use the quiescent phase-resolved spectroscopy to determine the origin of the photometric variability. Finally, we draw parallels between the different subclasses of SU UMa-type CVs and outbursting AM CVn systems. We conclude by predicting that the PTF may more than double the number of outbursting AM CVn systems known, which would greatly increase our understanding of AM CVn systems.", "date": "2011-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "739", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 68", "id_number": "CaltechAUTHORS:20131210-081051957", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131210-081051957", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/739/2/68", "primary_object": { "basename": "0004-637X_739_2_68.pdf", "url": "https://authors.library.caltech.edu/records/vkyzq-w2f49/files/0004-637X_739_2_68.pdf" }, "related_objects": [ { "basename": "1107.1209v1.pdf", "url": "https://authors.library.caltech.edu/records/vkyzq-w2f49/files/1107.1209v1.pdf" } ], "pub_year": "2011", "author_list": "Levitan, David; Fulton, Benjamin J.; et el." }, { "id": "https://authors.library.caltech.edu/records/v0a8t-myq97", "eprint_id": 25180, "eprint_status": "archive", "datestamp": "2023-08-22 03:24:01", "lastmod": "2023-10-24 15:40:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "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" } ] }, "title": "Real-time Detection and Rapid Multiwavelength Follow-up Observations of a Highly Subluminous Type II-P Supernova from the Palomar Transient Factory Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (PTF10vdl)", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 January 23; accepted 2011 May 15; published 2011 July 19. This paper is dedicated to the memory of our dear colleague,\nJ. Jacobsen, who contributed significantly to the success of this project. The Palomar Transient Factory project 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. Weizmann Institute participation in PTF is supported in part by grants from the Israeli Science\nFoundation (ISF) to A.G.-Y. Joint Weizmann-Caltech activity\nis supported by a grant from the Binational Science Foundation to A.G.-Y. and S.R.K. Support for Weizmann-UK collaborative work is provided by a Weizmann-UK \"making connections\" grant to A.G.-Y. and M.S. Joint activity by A.G.-Y. and P.A.M. is supported by a Weizmann-MINERVA grant. A.G.-Y. further acknowledges support from an EU/FP7 Marie Curie IRG Fellowship. E.O.O. and D.P. are grateful to NASA for Einstein Fellowships. The work of A.V.F.'s group at UC Berkeley is funded by US National Science Foundation (NSF) grant AST-0908886, the TABASGO Foundation, Gary and Cynthia Bengier, and the Richard and Rhoda Goldman Fund.\nLAIWO, a wide-angle camera operating on the 1m telescope\nat the Wise Observatory, Israel, was built at the Max Planck\nInstitute for Astronomy (MPIA) in Heidelberg, Germany, with\nfinancial support from the MPIA, grants from the German Israeli Science Foundation for Research and Development, and the ISF. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. The National Energy Research Scientific Computing Center, which is supported by the Office\nof Science of the U.S. Department of Energy under Contract\nNo. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. P.E.N. acknowledges support from the U.S. Department of Energy Scientific Discovery through Advanced Computing program under contract DE-FG02-06ER06-04. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership\namong 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. We thank the staffs of the many observatories at which data were obtained for their excellent assistance. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.\n\nPublished - GalYam2011p15618Astrophys_J.pdf
", "abstract": "The Palomar Transient Factory (PTF) is an optical wide-field variability survey carried out using a camera with a 7.8 deg^2 field of view mounted on the 48 inch Oschin Schmidt telescope at Palomar Observatory. One of the key goals of this survey is to conduct high-cadence monitoring of the sky in order to detect optical transient sources shortly after they occur. Here, we describe the real-time capabilities of the PTF and our related rapid multiwavelength follow-up programs, extending from the radio to the \u03b3-ray bands. We present as a case study observations of the optical transient PTF10vdl (SN 2010id), revealed to be a very young core-collapse (Type II-P) supernova having a remarkably low luminosity. Our results demonstrate that the PTF now provides for optical transients the real-time discovery and rapid-response follow-up capabilities previously reserved only for high-energy transients like gamma-ray bursts.", "date": "2011-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "736", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 159", "id_number": "CaltechAUTHORS:20110831-095038520", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110831-095038520", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Weizmann-Minerva" }, { "agency": "Marie Curie Fellowship" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman fund" }, { "agency": "Max Planck Institute for Astronomy" }, { "agency": "German-Israeli Foundation for Research and Development" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Hewlett-Packard Company" }, { "agency": "AutoScope Corporation" }, { "agency": "Lick Observatory" }, { "agency": "University of California" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "TABASGO Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/736/2/159", "primary_object": { "basename": "GalYam2011p15618Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/v0a8t-myq97/files/GalYam2011p15618Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Gal-Yam, Avishay; Kasliwal, Mansi M.; et el." }, { "id": "https://authors.library.caltech.edu/records/xar6e-mdj98", "eprint_id": 42909, "eprint_status": "archive", "datestamp": "2023-08-22 03:22:20", "lastmod": "2023-10-25 23:08:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "van-Eyken-J-C", "name": { "family": "van Eyken", "given": "Julian C." }, "orcid": "0000-0003-2192-5371" }, { "id": "Ciardi-D-R", "name": { "family": "Ciardi", "given": "David R." }, "orcid": "0000-0002-5741-3047" }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "John R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Akeson-R-L", "name": { "family": "Akeson", "given": "Rachel L." }, "orcid": "0000-0001-9674-1564" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "Charles A." }, "orcid": "0000-0002-5627-5471" }, { "id": "Boden-A-F", "name": { "family": "Boden", "given": "Andrew F." } }, { "id": "von-Braun-K", "name": { "family": "von Braun", "given": "Kaspar" }, "orcid": "0000-0002-5823-4630" }, { "id": "Gelino-D-M", "name": { "family": "Gelino", "given": "Dawn M." }, "orcid": "0000-0003-1274-2784" }, { "id": "Hoard-D-W", "name": { "family": "Hoard", "given": "D. W." }, "orcid": "0000-0002-6800-6519" }, { "id": "Kane-S-R", "name": { "family": "Kane", "given": "Stephen R." }, "orcid": "0000-0002-7084-0529" }, { "id": "Plavchan-P", "name": { "family": "Plavchan", "given": "Peter" }, "orcid": "0000-0002-8864-1667" }, { "id": "Ramirez-S-V", "name": { "family": "Ramirez", "given": "Solange" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Grillmair-C-J", "name": { "family": "Grillmair", "given": "Carl J." }, "orcid": "0000-0003-4072-169X" }, { "id": "Laher-R-R", "name": { "family": "Laher", "given": "Russ" }, "orcid": "0000-0003-2451-5482" }, { "id": "Surace-J-A", "name": { "family": "Surace", "given": "Jason A." }, "orcid": "0000-0001-7291-0087" } ] }, "title": "The Palomar Transient Factory Orion Project: Eclipsing Binaries and Young Stellar Objects", "ispublished": "pub", "full_text_status": "public", "keywords": "binaries: close; binaries: eclipsing; open clusters and associations: individual (25 Ori); planets and satellites: detection; stars: pre-main sequence; techniques: photometric", "note": "\u00a9 2011 The American Astronomical Society.\n\nReceived 2011 March 30; accepted 2011 June 12; published 2011 July 15.\n\nThe authors thank Cesar Brice\u00f1o for providing the reference\nstars for zero-point calibration, and for his advice regarding\nfield selection; and Tim Lister, Rachel Street, Andrej Pr\u0161a,\nDavid Bradstreet, Ed Guinan, and Adam Krauss, for valuable\ndiscussions and input. S.B.C. wishes to acknowledge generous\nsupport from Gary and Cynthia Bengier, the Richard and Rhoda\nGoldman Fund, National Aeronautics and Space Administration\n(NASA)/Swift grant NNX10AI21G, NASA/Fermi grant\nNNX1OA057G, and National Science Foundation (NSF) grant\nAST\u20130908886. Observations obtained with the Samuel Oschin\nTelescope at the Palomar Observatory as part of the PTF project,\na scientific collaboration between the California Institute of\nTechnology, Columbia University, Las Cumbres Observatory,\nthe Lawrence Berkeley National Laboratory, the National Energy\nResearch Scientific Computing Center, the University of\nOxford, and the Weizmann Institute of Science. This publication\nmakes use of data products from the Two Micron All-Sky Survey,\nwhich is a joint project of the University of Massachusetts\nand the Infrared Processing and Analysis Center/California Institute\nof Technology, funded by the National Aeronautics and\nSpace Administration and the National Science Foundation.\nThis work is based in part on archival data obtained with the\nSpitzer Space Telescope, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology under a contract\nwith NASA. This research has made use of the NASA/IPAC/\nNExScI Star and Exoplanet Database, which is operated by the\nJet Propulsion Laboratory, California Institute of Technology,\nunder contract with the National Aeronautics and Space Administration.\nThis research has made use of the NASA/IPAC\nInfrared Science Archive, which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under contract\nwith the National Aeronautics and Space Administration.\nThis research has made use of the VizieR catalogue access tool,\nCDS, Strasbourg, France. Support for this work was provided\nby an award issued by JPL/Caltech.\nFacilities: PO:1.2m (PTF), Spitzer\n\nPublished - 1538-3881_142_2_60.pdf
Submitted - 1106.3570v2.pdf
", "abstract": "The Palomar Transient Factory (PTF) Orion project is one of the experiments within the broader PTF survey, a systematic automated exploration of the sky for optical transients. Taking advantage of the wide (3\u00b0.5 \u00d7 2\u00b0.3) field of view available using the PTF camera installed at the Palomar 48 inch telescope, 40 nights were dedicated in 2009 December to 2010 January to perform continuous high-cadence differential photometry on a single field containing the young (7-10 Myr) 25 Ori association. Little is known empirically about the formation of planets at these young ages, and the primary motivation for the project is to search for planets around young stars in this region. The unique data set also provides for much ancillary science. In this first paper, we describe the survey and the data reduction pipeline, and present some initial results from an inspection of the most clearly varying stars relating to two of the ancillary science objectives: detection of eclipsing binaries and young stellar objects. We find 82 new eclipsing binary systems, 9 of which are good candidate 25 Ori or Orion OB1a association members. Of these, two are potential young W UMa type systems. We report on the possible low-mass (M-dwarf primary) eclipsing systems in the sample, which include six of the candidate young systems. Forty-five of the binary systems are close (mainly contact) systems, and one of these shows an orbital period among the shortest known for W UMa binaries, at 0.2156509 \u00b1 0.0000071 days, with flat-bottomed primary eclipses, and a derived distance that appears consistent with membership in the general Orion association. One of the candidate young systems presents an unusual light curve, perhaps representing a semi-detached binary system with an inflated low-mass primary or a star with a warped disk, and may represent an additional young Orion member. Finally, we identify 14 probable new classical T-Tauri stars in our data, along with one previously known (CVSO 35) and one previously reported as a candidate weak-line T-Tauri star (SDSS J052700.12+010136.8).", "date": "2011-08", "date_type": "published", "publication": "Astronomical Journal", "volume": "142", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 60", "id_number": "CaltechAUTHORS:20131209-135859792", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131209-135859792", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX1OA057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-6256/142/2/60", "primary_object": { "basename": "1106.3570v2.pdf", "url": "https://authors.library.caltech.edu/records/xar6e-mdj98/files/1106.3570v2.pdf" }, "related_objects": [ { "basename": "1538-3881_142_2_60.pdf", "url": "https://authors.library.caltech.edu/records/xar6e-mdj98/files/1538-3881_142_2_60.pdf" } ], "pub_year": "2011", "author_list": "van Eyken, Julian C.; Ciardi, David R.; et el." }, { "id": "https://authors.library.caltech.edu/records/00296-1fp59", "eprint_id": 24393, "eprint_status": "archive", "datestamp": "2023-08-22 03:11:08", "lastmod": "2023-10-23 22:39:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. B." }, "orcid": "0000-0003-1673-970X" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Rau-A", "name": { "family": "Rau", "given": "A." }, "orcid": "0000-0001-5990-6243" } ] }, "title": "Discovery of a New Photometric Sub-class of Faint and Fast Classical Novae", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (M81, M82, M31, NGC 2403, NGC 891); galaxies: starburst; novae, cataclysmic variables; surveys; techniques: photometric; techniques: spectroscopic", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 March 1; accepted 2011 April 22; published 2011 June 21. We thank Peter Jonker for timely Chandra/DDT observations\nfor the fast evolving nova, P60-M81OT-071213. We thank\nMarina Orio for discussion, in particular, the suggestion that some of the faint novae may be recurrent novae. We thank A. Shafter, M. Shara, L. Bildsten, and O. Yaron for valuable feedback. We are grateful to A. Becker for making his software hotpants and wcsremap available for public use. M.M.K. thanks the Gordon and Betty Moore Foundation for the Hale Fellowship in support of graduate study. S.B.C. is grateful for generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, and National Science Foundation (NSF) grant AST0908886. M.M.K. thanks the Palomar Observatory staff for their help in maximizing the efficiency and image quality of the Palomar 60 inch. 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 recognize and acknowledge the\nvery 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 - Kasliwal2011p14664Astrophys_J.pdf
", "abstract": "We present photometric and spectroscopic follow-up of a sample of extragalactic novae discovered by the Palomar 60 inch telescope during a search for \"Fast Transients In Nearest Galaxies\" (P60-FasTING). Designed as a fast cadence (1 day) and deep (g < 21 mag) survey, P60-FasTING was particularly sensitive to short-lived and faint optical transients. The P60-FasTING nova sample includes 10 novae in M 31, 6 in M 81, 3 in M 82, 1 in NGC 2403, and 1 in NGC 891. This significantly expands the known sample of extragalactic novae beyond the Local Group, including the first discoveries in a starburst environment. Surprisingly, our photometry shows that this sample is quite inconsistent with the canonical maximum-magnitude-rate-of-decline (MMRD) relation for classical novae. Furthermore, the spectra of the P60-FasTING sample are indistinguishable from classical novae. We suggest that we have uncovered a sub-class of faint and fast classical novae in a new phase space in luminosity-timescale of optical transients. Thus, novae span two orders of magnitude in both luminosity and time. Perhaps the MMRD, which is characterized only by the white dwarf mass, was an oversimplification. Nova physics appears to be characterized by a relatively rich four-dimensional parameter space in white dwarf mass, temperature, composition, and accretion rate.", "date": "2011-07-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "735", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 94", "id_number": "CaltechAUTHORS:20110712-154210482", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110712-154210482", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/735/2/94", "primary_object": { "basename": "Kasliwal2011p14664Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/00296-1fp59/files/Kasliwal2011p14664Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Kasliwal, M. M.; Cenko, S. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/d5ysh-9cz14", "eprint_id": 24455, "eprint_status": "archive", "datestamp": "2023-08-19 07:28:05", "lastmod": "2023-10-23 22:43:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levan-A-J", "name": { "family": "Levan", "given": "A. J." } }, { "id": "Cutri-R-M", "name": { "family": "Cutri", "given": "R. M." }, "orcid": "0000-0002-0077-2305" }, { "id": "Hoffman-D-I", "name": { "family": "Hoffman", "given": "D. I." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" } ] }, "title": "An Extremely Luminous Panchromatic Outburst from the Nucleus of a Distant Galaxy", "ispublished": "pub", "full_text_status": "restricted", "note": "\u00a9 2011 American Association for the Advancement of Science. Received for publication 18 April 2011. Accepted for publication 8 June 2011. Published Online 16 June 2011. We gratefully acknowledge the efforts of\nthe many observatories whose data are presented here.\nWe particularly thank D. Malesani for assistance in the\ncalibration of the optical photometry, M. Irwin for\nassistance with processing the UKIRT data, D. Fox for help\nwith the PTF data, and K. Hurley and J. Prochaska for\nassistance in obtaining the Keck data. A.J.L. and N.R.T.\nacknowledge support from the Science and Technology\nFacilities Council. Swift, launched in November 2004, is a\nNASA mission in partnership with the Italian Space\nAgency and the UK Space Agency. Swift is managed by\nNASA Goddard. Pennsylvania State University controls\nscience and flight operations from the Mission Operations\nCenter in University Park, Pennsylvania. Los Alamos\nNational Laboratory provides g-ray imaging analysis.\nS.B.C. acknowledges generous support from G. Bengier\nand C. Bengier, the Richard and Rhoda Goldman Fund,\nNASA/Swift grant NNX10AI21G, NASA/Fermi grant\nNNX1OA057G, and NSF grant AST-0908886. A.J.vdH.\nwas supported by NASA grant NNH07ZDA001-GLAST. G.L.\nis supported by a grant from the Carlsberg foundation.\nM.M. is supported by the Hubble Fellowship grant\nHST-HF-51277.01-A, awarded by the The Space Telescope\nScience Institute (STScI), which is operated by AURA\nunder NASA contract NAS5-26555. The Dark Cosmology\nCentre is funded by the Danish National Research\nFoundation. This work makes use of data obtained by the\nChandra X-ray Observatory (OBSID = 12920). This work\nis based on observations made with the NASA/ESA Hubble\nSpace Telescope (program ID 12447), obtained from\nthe data archive at the Space Telescope Institute. STScI is \noperated by the association of Universities for Research\nin Astronomy under the NASA contract NAS 5-26555.\nThis work is also based on observations obtained at the\nGemini Observatory, which is operated by the Association\nof Universities for Research in Astronomy, under a\ncooperative agreement with the NSF on behalf of the\nGemini partnership: the National Science Foundation\n(United States), the Science and Technology Facilities\nCouncil (UK), the National Research Council (Canada),\nConsejo Nacional de Investigaciones Cient\u00edficas y\nT\u00e9cnicas (Chile), the Australian Research Council (Australia),\nMinist\u00e9rio da Ci\u00eancia e Tecnologia (Brazil), and Ministerio\nde Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina).\nThe UK Infrared Telescope is operated by the Joint\nAstronomy Centre on behalf of the Science and\nTechnology Facilities Council of the UK. UKIRT data were\nprocessed by the Cambridge Astronomical Survey Unit.\nThis work is also based on observations made with the\nNordic Optical Telescope, operated on the island of\nLa Palma jointly by Denmark, Finland, Iceland, Norway,\nand Sweden, in the Spanish Observatorio del Roque de\nlos Muchachos of the Instituto de Astrofisica de Canarias.\nThis work is also based on observations made with the\nGTC and on observations obtained with the Samuel\nOschin Telescope at the Palomar Observatory as part of\nthe Palomar Transient Factory project. The National\nEnergy Research Scientific Computing Center, which is\nsupported by the Office of Science of the U.S. Department\nof Energy under contract DE-AC02-05CH11231, provided\nstaff, computational resources, and data storage for this\nproject. The WHT is operated on the island of La Palma by\nthe Isaac Newton Group in the Spanish Observatorio del\nRoque de los Muchachos of the Instituto de Astrof\u00edsica de\nCanarias. This work is also based on observations made with\nthe Italian Telescopio Nazionale Galileo operated on the\nisland of La Palma by the Fundacion Galileo Galilei of the\nINAF (Istituto Nazionale di Astrofisica) at the Spanish\nObservatorio del Roque de los Muchachos of the Instituto de\nAstrofisica de Canarias. The WSRT is operated by ASTRON,\nwith support from the Netherlands Foundation for Scientific\nResearch. This work is also based on observations carried\nout with the IRAM Plateau de Bure Interferometer. IRAM\nis supported by Institut National des Sciences de\nl'Univers/CNRS (France), Max-Planck-Gesellschaft (Germany),\nand Instituto Geogr\u00e1fico Nacional (Spain). Some of the\ndata presented here were obtained at the W.M. Keck\nObservatory, which is operated as a scientific partnership\namong the California Institute of Technology, the\nUniversity of California, and NASA. The Observatory was\nmade possible by the generous financial support of the\nW.M. Keck Foundation. J.G., A.J.C.T., R.S.R., and S.G.\nare partially supported by the Spanish programs\nAYA-2007-63677, AYA-2008-03467/ESP, and\nAYA-2009-14000-C03-01. R.L.C.S. is supported by a Royal\nSociety Fellowship. We acknowledge support by the Spanish\nMinistry of Science and Innovation under project grants\nAYA2008-03467/ESP and AYA2009-14000-C03-01 (including\nFeder funds). J.P.B. and A.J.R. were supported by the NSF\nthrough grants AST-0808099 and AST-0909237. A.N.M.\ngratefully acknowledges support from a NSF Graduate\nResearch Fellowship. A.P.K. is partially supported by NSF\naward AST-1008353. R.A.M.J.W. acknowledges support from\nthe European Research Council via Advanced Investigator\ngrant 247295. We acknowledge access to the major\nresearch facilities program supported by the Commonwealth\nof Australia under the International Science Linkages\nprogram. N.B. and C.P. are NASA Einstein Fellows. M.C.C. is\na Hubble Fellow. Data used in this paper are presented in\nthe SOM or taken from the literature as cited.", "abstract": "Variable x-ray and \u03b3-ray emission is characteristic of the most extreme physical processes in the universe. We present multiwavelength observations of a unique \u03b3-ray\u2013selected transient detected by the Swift satellite, accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z = 0.3534. Its high-energy emission has lasted much longer than any \u03b3-ray burst, whereas its peak luminosity was \u223c100 times higher than bright active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a rare mechanism involving the massive black hole in the nucleus of that galaxy.", "date": "2011-07-08", "date_type": "published", "publication": "Science", "volume": "333", "number": "6039", "publisher": "American Association for the Advancement of Science", "pagerange": "199-202", "id_number": "CaltechAUTHORS:20110719-081344168", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110719-081344168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NASA", "grant_number": "NNX10A057G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NASA", "grant_number": "NNH07ZDA001-GLAST" }, { "agency": "Carlsberg Foundation" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51277.01-A" }, { "agency": "Space Telescope Science Institute" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Danish National Research Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA-2007-63677" }, { "agency": "Royal Society Fellowship" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2008-03467/ESP" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2009-14000-C03-01" }, { "agency": "Fondo Europeo de Desarrollo Regional (FEDER)" }, { "agency": "NSF", "grant_number": "AST-0808099" }, { "agency": "NSF", "grant_number": "AST-0909237" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-1008353" }, { "agency": "European Research Council (ERC)", "grant_number": "247295" }, { "agency": "Commonwealth of Australia" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1126/science.1207143", "pub_year": "2011", "author_list": "Levan, A. J.; Cutri, R. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/zkrha-dba15", "eprint_id": 24226, "eprint_status": "archive", "datestamp": "2023-08-19 07:13:02", "lastmod": "2023-10-23 20:24:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "R." } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "G." } }, { "id": "Hale-D", "name": { "family": "Hale", "given": "D." } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "R." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "J." } }, { "id": "Velur-V", "name": { "family": "Velur", "given": "V." } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Henning-J", "name": { "family": "Henning", "given": "J." } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "K." } }, { "id": "McKenna-D", "name": { "family": "McKenna", "given": "D." } }, { "id": "Levitan-D", "name": { "family": "Levitan", "given": "D." } } ] }, "title": "Hydrogen-poor superluminous stellar explosions", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy", "note": "\u00a9 2011 Nature Publishing Group, a division of Macmillan Publishers Limited.\n\nReceived 17 February; accepted 1 April 2011. Published online 8 June 2011.\n\nObservations were obtained with the Samuel Oschin Telescope\nand the 60-inch telescope at PalomarObservatory as part of the PTF project, a scientific collaboration between the California Institute of Technology, Columbia University, \nLas Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford and the Weizmann\nInstitute of Science. Some of the data presented here were obtained at the W. M. Keck Observatory and the William Herschel Telescope. The National Energy Research\nScientific Computing Center, which is supported by the Office of Science of the US Department of Energy, provided staff, computational resources and data storage for\nthis project. Observations by the Weizmann PTF partnership and from the Wise Observatory are supported by grants from the Israel Science Foundation and the US\u2013Israel Binational Science Foundation. We acknowledge support from the US\nDepartment of Energy Scientific Discovery through Advanced Computing programme, the Hale Fellowship from the Gordon and Betty Moore foundation, the Bengier Foundation, the Richard and Rhoda Goldman Fund, and the Royal Society.\n\nAuthor Contributions: R.M.Q. initiated, coordinated and managed the project, carried\nout photometric and spectroscopic observations and analysis, and wrote the\nmanuscript. S.R.K. is the PTF principal investigator and contributed to manuscript\npreparation. M.M.K. obtained spectroscopy from the Keck I telescope and helped with\nthe P60 observations. A.G.-Y. oversaw the Wise observations and contributed to\nanalysis and manuscript writing. I.A. extracted the Wise photometry and helped obtain\nKeck I spectra. M.S. carried out and analysed spectroscopic observations from the\nWilliam Herschel Telescope. P.N. designed and implemented the image-subtraction\npipeline that detected the PTF events. R.T. analysed the combined spectra using his\nautomated SYNOWcode. D.A.H. helped to identify the PTF spectra as being like that of\nSN2005ap. E.N. contributed to the physical interpretation andmanuscript writing. L.B.\nadvised during the preparation of the manuscript. C.T. helped vet potential candidates\nand first identified PTF09atu and PTF09cwl. N.M.L. is the PTF project scientist and\noversaw the PTF system. R.D., G.R., D.H., R.S., E.O.O., J.Z., V.V., R.W., J.H., K.B. and D.M.\nhelped to build and commission the PTF system. D.P., S.B.C. and D.L. helped to vet PTF\ncandidates and obtain spectroscopic observations.\n\nSupplemental Material - nature10095-s1.pdf
", "abstract": "Supernovae are stellar explosions driven by gravitational or thermonuclear energy that is observed as electromagnetic radiation emitted over weeks or more. In all known supernovae, this radiation comes from internal energy deposited in the outflowing ejecta by one or more of the following processes: radioactive decay of freshly synthesized elements (typically ^(56)Ni), the explosion shock in the envelope of a supergiant star, and interaction between the debris and slowly moving, hydrogen-rich circumstellar material. Here we report observations of a class of luminous supernovae whose properties cannot be explained by any of these processes. The class includes four new supernovae that we have discovered and two previously unexplained events, (SN 2005ap and SCP 06F6) that we can now identify as members of the same class. These supernovae are all about ten times brighter than most type Ia supernova, do not show any trace of hydrogen, emit significant ultraviolet flux for extended periods of time and have late-time decay rates that are inconsistent with radioactivity. Our data require that the observed radiation be emitted by hydrogen-free material distributed over a large radius (~10^(15) centimetres) and expanding at high speeds (>10^4 kilometres per second). These long-lived, ultraviolet-luminous events can be observed out to redshifts z\u2009>\u20094.", "date": "2011-06-23", "date_type": "published", "publication": "Nature", "volume": "474", "number": "7352", "publisher": "Nature Publishing Group", "pagerange": "487-489", "id_number": "CaltechAUTHORS:20110627-141511557", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110627-141511557", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Bengier Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Royal Society" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1038/nature10095", "primary_object": { "basename": "nature10095-s1.pdf", "url": "https://authors.library.caltech.edu/records/zkrha-dba15/files/nature10095-s1.pdf" }, "pub_year": "2011", "author_list": "Quimby, R. M.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/h74j9-c8z63", "eprint_id": 23794, "eprint_status": "archive", "datestamp": "2023-08-22 02:43:57", "lastmod": "2023-10-23 20:01:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Thomas-R-C", "name": { "family": "Thomas", "given": "R. C." } }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Blake-S", "name": { "family": "Blake", "given": "S." } }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "J." }, "orcid": "0000-0001-5703-2108" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I. M." }, "orcid": "0000-0002-2960-978X" }, { "id": "Mazzali-P-A", "name": { "family": "Mazzali", "given": "P." }, "orcid": "0000-0001-6876-8284" }, { "id": "Podsiadlowski-P", "name": { "family": "Podsiadlowski", "given": "P." } }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "D." } } ] }, "title": "The Subluminous and Peculiar Type Ia Supernova PTF 09dav", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general; supernovae: individual (PTF09dav)", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 December 12; accepted 2011 March 9; published 2011 April 26.\n\nWe acknowledge useful discussions with Brian Schmidt and\nDan Kasen. We thank Richard Ellis for providing the P200/\nDBSP spectrum. M.S. acknowledges support from the Royal Society. E.O.O. is supported by an Einstein fellowship and NASA grants. L.B. is supported by the National Science Foundation under grants PHY 05-51164 and AST 07-07633. S.B.C. acknowledges generous support from Gary and Cynthia Bengier and the Richard and Rhoda Goldman Foundation. D.P. is supported by an Einstein fellowship. The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. Observations obtained with the Samuel Oschin Telescope and the 60 inch Telescope at the Palomar Observatory as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Weizmann Institute participation of\nin PTF is supported in part by grants from the Israeli Science Foundation to A.G. Weizmann-Caltech collaborative work on PTF is supported by a grant from the Binational Science Foundation (BSF) to A.G. and S.R.K. Collaborative work by A.G. and M.S. is supported by a grant from the Weizmann-UK \"making connection\" program. Collaborative work of A.G. and P.A.M. is supported by a Weizmann-Minerva grant. A.G. is supported by an EU/FP7 Marie Curie IRG fellowship and a research grant from the Peter and Patricia Gruber Awards.\nFacilities: PO:1.2m, ING: Herschel, PO:1.5m, Hale, Keck:I,\nLCOGT\n\nPublished - Sullivan2011p13853Astrophys_J.pdf
", "abstract": "PTF 09dav is a peculiar subluminous Type Ia supernova (SN) discovered by the Palomar Transient Factory (PTF). Spectroscopically, it appears superficially similar to the class of subluminous SN1991bg-like SNe, but it has several unusual features which make it stand out from this population. Its peak luminosity is fainter than any previously discovered SN1991bg-like SN Ia (MB ~ \u201315.5), but without the unusually red optical colors expected if the faint luminosity were due to extinction. The photospheric optical spectra have very unusual strong lines of Sc II and Mg I, with possible Sr II, together with stronger than average Ti II and low velocities of ~6000 km s^(\u20131). The host galaxy of PTF09dav is ambiguous. The SN lies either on the extreme outskirts (~41 kpc) of a spiral galaxy or in an very faint (MR \u2265 \u201312.8) dwarf galaxy, unlike other 1991bg-like SNe which are invariably associated with massive, old stellar populations. PTF 09dav is also an outlier on the light-curve-width-luminosity and color-luminosity relations derived for other subluminous SNe Ia. The inferred ^(56)Ni mass is small (0.019 \u00b1 0.003 M_\u2609), as is the estimated ejecta mass of 0.36 M_\u2609. Taken together, these properties make PTF 09dav a remarkable event. We discuss various physical models that could explain PTF 09dav. Helium shell detonation or deflagration on the surface of a CO white dwarf can explain some of the features of PTF 09dav, including the presence of Sc and the low photospheric velocities, but the observed Si and Mg are not predicted to be very abundant in these models. We conclude that no single model is currently capable of explaining all of the observed signatures of PTF 09dav.", "date": "2011-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "732", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 118", "id_number": "CaltechAUTHORS:20110525-113451676", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110525-113451676", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Foundation" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Weizmann-UK" }, { "agency": "Weizmann-Minerva" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Peter and Patricia Gruber Awards" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/732/2/118", "primary_object": { "basename": "Sullivan2011p13853Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/h74j9-c8z63/files/Sullivan2011p13853Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Sullivan, M.; Kasliwal, M. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/g5a2y-ews42", "eprint_id": 23284, "eprint_status": "archive", "datestamp": "2023-08-22 02:26:57", "lastmod": "2023-10-23 18:58:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shri R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Jacobsen-J", "name": { "family": "Jacobsen", "given": "Janet" } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Green-Y", "name": { "family": "Green", "given": "Yoav" } }, { "id": "Yaron-O", "name": { "family": "Yaron", "given": "Ofer" }, "orcid": "0000-0002-0301-8017" }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "Derek B." }, "orcid": "0000-0002-3714-672X" }, { "id": "Howell-J-L", "name": { "family": "Howell", "given": "Jacob L." } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Keliser-I-K-W", "name": { "family": "Kleiser", "given": "Io K. W." } }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam" }, "orcid": "0000-0001-9515-478X" }, { "id": "Li-Weidong", "name": { "family": "Li", "given": "Weidong" } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Starr-D", "name": { "family": "Starr", "given": "Dan" } }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "George" }, "orcid": "0000-0003-3367-3415" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." } }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Tendulkar-S-P", "name": { "family": "Tendulkar", "given": "Shriharsh P." }, "orcid": "0000-0003-2548-2926" }, { "id": "Gehrels-N", "name": { "family": "Gehrels", "given": "Neil" } }, { "id": "Kennea-J-A", "name": { "family": "Kennea", "given": "Jamie" }, "orcid": "0000-0002-6745-4790" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Bildsten-L", "name": { "family": "Bildsten", "given": "Lars" } }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "Gustavo" } }, { "id": "Hale-D-D-S", "name": { "family": "Hale", "given": "David" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger M." } }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "Jeff" } }, { "id": "Velur-V", "name": { "family": "Velur", "given": "Viswa" } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "Richard" }, "orcid": "0000-0002-1835-6078" }, { "id": "Henning-J-R", "name": { "family": "Henning", "given": "John" } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "McKenna-D-L", "name": { "family": "McKenna", "given": "Dan" } }, { "id": "Blake-C-H", "name": { "family": "Blake", "given": "Cullen" } } ] }, "title": "PTF 10fqs: A Luminous Red Nova in the Spiral Galaxy Messier 99", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: AGB and post-AGB; stars: mass-loss; supernovae: general; supernovae: individual (PTF 10fqs); surveys", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 July 20; accepted 2011 February 4; published 2011 March 14.\n\nM.M.K. thanks the Gordon and Betty Moore Foundation for\na Hale Fellowship in support of graduate study. The Weizmann Institute PTF participation is supported in part by the Israel Science Foundation via grants to A.G.Y. The Weizmann-Caltech collaborative PTF effort is supported by the US\u2013Israel Binational Science Foundation. A.G.Y. and M.S. are jointly supported by the \"making connections\" Weizmann\u2013UK program. A.G.Y. further acknowledges support by a Marie Curie IRG fellowship and the Peter and Patricia Gruber Award, as well as funding by the Benoziyo Center for Astrophysics and the Yeda-Sela center at the Weizmann Institute. A.V.F.'s group and KAIT are supported by National Science Foundation (NSF) grant AST-0908886, the Sylvia & Jim Katzman Foundation, the Richard & Rhoda Goldman Fund, Gary and Cynthia Bengier, and the TABASGO Foundation; additional funding was provided by NASA through Spitzer grant 1322321, as well as HST grant AR-11248 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. J.S.B. and his group are partially funded by a DOE SciDAC grant. E.O.O. and D.P. are supported by the Einstein fellowship. L.B. is supported by the National Science Foundation under grants PHY 05-51164 and AST 07-07633. We are grateful to the staff of the Gemini Observatory for their promptness and high efficiency in attending to our TOO request. Likewise, we thank the staff of the Very Large Array and the Hobby\u2013Eberly Telescope. We acknowledge the following internet repositories: SEDS (Messier Objects) and GOLDMine (Virgo Cluster), Finally, as always, we are grateful to the librarians who maintain the ADS, the NED, and SIMBAD\ndata systems. The Hobby\u2013Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universit\u00e4t M\u00fcnchen, and Georg-August-Universit\u00e4t G\u00f6ttingen. The HET is named in honor of its principal benefactors,William P. Hobby and Robert E. Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome Optics, who fabricated several optics for the instrument but died before its completion; it is a joint project of the Hobby\u2013Eberly Telescope partnership and the\nInstituto de Astronom\u00eda de la Universidad Nacional Aut\u00f3noma de M\u00e9xico. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. The Expanded Very Large Array is operated by the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - Kasliwal2011p13405Astrophys_J.pdf
", "abstract": "The Palomar Transient Factory (PTF) is systematically charting the optical transient and variable sky. A primary\nscience driver of PTF is building a complete inventory of transients in the local universe (distance less than 200 Mpc). Here, we report the discovery of PTF 10fqs, a transient in the luminosity \"gap\" between novae and supernovae. Located on a spiral arm of Messier 99, PTF 10fqs has a peak luminosity of M_r = \u221212.3, red color (g \u2212 r = 1.0), and is slowly evolving (decayed by 1 mag in 68 days). It has a spectrum dominated by intermediate-width H\u03b1\n(\u2248930 km s^(\u22121)) and narrow calcium emission lines. The explosion signature (the light curve and spectra) is overall\nsimilar to that of M85 OT2006-1, SN 2008S, and NGC 300 OT. The origin of these events is shrouded in mystery\nand controversy (and in some cases, in dust). PTF 10fqs shows some evidence of a broad feature (around 8600 \u00c5)\nthat may suggest very large velocities (\u224810,000 km s^(\u22121)) in this explosion. Ongoing surveys can be expected to find\na few such events per year. Sensitive spectroscopy, infrared monitoring, and statistics (e.g., disk versus bulge) will eventually make it possible for astronomers to unravel the nature of these mysterious explosions.", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 134", "id_number": "CaltechAUTHORS:20110412-115639625", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110412-115639625", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Weizmann Institute" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "Sylvia and Jim Katzman Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "TABASGO Foundation" }, { "agency": "NASA", "grant_number": "1322321" }, { "agency": "NASA", "grant_number": "AR-11248" }, { "agency": "NASA", "grant_number": "AR-11248" }, { "agency": "NASA Einstein Fellowship" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "TAPIR" }, { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/730/2/134", "primary_object": { "basename": "Kasliwal2011p13405Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/g5a2y-ews42/files/Kasliwal2011p13405Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Kasliwal, Mansi M.; Kulkarni, Shri R.; et el." }, { "id": "https://authors.library.caltech.edu/records/bx00s-1fq82", "eprint_id": 23350, "eprint_status": "archive", "datestamp": "2023-08-22 02:27:55", "lastmod": "2023-10-23 19:01:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "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": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "Gustavo" } }, { "id": "Hale-D", "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": "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", "name": { "family": "Henning", "given": "John" } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "McKenna-D", "name": { "family": "McKenna", "given": "Dan" } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" } ] }, "title": "Evidence for an FU Orionis-like Outburst from a Classical T Tauri Star", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: formation; stars: individual (LkHa 188-G4, HBC 722); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; stars: winds, outflows", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 November 9; accepted 2011 January 24; published 2011 March 8.\n\nWe thank Luisa Rebull for providing the Spitzer/MIPS data\nfor LkH\u03b1 188-G4 in advance of her publication. We are in debt to John Johnson, John Sebastian Pineda, and Michael Bottom who obtained the HIRES spectrum for us. We thank Cullen Blake, Dan Starr, and Emilo Falco for their efforts to build and maintain PAIRITEL. We thank Meredith Hughes for a fruitful discussion concerning YSO accretion disks and Ryan Foley for information on the spectrophotometric uncertainty associated with Kast spectra. An anonymous referee provided comments that have improved this manuscript. A. A. M. is supported by the National Science Foundation (NSF) Graduate Research Fellowship Program. K.R.C. acknowledges support for this work from the Hubble Fellowship Program, provided by the National Aeronautics and Space Administration (NASA) through Hubble Fellowship grant HSTHF-51253.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. J. S. B. acknowledges support of an NSF-CDI grant-0941742. A. A. M. and C. R. K. were partially supported by NSF-AAG grant-1009991. A.V.F.'s group is grateful for the support of NSF grant AST-0908886, the TABASGO Foundation, Gary and Cynthia Bengier, and the Richard and Rhoda Goldman Fund. 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, provided staff, computational resources, and data storage for this project. 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\nUniversity of California, andNASA. The Observatory was made\npossible by the generous financial support of the W. M. \nKeck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project and those working on PAIRITEL data are further supported by NASA/Swift Guest Investigator Programs NNX09AQ66Q and NNX10A128G. We are grateful for the assistance of the staffs at all of the observatories used to obtain the data.\nThis research has made use of NASA's Astrophysics Data\nSystem Bibliographic Services, the SIMBAD database operated\nat CDS, Strasbourg, France, the NASA/IPAC Extragalactic\nDatabase operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and the VizieR database of astronomical catalogs (Ochsenbein et al. 2000). 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 NASA and the NSF.\nFacilities: PO:1.2m (PTF), PO:1.5m, Hale (TripleSpec),\nKeck:I (HIRES), Shane (Kast), FLWO:2MASS (PAIRITEL)\n\nPublished - Miller2011p13390Astrophys_J.pdf
", "abstract": "We present pre- and post-outburst observations of the new FU Orionis-like young stellar object PTF 10qpf (also known as LkH\u03b1 188-G4 and HBC 722). Prior to this outburst, LkH\u03b1 188-G4 was classified as a classical T Tauri star (CTTS) on the basis of its optical emission-line spectrum superposed on a K8-type photosphere and its photometric variability. The mid-infrared spectral index of LkH\u03b1 188-G4 indicates a Class II-type object. LkH\u03b1 188-G4 exhibited a steady rise by ~1 mag over ~11 months starting in August 2009, before a subsequent more abrupt rise of >3 mag on a timescale of ~2 months. Observations taken during the eruption exhibit the defining characteristics of FU Orionis variables: (1) an increase in brightness by \u2273 4 mag, (2) a bright optical/near-infrared reflection nebula appeared, (3) optical spectra are consistent with a G supergiant and dominated by absorption lines, the only exception being H\u03b1 which is characterized by a P Cygni profile, (4) near-infrared spectra resemble those of late K-M giants/supergiants with enhanced absorption seen in the molecular bands of CO and H_(2)O, and (5) outflow signatures in H and He are seen in the form of blueshifted absorption profiles. LkH\u03b1 188-G4 is the first member of the FU Orionis-like class with a well-sampled optical to mid-infrared spectral energy distribution in the pre-outburst phase. The association of the PTF 10qpf outburst with the previously identified CTTS LkH\u03b1 188-G4 (HBC 722) provides strong evidence that FU Orionis-like eruptions represent periods of enhanced disk accretion and outflow, likely triggered by instabilities in the disk. The early identification of PTF 10qpf as an FU Orionis-like variable will enable detailed photometric and spectroscopic observations during its post-outburst evolution for comparison with other known outbursting objects.", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 80", "id_number": "CaltechAUTHORS:20110415-155909524", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110415-155909524", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51253.01-A" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "NSF", "grant_number": "AAG-1009991" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "TABASGO Foundation" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/730/2/80", "primary_object": { "basename": "Miller2011p13390Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/bx00s-1fq82/files/Miller2011p13390Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Miller, Adam A.; Hillenbrand, Lynne A.; et el." }, { "id": "https://authors.library.caltech.edu/records/df7xf-n1h91", "eprint_id": 23466, "eprint_status": "archive", "datestamp": "2023-08-22 02:23:21", "lastmod": "2023-10-23 19:36:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-A-M", "name": { "family": "Smith", "given": "A. M." } }, { "id": "Lynn-S", "name": { "family": "Lynn", "given": "S." } }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "M." }, "orcid": "0000-0001-9053-4820" }, { "id": "Lintott-C-J", "name": { "family": "Lintott", "given": "C. J." }, "orcid": "0000-0001-5578-359X" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "P. E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Botyanszki-J", "name": { "family": "Botyanszki", "given": "J." } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R." }, "orcid": "0000-0001-9171-5236" }, { "id": "Bamford-S-P", "name": { "family": "Bamford", "given": "S. P." }, "orcid": "0000-0001-7821-7195" }, { "id": "Fortson-L-F", "name": { "family": "Fortson", "given": "L. F." }, "orcid": "0000-0002-1067-8558" }, { "id": "Schawinski-K", "name": { "family": "Schawinski", "given": "K." }, "orcid": "0000-0001-5464-0888" }, { "id": "Hook-I-M", "name": { "family": "Hook", "given": "I." }, "orcid": "0000-0002-2960-978X" }, { "id": "Blake-S", "name": { "family": "Blake", "given": "S." } }, { "id": "Podsiadlowski-P", "name": { "family": "Podsiadlowski", "given": "P." } }, { "id": "J\u00f6nsson-J", "name": { "family": "J\u00f6nsson", "given": "J." } }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "A." }, "orcid": "0000-0002-3653-5598" }, { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "I." }, "orcid": "0000-0001-7090-4898" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. A." }, "orcid": "0000-0003-4253-656X" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Jacobsen-J", "name": { "family": "Jacobsen", "given": "J." } }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N. M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" } ] }, "title": "Galaxy Zoo Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis; surveys; supernovae: general", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2010 November 5. Received 2010 November 5; in original form 2010 September 29. Article first published online: 7 Feb. 2011. \n\nThis publication has been made possible by the participation of more than 10,000 volunteers in the Galaxy Zoo Supernovae project (http://supernova.galaxyzoo.org/authors). \n\nWe acknowledge the valuable contributions of the Zooniverse community without which this project would not have been possible. AMS acknowledges support from the Leverhulme Trust. MS acknowledges support from the Royal Society. MS and AG-Y acknowledge support from a Weizmann\u2013UK 'Making conenctions' grant. CJL acknowledges support from the STFC Science in Society Program and The Leverhulme Trust. PEN acknowledges support from the US Department of Energy Scientific Discovery through Advanced Computing program under contract DE-FG02-06ER06-04. KS acknowledges support from a NASA Einstein Postdoctoral Fellowship grant number PF9-00069, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. JSB acknowledges support of an NSF-CDI grant 'Real-time Classification of Massive Time-series Data Streams' (Award #0941742). 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, provided staff, computational resources and data storage for this project. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias. Observations obtained with the Samuel Oschin Telescope at the Palomar Observatory as part of the PTF 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.\n\nPublished - Smith2011p13551Mon_Not_R_Astron_Soc.pdf
", "abstract": "This paper presents the first results from a new citizen science project: Galaxy Zoo Supernovae. This proof-of-concept project uses members of the public to identify supernova candidates from the latest generation of wide-field imaging transient surveys. We describe the Galaxy Zoo Supernovae operations and scoring model, and demonstrate the effectiveness of this novel method using imaging data and transients from the Palomar Transient Factory (PTF). We examine the results collected over the period 2010 April\u2013July, during which nearly 14 000 supernova candidates from the PTF were classified by more than 2500 individuals within a few hours of data collection. We compare the transients selected by the citizen scientists to those identified by experienced PTF scanners and find the agreement to be remarkable \u2013 Galaxy Zoo Supernovae performs comparably to the PTF scanners and identified as transients 93 per cent of the ~130 spectroscopically confirmed supernovae (SNe) that the PTF located during the trial period (with no false positive identifications). Further analysis shows that only a small fraction of the lowest signal-to-noise ratio detections (r > 19.5) are given low scores: Galaxy Zoo Supernovae correctly identifies all SNe with \u22658\u03c3 detections in the PTF imaging data. The Galaxy Zoo Supernovae project has direct applicability to future transient searches, such as the Large Synoptic Survey Telescope, by both rapidly identifying candidate transient events and via the training and improvement of existing machine classifier algorithms.", "date": "2011-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "412", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1309-1319", "id_number": "CaltechAUTHORS:20110426-104725679", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110426-104725679", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Leverhulme Trust" }, { "agency": "Royal Society" }, { "agency": "Weizmann-UK" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF9-00069" }, { "agency": "NSF", "grant_number": "CDI-0941742" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1111/j.1365-2966.2010.17994.x", "primary_object": { "basename": "Smith2011p13551Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/df7xf-n1h91/files/Smith2011p13551Mon_Not_R_Astron_Soc.pdf" }, "pub_year": "2011", "author_list": "Smith, A. M.; Lynn, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/whjv0-z3c17", "eprint_id": 22879, "eprint_status": "archive", "datestamp": "2023-08-19 05:27:19", "lastmod": "2023-10-23 17:17:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooke-J", "name": { "family": "Cooke", "given": "Jeff" }, "orcid": "0000-0001-5703-2108" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "orcid": "0000-0001-7782-7071" }, { "id": "Sullivan-Mark", "name": { "family": "Sullivan", "given": "Mark" }, "orcid": "0000-0001-9053-4820" }, { "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter" }, "orcid": "0000-0002-3389-0586" }, { "id": "Howell-D-A", "name": { "family": "Howell", "given": "D. Andrew" }, "orcid": "0000-0003-4253-656X" }, { "id": "Gal-Yam-A", "name": { "family": "Gal-Yam", "given": "Avishay" }, "orcid": "0000-0002-3653-5598" }, { "id": "Lidman-C", "name": { "family": "Lidman", "given": "Chris" }, "orcid": "0000-0003-1731-0497" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "Joshua S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "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": "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" } ] }, "title": "Hubble Space Telescope Studies of Nearby Type Ia Supernovae: The Mean Maximum Light Ultraviolet Spectrum and its Dispersion", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmological parameters \u2013 supernovae: general \u2013 ultraviolet: general", "note": "\u00a9 2011 American Astronomical Society. Received 2010 October 11; accepted 2010 December 6; published 2011 January 10. R.S.E. acknowledges support from DOE grant DESC0001101,\nM.S. from the Royal Society, A.G. from the Israeli\nScience Foundation and a European Union Marie Curie\nfellowship. Support for program GO 11721 was provided by\nNASA through a grant from the Space Telescope Science Institute,\nwhich is operated by AURA, Inc., under NASA Contract\nNAS5-26555. The National Energy Research Scientific Computing\nCenter, which is supported by the Office of Science of\nthe U.S. Department of Energy under Contract No. DE-AC02-\n05CH11231, provided staff, computational resources, and data\nstorage for this project. P.E.N. acknowledges support from the\nUS Department of Energy Scientific Discovery through Advanced\nComputing program under contract DE-FG02-06ER06-\n04. S.B.C. acknowledges generous support from Gary and\nCynthia Bengier and the Richard and Rhoda Goldman Foundation.\n\nPublished - Cooke2011p13022Astrophys_J_Lett.pdf
", "abstract": "We present the first results of an ongoing campaign using the STIS spectrograph on board the Hubble Space Telescope (HST), whose primary goal is the study of near-ultraviolet (UV) spectra of local Type Ia supernovae (SNe Ia). Using events identified by the Palomar Transient Factory and subsequently verified by ground-based spectroscopy, we demonstrate the ability to locate and classify SNe Ia as early as 16 days prior to maximum light. This enables us to trigger HST in a non-disruptive mode to obtain near UV spectra within a few days of maximum light for comparison with earlier equivalent ground-based spectroscopic campaigns conducted at intermediate-redshifts, ^-_z \u2243 0.5. We analyze the spectra of 12 SNe Ia located in the Hubble flow with 0.01 < z < 0.08. Although a fraction of our eventual sample, these data, together with archival data, already provide a substantial advance over that previously available. Restricting samples to those of similar phase and stretch, the mean UV spectrum agrees reasonably closely with that at intermediate redshift, although some differences are found in the metallic absorption features. A larger sample will determine whether these differences reflect possible biases or are a genuine evolutionary effect. Significantly, the wavelength-dependent dispersion, which is larger in the UV, follows similar trends to those observed at intermediate redshift and is driven, in part, by differences in the various metallic features. While the origin of the UV dispersion remains uncertain, our comparison suggests that it may reflect compositional variations among our sample rather than being predominantly an evolutionary effect.", "date": "2011-02-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "727", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L35", "id_number": "CaltechAUTHORS:20110315-085705825", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-085705825", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0001101" }, { "agency": "Royal Society" }, { "agency": "Israel Science Foundation" }, { "agency": "European Union" }, { "agency": "NASA", "grant_number": "GO 11721" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "Space Telescope Science Institute" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/727/2/L35", "primary_object": { "basename": "Cooke2011p13022Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/whjv0-z3c17/files/Cooke2011p13022Astrophys_J_Lett.pdf" }, "pub_year": "2011", "author_list": "Cooke, Jeff; Ellis, Richard S.; et el." }, { "id": "https://authors.library.caltech.edu/records/wcaqs-7w403", "eprint_id": 22567, "eprint_status": "archive", "datestamp": "2023-08-22 01:54:52", "lastmod": "2023-10-23 17:00:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Covey-K-R", "name": { "family": "Covey", "given": "Kevin R." }, "orcid": "0000-0001-6914-7797" }, { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "id": "Miller-A-A", "name": { "family": "Miller", "given": "Adam A." }, "orcid": "0000-0001-9515-478X" }, { "id": "Poznanski-D", "name": { "family": "Poznanski", "given": "Dovi" } }, { "id": "Cenko-S-B", "name": { "family": "Cenko", "given": "S. Bradley" }, "orcid": "0000-0003-1673-970X" }, { "id": "Silverman-J-M", "name": { "family": "Silverman", "given": "Jeffrey M." }, "orcid": "0000-0003-3325-3365" }, { "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": "Fischer-William", "name": { "family": "Fischer", "given": "William" } }, { "id": "Rayner-J", "name": { "family": "Rayner", "given": "John" } }, { "id": "Rebull-L-M", "name": { "family": "Rebull", "given": "Luisa M." }, "orcid": "0000-0001-6381-515X" }, { "id": "Butler-N-R", "name": { "family": "Butler", "given": "Nathaniel R." } }, { "id": "Filippenko-A-V", "name": { "family": "Filippenko", "given": "Alexei V." }, "orcid": "0000-0003-3460-0103" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas M." }, "orcid": "0000-0001-9380-6457" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Ag\u00fceros-M-A", "name": { "family": "Ag\u00fceros", "given": "Marcel A." }, "orcid": "0000-0001-7077-3664" }, { "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": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "orcid": "0000-0002-3389-0586" }, { "id": "Jacobsen-J", "name": { "family": "Jacobsen", "given": "Janet" } }, { "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": "Klein-C", "name": { "family": "Klein", "given": "Christopher" } } ] }, "title": "PTF10nvg: An Outbursting Class I Protostar in the Pelican/North American Nebula", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: emission-line, Be; stars: formation; stars: pre-main sequence; stars: variables: general; stars: winds, outflows", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 October 14; accepted 2010 November 12; published 2011 January 5. The authors are grateful to Michael T. Kandrashoff, Christopher V. Griffith, A. Cucchiara, Daniel A. Perley, and A. N. Morgan for their assistance in obtaining the LRIS and Kast spectra presented here. We are also grateful to the Directors of the NASA Infrared Telescope Facility (IRTF) and Apache Point Observatory (APO), whose allocation of Director's Discretionary Time enabled the acquisition of the SpeX and TripleSpec spectra presented here. We also thank ErikaGibb for making available archival SpeX observations of V1647 Ori, Tom Greene for a helpful discussion of NIR shock tracers, and Michael Eracleous for a useful discussion of symbiotic binaries\nand other accreting systems. K.R.C. acknowledges support for this work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51253.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. J.S.B., D.A.P., C.K., A.A.M., and D.A.S. acknowledge support of an NSF-CDI grant, \"Real-Time Classification of Massive Time-Series Data Streams\" (Award 0941742).A.V.F.'s group is grateful for the support of NSF grant AST-0908886, the TABASGO Foundation, Gary and Cynthia Bengier, and the Richard and Rhoda Goldman Fund. 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 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\nfrom this mountain. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project and those working on PAIRITEL data are further supported by NASA/Swift Guest Investigator Programs NNX09AQ66Q and NNX10A128G. This work was also based in part on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. We are grateful for the assistance of the staffs at all of the observatories\nused to obtain the data. This research has made use of NASA's Astrophysics Data System Bibliographic Services, the SIMBAD database, operated at CDS, Strasbourg, France, the NASA/IPAC Extragalactic Database, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and the VizieR database of astronomical catalogs (Ochsenbein et al. 2000). 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\nFacilities: PO:1.2m, PO:1.5m, Hale, Keck:I, Keck:II, FLWO:\n1.2m, ARC, Shane\n\nPublished - Covey2011p12750Astron_J.pdf
", "abstract": "During a synoptic survey of the North American Nebula region, the Palomar Transient Factory (PTF) detected an optical outburst (dubbed PTF10nvg) associated with the previously unstudied flat or rising spectrum infrared source IRAS 20496+4354. The PTF R-band light curve reveals that PTF10nvg brightened by more than 5 mag during the current outburst, rising to a peak magnitude of R_(PTF) \u2248 13.5 in 2010 September. Follow-up observations indicate that PTF10nvg has undergone a similar ~5 mag brightening in the K band and possesses a rich emission-line spectrum, including numerous lines commonly assumed to trace mass accretion and outflows. Many of these lines are blueshifted by ~175 km s^(\u20131) from the North American Nebula's rest velocity, suggesting that PTF10nvg is driving an outflow. Optical spectra of PTF10nvg show several TiO/VO band heads fully in emission, indicating the presence of an unusual amount of dense (>10^(10) cm^(\u20133)), warm (1500-4000 K) circumstellar material. Near-infrared spectra of PTF10nvg appear quite similar to a spectrum of McNeil's Nebula/V1647 Ori, a young star which has undergone several brightenings in recent decades, and 06297+1021W, a Class I protostar with a similarly reached near-infrared emission line spectrum. While further monitoring is required to fully understand this event, we conclude that the brightening of PTF10nvg is indicative of enhanced accretion and outflow in this Class-I-type protostellar object, similar to the behavior of V1647 Ori in 2004-2005.", "date": "2011-02", "date_type": "published", "publication": "Astronomical Journal", "volume": "141", "number": "2", "publisher": "IOP", "pagerange": "Art. No. 40", "id_number": "CaltechAUTHORS:20110301-084206110", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110301-084206110", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51253.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "TABASGO Foundation" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Harvard University Milton Fund" }, { "agency": "NASA", "grant_number": "NNX09AQ66Q" }, { "agency": "NASA", "grant_number": "NNX10A128G" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-6256/141/2/40", "primary_object": { "basename": "Covey2011p12750Astron_J.pdf", "url": "https://authors.library.caltech.edu/records/wcaqs-7w403/files/Covey2011p12750Astron_J.pdf" }, "pub_year": "2011", "author_list": "Covey, Kevin R.; Hillenbrand, Lynne A.; et el." }, { "id": "https://authors.library.caltech.edu/records/ek4b5-abg28", "eprint_id": 23043, "eprint_status": "archive", "datestamp": "2023-08-22 01:51:57", "lastmod": "2023-10-23 17:50:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "Robert" }, "orcid": "0000-0001-9171-5236" }, { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "Eran" }, "orcid": "0000-0002-6786-8774" }, { "id": "Wyder-T-K", "name": { "family": "Wyder", "given": "Ted K." } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Barlow-T-A", "name": { "family": "Barlow", "given": "Tom A." } }, { "id": "Forster-K", "name": { "family": "Foster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Friedman-P-G", "name": { "family": "Friedman", "given": "Peter G." } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" } ] }, "title": "The Extreme Hosts of Extreme Supernovae", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; stars: luminosity function, mass function; stars: massive; supernovae: general", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 September 7; accepted 2010 November 12; published 2010 December 23.\n\nWe gratefully acknowledge the anonymous referee for a careful reading and useful suggestions that improved the presentation of this work. Joint research by A.G. and M.S. is supported by the Weizmann-UK program. A.G. is also supported by grants from the Israeli Science Foundation, an EU FP7 Marie Curie IRG Fellowship, and a research grant from the Peter and Patricia Gruber Awards. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/ The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology,\nthe Korean Scientist Group, the Chinese Academy of Sciences\n(LAMOST), Los Alamos National Laboratory, the Max-Planck-\nInstitute for Astronomy (MPIA), the Max-Planck-Institute for\nAstrophysics (MPA), New Mexico State University, Ohio State\nUniversity, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department\nof Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources and data storage for this\nproject.\n\nPublished - Neill2011p13135Astrophys_J.pdf
", "abstract": "We use GALEX ultraviolet (UV) and optical integrated photometry of the hosts of 17 luminous supernovae (LSNe, having peak M_V < \u201321) and compare them to a sample of 26, 000 galaxies from a cross-match between the SDSS DR4 spectral catalog and GALEX interim release 1.1. We place the LSN hosts on the galaxy NUV \u2013 r versus M_r color-magnitude diagram (CMD) with the larger sample to illustrate how extreme they are. The LSN hosts appear to favor low-density regions of the galaxy CMD falling on the blue edge of the blue cloud toward the low-luminosity end. From the UV-optical photometry, we estimate the star formation history of the LSN hosts. The hosts have moderately low star formation rates (SFRs) and low stellar masses (M_*) resulting in high specific star formation rates (sSFR). Compared with the larger sample, the LSN hosts occupy low-density regions of a diagram plotting sSFR versus M_* in the area having higher sSFR and lower M_*. This preference for low M_*, high sSFR hosts implies that the LSNe are produced by an effect having to do with their local environment. The correlation of mass with metallicity suggests that perhaps wind-driven mass loss is the factor that prevents LSNe from arising in higher-mass, higher-metallicity hosts. The massive progenitors of the LSNe (>100 M_\u2609), by appearing in low-SFR hosts, are potential tests for theories of the initial mass function that limit the maximum mass of a star based on the SFR.", "date": "2011-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "727", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 15", "id_number": "CaltechAUTHORS:20110322-095700336", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110322-095700336", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Weizmann-UK" }, { "agency": "Israel Science Foundation" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Peter and Patricia Gruber Foundation" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" } ] }, "doi": "10.1088/0004-637X/727/1/15", "primary_object": { "basename": "Neill2011p13135Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/ek4b5-abg28/files/Neill2011p13135Astrophys_J.pdf" }, "pub_year": "2011", "author_list": "Neill, James D.; Quimby, Robert; et el." }, { "id": "https://authors.library.caltech.edu/records/jvef9-dyw39", "eprint_id": 21416, "eprint_status": "archive", "datestamp": "2023-08-22 01:31:43", "lastmod": "2023-10-21 00:01:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ofek-E-O", "name": { "family": "Ofek", "given": "E. O." }, "orcid": "0000-0002-6786-8774" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "J. D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "K." }, "orcid": "0000-0001-5800-5531" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "M. M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "N." }, "orcid": "0000-0001-9380-6457" }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "C." }, "orcid": "0000-0002-8650-1644" }, { "id": "Quimby-R-M", "name": { "family": "Quimby", "given": "R. M." }, "orcid": "0000-0001-9171-5236" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "R." } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "G." } }, { "id": "Hale-D", "name": { "family": "Hale", "given": "D." } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "R." } }, { "id": "Zolkower-J", "name": { "family": "Zolkower", "given": "J." } }, { "id": "Velur-V", "name": { "family": "Velur", "given": "V." } }, { "id": "Walters-R", "name": { "family": "Walters", "given": "R." }, "orcid": "0000-0002-1835-6078" }, { "id": "Henning-J", "name": { "family": "Henning", "given": "J." } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "K." } }, { "id": "McKenna-D", "name": { "family": "McKenna", "given": "D." } } ] }, "title": "Supernova PTF 09UJ: A Possible Shock Breakout from a Dense Circumstellar Wind", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: mass-loss; supernovae: general; supernovae: individual (PTF 09uj)", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2010 July 9; accepted 2010 September 27; published 2010 November 12.\nWe thank an anonymous referee for useful comments. E.O.O.\nand D.P. are supported by an Einstein fellowship. S.B.C. and\nA.V.F. acknowledge generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/\nSwift grants NNX09AL08G and NNX10AI21G, and NSF grant\nAST-0908886. A.G. acknowledges support by the Israeli and\nthe US-Israel Binational Science Foundations, an EU/IRG fellowship,\nthe Benoziyo Center for Astrophysics, and the Peter\nand Patricia Gruber Awards. The National Energy Research\nScientific Computing Center, which is supported by the Office\nof Science of the U. S. Department of Energy under Contract\nNo. DE-AC02-05CH11231, provided staff, computational resources,\nand data storage for this project. P.E.N. acknowledges\nsupport from the US Department of Energy Scientific Discovery\nthrough Advanced Computing program under contract DEFG02-\n06ER06-04. J.S.B.'s work on PTF was supported by NSF/\nOIA award AST-0941742 (\"Real-Time Classification of Massive\nTime-Series Data Streams\"). L.B. and K.S. are supported\nby the NSF under grants PHY 05-51164 and AST 07-07633.\n\nPublished - Ofek2010p12144Astrophys_J.pdf
", "abstract": "Type-IIn supernovae (SNe IIn), which are characterized by strong interaction of their ejecta with the surrounding circumstellar matter (CSM), provide a unique opportunity to study the mass-loss history of massive stars shortly before their explosive death. We present the discovery and follow-up observations of an SN IIn, PTF 09uj, detected by the Palomar Transient Factory (PTF). Serendipitous observations by Galaxy Evolution Explorer (GALEX) at ultraviolet (UV) wavelengths detected the rise of the SN light curve prior to the PTF discovery. The UV light curve of the SN rose fast, with a timescale of a few days, to a UV absolute AB magnitude of about \u201319.5. Modeling our observations, we suggest that the fast rise of the UV light curve is due to the breakout of the SN shock through the dense CSM (n \u2248 10^(10) cm^(\u20133)). Furthermore, we find that prior to the explosion the progenitor went through a phase of high mass-loss rate (~0.1 M_\u2299 yr^(\u20131)) that lasted for a few years. The decay rate of this SN was fast relative to that of other SNe IIn.", "date": "2010-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "724", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1396-1401", "id_number": "CaltechAUTHORS:20101217-083631333", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101217-083631333", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gary and Cynthia Bengier" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "NASA", "grant_number": "NNX09AL08G" }, { "agency": "NASA", "grant_number": "NNX10AI21G" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "NSF", "grant_number": "PHY 05-51164" }, { "agency": "NSF", "grant_number": "AST 07-07633" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "NSF", "grant_number": "AST-0941742" }, { "agency": "NASA Einstein Fellowship" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Palomar-Transient-Factory" }, { "id": "Space-Astrophysics-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/724/2/1396", "primary_object": { "basename": "Ofek2010p12144Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/jvef9-dyw39/files/Ofek2010p12144Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Ofek, E. O.; Neill, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/an6t9-pan24", "eprint_id": 21374, "eprint_status": "archive", "datestamp": "2023-08-19 04:19:33", "lastmod": "2023-10-20 23:59:23", "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": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "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": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "Gustavo" } }, { "id": "Hale-D", "name": { "family": "Hale", "given": "David" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger" } }, { "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", "name": { "family": "Henning", "given": "John" } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "McKenna-D", "name": { "family": "McKenna", "given": "Dan" } } ] }, "title": "Rapidly decaying supernova 2010X: A candidate \".Ia\" explosion", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general, supernovae: individual (SN2010X, SN2002bj), surveys, white dwarfs", "note": "\u00a9 2010 American Astronomical Society. Received 2010 September 5; accepted 2010 September 27; published 2010 October 13. M.M.K. thanks the Gordon and Betty Moore Foundation for a\nHale Fellowship in support of graduate study.M.M.K. thanks the Pumarth Headquarters in Indore, India for their warm hospitality\nwhile writing this manuscript.\nWe thank the referee for accepting this Letter on a timescale\nfaster than that characterizing the rapid photometric evolution\nof this supernova.\nWe acknowledge the following discussions:M.M.K. & Paolo\nMazzali, A.G.Y. & David Branch, S.R.K. & Xiaofeng Wang,\nD.A.H. & Ryan Foley, M.M.K. & Rollin Thomas. We are\ngrateful to the staff of the Gemini Observatory and Swift\nObservatory for efficiently executing TOO triggers. We thank\nthe librarians who maintain the ADS, the NED, and SIMBAD\ndata systems.\nThe Weizmann Institute PTF participation is supported by\ngrants to A.G.Y. from the Israel Science Foundation and the\nUS-Israel Binational Science Foundation. E.O.O. and D.P.\nare supported by an Einstein Fellowship. S.B.C. is grateful\nfor support from Gary and Cynthia Bengier and the Richard\nand Rhoda Goldman Fund. Computational resources and data\nstorage were contributed by NERSC, supported by US DoE\ncontract DE-AC02-05CH11231. P.E.N. acknowledges support\nfrom the US DoE contract DE-FG02-06ER06-04.\nFacilities: PO:1.2m, Hale, Gemini:Gillett, Hiltner, Swift\n\nPublished - Kasliwal2010p12074Astrophys_J_Lett.pdf
", "abstract": "We present the discovery, photometric, and spectroscopic follow-up observations of SN 2010X (PTF 10bhp). This supernova decays exponentially with \u03c4_d = 5 days and rivals the current recordholder in speed, SN 2002bj. SN 2010X peaks at M_r = \u221217 mag and has mean velocities of 10,000 km s^(\u22121). Our light curve modeling suggests a radioactivity-powered event and an ejecta mass of 0.16M_\u2299. If powered by Nickel, we show that the Nickel mass must be very small (\u22480.02 M_\u2299) and that the supernova quickly becomes optically thin to \u03b3 -rays. Our spectral modeling suggests that SN 2010X and SN 2002bj have similar chemical compositions\nand that one of aluminum or helium is present. If aluminum is present, we speculate that this may be an accretion-induced collapse of an O-Ne-Mg white dwarf. If helium is present, all observables of SN 2010X are consistent with being a thermonuclear helium shell detonation on a white dwarf, a \".Ia\" explosion. With the 1 day dynamic-cadence experiment on the Palomar Transient Factory, we expect to annually discover a few such events.", "date": "2010-11-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "723", "number": "1", "publisher": "American Astronomical Society", "pagerange": "L98-L102", "id_number": "CaltechAUTHORS:20101215-092516250", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101215-092516250", "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": "NASA Einstein Fellowship" }, { "agency": "Richard and Rhoda Goldman Fund" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/2041-8205/723/1/L98", "primary_object": { "basename": "Kasliwal2010p12074Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/an6t9-pan24/files/Kasliwal2010p12074Astrophys_J_Lett.pdf" }, "pub_year": "2010", "author_list": "Kasliwal, Mansi M.; Kulkarni, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/03hbr-ap470", "eprint_id": 20468, "eprint_status": "archive", "datestamp": "2023-08-19 03:51:29", "lastmod": "2023-10-20 23:05:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arcavi-I", "name": { "family": "Arcavi", "given": "Iair" }, "orcid": "0000-0001-7090-4898" }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "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": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Law-N-M", "name": { "family": "Law", "given": "Nicholas" }, "orcid": "0000-0001-9380-6457" }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "Jeff" }, "orcid": "0000-0001-5703-2108" }, { "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard" } }, { "id": "Rahmer-G", "name": { "family": "Rahmer", "given": "Gustavo" } }, { "id": "Hale-D", "name": { "family": "Hale", "given": "David" } }, { "id": "Smith-R-M", "name": { "family": "Smith", "given": "Roger" } }, { "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", "name": { "family": "Henning", "given": "John" } }, { "id": "Bui-Khanh", "name": { "family": "Bui", "given": "Khanh" } }, { "id": "McKenna-D", "name": { "family": "McKenna", "given": "Dan" } } ] }, "title": "Core-collapse Supernovae from the Palomar Transient Factory: Indications for a Different Population in Dwarf Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "supernovae: general", "note": "\u00a9 2010 The American Astronomical Society.\n\nReceived 2010 April 16; accepted 2010 July 26; published 2010 September 1.\nThe Weizmann Institute PTF partnership is supported by the\nIsraeli Science Foundation via grants to A.G. Collaborative\nwork between A.G. and S.R.K. is supported by the US\u2013Israel\nBinational Science Foundation. A.G. further acknowledges\nsupport from the EU FP7 Marie Curie program via an IRG\nfellowship, the Benoziyo Center for Astrophysics, a Minerva\ngrant, and the Peter and Patricia Gruber Awards. P.E.N. is\nsupported by the US Department of Energy Scientific Discovery\nthrough Advanced Computing program under contract DEFG02-\n06ER06-04. M.S. acknowledges support from the Royal\nSociety; M.S. and A.G. are also grateful for a Weizmann-UK\nMaking Connections grant. A.V.F. and S.B.C. acknowledge\ngenerous support from Gary and Cynthia Bengier, the Richard\nand Rhoda Goldman Fund, US National Science Foundation\ngrant AST-0908886, and the TABASGO Foundation. J.S.B. was\npartially supported by a SciDAC grant from the US Department\nof Energy and a grant from the National Science Foundation\n(award 0941742). The National Energy Research Scientific\nComputing Center, which is supported by the Office of Science\nof the US Department of Energy under contract DE-AC02-\n05CH11231, provided staff, computational resources, and data\nstorage for this project.\nThe WHT is operated on the island of La Palma by the\nIsaac Newton Group in the Spanish Observatorio del Roque\nde los Muchachos of the Instituto de Astrof\u00b4\u0131sica de Canarias.\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 NASA; the observatory was made possible by\nthe generous financial support of the W. M. Keck Foundation.\nWe are grateful to the staff of the Keck, Lick, Palomar, Roque\nde los Muchachos, VLT, and Gemini Observatories for their\nassistance.We thank Chris Lidman for processing theX-Shooter\ndata used for the classification of PTF10bau.\n\nPublished - Arcavi2010p11585Astrophys_J.pdf
", "abstract": "We use the first compilation of 72 core-collapse supernovae (SNe) from the Palomar Transient Factory (PTF) to study their observed subtype distribution in dwarf galaxies compared to giant galaxies. Our sample is the largest single-survey, untargeted, spectroscopically classified, homogeneous collection of core-collapse events ever assembled, spanning a wide host-galaxy luminosity range (down to M_r \u2248 \u201314 mag) and including a substantial fraction (>20%) of dwarf (M_r \u2265 \u201318 mag) hosts. We find more core-collapse SNe in dwarf galaxies than expected and several interesting trends emerge. We use detailed subclassifications of stripped-envelope core-collapse SNe and find that all Type I core-collapse events occurring in dwarf galaxies are either SNe Ib or broad-lined SNe Ic (SNe Ic-BL), while \"normal\" SNe Ic dominate in giant galaxies. We also see a significant excess of SNe IIb in dwarf hosts. We hypothesize that in lower metallicity hosts, metallicity-driven mass loss is reduced, allowing massive stars that would have appeared as \"normal\" SNe Ic in metal-rich galaxies to retain some He and H, exploding as Ib/IIb events. At the same time, another mechanism allows some stars to undergo extensive stripping and explode as SNe Ic-BL (and presumably also as long-duration gamma-ray bursts). Our results are still limited by small-number statistics, and our measurements of the observed N(Ib/c)/N(II) number ratio in dwarf and giant hosts (0.25^(+0.3)_(\u20130.15) and 0.23^(+0.11)_(\u20130.08), respectively; 1\u03c3 uncertainties) are consistent with previous studies and theoretical predictions. As additional PTF data accumulate, more robust statistical analyses will be possible, allowing the evolution of massive stars to be probed via the dwarf-galaxy SN population.", "date": "2010-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "721", "number": "1", "publisher": "American Astronomical Society", "pagerange": "777-784", "id_number": "CaltechAUTHORS:20101021-112924786", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101021-112924786", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Israel Science Foundation" }, { "agency": "Binational Science Foundation (USA-Israel)" }, { "agency": "European Union" }, { "agency": "Benoziyo Center for Astrophysics" }, { "agency": "MINERVA (Israel)" }, { "agency": "Peter and Patricia Gruber Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-FG02-06ER06-04" }, { "agency": "Royal Society" }, { "agency": "Weizmann-UK Making Connections Programme" }, { "agency": "Gary and Cynthia Bengier" }, { "agency": "NSF", "grant_number": "AST-0908886" }, { "agency": "TABASGO Foundation" }, { "agency": "NSF", "grant_number": "CDI-0941742" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Palomar-Transient-Factory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.1088/0004-637X/721/1/777", "primary_object": { "basename": "Arcavi2010p11585Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/03hbr-ap470/files/Arcavi2010p11585Astrophys_J.pdf" }, "pub_year": "2010", "author_list": "Arcavi, Iair; Kasliwal, Mansi M.; et el." }, { "id": "https://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" }, "pub_year": "2009", "author_list": "Rau, Arne; Kulkarni, Shrinivas R.; et el." }, { "id": "https://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" }, "pub_year": "2009", "author_list": "Law, Nicholas M.; Kulkarni, Shrinivas R.; et el." } ]