\n
We investigate the efficacy of a systematic planetary nebula (PN) search in the Census of the Local Universe (CLU) narrowband (Hα) survey that covers a considerably larger sky region of above decl. −20° than most previous surveys. Using PNe observed by the Isaac Newton Telescope Photometric Hα Survey as validation, we are able to visually recover 432 out of 441 cataloged PNe (98%) within the CLU data set, with 5 sources having unusable CLU images and 4 missed due to limitations of imaging quality. Moreover, the reference PNe are conventionally divided into three PN classes in decreasing order of identification confidence given their spectra and morphologies. We record consistently high recovery rate across all classes: 95% of True, 71% of Likely, and 81% of Possible sources are readily recovered. To further demonstrate the ability of CLU to find new PNe, we undertake a preliminary search of compact PNe within a sub-region of the validation catalog, mainly utilizing the significance of narrow-band colors (Σ) as a metric for identification. In a 200 deg2 region, we search the CLU source catalog and find 31 PN candidates after automated and visual scrutiny, of which 12 are new sources not appearing in previous studies. As a demonstration of our ongoing follow-up campaign, we present medium-resolution optical spectra of six candidates and notice that four of them show emission signatures characteristic of confirmed PNe. As we refine our selection methods, CLU promises to provide a systematic catalog of PNe spanning 2/3 of the sky.
\n
In order to study transient phenomena in the Universe, existing and forthcoming imaging surveys are covering wide areas of sky repeatedly over time, with a range of cadences, point spread functions, and depths. We describe here a framework that allows an efficient search for different types of time-varying astrophysical phenomena in current and future, large data repositories. We first present a methodology to generate and store key survey parameters that enable researchers to determine if a survey, or a combination of surveys, allows specific time-variable astrophysical phenomena to be discovered. To facilitate further exploration of sources in regions of interest, we then generate a few sample metrics that capture the essential brightness characteristics of a sky pixel at a specific wavelength. Together, we refer to these as \"annotated coadds.\" The techniques presented here for WISE/NEOWISE-R data are sensitive to 10% brightness variations at around 12th Vega magnitude at 4.5 μm wavelength. Application of the technique to Zwicky Transient Factory data also enabled the detection of 0.5 mag variability at 20 AB mag in the r-band. We demonstrate the capabilities of these metrics for different classes of sources: high proper-motion stars, periodic variable stars, and supernovae, and find that each metric has its advantages depending on the nature of variability. We also present a data structure which will ease the search for temporally varying phenomena in future surveys.
",
"doi": "10.1088/1538-3873/aceeb6",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-08",
"series_number": "1050",
"volume": "135",
"issue": "1050",
"pages": "084503"
},
{
"id": "authors:5gf1p-hc010",
"collection": "authors",
"collection_id": "5gf1p-hc010",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230328-705664700.23",
"type": "article",
"title": "SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations",
"author": [
{
"family_name": "West",
"given_name": "S. L.",
"orcid": "0000-0002-4575-6157",
"clpid": "West-Stuart-L"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-Ragnhild"
},
{
"family_name": "Omand",
"given_name": "C. M. B.",
"orcid": "0000-0002-9646-8710",
"clpid": "Omand-Conor-M-B"
},
{
"family_name": "Kangas",
"given_name": "T.",
"orcid": "0000-0002-5477-0217",
"clpid": "Kangas-Tuomas"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-Steve"
},
{
"family_name": "Strotjohann",
"given_name": "N. L.",
"orcid": "0000-0002-4667-6730",
"clpid": "Strotjohann-Nora-Linn"
},
{
"family_name": "Yang",
"given_name": "S.",
"orcid": "0000-0002-2898-6532",
"clpid": "Yang-Sheng"
},
{
"family_name": "Fransson",
"given_name": "C.",
"orcid": "0000-0001-8532-3594",
"clpid": "Fransson-Claes"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Perley",
"given_name": "D.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Chen",
"given_name": "T.-W.",
"orcid": "0000-0002-1066-6098",
"clpid": "Chen-Ting-Wan"
},
{
"family_name": "Chen",
"given_name": "Z. H.",
"orcid": "0000-0001-5175-4652",
"clpid": "Chen-Zhihao"
},
{
"family_name": "Taggart",
"given_name": "K.",
"orcid": "0000-0002-5748-4558",
"clpid": "Taggart-Kirsty"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Bloom",
"given_name": "J. S.",
"orcid": "0000-0002-7777-216X",
"clpid": "Bloom-Joshua-S"
},
{
"family_name": "Drake",
"given_name": "A.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Laher",
"given_name": "R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Medford",
"given_name": "M. S.",
"orcid": "0000-0002-7226-0659",
"clpid": "Medford-Michael-S"
},
{
"family_name": "Neill",
"given_name": "J. D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "Context. SN 2020qlb (ZTF20abobpcb) is a hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (maximum M_g\u2004=\u2004\u221222.25 mag) and that has one of the longest rise times (77 days from explosion to maximum). We estimate the total radiated energy to be > 2.1\u2005\u00d7\u200510\u2075\u00b9 erg. SN 2020qlb has a well-sampled light curve that exhibits clear near and post peak undulations, a phenomenon seen in other SLSNe, whose physical origin is still unknown. \n\nAims. We discuss the potential power source of this immense explosion as well as the mechanisms behind its observed light curve undulations. \n\nMethods. We analyze photospheric spectra and compare them to other SLSNe-I. We constructed the bolometric light curve using photometry from a large data set of observations from the Zwicky Transient Facility (ZTF), Liverpool Telescope (LT), and Neil Gehrels Swift Observatory and compare it with radioactive, circumstellar interaction and magnetar models. Model residuals and light curve polynomial fit residuals are analyzed to estimate the undulation timescale and amplitude. We also determine host galaxy properties based on imaging and spectroscopy data, including a detection of the [O III]\u03bb4363, auroral line, allowing for a direct metallicity measurement. \n\nResults. We rule out the Arnett \u2075\u2076Ni decay model for SN 2020qlb's light curve due to unphysical parameter results. Our most favored power source is the magnetic dipole spin-down energy deposition of a magnetar. Two to three near peak oscillations, intriguingly similar to those of SN 2015bn, were found in the magnetar model residuals with a timescale of 32\u2005\u00b1\u20056 days and an amplitude of 6% of peak luminosity. We rule out centrally located undulation sources due to timescale considerations; and we favor the result of ejecta interactions with circumstellar material (CSM) density fluctuations as the source of the undulations.",
"doi": "10.1051/0004-6361/202244086",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2023-02",
"volume": "670",
"pages": "Art. No. A7"
},
{
"id": "authors:0ja92-v7s88",
"collection": "authors",
"collection_id": "0ja92-v7s88",
"cite_using_url": "https://authors.library.caltech.edu/records/0ja92-v7s88",
"type": "article",
"title": "The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package",
"author": [
{
"family_name": "The Astropy Collaboration"
},
{
"family_name": "Price-Whelan",
"given_name": "Adrian M.",
"orcid": "0000-0003-0872-7098"
},
{
"family_name": "Lim",
"given_name": "Pey Lian",
"orcid": "0000-0003-0079-4114"
},
{
"family_name": "Earl",
"given_name": "Nicholas",
"orcid": "0000-0003-1714-7415"
},
{
"family_name": "Starkman",
"given_name": "Nathaniel",
"orcid": "0000-0003-3954-3291"
},
{
"family_name": "Bradley",
"given_name": "Larry",
"orcid": "0000-0002-7908-9284"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Patil",
"given_name": "Aarya A.",
"orcid": "0000-0002-7626-506X"
},
{
"family_name": "Corrales",
"given_name": "Lia",
"orcid": "0000-0002-5466-3817"
},
{
"family_name": "Brasseur",
"given_name": "C. E.",
"orcid": "0000-0002-9314-960X"
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{
"family_name": "N\u00f6the",
"given_name": "Maximilian",
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{
"family_name": "Donath",
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{
"family_name": "Tollerud",
"given_name": "Erik",
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{
"family_name": "Morris",
"given_name": "Brett M.",
"orcid": "0000-0003-2528-3409"
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{
"family_name": "Ginsburg",
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"orcid": "0000-0001-6431-9633"
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{
"family_name": "Vaher",
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"orcid": "0000-0001-8736-1762"
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{
"family_name": "Weaver",
"given_name": "Benjamin A."
},
{
"family_name": "Tocknell",
"given_name": "James",
"orcid": "0000-0001-6637-6922"
},
{
"family_name": "Jamieson",
"given_name": "William",
"orcid": "0000-0001-5976-4492"
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{
"family_name": "van Kerkwijk",
"given_name": "Marten H.",
"orcid": "0000-0002-5830-8505"
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{
"family_name": "Robitaille",
"given_name": "Thomas P.",
"orcid": "0000-0002-8642-1329"
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{
"family_name": "Merry",
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{
"family_name": "Bachetti",
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{
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{
"family_name": "Alvarado-Montes",
"given_name": "Jaime A.",
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{
"family_name": "Archibald",
"given_name": "Anne M.",
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{
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{
"family_name": "Conroy",
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{
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{
"family_name": "Craig",
"given_name": "Matthew W.",
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{
"family_name": "Cross",
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{
"family_name": "Cruz",
"given_name": "Kelle L.",
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{
"family_name": "D'Eugenio",
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{
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{
"family_name": "Devillepoix",
"given_name": "Hadrien A. R.",
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{
"family_name": "Dietrich",
"given_name": "J\u00f6rg P.",
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{
"family_name": "Eigenbrot",
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{
"family_name": "Freij",
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{
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{
"family_name": "Gordon",
"given_name": "Karl D.",
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{
"family_name": "Groener",
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{
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"family_name": "Jones",
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{
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"family_name": "Kerzendorf",
"given_name": "Wolfgang E.",
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{
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{
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{
"family_name": "Maljaars",
"given_name": "Jakob M.",
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{
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"given_name": "N. A.",
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{
"family_name": "Oman",
"given_name": "Kyle A.",
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{
"family_name": "Pascual-Granado",
"given_name": "J.",
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{
"family_name": "Patil",
"given_name": "Rohit R.",
"orcid": "0000-0002-5923-4966"
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{
"family_name": "Perren",
"given_name": "Gabriel I",
"orcid": "0000-0002-1852-9653"
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{
"family_name": "Pickering",
"given_name": "Timothy E.",
"orcid": "0000-0002-9427-5448"
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{
"family_name": "Rastogi",
"given_name": "Tanuj"
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{
"family_name": "Roulston",
"given_name": "Benjamin R.",
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{
"family_name": "Ryan",
"given_name": "Daniel F",
"orcid": "0000-0001-8661-3825"
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{
"family_name": "Rykoff",
"given_name": "Eli S.",
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{
"family_name": "Sabater",
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{
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"orcid": "0000-0002-9523-5640"
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{
"family_name": "Salgado",
"given_name": "Jes\u00fas",
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{
"family_name": "Sanghi",
"given_name": "Aniket",
"orcid": "0000-0002-1838-4757"
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{
"family_name": "Saunders",
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"orcid": "0000-0003-2657-3889"
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{
"family_name": "Savchenko",
"given_name": "Volodymyr",
"orcid": "0000-0001-6353-0808"
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{
"family_name": "Schwardt",
"given_name": "Ludwig",
"orcid": "0000-0003-1234-1921"
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{
"family_name": "Seifert-Eckert",
"given_name": "Michael"
},
{
"family_name": "Shih",
"given_name": "Albert Y.",
"orcid": "0000-0001-6874-2594"
},
{
"family_name": "Jain",
"given_name": "Anany Shrey"
},
{
"family_name": "Shukla",
"given_name": "Gyanendra",
"orcid": "0000-0001-9268-3803"
},
{
"family_name": "Sick",
"given_name": "Jonathan",
"orcid": "0000-0003-3001-676X"
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{
"family_name": "Simpson",
"given_name": "Chris",
"orcid": "0000-0001-8589-4055"
},
{
"family_name": "Singanamalla",
"given_name": "Sudheesh",
"orcid": "0000-0003-2462-7273"
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{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597"
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{
"family_name": "Singhal",
"given_name": "Jaladh",
"orcid": "0000-0002-8310-0829"
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{
"family_name": "Sinha",
"given_name": "Manodeep",
"orcid": "0000-0002-4845-1228"
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{
"family_name": "Sip\u0151cz",
"given_name": "Brigitta M.",
"orcid": "0000-0002-3713-6337",
"clpid": "Sip\u0151cz-Brigitta-M"
},
{
"family_name": "Spitler",
"given_name": "Lee R.",
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{
"family_name": "Stansby",
"given_name": "David",
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{
"family_name": "Streicher",
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{
"family_name": "\u0160umak",
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{
"family_name": "Swinbank",
"given_name": "John D.",
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{
"family_name": "Taranu",
"given_name": "Dan S.",
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},
{
"family_name": "Tewary",
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},
{
"family_name": "Tremblay",
"given_name": "Grant R.",
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},
{
"family_name": "Val-Borro",
"given_name": "Miguel de",
"orcid": "0000-0002-0455-9384"
},
{
"family_name": "Van Kooten",
"given_name": "Samuel J.",
"orcid": "0000-0002-4472-8517"
},
{
"family_name": "Vasovi\u0107",
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},
{
"family_name": "Verma",
"given_name": "Shresth",
"orcid": "0000-0003-0370-5471"
},
{
"family_name": "de Miranda Cardoso",
"given_name": "Jos\u00e9 Vin\u00edcius",
"orcid": "0000-0001-5410-5551"
},
{
"family_name": "Williams",
"given_name": "Peter K. G.",
"orcid": "0000-0003-3734-3587"
},
{
"family_name": "Wilson",
"given_name": "Tom J.",
"orcid": "0000-0001-6352-9735"
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{
"family_name": "Winkel",
"given_name": "Benjamin",
"orcid": "0000-0001-6999-3635"
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{
"family_name": "Wood-Vasey",
"given_name": "W. M.",
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},
{
"family_name": "Xue",
"given_name": "Rui",
"orcid": "0000-0001-7689-9305"
},
{
"family_name": "Yoachim",
"given_name": "Peter",
"orcid": "0000-0003-2874-6464"
},
{
"family_name": "Zhang",
"given_name": "Chen",
"orcid": "0000-0002-9583-263X"
},
{
"family_name": "Zonca",
"given_name": "Andrea",
"orcid": "0000-0001-6841-1058"
},
{
"literal": "Astropy Project Contributors"
}
],
"abstract": "The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we summarize key features in the core package as of the recent major release, version 5.0, and provide major updates on the Project. We then discuss supporting a broader ecosystem of interoperable packages, including connections with several astronomical observatories and missions. We also revisit the future outlook of the Astropy Project and the current status of Learn Astropy. We conclude by raising and discussing the current and future challenges facing the Project.
",
"doi": "10.3847/1538-4357/ac7c74",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-08-20",
"series_number": "2",
"volume": "935",
"issue": "2",
"pages": "167"
},
{
"id": "authors:a16at-zc168",
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"collection_id": "a16at-zc168",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220503-351552600",
"type": "article",
"title": "Constraining Type Ia supernova explosions and early flux excesses with the Zwicky Transient Factory",
"author": [
{
"family_name": "Deckers",
"given_name": "M.",
"orcid": "0000-0001-8857-9843",
"clpid": "Deckers-Maxime"
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{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508",
"clpid": "Maguire-Kate"
},
{
"family_name": "Magee",
"given_name": "M. R.",
"orcid": "0000-0002-0629-8931",
"clpid": "Magee-Mark-R"
},
{
"family_name": "Dimitriadis",
"given_name": "Georgios",
"orcid": "0000-0001-9494-179X",
"clpid": "Dimitriadis-Georgios"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432",
"clpid": "Smith-Mathew"
},
{
"family_name": "Sainz\u00a0de\u00a0Murieta",
"given_name": "A.",
"orcid": "0000-0002-6975-6960",
"clpid": "Sainz-de-Murieta-Ana"
},
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-Adam-A"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-Ariel"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274",
"clpid": "Nordin-Jakob"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Coughlin",
"given_name": "M. W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Graham",
"given_name": "M.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
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{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
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],
"abstract": "In the new era of time-domain surveys, Type Ia supernovae are being caught sooner after explosion, which has exposed significant variation in their early light curves. Two driving factors for early-time evolution are the distribution of \u2075\u2076Ni in the ejecta and the presence of flux excesses of various causes. We perform an analysis of the largest young SN Ia sample to date. We compare 115 SN Ia light curves from the Zwicky Transient Facility to the TURTLS model grid containing light curves of Chandrasekhar mass explosions with a range of \u2075\u2076Ni masses, \u2075\u2076Ni distributions, and explosion energies. We find that the majority of our observed light curves are well reproduced by Chandrasekhar mass explosion models with a preference for highly extended \u2075\u2076Ni distributions. We identify six SNe Ia with an early-time flux excess in our gr-band data (four 'blue' and two 'red' flux excesses). We find an intrinsic rate of 18 \u00b1 11 per\u2009cent of early flux excesses in SNe Ia at z < 0.07, based on three detected flux excesses out of 30 (10 per\u2009cent) observed SNe Ia with a simulated efficiency of 57 per\u2009cent. This is comparable to rates of flux excesses in the literature but also accounts for detection efficiencies. Two of these events are mostly consistent with circumstellar material interaction, while the other four have longer lifetimes in agreement with companion interaction and 56Ni-clump models. We find a higher frequency of flux excesses in 91T/99aa-like events (44 \u00b1 13 per\u2009cent).",
"doi": "10.1093/mnras/stac558",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-05",
"series_number": "1",
"volume": "512",
"issue": "1",
"pages": "1317-1340"
},
{
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"collection_id": "1fdpf-qta64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220113-234555128",
"type": "article",
"title": "Microlensing Events in the Galactic Plane Using the Zwicky Transient Facility",
"author": [
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
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],
"abstract": "Microlensing is a powerful technique to study the Galactic population of \"dark\" objects such as exoplanets both bound and unbound, brown dwarfs, low-luminosity stars, old white dwarfs, and neutron stars, and it is almost the only way to study isolated stellar-mass black holes. The majority of previous efforts to search for gravitational microlensing events have concentrated toward high-density fields such as the Galactic bulge. Microlensing events in the Galactic plane have the advantage of closer proximity and better constrained relative proper motions, leading to better constrained estimates of lens mass at the expense of a lower optical depth, than events toward the Galactic bulge. We use the Zwicky Transient Facility Data Release 5 compiled from 2018\u20132021 to survey the Galactic plane in the region of \u2223b\u2223 < 20\u00b0. We find a total of 60 candidate microlensing events including three that show a strong microlensing parallax effect. The rate of events traces Galactic structure, decreasing exponentially as a function Galactic longitude with scale length \u2113\u2080 \u223c 37\u00b0. On average, we find Einstein timescales of our microlensing events to be about three times as long (\u223c60 days) as those toward the Galactic bulge (\u223c20 days). This pilot project demonstrates that microlensing toward the Galactic plane shows strong promise for characterization of dark objects within the Galactic disk.",
"doi": "10.3847/1538-4357/ac51cc",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-03-10",
"series_number": "2",
"volume": "927",
"issue": "2",
"pages": "Art. No. 150"
},
{
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"collection_id": "jv8sz-9yw10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211213-224953043",
"type": "article",
"title": "The Type Icn SN 2021csp: Implications for the Origins of the Fastest Supernovae and the Fates of Wolf\u2013Rayet Stars",
"author": [
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-9024-4150"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Baade",
"given_name": "Dietrich",
"orcid": "0000-0003-1637-9679"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Chen",
"given_name": "Ting-Wan",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Cikota",
"given_name": "Aleksandar",
"orcid": "0000-0001-7101-9831",
"clpid": "Cikota-Aleksandar"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya",
"clpid": "Dahiwale-Aishwarya-S"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Hoeflich",
"given_name": "Peter",
"orcid": "0000-0002-4338-6586"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Maund",
"given_name": "Justyn R.",
"orcid": "0000-0003-0733-7215"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Strotjohann",
"given_name": "Nora Linn",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
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{
"family_name": "Zheng",
"given_name": "WeiKang",
"orcid": "0000-0002-2636-6508"
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],
"abstract": "We present observations of SN 2021csp, the second example of a newly identified type of supernova (SN) hallmarked by strong, narrow, P Cygni carbon features at early times (Type Icn). The SN appears as a fast and luminous blue transient at early times, reaching a peak absolute magnitude of \u221220 within 3 days due to strong interaction between fast SN ejecta (v \u2248 30,000 km s\u207b\u00b9) and a massive, dense, fast-moving C/O wind shed by the WC-like progenitor months before explosion. The narrow-line features disappear from the spectrum 10\u201320 days after explosion and are replaced by a blue continuum dominated by broad Fe features, reminiscent of Type Ibn and IIn supernovae and indicative of weaker interaction with more extended H/He-poor material. The transient then abruptly fades \u223c60 days post-explosion when interaction ceases. Deep limits at later phases suggest minimal heavy-element nucleosynthesis, a low ejecta mass, or both, and imply an origin distinct from that of classical Type Ic SNe. We place SN 2021csp in context with other fast-evolving interacting transients, and discuss various progenitor scenarios: an ultrastripped progenitor star, a pulsational pair-instability eruption, or a jet-driven fallback SN from a Wolf\u2013Rayet (W-R) star. The fallback scenario would naturally explain the similarity between these events and radio-loud fast transients, and suggests a picture in which most stars massive enough to undergo a W-R phase collapse directly to black holes at the end of their lives.",
"doi": "10.3847/1538-4357/ac478e",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-03-10",
"series_number": "2",
"volume": "927",
"issue": "2",
"pages": "Art. No. 180"
},
{
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"collection_id": "c3bwk-dkc20",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211130-215713941",
"type": "article",
"title": "Less Than 1% of Core-collapse Supernovae in the Local Universe Occur in Elliptical Galaxies",
"author": [
{
"family_name": "Irani",
"given_name": "I.",
"orcid": "0000-0002-7996-8780",
"clpid": "Irani-Ido"
},
{
"family_name": "Prentice",
"given_name": "S. J.",
"orcid": "0000-0003-0486-6242"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Teffs",
"given_name": "Jacob",
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},
{
"family_name": "Mazzali",
"given_name": "Paolo",
"orcid": "0000-0001-6876-8284"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Gonzalez",
"given_name": "E. P."
},
{
"family_name": "Taggart",
"given_name": "K.",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "De",
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"orcid": "0000-0002-8989-0542",
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{
"family_name": "Fremling",
"given_name": "Christoffer",
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"clpid": "Fremling-Christoffer"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
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},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
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{
"family_name": "Howell",
"given_name": "A."
},
{
"family_name": "Dhawan",
"given_name": "S.",
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"clpid": "Dhawan-Suhail"
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{
"family_name": "Tzanidakis",
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{
"family_name": "Hiramatsu",
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{
"family_name": "Kool",
"given_name": "Erik C.",
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{
"family_name": "Anderson",
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{
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{
"family_name": "Dekany",
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{
"family_name": "Gromadzki",
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{
"family_name": "Carini",
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{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
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{
"family_name": "Burke",
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{
"family_name": "Pellegrino",
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{
"family_name": "Della Valle",
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{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Young",
"given_name": "D. R.",
"orcid": "0000-0002-1229-2499"
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "Claudia P.",
"orcid": "0000-0003-2375-2064"
},
{
"family_name": "Inserra",
"given_name": "Cosimo",
"orcid": "0000-0002-3968-4409"
},
{
"family_name": "Omer",
"given_name": "Rafia"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Chen",
"given_name": "T.-W.",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Shin",
"given_name": "Kyung Min",
"orcid": "0000-0002-1486-3582",
"clpid": "Shin-Kyung-Min"
},
{
"family_name": "Yaron",
"given_name": "Ofer",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "McCully",
"given_name": "Curtis",
"orcid": "0000-0001-5807-7893"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
}
],
"abstract": "We present observations of three core-collapse supernovae (CCSNe) in elliptical hosts, detected by the Zwicky Transient Facility Bright Transient Survey (BTS). SN 2019ape is a SN Ic that exploded in the main body of a typical elliptical galaxy. Its properties are consistent with an explosion of a regular SN Ic progenitor. A secondary g-band light-curve peak could indicate interaction of the ejecta with circumstellar material (CSM). An H\u03b1-emitting source at the explosion site suggests a residual local star formation origin. SN 2018fsh and SN 2020uik are SNe II which exploded in the outskirts of elliptical galaxies. SN 2020uik shows typical spectra for SNe II, while SN 2018fsh shows a boxy nebular H\u03b1 profile, a signature of CSM interaction. We combine these 3 SNe with 7 events from the literature and analyze their hosts as a sample. We present multi-wavelength photometry of the hosts, and compare this to archival photometry of all BTS hosts. Using the spectroscopically complete BTS, we conclude that 0.3%^(+0.3)_(-0.1) of all CCSNe occur in elliptical galaxies. We derive star formation rates and stellar masses for the host galaxies and compare them to the properties of other SN hosts. We show that CCSNe in ellipticals have larger physical separations from their hosts compared to SNe Ia in elliptical galaxies, and discuss implications for star-forming activity in elliptical galaxies.",
"doi": "10.3847/1538-4357/ac4709",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-03-01",
"series_number": "1",
"volume": "927",
"issue": "1",
"pages": "Art. No. 10"
},
{
"id": "authors:pcrbj-whc73",
"collection": "authors",
"collection_id": "pcrbj-whc73",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-150000950",
"type": "article",
"title": "Two c's in a pod: cosmology-independent measurement of the Type Ia supernova colour\u2013luminosity relation with a sibling pair",
"author": [
{
"family_name": "Biswas",
"given_name": "Rahul",
"orcid": "0000-0002-5741-7195",
"clpid": "Biswas-Rahul"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-Ariel"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979",
"clpid": "Dhawan-Suhail"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-Steve"
},
{
"family_name": "Johansson",
"given_name": "Joel",
"orcid": "0000-0001-5975-290X",
"clpid": "Johansson-Joel"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kim",
"given_name": "Young-Lo",
"orcid": "0000-0002-1031-0796",
"clpid": "Kim-Young-Lo"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Matthew",
"orcid": "0000-0003-0103-8820",
"clpid": "Smith-Matthew"
},
{
"family_name": "Walters",
"given_name": "Richard S.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
}
],
"abstract": "Using Zwicky Transient Facility (ZTF) observations, we identify a pair of 'sibling' Type Ia supernovae (SNe Ia), i.e. hosted by the same galaxy at z = 0.0541. They exploded within 200 d from each other at a separation of 0.6arcsec corresponding to a projected distance of only 0.6 kpc. Performing SALT2 light-curve fits to the gri ZTF photometry, we show that for these equally distant 'standardizable candles', there is a difference of 2 mag in their rest-frame B-band peaks, and the fainter supernova (SN) has a significantly red SALT2 colour c = 0.57 \u00b1 0.04, while the stretch values x\u2081 of the two SNe are similar, suggesting that the fainter SN is attenuated by dust in the interstellar medium of the host galaxy. We use these measurements to infer the SALT2 colour standardization parameter, \u03b2 = 3.5 \u00b1 0.3, independent of the underlying cosmology and Malmquist bias. Assuming the colour excess is entirely due to dust, the result differs by 2\u03c3 from the average Milky Way total-to-selective extinction ratio, but is in good agreement with the colour\u2013brightness corrections empirically derived from the most recent SN Ia Hubble\u2013Lemaitre diagram fits. Thus we suggest that SN 'siblings', which will increasingly be discovered in the coming years, can be used to probe the validity of the colour and light-curve shape corrections using in SN Ia cosmology while avoiding important systematic effects in their inference from global multiparameter fits to inhomogeneous data sets, and also help constrain the role of interstellar dust in SN Ia cosmology.",
"doi": "10.1093/mnras/stab2943",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-02",
"series_number": "4",
"volume": "509",
"issue": "4",
"pages": "5340-5356"
},
{
"id": "authors:xsjz1-nar55",
"collection": "authors",
"collection_id": "xsjz1-nar55",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211217-233205774",
"type": "article",
"title": "Inferring Kilonova Population Properties with a Hierarchical Bayesian Framework. I. Nondetection Methodology and Single-event Analyses",
"author": [
{
"family_name": "Mohite",
"given_name": "Siddharth R.",
"orcid": "0000-0003-1356-7156",
"clpid": "Mohite-Siddharth-R"
},
{
"family_name": "Rajkumar",
"given_name": "Priyadarshini",
"clpid": "Rajkumar-Priyadarshini"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-David-L"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Sagu\u00e9s-Carracedo",
"given_name": "Ana",
"orcid": "0000-0002-3498-2167",
"clpid": "Sagu\u00e9s-Carracedo-Ana"
},
{
"family_name": "Saleem",
"given_name": "Muhammed",
"clpid": "Saleem-Muhammed"
},
{
"family_name": "Creighton",
"given_name": "Jolien",
"orcid": "0000-0003-3600-2406",
"clpid": "Creighton-Jolien-D-E"
},
{
"family_name": "Brady",
"given_name": "Patrick R.",
"orcid": "0000-0002-4611-9387",
"clpid": "Brady-Patrick-R"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-Tom\u00e1s"
},
{
"family_name": "Almualla",
"given_name": "Mouza",
"orcid": "0000-0002-4694-7123",
"clpid": "Almualla-Mouza"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127",
"clpid": "Bulla-Mattia"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-Stephen"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Shin",
"given_name": "Kyung Min",
"orcid": "0000-0002-1486-3582",
"clpid": "Shin-Kyung-Min"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-Leo-P"
}
],
"abstract": "We present nimbus: a hierarchical Bayesian framework to infer the intrinsic luminosity parameters of kilonovae (KNe) associated with gravitational-wave (GW) events, based purely on nondetections. This framework makes use of GW 3D distance information and electromagnetic upper limits from multiple surveys for multiple events and self-consistently accounts for the finite sky coverage and probability of astrophysical origin. The framework is agnostic to the brightness evolution assumed and can account for multiple electromagnetic passbands simultaneously. Our analyses highlight the importance of accounting for model selection effects, especially in the context of nondetections. We show our methodology using a simple, two-parameter linear brightness model, taking the follow-up of GW190425 with the Zwicky Transient Facility as a single-event test case for two different prior choices of model parameters: (i) uniform/uninformative priors and (ii) astrophysical priors based on surrogate models of Monte Carlo radiative-transfer simulations of KNe. We present results under the assumption that the KN is within the searched region to demonstrate functionality and the importance of prior choice. Our results show consistency with simsurvey\u2014an astronomical survey simulation tool used previously in the literature to constrain the population of KNe. While our results based on uniform priors strongly constrain the parameter space, those based on astrophysical priors are largely uninformative, highlighting the need for deeper constraints. Future studies with multiple events having electromagnetic follow-up from multiple surveys should make it possible to constrain the KN population further.",
"doi": "10.3847/1538-4357/ac3981",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-01-20",
"series_number": "1",
"volume": "925",
"issue": "1",
"pages": "Art. No. 58"
},
{
"id": "authors:tw5q0-dex83",
"collection": "authors",
"collection_id": "tw5q0-dex83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210927-205831656",
"type": "article",
"title": "A WC/WO star exploding within an expanding carbon\u2013oxygen\u2013neon nebula",
"author": [
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-Avishay"
},
{
"family_name": "Bruch",
"given_name": "R.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Yang",
"given_name": "Y."
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Irani",
"given_name": "I.",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Kool",
"given_name": "E. C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Soumagnac",
"given_name": "M. T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Yaron",
"given_name": "O.",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Strotjohann",
"given_name": "N. L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Zimmerman",
"given_name": "E.",
"orcid": "0000-0001-8985-2493"
},
{
"family_name": "Barbarino",
"given_name": "C.",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Yao",
"given_name": "Y.",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Ofek",
"given_name": "E. O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Fransson",
"given_name": "C.",
"orcid": "0000-0001-8532-3594"
},
{
"family_name": "Filippenko",
"given_name": "A. V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Zheng",
"given_name": "W."
},
{
"family_name": "Brink",
"given_name": "T. G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Copperwheat",
"given_name": "C. M.",
"orcid": "0000-0001-7983-8698"
},
{
"family_name": "Foley",
"given_name": "R. J."
},
{
"family_name": "Brown",
"given_name": "J.",
"orcid": "0000-0002-1885-6419"
},
{
"family_name": "Siebert",
"given_name": "M.",
"orcid": "0000-0003-2445-3891"
},
{
"family_name": "Leloudas",
"given_name": "G.",
"orcid": "0000-0002-8597-0756"
},
{
"family_name": "Cabrera Lavers",
"given_name": "A. L.",
"orcid": "0000-0002-9153-8724"
},
{
"family_name": "Garcia Alvarez",
"given_name": "D."
},
{
"family_name": "Marante-Barreto",
"given_name": "A."
},
{
"family_name": "Frederick",
"given_name": "S.",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Hung",
"given_name": "T.",
"orcid": "0000-0002-9878-7889"
},
{
"family_name": "Wheeler",
"given_name": "J. C.",
"orcid": "0000-0003-1349-6538"
},
{
"family_name": "Vink\u00f3",
"given_name": "J.",
"orcid": "0000-0001-8764-7832"
},
{
"family_name": "Thomas",
"given_name": "B. P."
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Duev",
"given_name": "D. A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Drake",
"given_name": "A. J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes-C"
},
{
"family_name": "Knezevic",
"given_name": "N."
}
],
"abstract": "The final fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf\u2013Rayet stars emit strong and rapidly expanding winds with speeds greater than 1,000\u2009kilometres\u2009per second. A fraction of this population is also helium-depleted, with spectra dominated by highly ionized emission lines of carbon and oxygen (types\u2009WC/WO). Evidence indicates that the most commonly observed supernova explosions that lack hydrogen and helium (types\u2009Ib/Ic) cannot result from massive WC/WO stars , leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosion4. Here we report observations of SN\u20092019hgp, beginning about a day after the explosion. Its short rise time and rapid decline place it among an emerging population of rapidly evolving transients. Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen and neon. Narrow absorption features show that this material is expanding at high velocities (greater than 1,500\u2009kilometres\u2009per second), requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive Wolf\u2013Rayet stars may be the progenitors of some rapidly evolving transients.",
"doi": "10.1038/s41586-021-04155-1",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2022-01-13",
"series_number": "7892",
"volume": "601",
"issue": "7892",
"pages": "201-204"
},
{
"id": "authors:kyw21-8km96",
"collection": "authors",
"collection_id": "kyw21-8km96",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211207-393887000",
"type": "article",
"title": "AT 2018lqh and the Nature of the Emerging Population of Day-scale Duration Optical Transients",
"author": [
{
"family_name": "Ofek",
"given_name": "E. O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-Eran-O"
},
{
"family_name": "Adams",
"given_name": "S. M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Waxman",
"given_name": "E.",
"orcid": "0000-0002-9038-5877",
"clpid": "Waxman-Eli"
},
{
"family_name": "Sharon",
"given_name": "A.",
"clpid": "Sharon-A"
},
{
"family_name": "Kushnir",
"given_name": "D.",
"clpid": "Kushnir-D"
},
{
"family_name": "Horesh",
"given_name": "A.",
"orcid": "0000-0002-5936-1156",
"clpid": "Horesh-Assaf"
},
{
"family_name": "Ho",
"given_name": "A.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Yaron",
"given_name": "O.",
"orcid": "0000-0002-0301-8017",
"clpid": "Yaron-Ofer"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-Avishay"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Bellm",
"given_name": "E.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Graham",
"given_name": "M.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Duev",
"given_name": "D.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Mahabal",
"given_name": "A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Drake",
"given_name": "A.",
"clpid": "Drake-Andrew-J"
}
],
"abstract": "We report on the discovery of AT 2018lqh (ZTF 18abfzgpl)\u2014a rapidly evolving extragalactic transient in a star-forming host at 242 Mpc. The transient g-band light curve's duration above a half-maximum light is about 2.1 days, where 0.4/1.7 days are spent on the rise/decay, respectively. The estimated bolometric light curve of this object peaked at about 7 \u00d7 10\u2074\u00b2 erg s\u207b\u00b9\u2014roughly 7 times brighter than the neutron star (NS)\u2013NS merger event AT 2017gfo. We show that this event can be explained by an explosion with a fast (v \u223c 0.08 c) low-mass (\u22480.07 M_\u2299) ejecta, composed mostly of radioactive elements. For example, ejecta dominated by \u2075\u2076Ni with a timescale of t\u2080 \u2245 1.6 days for the ejecta to become optically thin for \u03b3-rays fits the data well. Such a scenario requires burning at densities that are typically found in the envelopes of neutron stars or the cores of white dwarfs. A combination of circumstellar material (CSM) interaction power at early times and shock cooling at late times is consistent with the photometric observations, but the observed spectrum of the event may pose some challenges for this scenario. We argue that the observations are not consistent with a shock breakout from a stellar envelope, while a model involving a low-mass ejecta ramming into low-mass CSM cannot explain both the early- and late-time observations.",
"doi": "10.3847/1538-4357/ac24fc",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-12-01",
"series_number": "2",
"volume": "922",
"issue": "2",
"pages": "Art. No. 247"
},
{
"id": "authors:e0emw-2nd96",
"collection": "authors",
"collection_id": "e0emw-2nd96",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210604-142603248",
"type": "article",
"title": "ZTFJ0038+2030: A Long-period Eclipsing White Dwarf and a Substellar Companion",
"author": [
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Bell",
"given_name": "Keaton J.",
"orcid": "0000-0002-0656-032X",
"clpid": "Bell-Keaton-J"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin-B"
},
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Porter",
"given_name": "Michael",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-Michael-D"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Shin",
"given_name": "Kyung Min",
"clpid": "Shin-Kyung-Min"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "In a search for eclipsing white dwarfs using the Zwicky Transient Facility lightcurves, we identified a deep eclipsing white dwarf with an orbital period of 10.4 hr and an undetected substellar companion. We obtained high-speed photometry and radial velocity measurements to characterize the system. The white dwarf has a mass of 0.50 \u00b1 0.02 M_\u2609 and a temperature of 10,900 \u00b1 200 K. The companion has a mass of 0.059 \u00b1 0.004 M_\u2609 and is a brown dwarf. It has a radius of 0.0783 \u00b1 0.0013 R_\u2609, and is one of the physically smallest transiting brown dwarfs known and likely old, \u22738 Gyr. The ZTF discovery efficiency of substellar objects transiting white dwarfs is limited by the number of epochs and as ZTF continues to collect data we expect to find more of these systems.",
"doi": "10.3847/2041-8213/ac22b7",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2021-10-01",
"series_number": "2",
"volume": "919",
"issue": "2",
"pages": "Art. No. L26"
},
{
"id": "authors:e8pv8-xbk49",
"collection": "authors",
"collection_id": "e8pv8-xbk49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-150004474",
"type": "article",
"title": "Fast-transient Searches in Real Time with ZTFReST: Identification of Three Optically Discovered Gamma-Ray Burst Afterglows and New Constraints on the Kilonova Rate",
"author": [
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kumar",
"given_name": "Harsh",
"orcid": "0000-0003-0871-4641"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "Carracedo",
"given_name": "Ana Sagu\u00e9s",
"orcid": "0000-0002-3498-2167"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Pang",
"given_name": "Peter T. H.",
"orcid": "0000-0001-7041-3239"
},
{
"family_name": "Saraogi",
"given_name": "Divita"
},
{
"family_name": "Sharma",
"given_name": "Kritti",
"orcid": "0000-0002-4477-3625"
},
{
"family_name": "Shenoy",
"given_name": "Vedant"
},
{
"family_name": "Burns",
"given_name": "Eric",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Fremling",
"given_name": "U. C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Crellin-Quick",
"given_name": "Arien"
},
{
"family_name": "Dietrich",
"given_name": "Tim",
"orcid": "0000-0003-2374-307X"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "The most common way to discover extragalactic fast transients, which fade within a few nights in the optical, is via follow-up of gamma-ray burst and gravitational-wave triggers. However, wide-field surveys have the potential to identify rapidly fading transients independently of such external triggers. The volumetric survey speed of the Zwicky Transient Facility (ZTF) makes it sensitive to objects as faint and fast fading as kilonovae, the optical counterparts to binary neutron star mergers, out to almost 200 Mpc. We introduce an open-source software infrastructure, the ZTF REaltime Search and Triggering, ZTFReST, designed to identify kilonovae and fast transients in ZTF data. Using the ZTF alert stream combined with forced point-spread-function photometry, we have implemented automated candidate ranking based on their photometric evolution and fitting to kilonova models. Automated triggering, with a human in the loop for monitoring, of follow-up systems has also been implemented. In 13 months of science validation, we found several extragalactic fast transients independently of any external trigger, including two supernovae with post-shock cooling emission, two known afterglows with an associated gamma-ray burst (ZTF20abbiixp, ZTF20abwysqy), two known afterglows without any known gamma-ray counterpart (ZTF20aajnksq, ZTF21aaeyldq), and three new fast-declining sources (ZTF20abtxwfx, ZTF20acozryr, ZTF21aagwbjr) that are likely associated with GRB200817A, GRB201103B, and GRB210204A. However, we have not found any objects that appear to be kilonovae. We constrain the rate of GW170817-like kilonovae to R < 900 Gpc\u207b\u00b3 yr\u207b\u00b9 (95% confidence). A framework such as ZTFReST could become a prime tool for kilonova and fast-transient discovery with the Vera Rubin Observatory.",
"doi": "10.3847/1538-4357/ac0bc7",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-09-10",
"series_number": "2",
"volume": "918",
"issue": "2",
"pages": "Art. No. 63"
},
{
"id": "authors:nbkf4-xcm60",
"collection": "authors",
"collection_id": "nbkf4-xcm60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210526-152342697",
"type": "article",
"title": "A Systematic Search for Outbursting AM CVn Systems with the Zwicky Transient Facility",
"author": [
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes"
},
{
"family_name": "Creter",
"given_name": "Leah",
"clpid": "Creter-Leah"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"orcid": "0000-0003-4373-7777",
"clpid": "Szkody-Paula"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Green",
"given_name": "Matthew J.",
"orcid": "0000-0002-0948-4801",
"clpid": "Green-Matthew-J"
},
{
"family_name": "Rich",
"given_name": "R. Michael",
"orcid": "0000-0003-0427-8387",
"clpid": "Rich-R-Michael"
},
{
"family_name": "Sepikas",
"given_name": "John",
"clpid": "Sepikas-John"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin-B"
},
{
"family_name": "Caiazzo",
"given_name": "Ilaria",
"orcid": "0000-0002-4770-5388",
"clpid": "Caiazzo-Ilaria"
},
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
}
],
"abstract": "AM CVn systems are a rare type of accreting binary that consists of a white dwarf and a helium-rich, degenerate donor star. Using the Zwicky Transient Facility (ZTF), we searched for new AM CVn systems by focusing on blue, outbursting stars. We first selected outbursting stars using the ZTF alerts. We cross matched the candidates with Gaia and Pan-STARRS catalogs. The initial selection of candidates based on the Gaia BP-RP contains 1751 unknown objects. We used the Pan-STARRS g-r and r-i color in combination with the Gaia color to identify 59 strong AM CVn candidates. We obtained identification spectra of 35 sources, of which 18 are high-priority candidates, and discovered nine new AM CVn systems and one magnetic CV that shows only He-ii lines. Using the outburst recurrence time, we estimate the orbital periods of the nine new AM CVn systems that are in the range of 29\u201350 minutes. We conclude that targeted follow up of blue, outbursting sources is an efficient method to find new AM CVn systems and we plan to follow up all candidates we identified to systematically study the population of outbursting AM CVn systems.",
"doi": "10.3847/1538-3881/ac0622",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-09",
"series_number": "3",
"volume": "162",
"issue": "3",
"pages": "Art. No. 113"
},
{
"id": "authors:amhq5-48y04",
"collection": "authors",
"collection_id": "amhq5-48y04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-150008009",
"type": "article",
"title": "SNIascore: Deep-learning Classification of Low-resolution Supernova Spectra",
"author": [
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Hall",
"given_name": "Xander J.",
"orcid": "0000-0002-9364-5419",
"clpid": "Hall-Xander-J"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya S.",
"clpid": "Dahiwale-Aishwarya-S"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-Adam-A"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"orcid": "0000-0002-6099-7565",
"clpid": "Rosnet-Philippe"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shin",
"given_name": "Kyung Min",
"orcid": "0000-0002-1486-3582",
"clpid": "Shin-Kyung-Min"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Walters",
"given_name": "Richard S.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "We present SNIascore, a deep-learning-based method for spectroscopic classification of thermonuclear supernovae (SNe Ia) based on very low-resolution (R ~ 100) data. The goal of SNIascore is the fully automated classification of SNe Ia with a very low false-positive rate (FPR) so that human intervention can be greatly reduced in large-scale SN classification efforts, such as that undertaken by the public Zwicky Transient Facility (ZTF) Bright Transient Survey (BTS). We utilize a recurrent neural network architecture with a combination of bidirectional long short-term memory and gated recurrent unit layers. SNIascore achieves a <0.6% FPR while classifying up to 90% of the low-resolution SN Ia spectra obtained by the BTS. SNIascore simultaneously performs binary classification and predicts the redshifts of secure SNe Ia via regression (with a typical uncertainty of <0.005 in the range from z = 0.01 to z = 0.12). For the magnitude-limited ZTF BTS survey (\u224870% SNe Ia), deploying SNIascore reduces the amount of spectra in need of human classification or confirmation by \u224860%. Furthermore, SNIascore allows SN Ia classifications to be automatically announced in real time to the public immediately following a finished observation during the night.",
"doi": "10.3847/2041-8213/ac116f",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2021-08-10",
"series_number": "1",
"volume": "917",
"issue": "1",
"pages": "Art. No. L2"
},
{
"id": "authors:c1bm9-7b434",
"collection": "authors",
"collection_id": "c1bm9-7b434",
"cite_using_url": "https://authors.library.caltech.edu/records/c1bm9-7b434",
"type": "article",
"title": "A tidal disruption event coincident with a high-energy neutrino",
"author": [
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Kowalski",
"given_name": "Marek",
"orcid": "0000-0001-8594-8666"
},
{
"family_name": "Franckowiak",
"given_name": "Anna",
"orcid": "0000-0002-5605-2219"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Miller-Jones",
"given_name": "James C. A.",
"orcid": "0000-0003-3124-2814"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Sfaradi",
"given_name": "Itai",
"orcid": "0000-0003-0466-3779"
},
{
"family_name": "Bietenholz",
"given_name": "Michael F."
},
{
"family_name": "Horesh",
"given_name": "Assaf",
"orcid": "0000-0002-5936-1156"
},
{
"family_name": "Fender",
"given_name": "Rob",
"orcid": "0000-0002-5654-2744"
},
{
"family_name": "Garrappa",
"given_name": "Simone",
"orcid": "0000-0003-2403-4582"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Belicki",
"given_name": "Justin",
"clpid": "Belicki-Justin"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "B\u00f6ttcher",
"given_name": "Markus"
},
{
"family_name": "Brinnel",
"given_name": "Valery"
},
{
"family_name": "Burruss",
"given_name": "Rick",
"clpid": "Burruss-Rick-S"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Cunningham",
"given_name": "Virginia",
"orcid": "0000-0003-2292-0441"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Farrar",
"given_name": "Glennys R."
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-Michael-E"
},
{
"family_name": "Foley",
"given_name": "Ryan J.",
"orcid": "0000-0002-2445-5275"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kilpatrick",
"given_name": "Charles D.",
"orcid": "0000-0002-5740-7747"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Necker",
"given_name": "Jannis",
"orcid": "0000-0003-0280-7484"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Reusch",
"given_name": "Simeon",
"orcid": "0000-0002-7788-628X"
},
{
"family_name": "Rodriguez",
"given_name": "Hector",
"clpid": "Rodriguez-Hector"
},
{
"family_name": "Rojas-Bravo",
"given_name": "C\u00e9sar",
"orcid": "0000-0002-7559-315X"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-Daniel"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "van Santen",
"given_name": "Jakob"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682"
},
{
"family_name": "Woudt",
"given_name": "Patrick A.",
"orcid": "0000-0002-6896-1655"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "Cosmic neutrinos provide a unique window into the otherwise hidden mechanism of particle acceleration in astrophysical objects. The IceCube Collaboration recently reported the likely association of one high-energy neutrino with a flare from the relativistic jet of an active galaxy pointed towards the Earth. However a combined analysis of many similar active galaxies revealed no excess from the broader population, leaving the vast majority of the cosmic neutrino flux unexplained. Here we present the likely association of a radio-emitting tidal disruption event, AT2019dsg, with a second high-energy neutrino. AT2019dsg was identified as part of our systematic search for optical counterparts to high-energy neutrinos with the Zwicky Transient Facility. The probability of finding any coincident radio-emitting tidal disruption event by chance is 0.5%, while the probability of finding one as bright in bolometric energy flux as AT2019dsg is 0.2%. Our electromagnetic observations can be explained through a multizone model, with radio analysis revealing a central engine, embedded in a UV photosphere, that powers an extended synchrotron-emitting outflow. This provides an ideal site for petaelectronvolt neutrino production. Assuming that the association is genuine, our observations suggest that tidal disruption events with mildly relativistic outflows contribute to the cosmic neutrino flux.",
"doi": "10.1038/s41550-020-01295-8",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2021-05",
"volume": "5",
"pages": "510-518"
},
{
"id": "authors:55882-yhy85",
"collection": "authors",
"collection_id": "55882-yhy85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200414-075012273",
"type": "article",
"title": "Seventeen Tidal Disruption Events from the First Half of ZTF Survey Observations: Entering a New Era of Population Studies",
"author": [
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-Sjoert"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Roth",
"given_name": "Nathaniel",
"orcid": "0000-0002-6485-2259"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Foley",
"given_name": "Ryan J."
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadejda",
"orcid": "0000-0003-0901-1606"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Brinnel",
"given_name": "Valery"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-Michael-E"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Giomi",
"given_name": "Matteo"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kilpatrick",
"given_name": "Charles D.",
"orcid": "0000-0002-5740-7747"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "van Santen",
"given_name": "Jakob"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
}
],
"abstract": "While tidal disruption events (TDEs) have long been heralded as laboratories for the study of quiescent black holes, the small number of known TDEs and uncertainties in their emission mechanism have hindered progress toward this promise. Here we present 17 new TDEs that have been detected recently by the Zwicky Transient Facility along with Swift UV and X-ray follow-up observations. Our homogeneous analysis of the optical/UV light curves, including 22 previously known TDEs from the literature, reveals a clean separation of light-curve properties with spectroscopic class. The TDEs with Bowen fluorescence features in their optical spectra have smaller blackbody radii, lower optical luminosities, and higher disruption rates compared to the rest of the sample. The small subset of TDEs that show only helium emission lines in their spectra have the longest rise times, the highest luminosities, and the lowest rates. A high detection rate of Bowen lines in TDEs with small photometric radii could be explained by the high density that is required for this fluorescence mechanism. The stellar debris can provide a source for this dense material. Diffusion of photons through this debris may explain why the rise and fade timescale of the TDEs in our sample are not correlated. We also report, for the first time, the detection of soft X-ray flares from a TDE on ~day timescales. Based on the fact that the X-ray flares peak at a luminosity similar to the optical/UV blackbody luminosity, we attribute them to brief glimpses through a reprocessing layer that otherwise obscures the inner accretion flow.",
"doi": "10.3847/1538-4357/abc258",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-02-10",
"series_number": "1",
"volume": "908",
"issue": "1",
"pages": "Art. No. 4"
},
{
"id": "authors:vy5xn-x2076",
"collection": "authors",
"collection_id": "vy5xn-x2076",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200717-162631605",
"type": "article",
"title": "Optical follow-up of the neutron star\u2013black hole mergers S200105ae and S200115j",
"author": [
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Sagu\u00e9s Carracedo",
"given_name": "Ana"
},
{
"family_name": "Almualla",
"given_name": "Mouza",
"orcid": "0000-0002-4694-7123"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387"
},
{
"family_name": "Foucart",
"given_name": "Fran\u00e7ois",
"orcid": "0000-0003-4617-4738"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bolin",
"given_name": "Bryce",
"orcid": "0000-0002-4950-6323",
"clpid": "Bolin-Bryce-T"
},
{
"family_name": "Caballero-Garc\u00eda",
"given_name": "M. D.",
"orcid": "0000-0001-7920-4564"
},
{
"family_name": "Castro-Tirado",
"given_name": "Alberto J."
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard G.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-Michael-E"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Guessoum",
"given_name": "Nidhal",
"orcid": "0000-0003-1585-8205"
},
{
"family_name": "Hankins",
"given_name": "Matthew J.",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
},
{
"family_name": "Hu",
"given_name": "Youdong",
"orcid": "0000-0002-7400-4608"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kumar",
"given_name": "Harsh"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Nissanke",
"given_name": "Samaya",
"orcid": "0000-0001-6573-7773"
},
{
"family_name": "Porter",
"given_name": "Michael",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-Michael-D"
},
{
"family_name": "Reusch",
"given_name": "Simeon"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rosnet",
"given_name": "Philippe"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-Eugene"
},
{
"family_name": "S\u00e1nchez-Ram\u00edrez",
"given_name": "R.",
"orcid": "0000-0002-7158-5099"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-Maayane-T"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Valeev",
"given_name": "Azamat F.",
"orcid": "0000-0003-3513-3527",
"clpid": "Valeev-Azamat-F"
}
],
"abstract": "LIGO and Virgo's third observing run revealed the first neutron star\u2013black hole (NSBH) merger candidates in gravitational waves. These events are predicted to synthesize r-process elements creating optical/near-infrared 'kilonova' emission. The joint gravitational wave and electromagnetic detection of an NSBH merger could be used to constrain the equation of state of dense nuclear matter, and independently measure the local expansion rate of the Universe. Here, we present the optical follow-up and analysis of two of the only three high-significance NSBH merger candidates detected to date, S200105ae and S200115j, with the Zwicky Transient Facility. The Zwicky Transient Facility observed ~48% of S200105ae and ~22% of S200115j's localization probabilities, with observations sensitive to kilonovae brighter than \u221217.5\u2009mag fading at 0.5\u2009mag\u2009d\u207b\u00b9 in the g- and r-bands; extensive searches and systematic follow-up of candidates did not yield a viable counterpart. We present state-of-the-art kilonova models tailored to NSBH systems that place constraints on the ejecta properties of these NSBH mergers. We show that with observed depths of apparent magnitude ~22\u2009mag, attainable in metre-class, wide-field-of-view survey instruments, strong constraints on ejecta mass are possible, with the potential to rule out low mass ratios, high black hole spins and large neutron star radii.",
"doi": "10.1038/s41550-020-1183-3",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2021-01",
"series_number": "1",
"volume": "5",
"issue": "1",
"pages": "46-53"
},
{
"id": "authors:rztcc-p0956",
"collection": "authors",
"collection_id": "rztcc-p0956",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200824-095838244",
"type": "article",
"title": "ZTF20aajnksq (AT 2020blt): A Fast Optical Transient at z \u2248 2.9 with No Detected Gamma-Ray Burst Counterpart",
"author": [
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Beniamini",
"given_name": "Paz",
"orcid": "0000-0001-7833-1043",
"clpid": "Beniamini-Paz"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-Bradley"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-Leo-P"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-Alexandre"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Zach"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-Ariel"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David-D-S"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-Adam-A"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Jan"
}
],
"abstract": "We present ZTF20aajnksq (AT 2020blt), a fast-fading (\u0394r = 2.3 mag in \u0394t = 1.3 days) red (g \u2212 r \u2248 0.6 mag) and luminous (M_(1626 \u00c5) = \u221225.9 mag) optical transient at z = 2.9 discovered by the Zwicky Transient Facility (ZTF). AT 2020blt shares several features in common with afterglows to long-duration gamma-ray bursts (GRBs): (1) an optical light curve well-described by a broken power law with a break at t_j = 1 d (observer frame); (2) a luminous (L_(0.3\u201310 KeV) = 10\u2074\u2076 erg s\u207b\u00b9) X-ray counterpart; and (3) luminous (L_(10 GHz) = 4 \u00d7 10\u00b3\u00b9 erg s\u207b\u00b9 Hz\u207b\u00b9) radio emission. However, no GRB was detected in the 0.74 days between the last ZTF nondetection (r > 21.36 mag) and the first ZTF detection (r = 19.60 mag), with an upper limit on the isotropic-equivalent gamma-ray energy release of E_(\u03b3,iso) < 7 \u00d7 10\u2075\u00b2 erg. AT 2020blt is thus the third afterglow-like transient discovered without a detected GRB counterpart (after PTF11agg and ZTF19abvizsw) and the second (after ZTF19abvizsw) with a redshift measurement. We conclude that the properties of AT 2020blt are consistent with a classical (initial Lorentz factor \u0393\u2080 \u2273 100) on-axis GRB that was missed by high-energy satellites. Furthermore, by estimating the rate of transients with light curves similar to that of AT 2020blt in ZTF high-cadence data, we agree with previous results that there is no evidence for an afterglow-like phenomenon that is significantly more common than classical GRBs, such as dirty fireballs. We conclude by discussing the status and future of fast-transient searches in wide-field high-cadence optical surveys.",
"doi": "10.3847/1538-4357/abc34d",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-20",
"series_number": "2",
"volume": "905",
"issue": "2",
"pages": "Art. No. 98"
},
{
"id": "authors:0z0sc-hap43",
"collection": "authors",
"collection_id": "0z0sc-hap43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151423784",
"type": "article",
"title": "The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses",
"author": [
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Adams",
"given_name": "Scott",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Aloisi",
"given_name": "Robert",
"orcid": "0000-0003-2822-616X"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-Ashot"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bildsten",
"given_name": "Lars"
},
{
"family_name": "Cannella",
"given_name": "Christopher",
"orcid": "0000-0003-2667-7290",
"clpid": "Cannella-Christopher-B"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-Alexandre"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"clpid": "Dugas-Alison-M"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Goldstein",
"given_name": "Daniel",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David-D-S"
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-Stephen"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Leadbeater",
"given_name": "Robin"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-Ragnhild"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"orcid": "0000-0002-1633-6495"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Quataert",
"given_name": "Eliot",
"orcid": "0000-0001-9185-5044"
},
{
"family_name": "Reiley",
"given_name": "Dan",
"clpid": "Reiley-Daniel-J"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "Using the Zwicky Transient Facility alert stream, we are conducting a large spectroscopic campaign to construct a complete, volume-limited sample of transients brighter than 20 mag, and coincident within 100\" of galaxies in the Census of the Local Universe catalog. We describe the experiment design and spectroscopic completeness from the first 16 months of operations, which have classified 754 supernovae. We present results from a systematic search for calcium-rich gap transients in the sample of 22 low-luminosity (peak absolute magnitude M > \u221217), hydrogen-poor events found in the experiment. We report the detection of eight new events, and constrain their volumetric rate to \u2273 15% \u00b1 5% of the SN Ia rate. Combining this sample with 10 previously known events, we find a likely continuum of spectroscopic properties ranging from events with SN Ia\u2013like features (Ca-Ia objects) to those with SN Ib/c\u2013like features (Ca-Ib/c objects) at peak light. Within the Ca-Ib/c events, we find two populations distinguished by their red (g \u2212 r \u2248 1.5 mag) or green (g - r \u2248 0.5 mag) colors at the r-band peak, wherein redder events show strong line blanketing features and slower light curves (similar to Ca-Ia objects), weaker He lines, and lower [Ca ii]/[O i] in the nebular phase. We find that all together the spectroscopic continuum, volumetric rates, and striking old environments are consistent with the explosive burning of He shells on low-mass white dwarfs. We suggest that Ca-Ia and red Ca-Ib/c objects arise from the double detonation of He shells, while green Ca-Ib/c objects are consistent with low-efficiency burning scenarios like detonations in low-density shells or deflagrations.",
"doi": "10.3847/1538-4357/abb45c",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-10",
"series_number": "1",
"volume": "905",
"issue": "1",
"pages": "Art. No. 58"
},
{
"id": "authors:ajckt-43s30",
"collection": "authors",
"collection_id": "ajckt-43s30",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112923664",
"type": "article",
"title": "A Non-equipartition Shock Wave Traveling in a Dense Circumstellar Environment around SN 2020oi",
"author": [
{
"family_name": "Horesh",
"given_name": "Assaf",
"orcid": "0000-0002-5936-1156",
"clpid": "Horesh-A"
},
{
"family_name": "Sfaradi",
"given_name": "Itai",
"orcid": "0000-0003-0466-3779"
},
{
"family_name": "Ergon",
"given_name": "Mattias"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Moldon",
"given_name": "Javier",
"orcid": "0000-0002-8079-7608"
},
{
"family_name": "Dobie",
"given_name": "Dougal",
"orcid": "0000-0003-0699-7019"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "P\u00e9rez-Torres",
"given_name": "Miguel",
"orcid": "0000-0001-5654-0266"
},
{
"family_name": "Williams",
"given_name": "David R. A.",
"orcid": "0000-0001-7361-0246"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "O'Brien",
"given_name": "Andrew",
"orcid": "0000-0003-4609-2791"
},
{
"family_name": "Lundqvist",
"given_name": "Peter",
"orcid": "0000-0002-3664-8082"
},
{
"family_name": "Murphy",
"given_name": "Tara",
"orcid": "0000-0002-2686-438X"
},
{
"family_name": "Fender",
"given_name": "Rob",
"orcid": "0000-0002-5654-2744"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Belicki",
"given_name": "Justin",
"clpid": "Belicki-J"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Green",
"given_name": "Dave A."
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Perrott",
"given_name": "Yvette",
"orcid": "0000-0002-6255-8240"
},
{
"family_name": "Porter",
"given_name": "Michael",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-M-D"
},
{
"family_name": "Reiley",
"given_name": "Daniel J.",
"clpid": "Reiley-D-J"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Rodriguez",
"given_name": "Hector",
"clpid": "Rodriguez-Hector"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Titterington",
"given_name": "David"
}
],
"abstract": "We report the discovery and panchromatic follow-up observations of the young Type Ic supernova (SN Ic) SN 2020oi in M100, a grand-design spiral galaxy at a mere distance of 14 Mpc. We followed up with observations at radio, X-ray, and optical wavelengths from only a few days to several months after explosion. The optical behavior of the supernova is similar to those of other normal SNe Ic. The event was not detected in the X-ray band but our radio observations revealed a bright mJy source (L_\u03bd \u2248 1.2 \u00d7 10\u00b2\u2077 ergs\u207b\u00b9 Hz\u207b\u00b9). Given the relatively small number of stripped envelope SNe for which radio emission is detectable, we used this opportunity to perform a detailed analysis of the comprehensive radio data set we obtained. The radio-emitting electrons initially experience a phase of inverse Compton cooling, which leads to steepening of the spectral index of the radio emission. Our analysis of the cooling frequency points to a large deviation from equipartition at the level of \u03f5_e/\u03f5_B \u2273 200, similar to a few other cases of stripped envelope SNe. Our modeling of the radio data suggests that the shock wave driven by the SN ejecta into the circumstellar matter (CSM) is moving at \u223c3 \u00d7 10\u2074 km s\u207b\u00b9. Assuming a constant mass loss from the stellar progenitor, we find that the mass-loss rate is \u1e40 \u2248 1.4 \u00d7 10\u207b\u2074 M_\u2299 yr\u207b\u00b9 for an assumed wind velocity of 1000 km s\u207b\u00b9. The temporal evolution of the radio emission suggests a radial CSM density structure steeper than the standard r\u207b\u00b2.",
"doi": "10.3847/1538-4357/abbd38",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-11-10",
"series_number": "2",
"volume": "903",
"issue": "2",
"pages": "Art. No. 132"
},
{
"id": "authors:gjgr5-y5131",
"collection": "authors",
"collection_id": "gjgr5-y5131",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200414-083356186",
"type": "article",
"title": "ZTF Early Observations of Type Ia Supernovae. III. Early-time Colors As a Test for Explosion Models and Multiple Populations",
"author": [
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127",
"clpid": "Bulla-M"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Dessart",
"given_name": "Luc",
"orcid": "0000-0003-0599-8407",
"clpid": "Dessart-L"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979",
"clpid": "Dhawan-S"
},
{
"family_name": "Papadogiannakis",
"given_name": "Semeli",
"orcid": "0000-0003-0783-3323",
"clpid": "Papadogiannakis-S"
},
{
"family_name": "Biswas",
"given_name": "Rahul",
"orcid": "0000-0002-5741-7195",
"clpid": "Biswas-R"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-A"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274",
"clpid": "Nordin-J"
},
{
"family_name": "Nugent",
"given_name": "Peter",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-P-E"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"orcid": "0000-0002-1633-6495",
"clpid": "Polin-A"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Porter",
"given_name": "Michael",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-M-D"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "Colors of Type Ia supernovae (SNe Ia) in the first few days after explosion provide a potential discriminant between different models. In this paper, we present g \u2212 r colors of 65 SNe Ia discovered within 5 days from first light by the Zwicky Transient Facility in 2018, a sample that is about three times larger than that in the literature. We find that g \u2212 r colors are intrinsically rather homogeneous at early phases, with about half of the dispersion attributable to photometric uncertainties (\u03c3_(noise)\u223c\u03c3_(int) ~ 0.18 mag). Colors are nearly constant starting from 6 days after first light (g \u2212 r ~ \u22120.15 mag), while the time evolution at earlier epochs is characterized by a continuous range of slopes, from events rapidly transitioning from redder to bluer colors (slope of ~\u22120.25 mag day\u207b\u00b9) to events with a flatter evolution. The continuum in the slope distribution is in good agreement both with models requiring some amount of \u2075\u2076Ni mixed in the outermost regions of the ejecta and with \"double-detonation\" models having thin helium layers (M_(He) = 0.01 M_\u2299) and varying carbon\u2013oxygen core masses. At the same time, six events show evidence for a distinctive \"red bump\" signature predicted by double-detonation models with larger helium masses. We finally identify a significant correlation between the early-time g \u2212 r slopes and supernova brightness, with brighter events associated to flatter color evolution (p-value = 0.006). The distribution of slopes, however, is consistent with being drawn from a single population, with no evidence for two components as claimed in the literature based on B \u2212 V colors.",
"doi": "10.3847/1538-4357/abb13c",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-10-10",
"series_number": "1",
"volume": "902",
"issue": "1",
"pages": "Art. No. 48"
},
{
"id": "authors:jg4xn-yge96",
"collection": "authors",
"collection_id": "jg4xn-yge96",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200825-092934011",
"type": "article",
"title": "Helium-rich Superluminous Supernovae from the Zwicky Transient Facility",
"author": [
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Perley",
"given_name": "D.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Chen",
"given_name": "Z."
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Taggart",
"given_name": "K.",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Chen",
"given_name": "T. W.",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Cunningham",
"given_name": "V.",
"orcid": "0000-0003-2292-0441"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Duev",
"given_name": "D.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Fransson",
"given_name": "C.",
"orcid": "0000-0001-8532-3594"
},
{
"family_name": "Laher",
"given_name": "R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Hankins",
"given_name": "M.",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-M-J"
},
{
"family_name": "Ho",
"given_name": "A. Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Jencson",
"given_name": "J.",
"orcid": "0000-0001-5754-4007"
},
{
"family_name": "Kaye",
"given_name": "S.",
"clpid": "Kaye-S-M"
},
{
"family_name": "Kulkarni",
"given_name": "S.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kasliwal",
"given_name": "M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Golkhou",
"given_name": "V.",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "M.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "J.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Ofek",
"given_name": "E.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Porter",
"given_name": "M.",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-M-D"
},
{
"family_name": "Mr\u00f3z",
"given_name": "P.",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Reiley",
"given_name": "D.",
"clpid": "Reiley-D-J"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "M.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Smith",
"given_name": "R.",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Tartaglia",
"given_name": "L.",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Yao",
"given_name": "Y.",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Yaron",
"given_name": "O.",
"orcid": "0000-0002-0301-8017",
"clpid": "Yaron-O"
}
],
"abstract": "Helium is expected to be present in the massive ejecta of some hydrogen-poor superluminous supernovae (SLSN-I). However, until now only one event has been identified with He features in its photospheric spectra (PTF10hgi). We present the discovery of a new He-rich SLSN-I, ZTF19aawfbtg (SN2019hge), at z = 0.0866. This event has more than 10 optical spectra at phases from \u221241 to +103 days relative to the peak, most of which match well with that of PTF10hgi. Confirmation comes from a near-IR spectrum taken at +34 days, revealing He I features with P-Cygni profiles at 1.083 and 2.058 \u03bcm. Using the optical spectra of PTF10hgi and SN2019hge as templates, we examined 70 other SLSNe-I discovered by Zwicky Transient Facility in the first two years of operation and found five additional SLSNe-I with distinct He-features. The excitation of He I atoms in normal core-collapse supernovae requires nonthermal radiation, as proposed by previous studies. These He-rich events cannot be explained by the traditional \u2075\u2076Ni mixing model because of their blue spectra, high peak luminosities, and long rise timescales. Magnetar models offer a possible solution since pulsar winds naturally generate high-energy particles, potential sources of nonthermal excitation. An alternative model is the interaction between the ejecta and dense H-poor circumstellar material, which may be supported by observed undulations in the light curves. These six SLSNe-Ib have relatively low-peak luminosities (rest frame M_g = \u221220.06 \u00b1 0.16).",
"doi": "10.3847/2041-8213/abb8c5",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2020-10-10",
"series_number": "1",
"volume": "902",
"issue": "1",
"pages": "Art. No. L8"
},
{
"id": "authors:qch5f-v4q29",
"collection": "authors",
"collection_id": "qch5f-v4q29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151430667",
"type": "article",
"title": "SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart",
"author": [
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Corsi",
"given_name": "Alessandra",
"orcid": "0000-0001-8104-3536"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-A"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Frederiks",
"given_name": "Dmitry D.",
"orcid": "0000-0002-1153-6340"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-D-D-S"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Martikainen",
"given_name": "Julia",
"orcid": "0000-0003-2211-4001"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Ridnaia",
"given_name": "Anna"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Savchenko",
"given_name": "Volodymyr",
"orcid": "0000-0001-6353-0808"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Svinkin",
"given_name": "Dmitry S.",
"orcid": "0000-0002-2208-2196"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492",
"clpid": "Tartaglia-L"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Zolkower",
"given_name": "Jeffry",
"clpid": "Zolkower-J"
}
],
"abstract": "We present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN-20bs, ZTF 20aalxlis), a nearby (z = 0.0252; d = 114 Mpc) broad-line (BL) Type Ic supernova (SN) and the first double-peaked Ic-BL discovered without a gamma-ray burst (GRB) trigger. Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio luminosity (L_(radio) \u2248 10\u00b3\u2077 erg s\u207b\u00b9)is brighter than ordinary core-collapse SNe but fainter than LLGRB SNe such as SN 1998bw (associated with LLGRB 980425). We model our VLA observations (spanning 13\u201343 days) as synchrotron emission from a mildly relativistic (v \u2273 0.3c) forward shock. Second, with Swift and Chandra, we detect X-ray emission (L_X \u2248 10\u2074\u00b9 erg s\u207b\u00b9) that is not naturally explained as inverse Compton emission or part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6\u00d7 night\u207b\u00b9) data from the Zwicky Transient Facility (ZTF) show a double-peaked optical light curve, the first peak from shock cooling of extended low-mass material (mass M_e < 10\u207b\u00b2 M_\u2299 at radius R_e > 10\u00b9\u00b2 cm) and the second peak from the radioactive decay of \u2075\u2076Ni. SN 2020bvc is the first double-peaked Ic-BL SN discovered without a GRB trigger, so it is noteworthy that it shows X-ray and radio emission similar to LLGRB SNe. For four of the five other nearby (z \u227e 0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e., that lasts \u22481 day and reaches a peak luminosity M \u2248 \u221218. Follow-up X-ray and radio observations of Ic-BL SNe with well-sampled early optical light curves will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission.",
"doi": "10.3847/1538-4357/aba630",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-10-10",
"series_number": "1",
"volume": "902",
"issue": "1",
"pages": "Art. No. 86"
},
{
"id": "authors:dwg58-a2940",
"collection": "authors",
"collection_id": "dwg58-a2940",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200413-154440794",
"type": "article",
"title": "ZTF Early Observations of Type Ia Supernovae. II. First Light, the Initial Rise, and Time to Reach Maximum Brightness",
"author": [
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Yao",
"given_name": "Y.",
"clpid": "Yao-Y"
},
{
"family_name": "Bulla",
"given_name": "M.",
"orcid": "0000-0002-8255-5127",
"clpid": "Bulla-M"
},
{
"family_name": "Pankow",
"given_name": "C.",
"orcid": "0000-0002-1128-3662",
"clpid": "Pankow-C"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Cenko",
"given_name": "S. B.",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kupfer",
"given_name": "T.",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-P-E"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Smith",
"given_name": "R. M.",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "While it is clear that Type Ia supernovae (SNe) are the result of thermonuclear explosions in C/O white dwarfs (WDs), a great deal remains uncertain about the binary companion that facilitates the explosive disruption of the WD. Here, we present a comprehensive analysis of a large, unique data set of 127 SNe Ia with exquisite coverage by the Zwicky Transient Facility (ZTF). High-cadence (six observations per night) ZTF observations allow us to measure the SN rise time and examine its initial evolution. We develop a Bayesian framework to model the early rise as a power law in time, which enables the inclusion of priors in our model. For a volume-limited subset of normal SNe Ia, we find that the mean power-law index is consistent with 2 in the r_(ZTF)-band (\u03b1_r=2.01\u00b10.02), as expected in the expanding fireball model. There are, however, individual SNe that are clearly inconsistent with \u03b1_r = 2. We estimate a mean rise time of 18.9 days (with a range extending from ~15 to 22 days), though this is subject to the adopted prior. We identify an important, previously unknown, bias whereby the rise times for higher-redshift SNe within a flux-limited survey are systematically underestimated. This effect can be partially alleviated if the power-law index is fixed to \u03b1 = 2, in which case we estimate a mean rise time of 21.7 days (with a range from ~18 to 23 days). The sample includes a handful of rare and peculiar SNe Ia. Finally, we conclude with a discussion of lessons learned from the ZTF sample that can eventually be applied to observations from the Vera C. Rubin Observatory.",
"doi": "10.3847/1538-4357/abb13b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-10-10",
"series_number": "1",
"volume": "902",
"issue": "1",
"pages": "Art. No. 47"
},
{
"id": "authors:3tybt-bep85",
"collection": "authors",
"collection_id": "3tybt-bep85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151437761",
"type": "article",
"title": "SN2019dge: a Helium-rich Ultra-Stripped Envelope Supernova",
"author": [
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-S"
},
{
"family_name": "Li",
"given_name": "Zhihui",
"orcid": "0000-0001-5113-7558",
"clpid": "Li-Zhihui"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Fruchter",
"given_name": "Andrew",
"orcid": "0000-0002-6652-9279",
"clpid": "Fruchter-A-S"
},
{
"family_name": "Rubin",
"given_name": "David",
"orcid": "0000-0001-5402-4647",
"clpid": "Rubin-David"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-D-A"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Piro",
"given_name": "Anthony L.",
"orcid": "0000-0001-6806-0673",
"clpid": "Piro-A-L"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Burruss",
"given_name": "Rick",
"clpid": "Burruss-R-S"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Zolkower",
"given_name": "Jeffry",
"clpid": "Zolkower-J"
}
],
"abstract": "We present observations of ZTF18abfcmjw (SN2019dge), a helium-rich supernova with a fast-evolving light curve indicating an extremely low ejecta mass (\u22480.33 M_\u2299) and low kinetic energy (\u22481.3 \u00d7 10\u2075\u2070 erg). Early-time (<4 days after explosion) photometry reveals evidence of shock cooling from an extended helium-rich envelope of ~0.1 M_\u2299 located ~1.2 \u00d7 10\u00b9\u00b3 cm from the progenitor. Early-time He II line emission and subsequent spectra show signatures of interaction with helium-rich circumstellar material, which extends from \u2273 5 \u00d7 10\u00b9\u00b3 cm to 2 \u00d7 10\u00b9\u2076 cm. We interpret SN2019dge as a helium-rich supernova from an ultra-stripped progenitor, which originates from a close binary system consisting of a mass-losing helium star and a low-mass main-sequence star or a compact object (i.e., a white dwarf, a neutron star, or a black hole). We infer that the local volumetric birth rate of 19dge-like ultra-stripped SNe is in the range of 1400\u20138200 Gpc\u207b\u00b3 yr\u207b\u00b9 (i.e., 2%\u201312% of core-collapse supernova rate). This can be compared to the observed coalescence rate of compact neutron star binaries that are not formed by dynamical capture.",
"doi": "10.3847/1538-4357/abaa3d",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-09-01",
"series_number": "1",
"volume": "900",
"issue": "1",
"pages": "Art. No. 46"
},
{
"id": "authors:sg3a4-64g26",
"collection": "authors",
"collection_id": "sg3a4-64g26",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200310-124512129",
"type": "article",
"title": "Early Ultraviolet Observations of Type IIn Supernovae Constrain the Asphericity of Their Circumstellar Material",
"author": [
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Liang",
"given_name": "Jingyi"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Nugent",
"given_name": "Peter",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Yang",
"given_name": "Yi"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"orcid": "0000-0001-7344-0208",
"clpid": "Dugas-A-M"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Hankins",
"given_name": "Matthew J.",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-M-J"
},
{
"family_name": "Strotjohann",
"given_name": "Nora Linn",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Moran",
"given_name": "Shane",
"orcid": "0000-0001-5221-0243"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sip\u0151cz",
"given_name": "Brigitta M.",
"orcid": "0000-0002-3713-6337"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Yaron",
"given_name": "Ofer",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Cannella",
"given_name": "Chris",
"orcid": "0000-0003-2667-7290"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kowalski",
"given_name": "Marek"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
}
],
"abstract": "We present a survey of the early evolution of 12 Type IIn supernovae (SNe IIn) at ultraviolet and visible light wavelengths. We use this survey to constrain the geometry of the circumstellar material (CSM) surrounding SN IIn explosions, which may shed light on their progenitor diversity. In order to distinguish between aspherical and spherical CSM, we estimate the blackbody radius temporal evolution of the SNe IIn of our sample, following the method introduced by Soumagnac et al. We find that higher-luminosity objects tend to show evidence for aspherical CSM. Depending on whether this correlation is due to physical reasons or to some selection bias, we derive a lower limit between 35% and 66% for the fraction of SNe IIn showing evidence for aspherical CSM. This result suggests that asphericity of the CSM surrounding SNe IIn is common\u2014consistent with data from resolved images of stars undergoing considerable mass loss. It should be taken into account for more realistic modeling of these events.",
"doi": "10.3847/1538-4357/ab94be",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-08-10",
"series_number": "1",
"volume": "899",
"issue": "1",
"pages": "Art. No. 51"
},
{
"id": "authors:3m8ct-c8w52",
"collection": "authors",
"collection_id": "3m8ct-c8w52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151434093",
"type": "article",
"title": "The Spectacular Ultraviolet Flash from the Peculiar Type Ia Supernova 2019yvq",
"author": [
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Magee",
"given_name": "M. R.",
"orcid": "0000-0002-0629-8931"
},
{
"family_name": "Polin",
"given_name": "A.",
"orcid": "0000-0002-1633-6495"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Zimmerman",
"given_name": "E.",
"orcid": "0000-0001-8985-2493"
},
{
"family_name": "Yao",
"given_name": "Y.",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Kromer",
"given_name": "M.",
"orcid": "0000-0003-4380-7536"
},
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979",
"clpid": "Dhawan-S"
},
{
"family_name": "Bulla",
"given_name": "M.",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Delacroix",
"given_name": "A.",
"clpid": "Delacroix-A"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Goldstein",
"given_name": "D. A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Z.",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Irani",
"given_name": "I.",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kaye",
"given_name": "S.",
"clpid": "Kaye-S-M"
},
{
"family_name": "Kim",
"given_name": "Y. -L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Ofek",
"given_name": "E.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-E-O"
},
{
"family_name": "Phinney",
"given_name": "E. S.",
"orcid": "0000-0002-9656-4032",
"clpid": "Phinney-E-S"
},
{
"family_name": "Prentice",
"given_name": "S. J.",
"orcid": "0000-0003-0486-6242"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Schweyer",
"given_name": "T."
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "M. T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Terreran",
"given_name": "G.",
"orcid": "0000-0003-0794-5982",
"clpid": "Terreran-G"
},
{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Zolkower",
"given_name": "J.",
"clpid": "Zolkower-J"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "Early observations of Type Ia supernovae (SNe Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN 2019yvq, the second observed SN Ia, after iPTF 14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN 2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for an SN Ia (M_g ~ -18.5 mag at peak) yet featured very high absorption velocities (v ~ 15,000 km s\u207b\u00b9 for Si ii \u03bb6355 at peak). We find that many of the observational features of SN 2019yvq, aside from the flash, can be explained if the explosive yield of radioactive \u2075\u2076Ni is relatively low (we measure M\u2085\u2086_(Ni) = 0.31 \u00b1 0.05 M_\u2299 and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN 2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of \u2075\u2076Ni in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations; it is clear additional tuning is required to better match SN 2019yvq. In closing, we predict that the nebular spectra of SN 2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca ii] emission, if it was a double detonation, or narrow [O i] emission, if it was due to a violent merger.",
"doi": "10.3847/1538-4357/ab9e05",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-07-20",
"series_number": "1",
"volume": "898",
"issue": "1",
"pages": "Art. No. 56"
},
{
"id": "authors:c0m6b-epf70",
"collection": "authors",
"collection_id": "c0m6b-epf70",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200724-100653916",
"type": "article",
"title": "A New Class of Roche Lobe\u2013filling Hot Subdwarf Binaries",
"author": [
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Bauer",
"given_name": "Evan B.",
"orcid": "0000-0002-4791-6724"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Hermes",
"given_name": "JJ",
"orcid": "0000-0001-5941-2286"
},
{
"family_name": "Marsh",
"given_name": "Thomas R.",
"orcid": "0000-0002-2498-7589"
},
{
"family_name": "Bildsten",
"given_name": "Lars"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Phinney",
"given_name": "E. S.",
"orcid": "0000-0002-9656-4032",
"clpid": "Phinney-E-S"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"orcid": "0000-0003-4373-7777"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Irrgang",
"given_name": "Andreas",
"orcid": "0000-0002-0465-3725"
},
{
"family_name": "Heber",
"given_name": "Ulrich",
"orcid": "0000-0001-7798-6769"
},
{
"family_name": "Schneider",
"given_name": "David"
},
{
"family_name": "Dhillon",
"given_name": "Vik S.",
"orcid": "0000-0003-4236-9642"
},
{
"family_name": "Murawski",
"given_name": "Gabriel",
"orcid": "0000-0001-7809-1457"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-A-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Littlefair",
"given_name": "S. P.",
"orcid": "0000-0001-7221-855X"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Porter",
"given_name": "Michael",
"clpid": "Porter-M"
},
{
"family_name": "Reiley",
"given_name": "Dan",
"clpid": "Reiley-D-J"
},
{
"family_name": "Rodriguez",
"given_name": "Hector",
"clpid": "Rodriguez-Hector"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
}
],
"abstract": "We present the discovery of the second binary with a Roche lobe\u2013filling hot subdwarf transferring mass to a white dwarf (WD) companion. This 56 minute binary was discovered using data from the Zwicky Transient Facility. Spectroscopic observations reveal an He-sdOB star with an effective temperature of T_(eff) = 33,700 \u00b1 1000 K and a surface gravity of log(g) = 5.54 \u00b1 0.11. The GTC+HiPERCAM light curve is dominated by the ellipsoidal deformation of the He-sdOB star and shows an eclipse of the He-sdOB by an accretion disk as well as a weak eclipse of the WD. We infer a He-sdOB mass of M_(sdOB) = 0.41 \u00b1 0.04 M_\u2299 and a WD mass of M WD = 0.68 \u00b1 0.05 M_\u2299. The weak eclipses imply a WD blackbody temperature of 63,000 \u00b1 10,000 K and a radius R_(WD) = 0.0148 \u00b1 0.0020 R_\u2299 as expected for a WD of such high temperature. The He-sdOB star is likely undergoing hydrogen shell burning and will continue transferring mass for \u22481 Myr at a rate of 10\u207b\u2079 M_\u2299 yr\u207b\u00b9, which is consistent with the high WD temperature. The hot subdwarf will then turn into a WD and the system will merge in \u224830 Myr. We suggest that Galactic reddening could bias discoveries toward preferentially finding Roche lobe\u2013filling systems during the short-lived shell-burning phase. Studies using reddening-corrected samples should reveal a large population of helium core\u2013burning hot subdwarfs with T_(eff) \u2248 25,000 K in binaries of 60\u201390 minutes with WDs. Though not yet in contact, these binaries would eventually come into contact through gravitational-wave emission and explode as a subluminous thermonuclear supernova or evolve into a massive single WD.",
"doi": "10.3847/2041-8213/aba3c2",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2020-07-20",
"series_number": "1",
"volume": "898",
"issue": "1",
"pages": "Art. No. L25"
},
{
"id": "authors:dcp0r-yy108",
"collection": "authors",
"collection_id": "dcp0r-yy108",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190802-105703823",
"type": "article",
"title": "Synthetic Tracking Using ZTF Deep Drilling Data Sets",
"author": [
{
"family_name": "Zhai",
"given_name": "Chengxing",
"orcid": "0000-0002-0291-4522",
"clpid": "Zhai-Chengxing"
},
{
"family_name": "Ye",
"given_name": "Quanzhi",
"orcid": "0000-0002-4838-7676",
"clpid": "Ye-Quanzhi"
},
{
"family_name": "Shao",
"given_name": "Michael",
"clpid": "Shao-Michael"
},
{
"family_name": "Trahan",
"given_name": "Russell",
"clpid": "Trahan-R"
},
{
"family_name": "Saini",
"given_name": "Navtej S.",
"clpid": "Saini-N-S"
},
{
"family_name": "Shen",
"given_name": "Janice",
"clpid": "Shen-Janice"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"clpid": "Rosnet-P"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "The Zwicky Transit Facility (ZTF) is a powerful time domain survey telescope with a large field of view of 47 deg\u00b2. We apply the synthetic tracking technique to integrate a ZTF's deep drilling data set, which consists of 133 nominal 30 s exposure frames spanning about 1.5 hr, to search for slowly moving asteroids down to approximately 23rd magnitude. We found 1168 objects from searching 40 of the 64 CCD-quadrant subfields, each of which covers a field size of about 0.73 deg\u00b2. While most of the objects are in the core region of the asteroid belt, there are asteroids belonging to families of Trojan, Hilda, Hungaria, Phocaea, and near-Earth-asteroids. Such an approach is effective and productive for discovering new asteroids. Here we report the data processing and results as well as discuss a potential deep drilling operation mode using this approach for survey facilities.",
"doi": "10.1088/1538-3873/ab828b",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2020-06",
"series_number": "1012",
"volume": "132",
"issue": "1012",
"pages": "Art. No. 064502"
},
{
"id": "authors:03s09-e9y28",
"collection": "authors",
"collection_id": "03s09-e9y28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191120-152035670",
"type": "article",
"title": "The Zwicky Transient Facility Bright Transient Survey I: Spectroscopic Classification and the Redshift Completeness of Local Galaxy Catalogs",
"author": [
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"clpid": "Sharma-Y"
},
{
"family_name": "Dugas",
"given_name": "A.",
"clpid": "Dugas-A-M"
},
{
"family_name": "Perley",
"given_name": "D. A."
},
{
"family_name": "Taggart",
"given_name": "K."
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Graham",
"given_name": "M. L."
},
{
"family_name": "Neill",
"given_name": "J. D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Nordin",
"given_name": "J."
},
{
"family_name": "Rigault",
"given_name": "M."
},
{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Bagdasaryan",
"given_name": "A.",
"clpid": "Bagdasaryan-A"
},
{
"family_name": "Belicki",
"given_name": "J.",
"clpid": "Belicki-J"
},
{
"family_name": "Cannella",
"given_name": "C."
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Cenko",
"given_name": "S. B.",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "R.",
"clpid": "Dekany-Richard"
},
{
"family_name": "Frederick",
"given_name": "S."
},
{
"family_name": "Golkhou",
"given_name": "V. Z."
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ho",
"given_name": "A. Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kupfer",
"given_name": "T.",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Schulze",
"given_name": "S."
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "R. M.",
"clpid": "Smith-R-M"
},
{
"family_name": "van Velzen",
"given_name": "S.",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-S"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Y.",
"clpid": "Yao-Y"
},
{
"family_name": "Zhuang",
"given_name": "Z.",
"clpid": "Zhuang-Z"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "The Zwicky Transient Facility (ZTF) is performing a three-day cadence survey of the visible northern sky (~3\u03c0) with newly found transient candidates announced via public alerts. The ZTF Bright Transient Survey (BTS) is a large spectroscopic campaign to complement the photometric survey. BTS endeavors to spectroscopically classify all extragalactic transients with m_(peak) \u2264 18.5 mag in either the g_(ZTF) or r_(ZTF) filters, and publicly announce said classifications. BTS discoveries are predominantly supernovae (SNe), making this the largest flux-limited SN survey to date. Here we present a catalog of 761 SNe, classified during the first nine months of ZTF (2018 April 1\u20132018 December 31). We report BTS SN redshifts from SN template matching and spectroscopic host-galaxy redshifts when available. We analyze the redshift completeness of local galaxy catalogs, the redshift completeness fraction (RCF; the ratio of SN host galaxies with known spectroscopic redshift prior to SN discovery to the total number of SN hosts). Of the 512 host galaxies with SNe Ia, 227 had previously known spectroscopic redshifts, yielding an RCF estimate of 44% \u00b1 4%. The RCF decreases with increasing distance and decreasing galaxy luminosity (for z < 0.05, or ~200 Mpc, RCF \u2248 0.6). Prospects for dramatically increasing the RCF are limited to new multifiber spectroscopic instruments or wide-field narrowband surveys. Existing galaxy redshift catalogs are only ~50% complete at r \u2248 16.9 mag. Pushing this limit several magnitudes deeper will pay huge dividends when searching for electromagnetic counterparts to gravitational wave events or sources of ultra-high-energy cosmic rays or neutrinos.",
"doi": "10.3847/1538-4357/ab8943",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-05-20",
"series_number": "1",
"volume": "895",
"issue": "1",
"pages": "Art. No. 32"
},
{
"id": "authors:k73kj-b3s87",
"collection": "authors",
"collection_id": "k73kj-b3s87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200309-115301856",
"type": "article",
"title": "The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at z = 0.27",
"author": [
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-D-A"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Dong",
"given_name": "Dillon Z. J.",
"clpid": "Dong-Dillon-Z-J"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Chandra",
"given_name": "Poonam",
"orcid": "0000-0002-0844-6563",
"clpid": "Chandra-P"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Coughlin",
"given_name": "Michael",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Fredericks",
"given_name": "Dmitry D.",
"orcid": "0000-0002-1153-6340",
"clpid": "Fredericks-D-D"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-D-D-S"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Horesh",
"given_name": "Assaf",
"orcid": "0000-0002-5936-1156",
"clpid": "Horesh-A"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Porter",
"given_name": "Michael",
"clpid": "Porter-M"
},
{
"family_name": "Ridnaia",
"given_name": "Anna",
"clpid": "Ridnaia-A"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Svinkin",
"given_name": "Dmitry S.",
"orcid": "0000-0002-2208-2196",
"clpid": "Svinkin-D-S"
}
],
"abstract": "We present ZTF18abvkwla (the \"Koala\"), a fast blue optical transient discovered in the Zwicky Transient Facility (ZTF) One-Day Cadence (1DC) Survey. ZTF18abvkwla has a number of features in common with the groundbreaking transient AT 2018cow: blue colors at peak (g \u2013 r \u2248 \u22120.5 mag), a short rise time from half-max of under two days, a decay time to half-max of only three days, a high optical luminosity (M_(g,peak) \u2248 \u221220.6 mag), a hot (\u227340,000 K) featureless spectrum at peak light, and a luminous radio counterpart. At late times (\u0394t > 80 days), the radio luminosity of ZTF18abvkwla (\u03bd_(L\u03bd) \u2273 10\u2074\u2070 erg\u207b\u00b9 at 10 GHz, observer-frame) is most similar to that of long-duration gamma-ray bursts (GRBs). The host galaxy is a dwarf starburst galaxy (M \u2248 5\u00d710\u2078 M\u2299, SFR \u2248 7 M\u2299 yr\u207b\u00b9) that is moderately metal-enriched (log[O/H] \u2248 8.5), similar to the hosts of GRBs and superluminous supernovae. As in AT2018cow, the radio and optical emission in ZTF18abvkwla likely arise from two separate components: the radio from fast-moving ejecta (\u0393\u03b2c > 0.38c) and the optical from shock-interaction with confined dense material (<0.07 M\u2299 in \u223c10\u00b9\u2075 cm). Compiling transients in the literature with t_(rise) < 5 days and M_(peak) < \u221220 mag, we find that a significant number are engine-powered, and suggest that the high peak optical luminosity is directly related to the presence of this engine. From 18 months of the 1DC survey, we find that transients in this rise-luminosity phase space are at least two to three orders of magnitude less common than CC SNe. Finally, we discuss strategies for identifying such events with future facilities like the Large Synoptic Survey Telescope, as well as prospects for detecting accompanying X-ray and radio emission.",
"doi": "10.3847/1538-4357/ab8bcf",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-05-20",
"series_number": "1",
"volume": "895",
"issue": "1",
"pages": "Art. No. 49"
},
{
"id": "authors:1yygm-shr42",
"collection": "authors",
"collection_id": "1yygm-shr42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200414-080500283",
"type": "article",
"title": "The Broad-lined Ic Supernova ZTF18aaqjovh (SN 2018bvw): An Optically-discovered Engine-driven Supernova Candidate with Luminous Radio Emission",
"author": [
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Corsi",
"given_name": "Alessandra",
"orcid": "0000-0001-8104-3536",
"clpid": "Corsi-A"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Taddia",
"given_name": "Francesco",
"orcid": "0000-0002-2387-6801",
"clpid": "Taddia-F"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Adams",
"given_name": "Scott",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Frederiks",
"given_name": "Dmitry D.",
"clpid": "Frederiks-D-D"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889",
"clpid": "Hung-Tiara"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Reiley",
"given_name": "Daniel",
"clpid": "Reiley-D-J"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Ridnaia",
"given_name": "Anna",
"clpid": "Ridnaia-A"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"clpid": "Sharma-Y"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Svinkin",
"given_name": "Dmitry S.",
"clpid": "Svinkin-D-S"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "We present ZTF18aaqjovh (SN 2018bvw), a high-velocity (\"broad-lined\") stripped-envelope (Type Ic) supernova (Ic-BL SN) discovered in the Zwicky Transient Facility one-day cadence survey. ZTF18aaqjovh shares a number of features in common with engine-driven explosions: the photospheric velocity and the shape of the optical light curve are very similar to those of the Type Ic-BL SN 1998bw, which was associated with a low-luminosity gamma-ray burst (LLGRB) and had relativistic ejecta. However, the radio luminosity of ZTF18aaqjovh is almost two orders of magnitude fainter than that of SN 1998bw at the same velocity phase, and the shock velocity is at most mildly relativistic (v = 0.06\u20130.4c). A search of high-energy catalogs reveals no compelling gamma-ray burst (GRB) counterpart to ZTF18aaqjovh, and the limit on the prompt GRB luminosity of L_(\u03b3,iso)\u22481.6\u00d710\u2074\u2078 erg/s\u207b\u00b9 excludes a classical GRB but not an LLGRB. Altogether, ZTF18aaqjovh represents another transition event between engine-driven SNe associated with GRBs and \"ordinary\" Ic-BL SNe.",
"doi": "10.3847/1538-4357/ab7f3b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-04-20",
"series_number": "2",
"volume": "893",
"issue": "2",
"pages": "Art. No. 132"
},
{
"id": "authors:4drc8-74a83",
"collection": "authors",
"collection_id": "4drc8-74a83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200304-082758333",
"type": "article",
"title": "First Ultracompact Roche Lobe\u2013Filling Hot Subdwarf Binary",
"author": [
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Bauer",
"given_name": "Evan B.",
"orcid": "0000-0002-4791-6724"
},
{
"family_name": "Marsh",
"given_name": "Thomas R.",
"orcid": "0000-0002-2498-7589"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Hermes",
"given_name": "JJ",
"orcid": "0000-0001-5941-2286"
},
{
"family_name": "Bildsten",
"given_name": "Lars"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"orcid": "0000-0003-4373-7777"
},
{
"family_name": "Dhillon",
"given_name": "Vik S.",
"orcid": "0000-0003-4236-9642"
},
{
"family_name": "Murawski",
"given_name": "Gabriel",
"orcid": "0000-0001-7809-1457"
},
{
"family_name": "Burruss",
"given_name": "Rick",
"clpid": "Burruss-R-S"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Delacroix",
"given_name": "Alex",
"clpid": "Delacroix-A"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-A-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Littlefair",
"given_name": "S. P.",
"orcid": "0000-0001-7221-855X"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Smith",
"given_name": "Roger M.",
"clpid": "Smith-R-M"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
}
],
"abstract": "We report the discovery of the first short-period binary in which a hot subdwarf star (sdOB) filled its Roche lobe and started mass transfer to its companion. The object was discovered as part of a dedicated high-cadence survey of the Galactic plane named the Zwicky Transient Facility and exhibits a period of P = 39.3401(1) minutes, making it the most compact hot subdwarf binary currently known. Spectroscopic observations are consistent with an intermediate He-sdOB star with an effective temperature of T_(eff) = 42,400 \u00b1 300 K and a surface gravity of log(g) = 5.77 \u00b1 0.05. A high signal-to-noise ratio GTC+HiPERCAM light curve is dominated by the ellipsoidal deformation of the sdOB star and an eclipse of the sdOB by an accretion disk. We infer a low-mass hot subdwarf donor with a mass M_(sdOB) = 0.337 \u00b1 0.015 M\u2299 and a white dwarf accretor with a mass M_(WD) = 0.545 \u00b1 0.020 M\u2299. Theoretical binary modeling indicates the hot subdwarf formed during a common envelope phase when a 2.5\u20132.8 M\u2299 star lost its envelope when crossing the Hertzsprung gap. To match its current P_(orb), T_(eff), log(g), and masses, we estimate a post\u2013common envelope period of P_(orb) \u2248 150 minutes and find that the sdOB star is currently undergoing hydrogen shell burning. We estimate that the hot subdwarf will become a white dwarf with a thick helium layer of \u22480.1 M\u2299, merge with its carbon/oxygen white dwarf companion after \u224817 Myr, and presumably explode as a thermonuclear supernova or form an R CrB star.",
"doi": "10.3847/1538-4357/ab72ff",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-03-01",
"series_number": "1",
"volume": "891",
"issue": "1",
"pages": "Art. No. 45"
},
{
"id": "authors:dmsmn-dgj43",
"collection": "authors",
"collection_id": "dmsmn-dgj43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191002-100608633",
"type": "article",
"title": "Evidence for Late-stage Eruptive Mass Loss in the Progenitor to SN2018gep, a Broad-lined Ic Supernova: Pre-explosion Emission and a Rapidly Rising Luminous Transient",
"author": [
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-S"
},
{
"family_name": "Khatami",
"given_name": "David K.",
"orcid": "0000-0003-4307-0589",
"clpid": "Khatami-D-K"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-D-A"
},
{
"family_name": "Ergon",
"given_name": "Mattias",
"clpid": "Ergon-M"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-A"
},
{
"family_name": "Corsi",
"given_name": "Alessandra",
"orcid": "0000-0001-8104-3536",
"clpid": "Corsi-A"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144",
"clpid": "Barbarino-C"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadia",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Bright",
"given_name": "Joe S.",
"orcid": "0000-0002-7735-5796",
"clpid": "Bright-J-S"
},
{
"family_name": "Burns",
"given_name": "E.",
"clpid": "Burns-E"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Cunningham",
"given_name": "Virginia",
"orcid": "0000-0003-2292-0441",
"clpid": "Cunningham-V"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"clpid": "Dugas-A-M"
},
{
"family_name": "Fender",
"given_name": "Rob P.",
"clpid": "Fender-R-P"
},
{
"family_name": "Fransson",
"given_name": "Claes",
"orcid": "0000-0001-8532-3594",
"clpid": "Fransson-C"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Goldstein",
"given_name": "Adam",
"orcid": "0000-0002-0587-7042",
"clpid": "Goldstein-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-D-D-S"
},
{
"family_name": "Horesh",
"given_name": "Assaf",
"orcid": "0000-0002-5936-1156",
"clpid": "Horesh-A"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889",
"clpid": "Hung-Tiara"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kuin",
"given_name": "N. Paul M.",
"orcid": "0000-0003-4650-4186",
"clpid": "Kuin-N-P-M"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554",
"clpid": "Ngeow-Chow-Choong"
},
{
"family_name": "Nugent",
"given_name": "Peter E.",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-P-E"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-E-O"
},
{
"family_name": "Patterson",
"given_name": "Maria T.",
"orcid": "0000-0002-4753-3387",
"clpid": "Patterson-M-T"
},
{
"family_name": "Petitpas",
"given_name": "Glen",
"clpid": "Petitpas-G"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Sai",
"given_name": "Hanna",
"clpid": "Sai-Hanna"
},
{
"family_name": "Sfaradi",
"given_name": "Itai",
"clpid": "Sfaradi-I"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Tachibana",
"given_name": "Yutaro",
"orcid": "0000-0001-6584-6945",
"clpid": "Tachibana-Yutaro"
},
{
"family_name": "Taddia",
"given_name": "Francesco",
"orcid": "0000-0002-2387-6801",
"clpid": "Taddia-F"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Wang",
"given_name": "Xiaofeng",
"orcid": "0000-0002-7334-2357",
"clpid": "Wang-Xiaofeng"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Zhang",
"given_name": "Xinhan",
"clpid": "Zhang-Xinhan"
}
],
"abstract": "We present detailed observations of ZTF18abukavn (SN2018gep), discovered in high-cadence data from the Zwicky Transient Facility as a rapidly rising (1.4 \u00b1 0.1 mag/hr) and luminous (M_(g,peak) = \u221220 mag) transient. It is spectroscopically classified as a broad-lined stripped-envelope supernova (Ic-BL SN). The high peak luminosity (L_(bol) \u2273 3\u00d710^(44) erg sec^(\u22121)), the short rise time (t_(rise) = 3 days in g-band), and the blue colors at peak (g\u2212r \u223c \u22120.4) all resemble the high-redshift Ic-BL iPTF16asu, as well as several other unclassified fast transients. The early discovery of SN2018gep (within an hour of shock breakout) enabled an intensive spectroscopic campaign, including the highest-temperature (T_(eff) \u2273 40,000 K) spectra of a stripped-envelope SN. A retrospective search revealed luminous (M_g \u223c M_r \u2248 \u221214mag) emission in the days to weeks before explosion, the first definitive detection of precursor emission for a Ic-BL. We find a limit on the isotropic gamma-ray energy release E_(\u03b3,iso) < 4.9\u00d710^(48) erg, a limit on X-ray emission L_X < 10^(40) erg sec^(\u22121), and a limit on radio emission \u03bdL_\u03bd \u2272 10^(37) erg sec^(\u22121). Taken together, we find that the early (< 10 days) data are best explained by shock breakout in a massive shell of dense circumstellar material (0.02 M_\u2299) at large radii (3\u00d710^(14)cm) that was ejected in eruptive pre-explosion mass-loss episodes. The late-time (>10 days) light curve requires an additional energy source, which could be the radioactive decay of Ni-56.",
"doi": "10.3847/1538-4357/ab55ec",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-12-20",
"series_number": "2",
"volume": "887",
"issue": "2",
"pages": "Art. No. 169"
},
{
"id": "authors:wcpgk-vfa98",
"collection": "authors",
"collection_id": "wcpgk-vfa98",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191120-154458675",
"type": "article",
"title": "ZTF Early Observations of Type Ia Supernovae I: Properties of the 2018 Sample",
"author": [
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Miller",
"given_name": "Adam A."
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Bulla",
"given_name": "Mattia"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Nugent",
"given_name": "Peter",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"clpid": "Dugas-A-M"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadia",
"orcid": "0000-0003-0901-1606"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Rigault",
"given_name": "Michael"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Nordin",
"given_name": "J."
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dhawan",
"given_name": "Suhail"
},
{
"family_name": "Feindt",
"given_name": "Ulrich",
"orcid": "0000-0002-9435-2167"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Hung",
"given_name": "T."
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Taggart",
"given_name": "K."
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "Early-time observations of Type Ia supernovae (SNe Ia) are essential to constrain the properties of their progenitors. In this paper, we present high-quality light curves of 127 SNe Ia discovered by the Zwicky Transient Facility (ZTF) in 2018. We describe our method to perform forced point-spread function photometry, which can be applied to other types of extragalactic transients. With a planned cadence of six observations per night (three g + three r), all of the 127 SNe Ia are detected in both g and r bands more than 10 days (in the rest frame) prior to the epoch of g-band maximum light. The redshifts of these objects range from z = 0.0181 to 0.165; the median redshift is 0.074. Among the 127 SNe, 50 are detected at least 14 days prior to maximum light (in the rest frame), with a subset of nine objects being detected more than 17 days before g-band peak. This is the largest sample of young SNe Ia collected to date; it can be used to study the shape and color evolution of the rising light curves in unprecedented detail. We discuss six peculiar events in this sample: one 02cx-like event ZTF18abclfee (SN 2018crl), one Ia-CSM SN ZTF18aaykjei (SN 2018cxk), and four objects with possible super-Chandrasekhar mass progenitors: ZTF18abhpgje (SN 2018eul), ZTF18abdpvnd (SN 2018dvf), ZTF18aawpcel (SN 2018cir), and ZTF18abddmrf (SN 2018dsx).",
"doi": "10.3847/1538-4357/ab4cf5",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-12-01",
"series_number": "2",
"volume": "886",
"issue": "2",
"pages": "Art. No. 152"
},
{
"id": "authors:45n07-53r39",
"collection": "authors",
"collection_id": "45n07-53r39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191118-120700599",
"type": "article",
"title": "Comet 240P/NEAT Is Stirring",
"author": [
{
"family_name": "Kelley",
"given_name": "Michael S. P.",
"orcid": "0000-0002-6702-7676",
"clpid": "Kelley-Michael-S-P"
},
{
"family_name": "Bodewits",
"given_name": "Dennis",
"orcid": "0000-0002-2668-7248",
"clpid": "Bodewits-Dennis"
},
{
"family_name": "Ye",
"given_name": "Quanzhi",
"orcid": "0000-0002-4838-7676",
"clpid": "Ye-Quanzhi"
},
{
"family_name": "Farnham",
"given_name": "Tony L.",
"orcid": "0000-0002-4767-9861",
"clpid": "Farnham-Tony-L"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-Maayane-T"
},
{
"family_name": "Zolkower",
"given_name": "Jeffry",
"clpid": "Zolkower-Jeffry-N"
}
],
"abstract": "Comets are primitive objects that formed in the protoplanetary disk, and have been largely preserved over the history of the solar system. However, they are not pristine, and surfaces of cometary nuclei do evolve. In order to understand the extent of their primitive nature, we must define the mechanisms that affect their surfaces and comae. We examine the lightcurve of comet 240P/NEAT over three consecutive orbits, and investigate three events of significant brightening (\u0394m ~ \u22122 mag). Unlike typical cometary outbursts, each of the three events are long-lived, with enhanced activity for at least 3\u20136 months. The third event, observed by the Zwicky Transient Facility, occurred in at least two stages. The anomalous behavior appears to have started after the comet was perturbed by Jupiter in 2007, reducing its perihelion distance from 2.53 to 2.12 au. We suggest that the brightening events are temporary transitions to a higher baseline activity level, brought on by the increased insolation, which has warmed previously insulated sub-surface layers. The new activity is isolated to one or two locations on the nucleus, indicating that the surface or immediate sub-surface is heterogeneous. Further study of this phenomenon may provide insight into cometary outbursts, the structure of the near-surface nucleus, and cometary nucleus mantling.",
"doi": "10.3847/2041-8213/ab53e0",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-11-20",
"series_number": "1",
"volume": "886",
"issue": "1",
"pages": "Art. No. L16"
},
{
"id": "authors:bbnt6-sag19",
"collection": "authors",
"collection_id": "bbnt6-sag19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190802-094555948",
"type": "article",
"title": "GROWTH on S190425z: Searching Thousands of Square Degrees to Identify an Optical or Infrared Counterpart to a Binary Neutron Star Merger with the Zwicky Transient Facility and Palomar Gattini-IR",
"author": [
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-T"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Hankins",
"given_name": "Matthew J.",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-L-P"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Cooke",
"given_name": "Jeff",
"orcid": "0000-0001-5703-2108",
"clpid": "Cooke-J"
},
{
"family_name": "Copperwheat",
"given_name": "Christopher M.",
"orcid": "0000-0001-7983-8698",
"clpid": "Copperwheat-C-M"
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{
"family_name": "Dugas",
"given_name": "Alison M.",
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},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-J-E"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-D-A"
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{
"family_name": "Yu",
"given_name": "Po-Chieh",
"orcid": "0000-0001-8894-0854",
"clpid": "Yu-Po-Chieh"
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{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609",
"clpid": "Bhalerao-V-B"
},
{
"family_name": "Kumar",
"given_name": "Harsh",
"clpid": "Kumar-Harsh"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X",
"clpid": "Bloom-J-S"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
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},
{
"family_name": "Ashley",
"given_name": "Michael C. B.",
"orcid": "0000-0003-1412-2028",
"clpid": "Ashley-M-C-B"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-A"
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{
"family_name": "Biswas",
"given_name": "Rahul",
"orcid": "0000-0002-5741-7195",
"clpid": "Biswas-R"
},
{
"family_name": "Buckley",
"given_name": "David A. H.",
"orcid": "0000-0002-7004-9956",
"clpid": "Buckley-D-A-H"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-D-O"
},
{
"family_name": "Cromer",
"given_name": "John",
"clpid": "Cromer-J-L"
},
{
"family_name": "Cunningham",
"given_name": "Virginia",
"orcid": "0000-0003-2292-0441",
"clpid": "Cunningham-V"
},
{
"family_name": "D'A\u00ec",
"given_name": "Antonino",
"orcid": "0000-0002-5042-1036",
"clpid": "D'A\u00ec-Antonio"
},
{
"family_name": "Dekany",
"given_name": "Richard G.",
"clpid": "Dekany-Richard"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-A"
},
{
"family_name": "Dichiara",
"given_name": "Simone",
"clpid": "Dichiara-S"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Dutta",
"given_name": "Anirban",
"clpid": "Dutta-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X",
"clpid": "Frederick-S"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Ghosh",
"given_name": "Shaon",
"orcid": "0000-0001-9901-6253",
"clpid": "Ghosh-Shaon"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hanayama",
"given_name": "Hidekazu",
"orcid": "0000-0001-8221-6048",
"clpid": "Hanayama-Hidekazu"
},
{
"family_name": "Horiuchi",
"given_name": "Takashi",
"clpid": "Horiuchi-Takashi"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889",
"clpid": "Hung-Tiara"
},
{
"family_name": "Jha",
"given_name": "Saurabh W.",
"orcid": "0000-0001-8738-6011",
"clpid": "Jha-S-W"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X",
"clpid": "Kong-Albert-K-H"
},
{
"family_name": "Giomi",
"given_name": "Matteo",
"clpid": "Giomi-M"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-D-L"
},
{
"family_name": "Karambelkar",
"given_name": "V. R.",
"clpid": "Karambelkar-V-R"
},
{
"family_name": "Kowalski",
"given_name": "Marek",
"clpid": "Kowalski-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Mazzali",
"given_name": "Paolo",
"orcid": "0000-0001-6876-8284",
"clpid": "Mazzali-P-A"
},
{
"family_name": "Moore",
"given_name": "Anna M.",
"orcid": "0000-0002-2894-6936",
"clpid": "Moore-A-M"
},
{
"family_name": "Mogotsi",
"given_name": "Moses",
"clpid": "Mogotsi-M"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554",
"clpid": "Ngeow-Chow-Choong"
},
{
"family_name": "Mart\u00ednez-Palomera",
"given_name": "Jorge",
"orcid": "0000-0002-7395-4935",
"clpid": "Mart\u00ednez-Palomera-J"
},
{
"family_name": "La Parola",
"given_name": "Valentina",
"orcid": "0000-0002-8087-6488",
"clpid": "La-Parola-V"
},
{
"family_name": "Pavana",
"given_name": "M.",
"orcid": "0000-0002-0000-1543",
"clpid": "Pavana-M"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-E-O"
},
{
"family_name": "Patil",
"given_name": "Atharva Sunil",
"clpid": "Patil-A-S"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-M"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Serabyn",
"given_name": "Eugene",
"clpid": "Serabyn-E"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"clpid": "Sharma-Y"
},
{
"family_name": "Singh",
"given_name": "Avinash",
"clpid": "Singh-Avinash"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Soon",
"given_name": "Jamie",
"clpid": "Soon-Jamie"
},
{
"family_name": "Staats",
"given_name": "Kai",
"clpid": "Staats-K"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558",
"clpid": "Taggart-K"
},
{
"family_name": "Tan",
"given_name": "Hanjie",
"clpid": "Tan-Hanjie"
},
{
"family_name": "Travouillon",
"given_name": "Tony",
"clpid": "Travouillon-T-D"
},
{
"family_name": "Troja",
"given_name": "Eleonora",
"orcid": "0000-0002-1869-7817",
"clpid": "Troja-E"
},
{
"family_name": "Waratkar",
"given_name": "Gaurav",
"orcid": "0000-0003-3630-9440",
"clpid": "Waratkar-G"
},
{
"family_name": "Yatsu",
"given_name": "Yoichi",
"orcid": "0000-0003-1890-3913",
"clpid": "Yatsu-Yoichi"
}
],
"abstract": "The third observing run by LVC has brought the discovery of many compact binary coalescences. Following the detection of the first binary neutron star merger in this run (LIGO/Virgo S190425z), we performed a dedicated follow-up campaign with the Zwicky Transient Facility (ZTF) and Palomar Gattini-IR telescopes. The initial skymap of this single-detector gravitational wave (GW) trigger spanned most of the sky observable from Palomar Observatory. Covering 8000 deg\u00b2 of the initial skymap over the next two nights, corresponding to 46% integrated probability, ZTF system achieved a depth of \u224821 m_(AB) in g- and r-bands. Palomar Gattini-IR covered 2200 square degrees in J-band to a depth of 15.5 mag, including 32% integrated probability based on the initial skymap. The revised skymap issued the following day reduced these numbers to 21% for the ZTF and 19% for Palomar Gattini-IR. We narrowed 338,646 ZTF transient \"alerts\" over the first two nights of observations to 15 candidate counterparts. Two candidates, ZTF19aarykkb and ZTF19aarzaod, were particularly compelling given that their location, distance, and age were consistent with the GW event, and their early optical light curves were photometrically consistent with that of kilonovae. These two candidates were spectroscopically classified as young core-collapse supernovae. The remaining candidates were ruled out as supernovae. Palomar Gattini-IR did not identify any viable candidates with multiple detections only after merger time. We demonstrate that even with single-detector GW events localized to thousands of square degrees, systematic kilonova discovery is feasible.",
"doi": "10.3847/2041-8213/ab4ad8",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-11-01",
"series_number": "1",
"volume": "885",
"issue": "1",
"pages": "Art. No. L19"
},
{
"id": "authors:pvkrq-baa86",
"collection": "authors",
"collection_id": "pvkrq-baa86",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191001-101354875",
"type": "article",
"title": "A Flaring AGN in a ULIRG Candidate in Stripe 82",
"author": [
{
"family_name": "Prakash",
"given_name": "Abhishek",
"orcid": "0000-0003-4451-4444",
"clpid": "Prakash-A"
},
{
"family_name": "Chary",
"given_name": "Ranga Ram",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-R-R"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-A-L"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Lee",
"given_name": "Bomee",
"orcid": "0000-0003-1954-5046",
"clpid": "Lee-Bomee"
}
],
"abstract": "We report the discovery of a mid-infrared variable AGN that is hosted by an ultraluminous infrared galaxy (ULIRG) in the Sloan Stripe 82 field. WISE J030654.88+010833.6 is a red, extended galaxy, which we estimate to be at a photometric redshift of 0.28 \u2264 z \u2264 0.31, based on its optical and near-infrared spectral energy distribution (SED). The factor of two variability over 8 yr seen in the Wide-field Infrared Survey Explorer (WISE) 3.4 and 4.6 \u03bcm wavelength channels is not clearly correlated with optical variability in archival data. Based on our estimation of the physical parameters of the host galaxy, J030654.88+010833.6 is possibly a composite AGN/starburst ULIRG in a phase where high star formation ~70 M_\u2299 yr^(\u22121) is occurring. Our estimate of the black hole mass to stellar mass ratio also appears to be consistent with that of broad line AGN in the local universe. The long-term variability of J030654.88+010833.6 as seen in the WISE W1 and W2 light curves is likely due to variations in the accretion rate, with the energy being reprocessed by dust in the vicinity of the AGN.",
"doi": "10.3847/1538-4357/ab3b0b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-10-01",
"series_number": "2",
"volume": "883",
"issue": "2",
"pages": "Art. No. 154"
},
{
"id": "authors:49vt9-n6197",
"collection": "authors",
"collection_id": "49vt9-n6197",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190619-084832405",
"type": "article",
"title": "A New Class of Changing-Look LINERs",
"author": [
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X",
"clpid": "Frederick-S"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154",
"clpid": "Gezari-S"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-S"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadejda",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889",
"clpid": "Hung-Tiara"
},
{
"family_name": "Kara",
"given_name": "Erin",
"orcid": "0000-0003-0172-0854",
"clpid": "Kara-E"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"clpid": "Ward-C"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feindt",
"given_name": "Ulrich",
"orcid": "0000-0002-9435-2167",
"clpid": "Feindt-U"
},
{
"family_name": "Giomi",
"given_name": "Matteo",
"clpid": "Giomi-M"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554",
"clpid": "Ngeow-Chow-Choong"
},
{
"family_name": "Patterson",
"given_name": "Maria T.",
"orcid": "0000-0002-4753-3387",
"clpid": "Patterson-M-T"
},
{
"family_name": "Porter",
"given_name": "Michael",
"clpid": "Porter-M"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
}
],
"abstract": "We report the discovery of six active galactic nuclei (AGNs) caught \"turning on\" during the first nine months of the Zwicky Transient Facility (ZTF) survey. The host galaxies were classified as low-ionization nuclear emission-line region galaxies (LINERs) by weak narrow forbidden line emission in their archival SDSS spectra, and detected by ZTF as nuclear transients. In five of the cases, we found via follow-up spectroscopy that they had transformed into broad-line AGNs, reminiscent of the changing-look LINER iPTF16bco. In one case, ZTF18aajupnt/AT2018dyk, follow-up Hubble Space Telescope ultraviolet and ground-based optical spectra revealed the transformation into a narrow-line Seyfert 1 with strong [Fe vii, x, xiv] and He ii \u03bb 4686 coronal lines. Swift monitoring observations of this source reveal bright UV emission that tracks the optical flare, accompanied by a luminous soft X-ray flare that peaks ~60 days later. Spitzer follow-up observations also detect a luminous mid-infrared flare, implying a large covering fraction of dust. Archival light curves of the entire sample from CRTS, ATLAS, and ASAS-SN constrain the onset of the optical nuclear flaring from a prolonged quiescent state. Here we present the systematic selection and follow-up of this new class of changing-look LINERs, compare their properties to previously reported changing-look Seyfert galaxies, and conclude that they are a unique class of transients well-suited to test the uncertain physical processes associated with the LINER accretion state.",
"doi": "10.3847/1538-4357/ab3a38",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-09-20",
"series_number": "1",
"volume": "883",
"issue": "1",
"pages": "Art. No. 31"
},
{
"id": "authors:x4q6x-9kr65",
"collection": "authors",
"collection_id": "x4q6x-9kr65",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190906-100700610",
"type": "article",
"title": "Outbursts at Comets 46P/Wirtanen, 64P/Swift-Gehrels, and 78P/Gehrels 2 in 2018",
"author": [
{
"family_name": "Kelley",
"given_name": "Michael S. P.",
"orcid": "0000-0002-6702-7676",
"clpid": "Kelley-Michael-S-P"
},
{
"family_name": "Bodewits",
"given_name": "Dennis",
"orcid": "0000-0002-2668-7248",
"clpid": "Bodewits-Dennis"
},
{
"family_name": "Ye",
"given_name": "Quanzhi",
"orcid": "0000-0002-4838-7676",
"clpid": "Ye-Quanzhi"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-Tom\u00e1s"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554",
"clpid": "Ngeow-Chow-Choong"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Cromer",
"given_name": "John",
"clpid": "Cromer-John-L"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
}
],
"abstract": "Cometary outbursts are brief increases in the mass-loss rates of comets (Hughes 1990). Most observed outbursts have \u0394m \u2273 1\u2009mag, but smaller outbursts do occur, such as those observed by the Deep Impact and Rosetta spacecraft at comets 9P/Tempel 1 and 67P/Churyumov-Gerasimenko (A'Hearn et al. 2005; Vincent et al. 2016). The outbursts are smaller than the Deep Impact excavation, suggesting strengths near \u22120.2 to \u22121\u2009mag (A'Hearn et al. 2005; Meech et al. 2005; Feldman et al. 2007). \n\nWide-field, time-domain surveys are well-suited to the discovery of cometary outbursts (Graham et al. 2019). We describe initial results from our outburst search using the Zwicky Transient Facility archive (ZTF; Bellm et al. 2019), based on observations of three comets: 46P/Wirtanen, 64P/Swift-Gehrels, and 78P/Gehrels 2. The data are calibrated to the Pan-STARRS 1 photometric system (Masci et al. 2019), and color corrected assuming a reddened solar spectrum (g\u2212r = 0.52\u2009mag, r\u2212i = 0.15\u2009mag). We measured photometry in 7'' radius apertures, then fit and removed a linear trend from each lightcurve: 46P, \u22120.053\u2009mag day^(\u22121) (rms 0.02\u2009mag); 64P, \u22120.053\u2009mag day^(\u22121) (rms 0.04\u2009mag); 78P, \u22120.039\u2009mag day^(\u22121) (rms 0.04\u2009mag).",
"doi": "10.3847/2515-5172/ab3fb4",
"issn": "2515-5172",
"publisher": "American Astronomical Society",
"publication": "Research Notes of the AAS",
"publication_date": "2019-09-05",
"series_number": "9",
"volume": "3",
"issue": "9",
"pages": "Art No. 126"
},
{
"id": "authors:p5e7p-11y60",
"collection": "authors",
"collection_id": "p5e7p-11y60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190821-143228300",
"type": "article",
"title": "Identification of Stellar Flares Using Differential Evolution Template Optimization",
"author": [
{
"family_name": "Lawson",
"given_name": "Kellen D.",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-K-D"
},
{
"family_name": "Wisniewski",
"given_name": "John P.",
"orcid": "0000-0001-9209-1808",
"clpid": "Wisniewski-J-P"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Kowalski",
"given_name": "Adam F.",
"orcid": "0000-0001-7458-1176",
"clpid": "Kowalski-A-F"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "We explore methods for the identification of stellar flare events in irregularly sampled data of ground-based time domain surveys. In particular, we describe a new technique for identifying flaring stars, which we have implemented in a publicly available Python module called \"PyVAN.\" The approach uses the Differential Evolution algorithm to optimize parameters of empirically derived light curve templates for different types of stars to fit a candidate light curve. The difference of the likelihoods that these best-fit templates produced the observed data is then used to delineate targets that are well-explained by a flare template but simultaneously poorly explained by templates of common contaminants. By testing on light curves of known identity and morphology, we show that our technique is capable of recovering flaring status in 69% of all light curves containing a flare event above thresholds drawn to include <1% of any contaminant population. By applying to Palomar Transient Factory data, we show consistency with prior samples of flaring stars, and identify a small selection of candidate flaring G-type stars for possible follow-up.",
"doi": "10.3847/1538-3881/ab3461",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-09",
"series_number": "3",
"volume": "158",
"issue": "3",
"pages": "Art. No. 119"
},
{
"id": "authors:jxq4g-9zq68",
"collection": "authors",
"collection_id": "jxq4g-9zq68",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190514-142944629",
"type": "article",
"title": "General relativistic orbital decay in a seven-minute-orbital-period eclipsing binary system",
"author": [
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Bildsten",
"given_name": "Lars",
"clpid": "Bildsten-L"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-D-L"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Dekany",
"given_name": "Richard G.",
"clpid": "Dekany-Richard"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Giomi",
"given_name": "Matteo",
"clpid": "Giomi-M"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-S"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Smith",
"given_name": "Roger M.",
"clpid": "Smith-R-M"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"clpid": "Szkody-P"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
}
],
"abstract": "General relativity predicts that short-orbital-period binaries emit considerable amounts of gravitational radiation. The upcoming Laser Interferometer Space Antenna (LISA) is expected to detect tens of thousands of such systems but few have been identified4, of which only one5 is eclipsing\u2014the double-white-dwarf binary SDSS J065133.338+284423.37, which has an orbital period of 12.75 minutes. Here we report the discovery of an eclipsing double-white-dwarf binary system, ZTF J153932.16+502738.8, with an orbital period of 6.91 minutes. This system has an orbit so compact that the entire binary could fit within the diameter of the planet Saturn. The system exhibits a deep eclipse, and a double-lined spectroscopic nature. We see rapid orbital decay, consistent with that expected from general relativity. ZTF J153932.16+502738.8 is a strong source of gravitational radiation close to the peak of LISA's sensitivity, and we expect it to be detected within the first week of LISA observations, once LISA launches in approximately 2034.",
"doi": "10.1038/s41586-019-1403-0",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2019-07-24",
"series_number": "7767",
"volume": "571",
"issue": "7767",
"pages": "528-531"
},
{
"id": "authors:43bjy-4dr06",
"collection": "authors",
"collection_id": "43bjy-4dr06",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190107-091211377",
"type": "article",
"title": "Census of the Local Universe (CLU) Narrowband Survey. I. Galaxy Catalogs from Preliminary Fields",
"author": [
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-D-O"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Van Sistine",
"given_name": "Angela",
"orcid": "0000-0003-4131-173X",
"clpid": "Van-Sistine-A"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881",
"clpid": "Kaplan-D-L"
},
{
"family_name": "Sutter",
"given_name": "Jessica S.",
"orcid": "0000-0002-9183-8102",
"clpid": "Sutter-J-S"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Dale",
"given_name": "Daniel A.",
"orcid": "0000-0002-5782-9093",
"clpid": "Dale-D-A"
},
{
"family_name": "Sesar",
"given_name": "Branimir",
"orcid": "0000-0002-0834-3978",
"clpid": "Sesar-B"
},
{
"family_name": "Brady",
"given_name": "Patrick R.",
"orcid": "0000-0002-4611-9387",
"clpid": "Brady-P-R"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-E-O"
},
{
"family_name": "Reitze",
"given_name": "David H.",
"clpid": "Reitze-D-H"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "We present the Census of the Local Universe (CLU) narrowband survey to search for emission-line (H\u03b1) galaxies. CLU-H\u03b1 has imaged \u22483\u03c0 of the sky (26,470 deg^2) with four narrowband filters that probe a distance out to 200 Mpc. We have obtained spectroscopic follow-up for galaxy candidates in 14 preliminary fields (101.6 deg2) to characterize the limits and completeness of the survey. In these preliminary fields, CLU can identify emission lines down to an H\u03b1 flux limit of 10^(\u221214) erg s^(\u22121) cm^(\u22122) at 90% completeness, and recovers 83% (67%) of the H\u03b1 flux from cataloged galaxies in our search volume at the \u03a3 = 2.5 (\u03a3 = 5) color excess levels. The contamination from galaxies with no emission lines is 61% (12%) for \u03a3 = 2.5 (\u03a3 = 5). Also, in the regions of overlap between our preliminary fields and previous emission-line surveys, we recover the majority of the galaxies found in previous surveys and identify an additional \u2248300 galaxies. In total, we find 90 galaxies with no previous distance information, several of which are interesting objects: 7 blue compact dwarfs, 1 green pea, and a Seyfert galaxy; we also identify a known planetary nebula. These objects show that the CLU-H\u03b1 survey can be a discovery machine for objects in our own Galaxy and extreme galaxies out to intermediate redshifts. However, the majority of the CLU-H\u03b1 galaxies identified in this work show properties consistent with normal star-forming galaxies. CLU-H\u03b1 galaxies with new redshifts will be added to existing galaxy catalogs to focus the search for the electromagnetic counterpart to gravitational wave events.",
"doi": "10.3847/1538-4357/ab2131",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-07-20",
"series_number": "1",
"volume": "880",
"issue": "1",
"pages": "Art. No. 7"
},
{
"id": "authors:ak75k-t5750",
"collection": "authors",
"collection_id": "ak75k-t5750",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190618-090909587",
"type": "article",
"title": "Discovery of Highly Blueshifted Broad Balmer and Metastable Helium Absorption Lines in a Tidal Disruption Event",
"author": [
{
"family_name": "Hung",
"given_name": "T.",
"clpid": "Hung-T-K"
},
{
"family_name": "Cenko",
"given_name": "S. B.",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Roth",
"given_name": "Nathaniel",
"clpid": "Roth-N"
},
{
"family_name": "Gezari",
"given_name": "S.",
"orcid": "0000-0003-3703-5154",
"clpid": "Gezari-S"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-S"
},
{
"family_name": "Gaskell",
"given_name": "C. Martin",
"clpid": "Gaskell-C-M"
},
{
"family_name": "Foley",
"given_name": "Ryan J.",
"clpid": "Foley-R-J"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Brown",
"given_name": "J. S.",
"orcid": "0000-0002-1885-6419",
"clpid": "Brown-J-S"
},
{
"family_name": "Siebert",
"given_name": "M. R.",
"clpid": "Siebert-M-R"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X",
"clpid": "Frederick-S"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"clpid": "Ward-C"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-P"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-A"
},
{
"family_name": "Yang",
"given_name": "Yi",
"clpid": "Yang-Yi"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-S"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"clpid": "Dimitriadis-G"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
}
],
"abstract": "We report the discovery of nonstellar hydrogen Balmer and metastable helium absorption lines accompanying a transient, high-velocity (0.05c) broad absorption line (BAL) system in the optical spectra of the tidal disruption event (TDE) AT2018zr (z = 0.071). In the Hubble Space Telescope UV spectra, absorption of high- and low-ionization lines is also present at this velocity, making AT2018zr resemble a low-ionization BALQSO. We conclude that these transient absorption features are more likely to arise in fast outflows produced by the TDE than absorbed by the unbound debris. In accordance with the outflow picture, we are able to reproduce the flat-topped H\u03b1 emission in a spherically expanding medium without invoking the typical prescription of an elliptical disk. We also report the appearance of narrow (~1000 kms^(\u22121)) N III \u03bb4640, He II \u03bb4686, H\u03b1, and H\u03b2 emission in the late-time optical spectra of AT2018zr, which may be a result of UV continuum hardening at late times, as observed by Swift. Including AT2018zr, we find a high association rate (three out of four) of BALs in the UV spectra of TDEs. This suggests that outflows may be ubiquitous among TDEs and less sensitive to viewing angle effects compared to QSO outflows.",
"doi": "10.3847/1538-4357/ab24de",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-07-10",
"series_number": "2",
"volume": "879",
"issue": "2",
"pages": "Art. No. 119"
},
{
"id": "authors:qr7vb-95k31",
"collection": "authors",
"collection_id": "qr7vb-95k31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190213-135514906",
"type": "article",
"title": "The Zwicky Transient Facility: Science Objectives",
"author": [
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-Eric-C"
},
{
"family_name": "Adams",
"given_name": "S. M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144",
"clpid": "Barbarino-Cristina"
},
{
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"abstract": "The Zwicky Transient Facility (ZTF), a public\u2013private enterprise, is a new time-domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg^2 field of view and an 8 second readout time. It is well positioned in the development of time-domain astronomy, offering operations at 10% of the scale and style of the Large Synoptic Survey Telescope (LSST) with a single 1-m class survey telescope. The public surveys will cover the observable northern sky every three nights in g and r filters and the visible Galactic plane every night in g and r. Alerts generated by these surveys are sent in real time to brokers. A consortium of universities that provided funding (\"partnership\") are undertaking several boutique surveys. The combination of these surveys producing one million alerts per night allows for exploration of transient and variable astrophysical phenomena brighter than r ~ 20.5 on timescales of minutes to years. We describe the primary science objectives driving ZTF, including the physics of supernovae and relativistic explosions, multi-messenger astrophysics, supernova cosmology, active galactic nuclei, and tidal disruption events, stellar variability, and solar system objects.",
"doi": "10.1088/1538-3873/ab006c",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-07",
"series_number": "1001",
"volume": "131",
"issue": "1001",
"pages": "Art. No. 078001"
},
{
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"collection": "authors",
"collection_id": "z24gp-a1228",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190501-093856077",
"type": "article",
"title": "Towards Efficient Detection of Small Near-Earth Asteroids Using the Zwicky Transient Facility (ZTF)",
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},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682",
"clpid": "Ward-Charlotte-A"
}
],
"abstract": "We describe ZStreak, a semi-real-time pipeline specialized in detecting small, fast-moving, near-Earth asteroids (NEAs), which is currently operating on the data from the newly commissioned Zwicky Transient Facility (ZTF) survey. Based on a prototype originally developed by Waszczak et al. (2017) for the Palomar Transient Factory (PTF), the predecessor of ZTF, ZStreak features an improved machine-learning model that can cope with the 10\u00d7 data rate increment between PTF and ZTF. Since its first discovery on 2018 February 5 (2018 CL), ZTF/ZStreak has discovered 45 confirmed new NEAs over a total of 232 observable nights until 2018 December 31. Most of the discoveries are small NEAs, with diameters less than ~100 m. By analyzing the discovery circumstances, we find that objects having the first to last detection time interval under 2 hr are at risk of being lost. We will further improve real-time follow-up capabilities, and work on suppressing false positives using deep learning.",
"doi": "10.1088/1538-3873/ab1b18",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-07",
"series_number": "1001",
"volume": "131",
"issue": "1001",
"pages": "Art. No. 078002"
},
{
"id": "authors:trwjm-4zm88",
"collection": "authors",
"collection_id": "trwjm-4zm88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190617-135126883",
"type": "article",
"title": "A New Class of Large-amplitude Radial-mode Hot Subdwarf Pulsators",
"author": [
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Bauer",
"given_name": "Evan B.",
"orcid": "0000-0002-4791-6724",
"clpid": "Bauer-E-B"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Bildsten",
"given_name": "Lars",
"clpid": "Bildsten-L"
},
{
"family_name": "Fuller",
"given_name": "Jim",
"orcid": "0000-0002-4544-0750",
"clpid": "Fuller-J"
},
{
"family_name": "Hermes",
"given_name": "J. J.",
"clpid": "Hermes-J-J"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M-E"
},
{
"family_name": "Giomi",
"given_name": "Matteo",
"clpid": "Giomi-M"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-S"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Porter",
"given_name": "Michael",
"clpid": "Porter-M"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Roger M.",
"clpid": "Smith-R-M"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"clpid": "Szkody-P"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"clpid": "Ward-C"
}
],
"abstract": "Using high-cadence observations from the Zwicky Transient Facility at low Galactic latitudes, we have discovered a new class of pulsating, hot compact stars. We have found four candidates, exhibiting blue colors (g \u2212 r \u2264 \u22120.1 mag), pulsation amplitudes of >5%, and pulsation periods of 200\u2013475 s. Fourier transforms of the light curves show only one dominant frequency. Phase-resolved spectroscopy for three objects reveals significant radial velocity, T_(eff), and log(g) variations over the pulsation cycle, which are consistent with large-amplitude radial oscillations. The mean T_(eff) and log(g) for these stars are consistent with hot subdwarf B (sdB) effective temperatures and surface gravities. We calculate evolutionary tracks using MESA and adiabatic pulsations using GYRE for low-mass, helium-core pre-white dwarfs (pre-WDs) and low-mass helium-burning stars. Comparison of low-order radial oscillation mode periods with the observed pulsation periods show better agreement with the pre-WD models. Therefore, we suggest that these new pulsators and blue large-amplitude pulsators (BLAPs) could be members of the same class of pulsators, composed of young \u22480.25\u20130.35 M_\u2299 helium-core pre-WDs.",
"doi": "10.3847/2041-8213/ab263c",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-06-20",
"series_number": "2",
"volume": "878",
"issue": "2",
"pages": "Art. No. L35"
},
{
"id": "authors:pzdaj-seq49",
"collection": "authors",
"collection_id": "pzdaj-seq49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190314-111129588",
"type": "article",
"title": "ZTF 18aaqeasu (SN2018byg): A Massive Helium-shell Double Detonation on a Sub-Chandrasekhar-mass White Dwarf",
"author": [
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"clpid": "Polin-A"
},
{
"family_name": "Nugent",
"given_name": "P. E.",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-P-E"
},
{
"family_name": "Bildsten",
"given_name": "Lars",
"clpid": "Bildsten-L"
},
{
"family_name": "Adams",
"given_name": "Scott M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Cannella",
"given_name": "Christopher",
"orcid": "0000-0003-2667-7290",
"clpid": "Cannella-C-B"
},
{
"family_name": "Cenko",
"given_name": "S. B.",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-M"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-D"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-J-E"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Patterson",
"given_name": "Maria T.",
"orcid": "0000-0002-4753-3387",
"clpid": "Patterson-M-T"
},
{
"family_name": "Rebbapragada",
"given_name": "Umaa",
"orcid": "0000-0002-2560-3495",
"clpid": "Rebbapragada-U-D"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Roger M.",
"clpid": "Smith-R-M"
}
],
"abstract": "The detonation of a helium shell on a white dwarf (WD) has been proposed as a possible explosion triggering mechanism for SNe Ia. Here, we report ZTF 18aaqeasu (SN 2018byg/ATLAS 18pqq), a peculiar Type I supernova, consistent with being a helium-shell double-detonation. With a rise time of \u224818 days from explosion, the transient reached a peak absolute magnitude of M_R \u2248 \u221218.2 mag, exhibiting a light curve akin to sub-luminous SN 1991bg-like SNe Ia, albeit with an unusually steep increase in brightness within a week from explosion. Spectra taken near peak light exhibit prominent Si absorption features together with an unusually red color (g \u2212 r \u2248 2 mag) arising from nearly complete line blanketing of flux blueward of 5000 \u00c5. This behavior is unlike any previously observed thermonuclear transient. Nebular phase spectra taken at and after \u224830 days from peak light reveal evidence of a thermonuclear detonation event dominated by Fe-group nucleosynthesis. We show that the peculiar properties of ZTF 18aaqeasu are consistent with the detonation of a massive (\u22480.15 M\u2299) helium shell on a sub-Chandrasekhar mass (\u22480.75 M\u2299) WD after including mixing of \u22480.2 M\u2299 of material in the outer ejecta. These observations provide evidence of a likely rare class of thermonuclear supernovae arising from detonations of massive helium shells.",
"doi": "10.3847/2041-8213/ab0aec",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-03-10",
"series_number": "2",
"volume": "873",
"issue": "2",
"pages": "Art. No. L18"
},
{
"id": "authors:v48zy-yvj17",
"collection": "authors",
"collection_id": "v48zy-yvj17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190131-104830427",
"type": "article",
"title": "Machine Learning for the Zwicky Transient Facility",
"author": [
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Rebbapragada",
"given_name": "U. D.",
"orcid": "0000-0002-2560-3495",
"clpid": "Rebbapragada-U-D"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Blagorodnova",
"given_name": "N.",
"orcid": "0000-0003-0901-1606",
"clpid": "Blagorodnova-N"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Biswas",
"given_name": "Rahul",
"orcid": "0000-0002-5741-7195",
"clpid": "Biswas-R"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Chang",
"given_name": "Chan-Kao",
"orcid": "0000-0003-1656-4540",
"clpid": "Chang-Chan-Kao"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506",
"clpid": "Golkhou-V-Z"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"clpid": "Miller-AA"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"clpid": "Nordin-J"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"clpid": "Ward-C"
},
{
"family_name": "Adams",
"given_name": "Scott M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Branton",
"given_name": "Doug",
"clpid": "Branton-D"
},
{
"family_name": "Bue",
"given_name": "Brian D.",
"orcid": "0000-0002-7856-3570",
"clpid": "Bue-B-D"
},
{
"family_name": "Cannella",
"given_name": "C.",
"orcid": "0000-0003-2667-7290",
"clpid": "Cannella-C-B"
},
{
"family_name": "Connolly",
"given_name": "Andrew",
"clpid": "Connolly-A"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Feindt",
"given_name": "Ulrich",
"orcid": "0000-0002-9435-2167",
"clpid": "Feindt-U"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889",
"clpid": "Hung-Tiara"
},
{
"family_name": "Fortson",
"given_name": "Lucy F.",
"orcid": "0000-0002-1067-8558",
"clpid": "Fortson-L-F"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X",
"clpid": "Frederick-S"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154",
"clpid": "Gezari-S"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Groom",
"given_name": "Steven",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-S-L"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Lin",
"given_name": "Hsing Wen",
"orcid": "0000-0001-7737-6784",
"clpid": "Lin-Hsing-Wen"
},
{
"family_name": "Lintott",
"given_name": "Chris J.",
"orcid": "0000-0001-5578-359X",
"clpid": "Lintott-C-J"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-R"
},
{
"family_name": "Parejko",
"given_name": "John",
"clpid": "Parejko-J-K"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Saunders",
"given_name": "Nicholas",
"orcid": "0000-0003-2657-3889",
"clpid": "Saunders-N"
},
{
"family_name": "Sedaghat",
"given_name": "Nima",
"clpid": "Sedaghat-N"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-L-P"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-M-T"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"clpid": "Szkody-P"
},
{
"family_name": "Tachibana",
"given_name": "Yutaro",
"orcid": "0000-0001-6584-6945",
"clpid": "Tachibana-Yutaro"
},
{
"family_name": "Tirumala",
"given_name": "Kushal",
"clpid": "Tirumala-K"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-S"
},
{
"family_name": "Wright",
"given_name": "Darryl",
"clpid": "Wright-D"
}
],
"abstract": "The Zwicky Transient Facility is a large optical survey in multiple filters producing hundreds of thousands of transient alerts per night. We describe here various machine learning (ML) implementations and plans to make the maximal use of the large data set by taking advantage of the temporal nature of the data, and further combining it with other data sets. We start with the initial steps of separating bogus candidates from real ones, separating stars and galaxies, and go on to the classification of real objects into various classes. Besides the usual methods (e.g., based on features extracted from light curves) we also describe early plans for alternate methods including the use of domain adaptation, and deep learning. In a similar fashion we describe efforts to detect fast moving asteroids. We also describe the use of the Zooniverse platform for helping with classifications through the creation of training samples, and active learning. Finally we mention the synergistic aspects of ZTF and LSST from the ML perspective.",
"doi": "10.1088/1538-3873/aaf3fa",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-03",
"series_number": "997",
"volume": "131",
"issue": "997",
"pages": "Art. No. 038002"
},
{
"id": "authors:pfh76-zfr89",
"collection": "authors",
"collection_id": "pfh76-zfr89",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181207-084047467",
"type": "article",
"title": "The Zwicky Transient Facility: Data Processing, Products, and Archive",
"author": [
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Groom",
"given_name": "Steven",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-S-L"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
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"abstract": "The Zwicky Transient Facility (ZTF) is a new robotic time-domain survey currently in progress using the Palomar 48-inch Schmidt Telescope. ZTF uses a 47 square degree field with a 600 megapixel camera to scan the entire northern visible sky at rates of ~3760 square degrees/hour to median depths of g ~ 20.8 and r ~ 20.6 mag (AB, 5\u03c3 in 30 sec). We describe the Science Data System that is housed at IPAC, Caltech. This comprises the data-processing pipelines, alert production system, data archive, and user interfaces for accessing and analyzing the products. The real-time pipeline employs a novel image-differencing algorithm, optimized for the detection of point-source transient events. These events are vetted for reliability using a machine-learned classifier and combined with contextual information to generate data-rich alert packets. The packets become available for distribution typically within 13 minutes (95th percentile) of observation. Detected events are also linked to generate candidate moving-object tracks using a novel algorithm. Objects that move fast enough to streak in the individual exposures are also extracted and vetted. We present some preliminary results of the calibration performance delivered by the real-time pipeline. The reconstructed astrometric accuracy per science image with respect to Gaia DR1 is typically 45 to 85 milliarcsec. This is the RMS per-axis on the sky for sources extracted with photometric S/N \u2265 10 and hence corresponds to the typical astrometric uncertainty down to this limit. The derived photometric precision (repeatability) at bright unsaturated fluxes varies between 8 and 25 millimag. The high end of these ranges corresponds to an airmass approaching ~2\u2014the limit of the public survey. Photometric calibration accuracy with respect to Pan-STARRS1 is generally better than 2%. The products support a broad range of scientific applications: fast and young supernovae; rare flux transients; variable stars; eclipsing binaries; variability from active galactic nuclei; counterparts to gravitational wave sources; a more complete census of Type Ia supernovae; and solar-system objects.",
"doi": "10.1088/1538-3873/aae8ac",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-01-01",
"series_number": "995",
"volume": "131",
"issue": "995",
"pages": "Art. No. 018003"
},
{
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"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181207-084047368",
"type": "article",
"title": "The Zwicky Transient Facility: System Overview, Performance, and First Results",
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{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Jan"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "van Santen",
"given_name": "J.",
"clpid": "van-Santen-J"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-Steve"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Singer",
"given_name": "Leo P.",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-Leo-P"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488",
"clpid": "Soumagnac-Maayane-T"
},
{
"family_name": "Stein",
"given_name": "Robert",
"clpid": "Stein-Robert-M"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-Jason-A"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-J"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"orcid": "0000-0003-4373-7777",
"clpid": "Szkody-Paula"
},
{
"family_name": "Taddia",
"given_name": "F.",
"orcid": "0000-0002-2387-6801",
"clpid": "Taddia-Francesco"
},
{
"family_name": "Terek",
"given_name": "Scott",
"clpid": "Terek-Scott"
},
{
"family_name": "Van Sistine",
"given_name": "Angela",
"orcid": "0000-0003-4131-173X",
"clpid": "Van-Sistine-Angela"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-Sjoert"
},
{
"family_name": "Vestrand",
"given_name": "W. T.",
"orcid": "0000-0001-7120-7234",
"clpid": "Vestrand-W-Thomas"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682",
"clpid": "Ward-Charlotte-A"
},
{
"family_name": "Yi",
"given_name": "Quan-Zhi",
"clpid": "Yi-Quan-Zhi"
},
{
"family_name": "Yu",
"given_name": "Po-Chieh",
"orcid": "0000-0001-8894-0854",
"clpid": "Yu-Po-Chieh"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "The Zwicky Transient Facility (ZTF) is a new optical time-domain survey that uses the Palomar 48 inch Schmidt telescope. A custom-built wide-field camera provides a 47 deg^2 field of view and 8 s readout time, yielding more than an order of magnitude improvement in survey speed relative to its predecessor survey, the Palomar Transient Factory. We describe the design and implementation of the camera and observing system. The ZTF data system at the Infrared Processing and Analysis Center provides near-real-time reduction to identify moving and varying objects. We outline the analysis pipelines, data products, and associated archive. Finally, we present on-sky performance analysis and first scientific results from commissioning and the early survey. ZTF's public alert stream will serve as a useful precursor for that of the Large Synoptic Survey Telescope.",
"doi": "10.1088/1538-3873/aaecbe",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-01",
"series_number": "995",
"volume": "131",
"issue": "995",
"pages": "Art. No. 018002"
},
{
"id": "authors:jxnvh-ns628",
"collection": "authors",
"collection_id": "jxnvh-ns628",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180823-133002945",
"type": "article",
"title": "The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package",
"author": [
{
"family_name": "Price-Whelan",
"given_name": "A. M.",
"orcid": "0000-0003-0872-7098",
"clpid": "Price-Whelan-A-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"literal": "The Astropy Collaboration"
}
],
"abstract": "The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.",
"doi": "10.3847/1538-3881/aabc4f",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-09",
"series_number": "3",
"volume": "156",
"issue": "3",
"pages": "Art. No. 123"
},
{
"id": "authors:pekdb-25660",
"collection": "authors",
"collection_id": "pekdb-25660",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180329-132609534",
"type": "article",
"title": "Discovery of 36 eclipsing EL CVn binaries found by the Palomar Transient Factory",
"author": [
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Kupfer",
"given_name": "T.",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Ruiz-Carmona",
"given_name": "R.",
"clpid": "Ruiz-Carmona-R"
},
{
"family_name": "Groot",
"given_name": "P. J.",
"orcid": "0000-0002-4488-726X",
"clpid": "Groot-P-J"
},
{
"family_name": "Prince",
"given_name": "T. A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Burdge",
"given_name": "K.",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Laher",
"given_name": "R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Bellm",
"given_name": "E.",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
}
],
"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.",
"doi": "10.1093/mnras/stx3291",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2018-04-01",
"series_number": "2",
"volume": "475",
"issue": "2",
"pages": "2560-2590"
},
{
"id": "authors:ha4er-e6221",
"collection": "authors",
"collection_id": "ha4er-e6221",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180327-075241554",
"type": "article",
"title": "The Binary Dwarf Carbon Star SDSS J125017.90+252427.6",
"author": [
{
"family_name": "Margon",
"given_name": "Bruce",
"orcid": "0000-0002-7837-3363",
"clpid": "Margon-B"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-K-B"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "Although dwarf carbon (dC) stars are universally thought to be binaries in order to explain the presence of C_2 in their spectra while still near main-sequence luminosity, direct observational evidence for their binarity is remarkably scarce. Here, we report the detection of a 2.92 day periodicity in both the photometry and radial velocity of SDSS J125017.90+252427.6, an r = 16.4 dC star. This is the first photometric binary dC, and only the second dC spectroscopic binary. The relative phase of the photometric period to the spectroscopic observations suggests that the photometric variations are a reflection effect due to heating from an unseen companion. The observed radial velocity amplitude of the dC component (K = 98.8 \u00b1 10.7 km s^(\u22121)) is consistent with a white dwarf companion, presumably the evolved star that earlier donated the carbon to the dC, although substantial orbital evolution must have occurred. Large synoptic photometric surveys such as the Palomar Transient Factory, which was used for this work, may prove useful for identifying binaries among the shorter-period dC stars.",
"doi": "10.3847/2041-8213/aab42a",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2018-03-20",
"series_number": "1",
"volume": "856",
"issue": "1",
"pages": "Art. No. L2"
},
{
"id": "authors:pkh2c-rxx76",
"collection": "authors",
"collection_id": "pkh2c-rxx76",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170828-074937096",
"type": "article",
"title": "Red but not dead: unveiling the star-forming far-infrared spectral energy distribution of SpARCS brightest cluster galaxies at 0 < z < 1.8",
"author": [
{
"family_name": "Bonaventura",
"given_name": "N. R.",
"clpid": "Bonaventura-N-R"
},
{
"family_name": "Webb",
"given_name": "T. M. A.",
"clpid": "Webb-T-M-A"
},
{
"family_name": "Muzzin",
"given_name": "A.",
"orcid": "0000-0002-9330-9108",
"clpid": "Muzzin-A"
},
{
"family_name": "Noble",
"given_name": "A.",
"orcid": "0000-0003-1832-4137",
"clpid": "Noble-A-G"
},
{
"family_name": "Lidman",
"given_name": "C.",
"orcid": "0000-0003-1731-0497",
"clpid": "Lidman-C"
},
{
"family_name": "Wilson",
"given_name": "G.",
"clpid": "Wilson-G-W"
},
{
"family_name": "Yee",
"given_name": "H. K. C.",
"clpid": "Yee-H-K-C"
},
{
"family_name": "Geach",
"given_name": "J.",
"orcid": "0000-0003-4964-4635",
"clpid": "Geach-J-E"
},
{
"family_name": "Hezaveh",
"given_name": "Y.",
"clpid": "Hezaveh-Y-D"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
}
],
"abstract": "We present the results of a Spitzer/Herschel infrared photometric analysis of the largest (716) and the highest-redshift (z = 1.8) sample of brightest cluster galaxies (BCGs), those from the Spitzer Adaptation of the Red-Sequence Cluster Survey Given the tension that exists between model predictions and recent observations of BCGs at z < 2, we aim to uncover the dominant physical mechanism(s) guiding the stellar mass buildup of this special class of galaxies, the most massive in the Universe and uniquely residing at the centres of galaxy clusters. Through a comparison of their stacked, broad-band, infrared spectral energy distributions (SEDs) to a variety of model templates in the literature, we identify the major sources of their infrared energy output, in multiple redshift bins between 0 < z < 1.8. We derive estimates of various BCG physical parameters from the stacked \u03bdL\u03bd SEDs, from which we infer a star-forming, as opposed to a 'red and dead' population of galaxies, producing tens to hundreds of solar masses per year down to z = 0.5. This discovery challenges the accepted belief that BCGs should only passively evolve through a series of gas-poor, minor mergers since z \u223c 4, but agrees with an improved semi-analytic model of hierarchical structure formation that predicts star-forming BCGs throughout the epoch considered. We attribute the star formation inferred from the stacked infrared SEDs to both major and minor 'wet' (gas-rich) mergers, based on a lack of key signatures (to date) of cooling-flow-induced star formation, as well as a number of observational and simulation-based studies that support this scenario.",
"doi": "10.1093/mnras/stx722",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2017-08",
"series_number": "2",
"volume": "469",
"issue": "2",
"pages": "1259-1281"
},
{
"id": "authors:ahaj9-cpm89",
"collection": "authors",
"collection_id": "ahaj9-cpm89",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170623-141442582",
"type": "article",
"title": "PTF1 J085713+331843, a new post-common-envelope binary in the orbital period gap of cataclysmic variables",
"author": [
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Groot",
"given_name": "P. J.",
"orcid": "0000-0002-4488-726X",
"clpid": "Groot-P-J"
},
{
"family_name": "Levitan",
"given_name": "D.",
"clpid": "Levitan-D-B"
},
{
"family_name": "Prince",
"given_name": "T. A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Bloemen",
"given_name": "S.",
"clpid": "Bloemen-S"
},
{
"family_name": "Marsh",
"given_name": "T. R.",
"orcid": "0000-0002-2498-7589",
"clpid": "Marsh-T-R"
},
{
"family_name": "Dhillon",
"given_name": "V. S.",
"clpid": "Dhillon-V-S"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Laher",
"given_name": "R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
}
],
"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.",
"doi": "10.1093/mnras/stx625",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2017-07",
"series_number": "3",
"volume": "468",
"issue": "3",
"pages": "3109-3122"
},
{
"id": "authors:zm5ws-hqd60",
"collection": "authors",
"collection_id": "zm5ws-hqd60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170331-143835493",
"type": "article",
"title": "The Great Observatories All-Sky LIRG Survey: Herschel Image Atlas and Aperture Photometry",
"author": [
{
"family_name": "Chu",
"given_name": "Jason K.",
"orcid": "0000-0003-3955-2470",
"clpid": "Chu-Jason-K"
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998",
"clpid": "Sanders-D-B"
},
{
"family_name": "Larson",
"given_name": "K. L.",
"orcid": "0000-0003-3917-6460",
"clpid": "Larson-K-L"
},
{
"family_name": "Mazzarella",
"given_name": "J. M.",
"orcid": "0000-0002-8204-8619",
"clpid": "Mazzarella-J-M"
},
{
"family_name": "Howell",
"given_name": "J. H.",
"clpid": "Howell-J-H"
},
{
"family_name": "D\u00edaz-Santos",
"given_name": "T.",
"orcid": "0000-0003-0699-6083",
"clpid": "D\u00edaz-Santos-T"
},
{
"family_name": "Xu",
"given_name": "K. C.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Paladini",
"given_name": "R.",
"orcid": "0000-0002-5158-243X",
"clpid": "Paladini-Roberta"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Appleton",
"given_name": "P.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Billot",
"given_name": "N.",
"clpid": "Billot-N-P"
},
{
"family_name": "Chan",
"given_name": "B. H. P.",
"clpid": "Chan-Ben-Hiu-Pan"
},
{
"family_name": "Evans",
"given_name": "A. S.",
"orcid": "0000-0003-2638-1334",
"clpid": "Evans-A-S"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Haan",
"given_name": "S.",
"clpid": "Haan-S"
},
{
"family_name": "Ishida",
"given_name": "C. M.",
"clpid": "Ishida-Catherine-M"
},
{
"family_name": "Iwasawa",
"given_name": "K.",
"orcid": "0000-0002-4923-3281",
"clpid": "Iwasawa-Kazushi"
},
{
"family_name": "Kim",
"given_name": "D.-C.",
"clpid": "Kim-Dong-Chan"
},
{
"family_name": "Lord",
"given_name": "S.",
"clpid": "Lord-S"
},
{
"family_name": "Murphy",
"given_name": "E.",
"orcid": "0000-0001-7089-7325",
"clpid": "Murphy-E-J"
},
{
"family_name": "Petric",
"given_name": "A.",
"orcid": "0000-0003-4030-3455",
"clpid": "Petric-A-O"
},
{
"family_name": "Privon",
"given_name": "G. C.",
"orcid": "0000-0003-3474-1125",
"clpid": "Privon-G-C"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Treister",
"given_name": "E.",
"orcid": "0000-0001-7568-6412",
"clpid": "Treister-E"
}
],
"abstract": "Far-infrared images and photometry are presented for 201 Luminous and Ultraluminous Infrared Galaxies [LIRGs: log (L_(IR)/L\u2299) = 11.00-11.99, ULIRGs: log (L_(IR)/L\u2299) = 12.00-12.99], in the Great Observatories All-Sky LIRG Survey (GOALS), based on observations with the Herschel Space Observatory Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE) instruments. The image atlas displays each GOALS target in the three PACS bands (70, 100, and 160 \u03bcm) and the three SPIRE bands (250, 350, and 500 \u03bcm), optimized to reveal structures at both high and low surface brightness levels, with images scaled to simplify comparison of structures in the same physical areas of ~100 \u00d7 100 kpc^2. Flux densities of companion galaxies in merging systems are provided where possible, depending on their angular separation and the spatial resolution in each passband, along with integrated system fluxes (sum of components). This data set constitutes the imaging and photometric component of the GOALS Herschel OT1 observing program, and is complementary to atlases presented for the Hubble Space Telescope, Spitzer Space Telescope, and Chandra X-ray Observatory. Collectively, these data will enable a wide range of detailed studies of active galactic nucleus and starburst activity within the most luminous infrared galaxies in the local universe.",
"doi": "10.3847/1538-4365/aa5d15",
"issn": "1538-4365",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2017-04",
"series_number": "2",
"volume": "229",
"issue": "2",
"pages": "Art. No. 25"
},
{
"id": "authors:mpsdx-2xf13",
"collection": "authors",
"collection_id": "mpsdx-2xf13",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170127-143159985",
"type": "article",
"title": "PTF1 J082340.04+081936.5: A Hot Subdwarf B Star with a Low-mass White Dwarf Companion in an 87-minute Orbit",
"author": [
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-T"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-J"
},
{
"family_name": "Brooks",
"given_name": "Jared",
"clpid": "Brooks-J"
},
{
"family_name": "Geier",
"given_name": "Stephan",
"orcid": "0000-0002-3948-9339",
"clpid": "Geier-S"
},
{
"family_name": "Marsh",
"given_name": "Tom R.",
"orcid": "0000-0002-2498-7589",
"clpid": "Marsh-T-R"
},
{
"family_name": "Groot",
"given_name": "Paul J.",
"orcid": "0000-0002-4488-726X",
"clpid": "Groot-P-J"
},
{
"family_name": "Bloemen",
"given_name": "Steven",
"clpid": "Bloemen-S"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Bellm",
"given_name": "Eric",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Heber",
"given_name": "Ulrich",
"orcid": "0000-0001-7798-6769",
"clpid": "Heber-U"
},
{
"family_name": "Bildsten",
"given_name": "Lars",
"clpid": "Bildsten-L"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Dyer",
"given_name": "Martin J.",
"clpid": "Dyer-M-J"
},
{
"family_name": "Dhillon",
"given_name": "Vik S.",
"clpid": "Dhillon-V-S"
},
{
"family_name": "Green",
"given_name": "Matthew",
"clpid": "Green-M"
},
{
"family_name": "Irawati",
"given_name": "Puji",
"clpid": "Irawati-P"
},
{
"family_name": "Laher",
"given_name": "Russ",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Littlefair",
"given_name": "Stuart P.",
"orcid": "0000-0001-7221-855X",
"clpid": "Littlefair-S-P"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Steidel",
"given_name": "Charles C.",
"orcid": "0000-0002-4834-7260",
"clpid": "Steidel-C-C"
},
{
"family_name": "Rattansoon",
"given_name": "Somsawat",
"clpid": "Rattansoon-S"
},
{
"family_name": "Pettini",
"given_name": "Max",
"orcid": "0000-0002-5139-4359",
"clpid": "Pettini-M"
}
],
"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.",
"doi": "10.3847/1538-4357/835/2/131",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-02-01",
"series_number": "2",
"volume": "835",
"issue": "2",
"pages": "Art. No. 131"
},
{
"id": "authors:ry2tb-7qb18",
"collection": "authors",
"collection_id": "ry2tb-7qb18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160817-123122578",
"type": "article",
"title": "The IPAC Image Subtraction and Discovery Pipeline for the intermediate Palomar Transient Factory",
"author": [
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Rebbapragada",
"given_name": "Umaa D.",
"orcid": "0000-0002-2560-3495",
"clpid": "Rebbapragada-U-D"
},
{
"family_name": "Doran",
"given_name": "Gary B.",
"clpid": "Doran-G-B"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-A-A"
},
{
"family_name": "Bellm",
"given_name": "Eric",
"orcid": "0000-0001-8018-5348",
"clpid": "Bellm-E-C"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-E-O"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Grillmair",
"given_name": "Carl J.",
"orcid": "0000-0003-4072-169X",
"clpid": "Grillmair-C-J"
},
{
"family_name": "Jackson",
"given_name": "Ed",
"clpid": "Jackson-E"
},
{
"family_name": "Barlow",
"given_name": "Tom",
"clpid": "Barlow-T-A"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Cao",
"given_name": "Yi",
"orcid": "0000-0002-8036-8491",
"clpid": "Cao-Yi"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X",
"clpid": "Cenko-S-B"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "Lisa J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"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.",
"doi": "10.1088/1538-3873/129/971/014002",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2017-01-01",
"series_number": "971",
"volume": "129",
"issue": "971",
"pages": "Art. No. 014002"
},
{
"id": "authors:8amm1-wnt25",
"collection": "authors",
"collection_id": "8amm1-wnt25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160427-105744845",
"type": "article",
"title": "The HerMES submillimetre local and low-redshift luminosity functions",
"author": [
{
"family_name": "Marchetti",
"given_name": "L.",
"orcid": "0000-0003-3948-7621",
"clpid": "Marchetti-L"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We used wide-area surveys over 39 deg2 by the HerMES (Herschel Multi-tiered Extragalactic Survey) collaboration, performed with the Herschel Observatory SPIRE multiwavelength camera, to estimate the low-redshift, 0.02 < z < 0.5, monochromatic luminosity functions (LFs) of galaxies at 250, 350 and 500\u2009\u03bcm. Within this redshift interval, we detected 7087 sources in five independent sky areas, \u223c40 per cent of which have spectroscopic redshifts, while for the remaining objects photometric redshifts were used. The SPIRE LFs in different fields did not show any field-to-field variations beyond the small differences to be expected from cosmic variance. SPIRE flux densities were also combined with Spitzer photometry and multiwavelength archival data to perform a complete spectral energy distribution fitting analysis of SPIRE detected sources to calculate precise k-corrections, as well as the bolometric infrared (IR; 8\u20131000\u2009\u03bcm) LFs and their low-z evolution from a combination of statistical estimators. Integration of the latter prompted us to also compute the local luminosity density and the comoving star formation rate density (SFRD) for our sources, and to compare them with theoretical predictions of galaxy formation models. The LFs show significant and rapid luminosity evolution already at low redshifts, 0.02 < z < 0.2, with L^\u2217_(IR)\u221d(1+z)^(6.0\u00b10.4) and \u03a6^\u2217_(IR) \u221d(1+z)^(\u22122.1\u00b10.4), L^\u2217_(250)\u221d(1+z)5.3\u00b10.2 and \u03a6^\u2217_(250)\u221d(1+z)^(\u22120.6\u00b10.4) estimated using the IR bolometric and the 250\u2009\u03bcm LFs, respectively. Converting our IR LD estimate into an SFRD assuming a standard Salpeter initial mass function and including the unobscured contribution based on the UV dust-uncorrected emission from local galaxies, we estimate an SFRD scaling of SFRD_0 + 0.08z, where SFRD_0 \u2243 (1.9 \u00b1 0.03) \u00d7 10^(\u22122)\u2009[M_\u2299\u2009Mpc^(\u22123)] is our total SFRD estimate at z \u223c 0.02.",
"doi": "10.1093/mnras/stv2717",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2016-02-21",
"series_number": "2",
"volume": "456",
"issue": "2",
"pages": "1999-2023"
},
{
"id": "authors:45erq-90t63",
"collection": "authors",
"collection_id": "45erq-90t63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160205-114722704",
"type": "article",
"title": "The Phase Space of z ~ 1.2 SpARCS Clusters: Using Herschel to Probe Dust Temperature as a Function of Environment and Accretion History",
"author": [
{
"family_name": "Noble",
"given_name": "A. G.",
"orcid": "0000-0003-1832-4137",
"clpid": "Noble-A-G"
},
{
"family_name": "Webb",
"given_name": "T. M. A.",
"clpid": "Webb-T-M-A"
},
{
"family_name": "Yee",
"given_name": "H. K. C.",
"clpid": "Yee-H-K-C"
},
{
"family_name": "Muzzin",
"given_name": "A.",
"orcid": "0000-0002-9330-9108",
"clpid": "Muzzin-A"
},
{
"family_name": "Wilson",
"given_name": "G.",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G-W"
},
{
"family_name": "van der Burg",
"given_name": "R. F. J.",
"clpid": "van-der-Burg-R-F-J"
},
{
"family_name": "Balogh",
"given_name": "M. L.",
"clpid": "Balogh-M-L"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "We present a five-band Herschel study (100\u2013500 \u03bcm) of three galaxy clusters at z ~ 1.2 from the Spitzer Adaptation of the Red-Sequence Cluster Survey. With a sample of 120 spectroscopically confirmed cluster members, we investigate the role of environment on galaxy properties utilizing the projected cluster phase space (line-of-sight velocity versus clustercentric radius), which probes the time-averaged galaxy density to which a galaxy has been exposed. We divide cluster galaxies into phase-space bins of r/r_(200) x \u0394v/\u03c3_v, tracing a sequence of accretion histories in phase space. Stacking optically star-forming cluster members on the Herschel maps, we measure average infrared star formation rates, and, for the first time in high-redshift galaxy clusters, dust temperatures for dynamically distinct galaxy populations\u2014namely, recent infalls and those that were accreted onto the cluster at an earlier epoch. Proceeding from the infalling to virialized (central) regions of phase space, we find a steady decrease in the specific star formation rate and increase in the stellar age of star-forming cluster galaxies. We perform a probability analysis to investigate all acceptable infrared spectral energy distributions within the full parameter space and measure a ~4\u03c3 drop in the average dust temperature of cluster galaxies in an intermediate phase-space bin, compared to an otherwise flat trend with phase space. We suggest one plausible quenching mechanism which may be consistent with these trends, invoking ram-pressure stripping of the warmer dust for galaxies within this intermediate accretion phase.",
"doi": "10.3847/0004-637X/816/2/48",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2016-01-10",
"series_number": "2",
"volume": "816",
"issue": "2",
"pages": "Art. No. 48"
},
{
"id": "authors:cq7sf-cyq31",
"collection": "authors",
"collection_id": "cq7sf-cyq31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151222-105600116",
"type": "article",
"title": "The Star-Formation History of BCGs to z = 1.8 from the SpARCS/SWIRE Survey: Evidence for significant in-situ star formation at high-redshift",
"author": [
{
"family_name": "Webb",
"given_name": "Tracy M. A.",
"clpid": "Webb-T-M-A"
},
{
"family_name": "Muzzin",
"given_name": "Adam",
"orcid": "0000-0002-9330-9108",
"clpid": "Muzzin-A"
},
{
"family_name": "Noble",
"given_name": "Alison",
"orcid": "0000-0003-1832-4137",
"clpid": "Noble-A-G"
},
{
"family_name": "Bonaventura",
"given_name": "Nina",
"clpid": "Bonaventura-N"
},
{
"family_name": "Geach",
"given_name": "James",
"orcid": "0000-0003-4964-4635",
"clpid": "Geach-J-E"
},
{
"family_name": "Hezevah",
"given_name": "Yashar",
"clpid": "Hezevah-Y"
},
{
"family_name": "Lidman",
"given_name": "Chris",
"orcid": "0000-0003-1731-0497",
"clpid": "Lidman-C"
},
{
"family_name": "Wilson",
"given_name": "Gillian",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G"
},
{
"family_name": "Yee",
"given_name": "H. K. C.",
"clpid": "Yee-H-K-C"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "David",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "We present the results of an MIPS-24 \u03bcm study of the brightest cluster galaxies (BCGs) of 535 high-redshift galaxy clusters. The clusters are drawn from the Spitzer Adaptation of the Red-Sequence Cluster Survey, which effectively provides a sample selected on total stellar mass, over 0.2 < z < 1.8 within the Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey fields. Twenty percent, or 106 clusters, have spectroscopically confirmed redshifts, and the rest have redshifts estimated from the color of their red sequence. A comparison with the public SWIRE images detects 125 individual BCGs at 24 \u03bcm \u2273 100 \u03bcJy, or 23%. The luminosity-limited detection rate of BCGs in similar richness clusters (N_(gal) > 12) increases rapidly with redshift. Above z ~ 1, an average of ~20% of the sample have 24 \u03bcm inferred infrared luminosities of L_(IR) > 10^(12) L_\u2299, while the fraction below z ~ 1 exhibiting such luminosities is <1%. The Spitzer-IRAC colors indicate the bulk of the 24 \u03bcm detected population is predominantly powered by star formation, with only 7/125 galaxies lying within the color region inhabited by active galactic nuclei (AGNs). Simple arguments limit the star formation activity to several hundred million years and this may therefore be indicative of the timescale for AGN feedback to halt the star formation. Below redshift z ~ 1, there is not enough star formation to significantly contribute to the overall stellar mass of the BCG population, and therefore BCG growth is likely dominated by dry mergers. Above z ~ 1, however, the inferred star formation would double the stellar mass of the BCGs and is comparable to the mass assembly predicted by simulations through dry mergers. We cannot yet constrain the process driving the star formation for the overall sample, though a single object studied in detail is consistent with a gas-rich merger.",
"doi": "10.1088/0004-637X/814/2/96",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-12-01",
"series_number": "2",
"volume": "814",
"issue": "2",
"pages": "Art. No. 96"
},
{
"id": "authors:m5jzk-nhk16",
"collection": "authors",
"collection_id": "m5jzk-nhk16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151105-132712181",
"type": "article",
"title": "Learning from FITS: Limitations in use in modern astronomical research",
"author": [
{
"family_name": "Thomas",
"given_name": "B.",
"clpid": "Thomas-B"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Good",
"given_name": "J.",
"clpid": "Good-J-C"
},
{
"family_name": "Berriman",
"given_name": "G. B.",
"orcid": "0000-0001-8388-534X",
"clpid": "Berriman-G-B"
},
{
"family_name": "Landry",
"given_name": "W.",
"clpid": "Landry-Walter"
}
],
"abstract": "The Flexible Image Transport System (FITS) standard has been a great boon to astronomy, allowing observatories, scientists and the public to exchange astronomical information easily. The FITS standard, however, is showing its age. Developed in the late 1970s, the FITS authors made a number of implementation choices that, while common at the time, are now seen to limit its utility with modern data. The authors of the FITS standard could not anticipate the challenges which we are facing today in astronomical computing. Difficulties we now face include, but are not limited to, addressing the need to handle an expanded range of specialized data product types (data models), being more conducive to the networked exchange and storage of data, handling very large datasets, and capturing significantly more complex metadata and data relationships.\n\nThere are members of the community today who find some or all of these limitations unworkable, and have decided to move ahead with storing data in other formats. If this fragmentation continues, we risk abandoning the advantages of broad interoperability, and ready archivability, that the FITS format provides for astronomy. In this paper we detail some selected important problems which exist within the FITS standard today. These problems may provide insight into deeper underlying issues which reside in the format and we provide a discussion of some lessons learned. It is not our intention here to prescribe specific remedies to these issues; rather, it is to call attention of the FITS and greater astronomical computing communities to these problems in the hope that it will spur action to address them.",
"doi": "10.1016/j.ascom.2015.01.009",
"issn": "2213-1337",
"publisher": "Elsevier",
"publication": "Astronomy and Computing",
"publication_date": "2015-09",
"volume": "12",
"pages": "133-145"
},
{
"id": "authors:bs4hv-dsd49",
"collection": "authors",
"collection_id": "bs4hv-dsd49",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140902-091644578",
"type": "article",
"title": "SPIRE point source photometry: within the Herschel interactive processing environment (HIPE)",
"author": [
{
"family_name": "Pearson",
"given_name": "Chris",
"orcid": "0000-0001-6139-649X",
"clpid": "Pearson-C-P"
},
{
"family_name": "Lim",
"given_name": "Tanya",
"clpid": "Lim-Tanya-L"
},
{
"family_name": "North",
"given_name": "Chris",
"clpid": "North-C"
},
{
"family_name": "Bendo",
"given_name": "George",
"clpid": "Bendo-G"
},
{
"family_name": "Conversi",
"given_name": "Luca",
"clpid": "Conversi-L"
},
{
"family_name": "Dowell",
"given_name": "Darren",
"clpid": "Dowell-D"
},
{
"family_name": "Griffin",
"given_name": "Matt",
"clpid": "Griffin-M"
},
{
"family_name": "Jin",
"given_name": "Terry",
"clpid": "Jin-Terry"
},
{
"family_name": "Laporte",
"given_name": "Nicolas",
"clpid": "Laporte-N"
},
{
"family_name": "Papageorgiou",
"given_name": "Andreas",
"orcid": "0000-0002-3039-9257",
"clpid": "Papageorgiou-A"
},
{
"family_name": "Schulz",
"given_name": "Bernhard",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "Dave",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "Anthony J.",
"clpid": "Smith-A-J"
},
{
"family_name": "Xu",
"given_name": "Kevin",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
}
],
"abstract": "The different algorithms appropriate for point source photometry on data from the SPIRE instrument on-board the Herschel Space Observatory, within the Herschel Interactive Processing Environment (HIPE) are compared. Point source photometry of a large ensemble of standard calibration stars and dark sky observations is carried out using the 4 major methods within HIPE: SUSSEXtractor, DAOphot, the SPIRE Timeline Fitter and simple Aperture Photometry. Colour corrections and effective beam areas as a function of the assumed source spectral index are also included to produce a large number of photometric measurements per individual target, in each of the 3 SPIRE bands (250, 350, 500\u03bcm), to examine both the accuracy and repeatability of each of the 4 algorithms. It is concluded that for flux densities down to the level of 30mJy that the SPIRE Timeline Fitter is the method of choice. However, at least in the 250 and 350\u03bcm bands, all 4 methods provide photometric repeatability better than a few percent down to at approximately 100mJy. The DAOphot method appears in many cases to have a systematic offset of \u223c8 % in all SPIRE bands which may be indicative of a sub-optimal aperture correction. In general, aperture photometry is the least reliable method, i.e. largest scatter between observations, especially in the longest wavelength band. At the faintest fluxes, <30mJy, SUSSEXtractor or DAOphot provide a better alternative to the Timeline Fitter.",
"doi": "10.1007/s10686-013-9351-4",
"issn": "0922-6435",
"publisher": "Springer",
"publication": "Experimental Astronomy",
"publication_date": "2014-07",
"series_number": "2",
"volume": "37",
"issue": "2",
"pages": "175-194"
},
{
"id": "authors:d44q1-ks913",
"collection": "authors",
"collection_id": "d44q1-ks913",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140131-080059273",
"type": "article",
"title": "HerMES: Candidate High-redshift Galaxies Discovered with Herschel/SPIRE",
"author": [
{
"family_name": "Dowell",
"given_name": "C. Darren",
"clpid": "Dowell-C-D"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Riechers",
"given_name": "D.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Sayers",
"given_name": "J.",
"orcid": "0000-0002-8213-3784",
"clpid": "Sayers-Jack"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 \u03bcm flux densities to search for red sources. We apply this method to 21 deg^2 of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e.g., 850 \u03bcm) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S_(500\u03bcm) \u2265 30 mJy), red Herschel sources is 3.3 \u00b1 0.8 deg^(\u20132). This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z ~ 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction.",
"doi": "10.1088/0004-637X/780/1/75",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2014-01-01",
"series_number": "1",
"volume": "780",
"issue": "1",
"pages": "Art. No. 75"
},
{
"id": "authors:0xgjc-9j766",
"collection": "authors",
"collection_id": "0xgjc-9j766",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130904-083919768",
"type": "article",
"title": "Flux calibration of the Herschel-SPIRE photometer",
"author": [
{
"family_name": "Bendo",
"given_name": "G. J.",
"clpid": "Bendo-G-J"
},
{
"family_name": "Griffin",
"given_name": "M. J.",
"clpid": "Griffin-M-J"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Conversi",
"given_name": "L.",
"clpid": "Conversi-L"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Lim",
"given_name": "T.",
"clpid": "Lim-Tanya-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "North",
"given_name": "C. E.",
"clpid": "North-C-E"
},
{
"family_name": "Papageorgiou",
"given_name": "A.",
"orcid": "0000-0002-3039-9257",
"clpid": "Papageorgiou-A"
},
{
"family_name": "Pearson",
"given_name": "C. P.",
"orcid": "0000-0001-6139-649X",
"clpid": "Pearson-C-P"
},
{
"family_name": "Pohlen",
"given_name": "M.",
"clpid": "Pohlen-M"
},
{
"family_name": "Polehampton",
"given_name": "E. T.",
"clpid": "Polehampton-E-T"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sibthorpe",
"given_name": "B.",
"clpid": "Sibthorpe-B"
},
{
"family_name": "Spencer",
"given_name": "L. D.",
"clpid": "Spencer-L-D"
},
{
"family_name": "Swinyard",
"given_name": "B. M.",
"clpid": "Swinyard-B-M"
},
{
"family_name": "Valtchanov",
"given_name": "I.",
"orcid": "0000-0001-9930-7886",
"clpid": "Valtchanov-I"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
}
],
"abstract": "We describe the procedure used to flux calibrate the three-band submillimetre photometer in the Spectral and Photometric Imaging Receiver instrument on the Herschel Space Observatory. This includes the equations describing the calibration scheme, a justification for using Neptune as the primary calibration source, a description of the observations and data processing procedures used to derive flux calibration parameters (for converting from voltage to flux density) for every bolometer in each array, an analysis of the error budget in the flux calibration for the individual bolometers and tests of the flux calibration on observations of primary and secondary calibrators. The procedure for deriving the flux calibration parameters is divided into two parts. In the first part, we use observations of astronomical sources in conjunction with the operation of the photometer internal calibration source to derive the unscaled derivatives of the flux calibration curves. To scale the calibration curves in Jy beam^(\u22121) V^(\u22121), we then use observations of Neptune in which the beam of each bolometer is mapped using a very fine scan pattern. The total instrumental uncertainties in the flux calibration for most individual bolometers is \u223c0.5\u2009 per\u2009cent, although a few bolometers have uncertainties of \u223c1\u20135\u2009 per\u2009cent because of issues with the Neptune observations. Based on application of the flux calibration parameters to Neptune observations performed using typical scan map observing modes, we determined that measurements from each array as a whole have instrumental uncertainties of 1.5\u2009 per\u2009cent. This is considerably less than the absolute calibration uncertainty associated with the model of Neptune, which is estimated at 4 \u2009per\u2009cent.",
"doi": "10.1093/mnras/stt948",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2013-08",
"series_number": "4",
"volume": "433",
"issue": "4",
"pages": "3062-3078"
},
{
"id": "authors:khv1r-jcd61",
"collection": "authors",
"collection_id": "khv1r-jcd61",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130815-100959854",
"type": "article",
"title": "HerMES: Cosmic Infrared Background Anisotropies and the Clustering of Dusty Star-forming Galaxies",
"author": [
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
}
],
"abstract": "We present measurements of the auto- and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 \u03bcm (1200, 860, and 600 GHz) from observations totaling ~70 deg^2 made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy \u03b4I/I = 14% \u00b1 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and nonlinear (1-halo) regimes; and that the transition from the 2- to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k_\u03b8 ~ 0.10-0.12 arcmin^\u20131 (\u2113 ~ 2160-2380), from 250 to 500 \u03bcm. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources\u2014suggesting that some fraction of the more luminous sources occupy more massive halos as satellites, or are possibly close pairs. We measure the cross-correlation power spectra between bands, finding that bands which are farthest apart are the least correlated, as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked. In the second part of the paper, we attempt to interpret the measurements in the framework of the halo model. With the aim of fitting simultaneously with one model the power spectra, number counts, and absolute CIB level in all bands, we find that this is achievable by invoking a luminosity-mass relationship, such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines toward lower and higher mass halos. Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity, z ~ 1-3, is log(M_peak/M_\u2609) ~ 12.1 \u00b1 0.5, and that the minimum halo mass to host infrared galaxies is log(M_min/M_\u2609) ~ 10.1 \u00b1 0.6.",
"doi": "10.1088/0004-637X/772/1/77",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-07-20",
"series_number": "1",
"volume": "772",
"issue": "1",
"pages": "Art. No. 77"
},
{
"id": "authors:e13v9-n4q19",
"collection": "authors",
"collection_id": "e13v9-n4q19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130730-104305133",
"type": "article",
"title": "The Herschel PEP/HerMES luminosity function \u2013 I. Probing the evolution of PACS selected Galaxies to z \u2243 4",
"author": [
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056",
"clpid": "Gruppioni-C"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We exploit the deep and extended far-IR data sets (at 70, 100 and 160 \u03bcm) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 \u03bcm, to derive the evolution of the rest-frame 35-, 60-, 90- and total infrared (IR) luminosity functions (LFs) up to z \u223c 4. We detect very strong luminosity evolution for the total IR LF (L_IR \u221d (1 + z)^3.55 \u00b1 0.10) up to z \u223c 2, and \u221d (1 + z)^(1.62 \u00b1 0.51) at 2 < z \u2272 4) combined with a density evolution (\u221d(1 + z)^(\u22120.57 \u00b1 0.22) up to z \u223c 1 and \u221d (1 + z)^(\u22123.92 \u00b1 0.34) at 1 < z \u2272 4). In agreement with previous findings, the IR luminosity density (\u03c1IR) increases steeply to z \u223c 1, then flattens between z \u223c 1 and z \u223c 3 to decrease at z \u2273 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to \u03c1IR. Galaxies occupying the well-established SFR\u2013stellar mass main sequence (MS) are found to dominate both the total IR LF and \u03c1IR at all redshifts, with the contribution from off-MS sources (\u22650.6 dex above MS) being nearly constant (\u223c20 per cent of the total \u03c1IR) and showing no significant signs of increase with increasing z over the whole 0.8 < z < 2.2 range. Sources with mass in the range 10 \u2264 log(M/M_\u2299) \u2264 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (\u22732) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies.",
"doi": "10.1093/mnras/stt308",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2013-06-11",
"series_number": "1",
"volume": "432",
"issue": "1",
"pages": "23-52"
},
{
"id": "authors:vrdmq-8pg94",
"collection": "authors",
"collection_id": "vrdmq-8pg94",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130709-110259992",
"type": "article",
"title": "HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background due to Galaxy Cluster Gravitational Lensing",
"author": [
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
}
],
"abstract": "We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I_250 \u00b5m > 0.69^(+0.03)_(-0.03) (stat)^(+0.11)_(-0.06)(sys.) MJy sr^(-1), with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB.",
"doi": "10.1088/2041-8205/769/2/L31",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2013-06-01",
"series_number": "2",
"volume": "769",
"issue": "2",
"pages": "Art. No. L31"
},
{
"id": "authors:kzms5-yq422",
"collection": "authors",
"collection_id": "kzms5-yq422",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-134204476",
"type": "article",
"title": "The Herschel census of infrared SEDs through cosmic time",
"author": [
{
"family_name": "Symeonidis",
"given_name": "M.",
"clpid": "Symeonidis-M"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Capak",
"given_name": "P. L.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-P"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS, GOODS-S and GOODS-N, we examine the dust properties of infrared (IR)-luminous (L_IR > 10^10 L_\u2299) galaxies at 0.1 < z < 2 and determine how these evolve with cosmic time. The unique angle of this work is the rigorous analysis of survey selection effects, making this the first study of the star-formation-dominated, IR-luminous population within a framework almost entirely free of selection biases. We find that IR-luminous galaxies have spectral energy distributions (SEDs) with broad far-IR peaks characterized by cool/extended dust emission and average dust temperatures in the 25\u201345 K range. Hot (T > 45\u2009K) SEDs and cold (T < 25\u2009K), cirrus-dominated SEDs are rare, with most sources being within the range occupied by warm starbursts such as M82 and cool spirals such as M51. We observe a luminosity\u2013temperature (L-T) relation, where the average dust temperature of log [L_IR/L_\u2299] \u223c 12.5 galaxies is about 10 K higher than that of their log [L_IR/L_\u2299] \u223c 10.5 counterparts. However, although the increased dust heating in more luminous systems is the driving factor behind the L-T relation, the increase in dust mass and/or starburst size with luminosity plays a dominant role in shaping it. Our results show that the dust conditions in IR-luminous sources evolve with cosmic time: at high redshift, dust temperatures are on average up to 10 K lower than what is measured locally (z \u2272 0.1). This is manifested as a flattening of the L-T relation, suggesting that (ultra)luminous infrared galaxies [(U)LIRGs] in the early Universe are typically characterized by a more extended dust distribution and/or higher dust masses than local equivalent sources. Interestingly, the evolution in dust temperature is luminosity dependent, with the fraction of LIRGs with T < 35 K showing a two-fold increase from z \u223c 0 to z \u223c 2, whereas that of ULIRGs with T < 35 K shows a six-fold increase. Our results suggest a greater diversity in the IR-luminous population at high redshift, particularly for ULIRGs.",
"doi": "10.1093/mnras/stt330",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2013-05-21",
"series_number": "3",
"volume": "431",
"issue": "3",
"pages": "2317-2340"
},
{
"id": "authors:w0brf-s4j82",
"collection": "authors",
"collection_id": "w0brf-s4j82",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130205-093943506",
"type": "article",
"title": "HerMES: Candidate Gravitationally Lensed Galaxies and Lensing Statistics at Submillimeter Wavelengths",
"author": [
{
"family_name": "Wardlow",
"given_name": "Julie L.",
"orcid": "0000-0003-2376-8971",
"clpid": "Wardlow-J-L"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C"
},
{
"family_name": "Carpenter",
"given_name": "J. M.",
"orcid": "0000-0003-2251-0602",
"clpid": "Carpenter-J-M"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Riechers",
"given_name": "D.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Scoville",
"given_name": "N.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present a list of 13 candidate gravitationally lensed submillimeter galaxies (SMGs) from 95 deg^2 of the Herschel Multi-tiered Extragalactic Survey, a surface density of 0.14 \u00b1 0.04 deg^(\u20132). The selected sources have 500 \u03bcm flux densities (S_(500)) greater than 100 mJy. Gravitational lensing is confirmed by follow-up observations in 9 of the 13 systems (70%), and the lensing status of the four remaining sources is undetermined. We also present a supplementary sample of 29 (0.31 \u00b1 0.06 deg^(\u20132)) gravitationally lensed SMG candidates with S_(500) = 80-100 mJy, which are expected to contain a higher fraction of interlopers than the primary candidates. The number counts of the candidate lensed galaxies are consistent with a simple statistical model of the lensing rate, which uses a foreground matter distribution, the intrinsic SMG number counts, and an assumed SMG redshift distribution. The model predicts that 32%-74% of our S_(500) \u2265 100 mJy candidates are strongly gravitationally lensed (\u03bc \u2265 2), with the brightest sources being the most robust; this is consistent with the observational data. Our statistical model also predicts that, on average, lensed galaxies with S_(500) = 100 mJy are magnified by factors of ~9, with apparently brighter galaxies having progressively higher average magnification, due to the shape of the intrinsic number counts. 65% of the sources are expected to have intrinsic 500 \u03bcm flux densities less than 30 mJy. Thus, samples of strongly gravitationally lensed SMGs, such as those presented here, probe below the nominal Herschel detection limit at 500 \u03bcm. They are good targets for the detailed study of the physical conditions in distant dusty, star-forming galaxies, due to the lensing magnification, which can lead to spatial resolutions of ~0.\"01 in the source plane.",
"doi": "10.1088/0004-637X/762/1/59",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-01-01",
"series_number": "1",
"volume": "762",
"issue": "1",
"pages": "Art. No. 59"
},
{
"id": "authors:a49bh-jb229",
"collection": "authors",
"collection_id": "a49bh-jb229",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121218-105629072",
"type": "article",
"title": "Cosmic Evolution of Star Formation Enhancement in Close Major-merger Galaxy Pairs Since z = 1",
"author": [
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Aussel",
"given_name": "H.",
"orcid": "0000-0002-1371-5705",
"clpid": "Aussel-Herve"
},
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Conley",
"given_name": "A.",
"clpid": "Conley-A"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Elbaz",
"given_name": "D.",
"orcid": "0000-0002-7631-647X",
"clpid": "Elbaz-David"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Le Floc'h",
"given_name": "E.",
"clpid": "Le-Floc'h-Emeric"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Magnelli",
"given_name": "B.",
"orcid": "0000-0002-6777-6490",
"clpid": "Magnelli-B"
},
{
"family_name": "Marsden",
"given_name": "G.",
"clpid": "Marsden-G"
},
{
"family_name": "Oliver",
"given_name": "S. J.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"clpid": "Pozzi-F"
},
{
"family_name": "Riguccini",
"given_name": "L.",
"clpid": "Riguccini-L"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Scoville",
"given_name": "N.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Wang",
"given_name": "L.",
"clpid": "Wang-Lingyu"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The infrared (IR) emission of \"M_* galaxies\" (10^(10.4) \u2264 M_(star) \u2264 10^(11.0) M_\u2609) in galaxy pairs, derived using data obtained in Herschel (PEP/HerMES) and Spitzer (S-COSMOS) surveys, is compared to that of single-disk galaxies in well-matched control samples to study the cosmic evolution of the star formation enhancement induced by galaxy-galaxy interaction. Both the mean IR spectral energy distribution and mean IR luminosity of star-forming galaxies (SFGs) in SFG+SFG (S+S) pairs in the redshift bin of 0.6 < z < 1 are consistent with no star formation enhancement. SFGs in S+S pairs in a lower redshift bin of 0.2 < z < 0.6 show marginal evidence for a weak star formation enhancement. Together with the significant and strong sSFR enhancement shown by SFGs in a local sample of S+S pairs (obtained using previously published Spitzer observations), our results reveal a trend for the star formation enhancement in S+S pairs to decrease with increasing redshift. Between z = 0 and z = 1, this decline of interaction-induced star formation enhancement occurs in parallel with the dramatic increase (by a factor of ~10) of the sSFR of single SFGs, both of which can be explained by the higher gas fraction in higher-z disks. SFGs in mixed pairs (S+E pairs) do not show any significant star formation enhancement at any redshift. The difference between SFGs in S+S pairs and in S+E pairs suggests a modulation of the sSFR by the intergalactic medium (IGM) in the dark matter halos hosting these pairs.",
"doi": "10.1088/0004-637X/760/1/72",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2012-11-20",
"series_number": "1",
"volume": "760",
"issue": "1",
"pages": "Art. No. 72"
},
{
"id": "authors:vdjgt-62z57",
"collection": "authors",
"collection_id": "vdjgt-62z57",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120927-094554573",
"type": "article",
"title": "The Herschel Multi-tiered Extragalactic Survey: HerMES",
"author": [
{
"family_name": "Oliver",
"given_name": "S. J.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N. Y.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Marshall",
"given_name": "J.",
"clpid": "Marshall-J"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling \u223c380\u2009deg^2. Fields range in size from 0.01 to \u223c20\u2009deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500\u2009\u03bcm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160\u2009\u03bcm), with an additional wider component of 270\u2009deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. \n\nThe survey will detect of the order of 100\u2009000 galaxies at 5\u03c3 in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. \n\nThis paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.",
"doi": "10.1111/j.1365-2966.2012.20912.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2012-08-11",
"series_number": "3",
"volume": "424",
"issue": "3",
"pages": "1614-1635"
},
{
"id": "authors:h7c7n-ksg79",
"collection": "authors",
"collection_id": "h7c7n-ksg79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120801-084702053",
"type": "article",
"title": "HerMES: deep number counts at 250 \u03bcm, 350 \u03bcm and 500 \u03bcm\n in the COSMOS and GOODS-N fields and the build-up\n of the cosmic infrared background",
"author": [
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Aims. The Spectral and Photometric Imaging REceiver (SPIRE) onboard the Herschel space telescope has provided confusion limited maps of deep fields at 250 \u03bcm, 350 \u03bcm, and 500 \u03bcm, as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). Unfortunately, due to confusion, only a small fraction of the cosmic infrared background (CIB) can be resolved into individually-detected sources. Our goal is to produce deep galaxy number counts and redshift distributions below the confusion limit at SPIRE wavelengths (~20 mJy), which we then use to place strong constraints on the origins of the cosmic infrared background and on models of galaxy evolution.\nMethods. We individually extracted the bright SPIRE sources (>20 mJy) in the COSMOS field with a method using the positions, the flux densities, and the redshifts of the 24 \u03bcm sources as a prior, and derived the number counts and redshift distributions of the bright SPIRE sources. For fainter SPIRE sources (<20 mJy), we reconstructed the number counts and the redshift distribution below the confusion limit using the deep 24 \u03bcm catalogs associated with photometric redshift and information provided by the stacking of these sources into the deep SPIRE maps of the GOODS-N and COSMOS fields. Finally, by integrating all these counts, we studied the contribution of the galaxies to the CIB as a function of their flux density and redshift.\nResults. Through stacking, we managed to reconstruct the source counts per redshift slice down to ~2 mJy in the three SPIRE bands, which lies about a factor 10 below the 5\u03c3 confusion limit. Our measurements place tight constraints on source population models. None of the pre-existing models are able to reproduce our results at better than 3-\u03c3. Finally, we extrapolate our counts to zero flux density in order to derive an estimate of the total contribution of galaxies to the CIB, finding 10.1_(-2.3)^(+2.6)\u2009nW\u2009m^(-2)\u2009sr^(-1), 6.5_(-1.6)^(+1.7)\u2009nW\u2009m^(-2)\u2009sr^(-1), and 2.8_(-0.8)^(+0.9)\u2009nW\u2009m^(-2)\u2009sr^(-1) at 250 \u03bcm, 350 \u03bcm, and 500 \u03bcm, respectively. These values agree well with FIRAS absolute measurements, suggesting our number counts and their extrapolation are sufficient to explain the CIB. We find that half of the CIB is emitted at z = 1.04, 1.20, and 1.25, respectively. Finally, combining our results with other works, we estimate the energy budget contained in the CIB between 8 \u03bcm and 1000 \u03bcm: 26_(-3)^(+7)\u2009nW\u2009m^(-2)\u2009sr^(-1).",
"doi": "10.1051/0004-6361/201118698",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2012-06",
"volume": "542",
"pages": "Art. No. A58"
},
{
"id": "authors:xy831-kwb94",
"collection": "authors",
"collection_id": "xy831-kwb94",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120606-132737240",
"type": "article",
"title": "The suppression of star formation by powerful active galactic nuclei",
"author": [
{
"family_name": "Page",
"given_name": "M. J.",
"orcid": "0000-0002-6689-6271",
"clpid": "Page-M-J"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths. Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2\u20136 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10^(44) ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow, expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time.",
"doi": "10.1038/nature11096",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2012-05-10",
"series_number": "7397",
"volume": "485",
"issue": "7397",
"pages": "213-216"
},
{
"id": "authors:tn1ya-87q47",
"collection": "authors",
"collection_id": "tn1ya-87q47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120328-085250071",
"type": "article",
"title": "The Herschel Multi-tiered Extragalactic Survey: SPIRE\u2013mm photometric redshifts",
"author": [
{
"family_name": "Roseboom",
"given_name": "I. G.",
"clpid": "Roseboom-I-G"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We investigate the potential of submm\u2013mm and submm\u2013mm\u2013radio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500\u03bcm by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm sources with reliable radio identifications in the Great Observatories Origins Deep Survey North and Lockman Hole North fields, 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm sources are adequately described by a modified blackbody with constant optical depth \u03c4= (\u03bd/nu_0)^\u03b2, where \u03b2=+1.8 and \u03bd_0=c/100 \u03bcm. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation, we derive photometric redshift estimates for the 46 SPIRE-detected mm sources. Testing against the 22 sources with known spectroscopic or good quality optical/near-IR photometric redshifts, we find submm/mm photometric redshifts offer a redshift accuracy of |\u0394z|/(1 +z) = 0.16 (\u3008|\u0394z|\u3009= 0.51). Including constraints from the radio\u2013far-IR correlation, the accuracy is improved to |\u0394z|/(1 +z) = 0.15 (\u3008|\u0394z|\u3009= 0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to \u223c 850 \u03bcm selected samples.",
"doi": "10.1111/j.1365-2966.2011.19827.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2012-02",
"series_number": "4",
"volume": "419",
"issue": "4",
"pages": "2758-2773"
},
{
"id": "authors:b4b0d-akx18",
"collection": "authors",
"collection_id": "b4b0d-akx18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111004-113055775",
"type": "article",
"title": "Modeling of the HerMES Submillimeter Source Lensed by a Dark Matter Dominated Foreground Group of Galaxies",
"author": [
{
"family_name": "Gavazzi",
"given_name": "R.",
"clpid": "Gavazzo-R"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bradford",
"given_name": "C. M.",
"orcid": "0000-0001-5261-7094",
"clpid": "Bradford-C-M"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C"
},
{
"family_name": "Djorgovski",
"given_name": "S. G.",
"orcid": "0000-0002-0603-3087",
"clpid": "Djorgovski-S-G"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Fu",
"given_name": "H.",
"orcid": "0000-0001-9608-6395",
"clpid": "Fu-Hai"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Mahabal",
"given_name": "A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Murphy",
"given_name": "E.",
"orcid": "0000-0001-7089-7325",
"clpid": "Murphy-E-J"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Riechers",
"given_name": "D.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"family_name": "Zmuidzinas",
"given_name": "J.",
"orcid": "0000-0002-3330-5439",
"clpid": "Zmuidzinas-J"
}
],
"abstract": "We present the results of a gravitational lensing analysis of the bright z_s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be \u03bc = 10.9 \u00b1 0.7. We measure the half-light radius R_(eff) of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R_(eff),* = [2.0 \u00b1 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R_(eff,gas) = [1.1 \u00b1 0.5] kpc) by mapping back in the source plane the CO (J = 5 \u2192 4) transition line emission. The lens modeling yields a relatively large Einstein radius R_(Ein) = 4\".10 \u00b1 0\".02, corresponding to a deflector velocity dispersion of [483 \u00b1 16] km s^(\u20131). This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z_l ~ 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f_(dm)(< R_(Ein)) ~ 80%. This fraction reduces to f_(dm)(< R_(eff,G1) \u2243 4.5 kpc) ~ 47% within the effective radius of the main deflecting galaxy of stellar mass M_(*,G1) = [8.5 \u00b1 1.6] \u00d7 10^(11) M_\u2609. At this smaller scale the dark matter fraction is consistent with results already found for massive lensing ellipticals at z ~ 0.2 from the Sloan Lens ACS Survey.",
"doi": "10.1088/0004-637X/738/2/125",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2011-09-10",
"series_number": "2",
"volume": "738",
"issue": "2",
"pages": "Art. No. 125"
},
{
"id": "authors:2qa3f-jy958",
"collection": "authors",
"collection_id": "2qa3f-jy958",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110824-083050070",
"type": "article",
"title": "Discovery of a Multiply Lensed Submillimeter Galaxy in Early HerMES Herschel/SPIRE Data",
"author": [
{
"family_name": "Conley",
"given_name": "A.",
"clpid": "Conley-A"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bradford",
"given_name": "C. M.",
"orcid": "0000-0001-5261-7094",
"clpid": "Bradford-C-M"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C"
},
{
"family_name": "Carpenter",
"given_name": "J. M.",
"orcid": "0000-0003-2251-0602",
"clpid": "Carpenter-J-M"
},
{
"family_name": "Djorgovski",
"given_name": "S. G.",
"orcid": "0000-0002-0603-3087",
"clpid": "Djorgovski-S-G"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Fu",
"given_name": "H.",
"orcid": "0000-0001-9608-6395",
"clpid": "Fu-Hai"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Mahabal",
"given_name": "A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Murphy",
"given_name": "E.",
"orcid": "0000-0001-7089-7325",
"clpid": "Murphy-E-J"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Riechers",
"given_name": "D.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"family_name": "Zmuidzinas",
"given_name": "J.",
"orcid": "0000-0002-3330-5439",
"clpid": "Zmuidzinas-J"
}
],
"abstract": "We report the discovery of a bright (f(250 \u03bcm)>400 mJy), multiply lensed submillimeter galaxy HERMES J105751.1+573027 in Herschel/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880 \u03bcm Submillimeter Array observations resolve at least four images with a large separation of ~9\". A high-resolution adaptive optics K_p image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of z = 2.9575, and the lensing model gives a total magnification of \u03bc ~ 11 \u00b1 1. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified blackbody fit with an unusually warm dust temperature, 88 \u00b1 3 K. We derive a lensing-corrected total IR luminosity of (1.43 \u00b1 0.09) \u00d7 10^(13) L_\u2609, implying a star formation rate of ~2500 M_\u2609 yr^(\u20131). However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early Herschel data, and many more are expected as additional data are collected.",
"doi": "10.1088/2041-8205/732/2/L35",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2011-05-10",
"series_number": "2",
"volume": "732",
"issue": "2",
"pages": "Art. No. L35"
},
{
"id": "authors:k5qvx-3ng62",
"collection": "authors",
"collection_id": "k5qvx-3ng62",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110531-151240573",
"type": "article",
"title": "HerMES: SPIRE emission from radio-selected active galactic nuclei",
"author": [
{
"family_name": "Seymour",
"given_name": "N.",
"orcid": "0000-0003-3506-5536",
"clpid": "Seymour-N"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We examine the rest-frame far-infrared emission from powerful radio sources with 1.4-GHz luminosity densities of\u200225 \u2264 log(L_(1.4)/W Hz^(\u22121)) \u2264 26.5\u2002in the extragalactic\u2002Spitzer\u2002First Look Survey field. We combine\u2002Herschel/SPIRE flux densities with\u2002Spitzer/Infrared Array Camera and Multiband Imaging Photometer for\u2002Spitzer\u2002infrared data to obtain total (8-1000 \u00b5m) infrared luminosities for these radio sources. We separate our sources into a moderate,\u20020.4 <\u2002z\u2002< 0.9, and a high,\u20021.2 <\u2002z\u2002< 3.0, redshift sub-sample and we use\u2002Spitzer\u2002observations of a\u2002z\u2002< 0.1\u20023CRR sample as a local comparison. By comparison to numbers from the Square Kilometre Array (SKA) Simulated Skies, we find that our moderate-redshift sample is complete and our high-redshift sample is 14 per cent complete. We constrain the ranges of mean star formation rates (SFRs) to be 3.4\u20134.2, 18\u201341 and\u200280\u2013581 M_\u2299 yr^(\u22121)\u2002for the local, moderate- and high-redshift samples, respectively. Hence, we observe an increase in the mean SFR with increasing redshift which we can parametrize as\u2002\u223c(1 +\u2002z)^Q, where\u2002Q\u2002= 4.2 \u00b1 0.8. However, we observe no trends of mean SFR with radio luminosity within the moderate- or high-redshift bins. We estimate that radio-loud active galactic nuclei (AGN) in the high-redshift sample contribute 0.1\u20130.5 per cent to the total SFR density at that epoch. Hence, if all luminous starbursts host radio-loud AGN we infer a radio-loud phase duty cycle of 0.001\u20130.005.",
"doi": "10.1111/j.1365-2966.2011.18253.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2011-05",
"series_number": "3",
"volume": "413",
"issue": "3",
"pages": "1777-1786"
},
{
"id": "authors:gv0gy-paj42",
"collection": "authors",
"collection_id": "gv0gy-paj42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110314-094552984",
"type": "article",
"title": "Submillimetre galaxies reside in dark matter haloes with masses greater than 3\u2009\u00d7\u200910^(11) solar masses",
"author": [
{
"family_name": "Amblard",
"given_name": "Alexandre",
"clpid": "Amblard-A"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L-R"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The extragalactic background light at far-infrared wavelengths comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum\nof brightness fluctuations at 250, 350 and 500 \u00b5m. From this excess, we find that submillimetre galaxies are located in darkmatter haloes with a minimum mass, M_(min), such that log_(10)[M_(min)/M_\u2299] = 11.5^(+0.7)_(-0.2) at 350 \u00b5m, where M_\u2299 is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation.",
"doi": "10.1038/nature09771",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2011-02-24",
"series_number": "7335",
"volume": "470",
"issue": "7335",
"pages": "510-512"
},
{
"id": "authors:e7cgw-0cp42",
"collection": "authors",
"collection_id": "e7cgw-0cp42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101222-113213930",
"type": "article",
"title": "Mid-infrared spectroscopy of Spitzer-selected ultra-luminous starbursts at z ~ 2",
"author": [
{
"family_name": "Fiolet",
"given_name": "N.",
"clpid": "Fiolet-N"
},
{
"family_name": "Omont",
"given_name": "A.",
"orcid": "0000-0002-4721-3922",
"clpid": "Omont-A"
},
{
"family_name": "Lagache",
"given_name": "G.",
"orcid": "0000-0003-1492-2519",
"clpid": "Lagache-Guilaine"
},
{
"family_name": "Bertincourt",
"given_name": "B.",
"clpid": "Bertincourt-B"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Baker",
"given_name": "A. J.",
"clpid": "Baker-A-J"
},
{
"family_name": "Beelen",
"given_name": "A.",
"clpid": "Beelen-A"
},
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Boulanger",
"given_name": "F.",
"clpid": "Boulanger-F"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Kov\u00e1cs",
"given_name": "A.",
"clpid": "Kov\u00e1cs-A"
},
{
"family_name": "Lonsdale",
"given_name": "A.",
"clpid": "Lonsdale-A"
},
{
"family_name": "Owen",
"given_name": "F.",
"clpid": "Owen-F-N"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "Context. Spitzer's wide-field surveys and followup capabilities have allowed a new breakthrough in mid-IR spectroscopy up to redshifts \u2265 2, especially for 24 \u03bcm detected sources.\n\nAims. We want to study the mid-infrared properties and the starburst and AGN contributions, of 24 \u03bcm sources at z ~ 2, through analysis of mid-infrared spectra combined with millimeter, radio, and infrared photometry. Mid-infrared spectroscopy allows us to recover accurate redshifts.\n\nMethods. A complete sample of 16 Spitzer-selected sources (ULIRGs) believed to be starbursts at z ~ 2 (\"5.8 \u03bcm-peakers\") was selected in the (0.5 deg^2) J1064+56 SWIRE Lockman Hole field (\"Lockman-North\"). These sources have S_(24\u00b5) > 0.5 mJy, a stellar emission peak redshifted to 5.8 \u03bcm, and r'_(Vega) > 23. The entire sample was observed with the low resolution units of the Spitzer/IRS infrared spectrograph. These sources have 1.2 mm observations with IRAM 30 m/MAMBO and very deep 20 cm observations from the VLA. Nine of our sources also benefit from 350 \u03bcm observation and detection from CSO/SHARC-II. All these data were jointly analyzed.\n\nResults. The entire sample shows good quality IRS spectra dominated by strong PAH features. The main PAH features at 6.2, 7.7, 8.6, and 11.3 \u03bcm have high S/N average luminosities of 2.90\u00b10.31, 10.38\u00b11.09, 3.62\u00b10.27, and 2.29\u00b10.26\u00d710^(10) L_\u2609, respectively. Thanks to their PAH spectra, we derived accurate redshifts spanning from 1.750 to 2.284. The average of these redshifts is 2.017\u00b10.038. This result confirms that the selection criteria of \"5.8 \u03bcm-peakers\" associated with a strong detection at 24 \u03bcm are reliable to select sources at z ~ 2. We have analyzed the different correlations between PAH emission and infrared, millimeter, and radio emissions. Practically all our sources are strongly dominated by starburst emission, with only one source showing an important AGN contribution. We have also defined two subsamples based on the equivalent width at 7.7 \u03bcm to investigate AGN contributions.\n\nConclusions. Our sample contains strong starbursts and represents a particularly 24 \u03bcm-bright class of SMGs. The very good correlation between PAH and far-IR luminosities is now confirmed in high-z starburst ULIRGs. These sources show a small AGN contribution to the mid-IR, around ~20% or less in most cases.",
"doi": "10.1051/0004-6361/201015504",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-12",
"volume": "524",
"pages": "A33"
},
{
"id": "authors:8007b-r9t74",
"collection": "authors",
"collection_id": "8007b-r9t74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101216-153515222",
"type": "article",
"title": "Cold dust and young starbursts: spectral energy distributions of Herschel SPIRE sources from the HerMES survey",
"author": [
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N. Y.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present spectral energy distributions (SEDs) for 68 Herschel sources detected at 5\u03c3 at 250, 350 and 500 \u03bcm in the HerMES SWIRE-Lockman field. We explore whether existing models for starbursts, quiescent star-forming galaxies and active galactic nucleus dust tori are able to model the full range of SEDs measured with Herschel. We find that while many galaxies (~56 per cent) are well fitted with the templates used to fit IRAS, Infrared Space Observatory (ISO) and Spitzer sources, for about half the galaxies two new templates are required: quiescent ('cirrus') models with colder (10\u201320 K) dust and a young starburst model with higher optical depth than Arp 220. Predictions of submillimetre fluxes based on model fits to 4.5\u201324 \u03bcm data agree rather poorly with the observed fluxes, but the agreement is better for fits to 4.5\u201370 \u03bcm data. Herschel galaxies detected at 500 \u03bcm tend to be those with the highest dust masses.",
"doi": "10.1111/j.1365-2966.2010.17041.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "2-11"
},
{
"id": "authors:fweya-62524",
"collection": "authors",
"collection_id": "fweya-62524",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101213-112741295",
"type": "article",
"title": "The Deep SPIRE HerMES Survey: spectral energy distributions and their astrophysical indications at high redshift",
"author": [
{
"family_name": "Brisbin",
"given_name": "D.",
"orcid": "0000-0002-4795-419X",
"clpid": "Brisbin-D"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The Spectral and Photometric Imaging Receiver on-board Herschel has been carrying out deep extragalactic surveys, one of the aims of which is to establish spectral energy distributions of individual galaxies spanning the infrared/submillimetre (IR/SMM) wavelength region. We report observations of the IR/SMM emission from the Lockman North field and Great Observatories Origins Deep Survey Field-North. Because galaxy images in the wavelength range covered by Herschel generally represent a blend with contributions from neighbouring galaxies, we present sets of galaxies in each field, especially free of blending at 250, 350 and 500 \u03bcm. We identify the cumulative emission of these galaxies and the fraction of the FIR cosmic background radiation they contribute. Our surveys reveal a number of highly luminous galaxies at redshift z \u2272 3 and a novel relationship between IR and visible emission that shows a dependence on luminosity and redshift.",
"doi": "10.1111/j.1365-2966.2010.17643.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "66-74"
},
{
"id": "authors:j60ta-t8a10",
"collection": "authors",
"collection_id": "j60ta-t8a10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101213-112923482",
"type": "article",
"title": "HerMES: SPIRE Science Demonstration Phase maps",
"author": [
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
}
],
"abstract": "We describe the production and verification of sky maps of the five Spectral and Photometric Imaging Receiver (SPIRE) fields observed as part of the Herschel Multi-tiered Extragalactic Survey (HerMES) during the Science Demonstration Phase (SDP) of the Herschel mission. We have implemented an iterative map-making algorithm [The SPIRE-HerMES Iterative Mapper (SHIM)] to produce high fidelity maps that preserve extended diffuse emission on the sky while exploiting the repeated observations of the same region of the sky with many detectors in multiple scan directions to minimize residual instrument noise. We specify here the SHIM algorithm and outline the various tests that were performed to determine and characterize the quality of the maps and verify that the astrometry, point source flux and power on all relevant angular scales meet the needs of the HerMES science goals. These include multiple jackknife tests, determination of the map transfer function and detailed examination of the power spectra of both sky and jackknife maps. The map transfer function is approximately unity on scales from 1 arcmin to 1\u00b0. Final maps (v1.0), including multiple jackknives, as well as the SHIM pipeline, have been used by the HerMES team for the production of SDP papers.",
"doi": "10.1111/j.1365-2966.2010.17771.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "83-91"
},
{
"id": "authors:cjgcb-d3a60",
"collection": "authors",
"collection_id": "cjgcb-d3a60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110506-141700003",
"type": "article",
"title": "Measures of star formation rates from infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields",
"author": [
{
"family_name": "Buat",
"given_name": "V.",
"clpid": "Buat-V"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The reliability of infrared (IR) and ultraviolet (UV) emissions to measure star formation rates (SFRs) in galaxies is investigated for a large sample of galaxies observed with the Spectral and Photometric Imaging Receiver (SPIRE) and the Photodetector Array Camera and Spectrometer (PACS) instruments on\u2002Herschel\u2002as part of the\u2002Herschel\u2002Multi-Tiered Extragalactic Survey (HerMES) project. We build flux-limited 250-\u03bcm samples of sources at redshift\u2002z\u2002< 1, cross-matched with the\u2002Spitzer/MIPS and\u2002GALEX\u2002catalogues. About 60 per cent of the\u2002Herschel\u2002sources are detected in UV. The total IR luminosities,\u2002L_(IR), of the sources are estimated using a spectral energy distribution (SED) fitting code that fits to fluxes between 24 and 500 \u03bcm. Dust attenuation is discussed on the basis of commonly used diagnostics: the\u2002L_(IR)/L_(UV)\u2002ratio and the slope, \u03b2, of the UV continuum. A mean dust attenuation\u2002A_(UV)\u2002of\u2002\u2243\u20023 mag is measured in the samples.\u2002L_(IR)/L_(UV)\u2002is found to correlate with\u2002L_(IR). Galaxies with\u2002L_(IR) \u2002> 10^(11) L_\u2299 and\u20020.5 <\u2002z\u2002< 1\u2002exhibit a mean dust attenuation\u2002A_(UV)\u2002of about 0.7 mag lower than that found for their local counterparts, although with a large dispersion. Our galaxy samples span a large range of \u03b2 and\u2002L_(IR)/L_(UV)\u2002values which, for the most part, are distributed between the ranges defined by the relations found locally for starburst and normal star-forming galaxies. As a consequence the recipe commonly applied to local starbursts is found to overestimate the dust attenuation correction in our galaxy sample by a factor of ~2\u20133. The SFRs deduced from\u2002L_(IR)\u2002are found to account for about 90 per cent of the total SFR; this percentage drops to 71 per cent for galaxies with\u2002SFR < 1 M_\u2299\u2002yr^(-1) (or\u2002L_(RI) < 10^(10) L_\u2299). For these faint objects, one needs to combine UV and IR emissions to obtain an accurate measure of the SFR.",
"doi": "10.1111/j.1745-3933.2010.00916.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "L1-L6"
},
{
"id": "authors:cexj5-d5d95",
"collection": "authors",
"collection_id": "cexj5-d5d95",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110103-110253076",
"type": "article",
"title": "Evolution of dust temperature of galaxies through cosmic time as seen by Herschel",
"author": [
{
"family_name": "Hwang",
"given_name": "H. S.",
"clpid": "Hwang-H-S"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chary",
"given_name": "R.-R.",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-R-R"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We study the dust properties of galaxies in the redshift range 0.1 \u2272 z \u2272 2.8 observed by the Herschel Space Observatory in the field of the Great Observatories Origins Deep Survey-North as part of the PACS Extragalactic Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) key programmes. Infrared (IR) luminosity (L_(IR)) and dust temperature (T_dust) of galaxies are derived from the spectral energy distribution fit of the far-IR (FIR) flux densities obtained with the PACS and SPIRE instruments onboard Herschel. As a reference sample, we also obtain IR luminosities and dust temperatures of local galaxies at z < 0.1 using AKARI and IRAS data in the field of the Sloan Digital Sky Survey. We compare the L_(IR)\u2013T_dust relation between the two samples and find that the median Tdust of Herschel-selected galaxies at z \u2273 0.5 with L_(IR) \u2273 5 \u00d7 10^(10) L_\u2299 appears to be 2\u20135 K colder than that of AKARI-selected local galaxies with similar luminosities, and the dispersion in T_dust for high-z galaxies increases with L_(IR) due to the existence of cold galaxies that are not seen among local galaxies. We show that this large dispersion of the L_(IR)\u2212T_dust relation can bridge the gap between local star-forming galaxies and high-z submillimetre galaxies (SMGs). We also find that three SMGs with very low T_dust\u2002(\u227220 K) covered in this study have close neighbouring sources with similar 24-\u03bcm brightness, which could lead to an overestimation of FIR/(sub)millimetre fluxes of the SMGs.",
"doi": "10.1111/j.1365-2966.2010.17645.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "75-82"
},
{
"id": "authors:ny3sn-gcj60",
"collection": "authors",
"collection_id": "ny3sn-gcj60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110112-141736463",
"type": "article",
"title": "Herschel reveals a T_(dust)-unbiased selection of z ~ 2 ultraluminous infrared galaxies",
"author": [
{
"family_name": "Magdis",
"given_name": "G. E.",
"orcid": "0000-0002-4872-2294",
"clpid": "Magdis-G-E"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Using Herschel Photodetector Array Camera (PACS) and Spectral and Photometric Imaging\nReceiver (SPIRE) observations of Lockman Hole-North and Great Observatories Origins\nDeep Survey-North (GOODS-N) as part of the Herschel Multi-tiered Extragalactic Survey\n(HerMES) project, we explore the far-infrared (IR) properties of a sample of mid-IR-selected\nstarburst-dominated ultraluminous infrared galaxies (ULIRGs) at z ~ 2. The selection of the\nsample is based on the detection of the stellar bump that appears in the spectral energy distribution\nof star-forming galaxies at 1.6 \u03bcm. We derive robust estimates of infrared luminosities\n(L_(IR)) and dust temperatures (T_d) of the population and find that while the luminosities in our\nsample span less than an order of magnitude (12.24 \u2264 log(L_(IR)/L_\u2299) \u2264 12.94), they cover\na wide range of dust temperatures (25 \u2264 T_d \u2264 62 K). Galaxies in our sample range from\nthose that are as cold as high-z submillimetre galaxies (SMGs) to those that are as warm\nas optically faint radio galaxies (OFRGs) and local ULIRGs. Nevertheless, our sample has\nmedian T_d = 42.3 K, filling the gap between SMGs and OFRGs, bridging the two populations.\nWe demonstrate that a significant fraction of our sample would be missed from ground-based\n(sub)mm surveys (850\u20131200 \u03bcm), showing that the latter introduce a bias towards the detection\nof colder sources. We conclude that Herschel observations confirm the existence of\nhigh-z ULIRGs warmer than SMGs, show that the mid-IR selection of high-z ULIRGs is\nnot T_d dependent, reveal a large dispersion in T_d of high-z ULIRGs and provide the means\nto characterize the bulk of the ULIRG population, free from selection biases introduced by\nground-based (sub)mm surveys.",
"doi": "10.1111/j.1365-2966.2010.17551.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "22-28"
},
{
"id": "authors:2qmem-vh395",
"collection": "authors",
"collection_id": "2qmem-vh395",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101217-091446952",
"type": "article",
"title": "HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations",
"author": [
{
"family_name": "Glenn",
"given_name": "J.",
"orcid": "0000-0001-7527-2017",
"clpid": "Glenn-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 \u03bcm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam^(\u22121), approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam.",
"doi": "10.1111/j.1365-2966.2010.17781.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "109-121"
},
{
"id": "authors:75c17-eas67",
"collection": "authors",
"collection_id": "75c17-eas67",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110509-110943988",
"type": "article",
"title": "HerMES: Herschel-SPIRE observations of Lyman break galaxies",
"author": [
{
"family_name": "Rigopoulou",
"given_name": "D.",
"orcid": "0000-0001-6854-7545",
"clpid": "Rigopoulou-D"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present first results of a study of the submillimetre (submm) (rest-frame far-infrared) properties of z ~ 3 Lyman break galaxies (LBGs) and their lower redshift counterparts BX/BM galaxies, based on Herschel-SPIRE observations of the Northern field of the Great Observatories Origins Deep Survey (GOODS-N). We use stacking analysis to determine the properties of LBGs well below the current limit of the survey. Although LBGs are not detected individually, stacking the infrared luminous LBGs (those detected with Spitzer at 24 \u03bcm) yields a statistically significant submm detection with mean flux \u3008S_(250)\u3009= 5.9 \u00b1 1.4 mJy confirming the power of SPIRE in detecting UV-selected high-redshift galaxies at submm wavelengths. In comparison, the Spitzer 24 \u03bcm detected BX/BM galaxies appear fainter with a stacked value of\u3008S_(250)\u3009= 2.7 \u00b1 0.8 mJy. By fitting the spectral energy distributions (SEDs) we derive median infrared luminosities, L_(IR), of 2.8 \u00d7 10^(12) L_\u2299 and 1.5 \u00d7 10^(11) L_\u2299 for z ~ 3 LBGs and BX/BMs, respectively. We find that LIR estimates derived from present measurements are in good agreement with those based on UV data for z ~ 2 BX/BM galaxies, unlike the case for z ~ 3 infrared luminous LBGs where the UV underestimates the true L_(IR). Although sample selection effects may influence this result we suggest that differences in physical properties (such as morphologies, dust distribution and extent of star-forming regions) between z ~ 3 LBGs and z ~ 2 BX/BMs may also play a significant role.",
"doi": "10.1111/j.1745-3933.2010.00950.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "L7-L12"
},
{
"id": "authors:w46bb-y4x92",
"collection": "authors",
"collection_id": "w46bb-y4x92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110105-153945195",
"type": "article",
"title": "The Herschel Multi-Tiered Extragalactic Survey: source extraction and cross-identifications in confusion-dominated SPIRE images",
"author": [
{
"family_name": "Roseboom",
"given_name": "I. G.",
"clpid": "Roseboom-I-G"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present the cross-identification and source photometry techniques used to process Herschel SPIRE imaging taken as part of the Herschel Multi-Tiered Extragalactic Survey (HerMES). Cross-identifications are performed in map-space so as to minimize source-blending effects. We make use of a combination of linear inversion and model selection techniques to produce reliable cross-identification catalogues based on Spitzer MIPS 24-\u03bcm source positions. Testing on simulations and real Herschel observations shows that this approach gives robust results for even the faintest sources (S_(250) ~10 mJy). We apply our new technique to HerMES SPIRE observations taken as part of the science demonstration phase of Herschel. For our real SPIRE observations, we show that, for bright unconfused sources, our flux density estimates are in good agreement with those produced via more traditional point source detection methods (SUSSEXtractor) by Smith et al. When compared to the measured number density of sources in the SPIRE bands, we show that our method allows the recovery of a larger fraction of faint sources than these traditional methods. However, this completeness is heavily dependent on the relative depth of the existing 24-\u03bcm catalogues and SPIRE imaging. Using our deepest multiwavelength data set in the GOODS-N, we estimate that the use of shallow 24-\u03bcm catalogues in our other fields introduces an incompleteness at faint levels of between 20\u201340 per cent at 250 \u03bcm.",
"doi": "10.1111/j.1365-2966.2010.17634.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2010-11",
"series_number": "1",
"volume": "409",
"issue": "1",
"pages": "48-65"
},
{
"id": "authors:wtvng-g8j47",
"collection": "authors",
"collection_id": "wtvng-g8j47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-143136718",
"type": "article",
"title": "HerMES: The SPIRE confusion limit",
"author": [
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Marshall",
"given_name": "J.",
"clpid": "Marshall-J"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We report on the sensitivity of SPIRE photometers on the Herschel Space Observatory. Specifically, we measure the confusion noise from observations taken during the science demonstration phase of the Herschel Multi-tiered Extragalactic Survey. Confusion noise is defined to be the\nspatial variation of the sky intensity in the limit of infinite integration time, and is found to be consistent among the different fields in our survey at the level of 5.8, 6.3 and 6.8 mJy/beam at 250, 350 and 500 \u03bcm, respectively. These results, together with the measured instrument noise, may be used to estimate the integration time required for confusion limited maps, and provide a noise estimate for maps obtained by SPIRE.",
"doi": "10.1051/0004-6361/201014680",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "Art. No. L5"
},
{
"id": "authors:q0t58-eeb38",
"collection": "authors",
"collection_id": "q0t58-eeb38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-100221983",
"type": "article",
"title": "The far-infrared/radio correlation as probed by Herschel",
"author": [
{
"family_name": "Ivison",
"given_name": "R. J.",
"orcid": "0000-0001-5118-1313",
"clpid": "Ivison-R-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J.",
"clpid": "Vieira-J"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We set out to determine the ratio, q_(IR), of rest-frame 8\u20131000-\u03bcm flux, S_(IR), to monochromatic radio flux, S_(1.4 GHz), for galaxies selected at far-infrared (IR) and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, T_d, and to identify any far-IR-bright outliers \u2013 useful laboratories for exploring why the far-IR/radio correlation (FIRRC) is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-\u03bcm and 1.4-GHz samples, obtained using Herschel and the Very Large Array (VLA) in GOODS-North (-N). We determine bolometric IR output using ten bands spanning \u03bb_(obs) = 24\u22121250 \u03bcm, exploiting data from PACS and SPIRE (PEP; HerMES), as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an L_(IR)-matched sample, designed to reveal evolution of q_(IR) with redshift, spanning log L_(IR) = 11\u201312 L_\u2299 and z = 0\u22122, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies in GOODS-N, we see tentative evidence of a break in the flux ratio, q_(IR), at L_(1.4 GHz) ~ 10^(22.7) WHz^(\u22121) where active galactic nuclei (AGN) are starting to dominate the radio power density, and of weaker correlations with redshift and T_d. From our 250-\u03bcm-selected sample we identify a small number of far-IR-bright outliers, and see trends of q_(IR) with L_(1.4 GHz), L_(IR), T_d and redshift, noting that some of these are inter-related. For our L_(IR-)matched sample, there is no evidence that q_(IR) changes significantly as we move back into the epoch of galaxy formation: we find q_(IR) \u221d (1+z)^\u03b3, where \u03b3 = \u22120.04 \u00b1 0.03 at z = 0 \u2212 2; however, discounting the least reliable data at z < 0.5 we find \u03b3 = \u22120.26 \u00b1 0.07, modest evolution which may be related to the radio background seen by ARCADE 2, perhaps driven by <10-\u03bcJy radio activity amongst ordinary star-forming galaxies at z > 1.",
"doi": "10.1051/0004-6361/201014552",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "Art. No. L31"
},
{
"id": "authors:rbr1c-6te72",
"collection": "authors",
"collection_id": "rbr1c-6te72",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101115-102412434",
"type": "article",
"title": "The HerMES SPIRE submillimeter local luminosity function",
"author": [
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric luminosity density in the local Universe, and Herschel offers the first opportunity to do so in an unbiased way by imaging large sky areas at several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0 < z < 0.2 local luminosity function and infrared bolometric (8\u20131000 \u03bcm) local luminosity density based on SPIRE data from the HerMES Herschel key program over 14.7 deg^2. Flux measurements in the three SPIRE channels at 250, 350 and 500 \u03bcm are combined with Spitzer photometry and archival data. We fit the observed optical-to-submillimeter spectral energy distribution of SPIRE sources and use the 1/V_(max) estimator to provide the first constraints on the monochromatic 250, 350 and 500 \u03bcm as well as on the infrared bolometric (8\u20131000 \u03bcm) local luminosity function based on Herschel data. We compare our results with modeling predictions and find a slightly more abundant local submillimeter population than predicted by a number of models. Our measurement of the infrared bolometric (8\u20131000 \u03bcm) local luminosity function suggests a flat slope at low luminosity, and the inferred local luminosity density, 1.31_(-0.21)^(+0.24)\u2009 \u00d7\u200910^8\u2009L_\u2609 Mpc^(-3), is consistent with the range of values reported in recent literature.",
"doi": "10.1051/0004-6361/201014694",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "L20"
},
{
"id": "authors:rrfsc-srz18",
"collection": "authors",
"collection_id": "rrfsc-srz18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-085141496",
"type": "article",
"title": "Herschel unveils a puzzling uniformity of distant dusty galaxies",
"author": [
{
"family_name": "Elbaz",
"given_name": "D.",
"orcid": "0000-0002-7631-647X",
"clpid": "Elbaz-David"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chary",
"given_name": "R.-R.",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-R-R"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved over the last 80% of the age of the Universe. We discuss possible consequences for the determination of starformation\nrates (SFR) and any evidence for a major change in their star-formation properties. We use Herschel deep extragalactic surveys from 100 to 500 \u03bcm to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and\nHerMES key programs). An extension to fainter luminosities is done by stacking images on 24 \u03bcm prior positions. We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used, e.g. at 24 \u03bcm, to identify\n\"isolated\" galaxies whose flux is not boosted by bright neighbors. Below z ~ 1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15 dex), therefore similar to z ~ 0 galaxies, over three decades in luminosity below the regime of ultra-luminous IR galaxies (ULIRGs, L_(IR) \u2265 10^(12) L_\u2299). This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160 \u03bcm, 250 \u03bcm or 350 \u03bcm bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ~150 \u03bcm (rest-frame) before Herschel on those templates. We also note that the dust temperature of luminous IR galaxies (LIRGs, L_(IR) \u2265 10^(11) L_\u2299) around z ~ 1 is mildly colder by 10\u201315% than their local analogs and up to 20% for ULIRGs at z ~ 1.6 (using a single modified blackbody-fit to the peak far-IR emission with an emissivity index of \u03b2 = 1.5). Above z = 1.5, distant galaxies are found to exhibit a substantially larger mid- over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor coeval star formation at very high SFR and in conditions similar to purely star-forming galaxies.",
"doi": "10.1051/0004-6361/201014687",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "Art. No. L29"
},
{
"id": "authors:ptb0m-cd375",
"collection": "authors",
"collection_id": "ptb0m-cd375",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-111403706",
"type": "article",
"title": "First results from HerMES on the evolution of the submillimetre luminosity function",
"author": [
{
"family_name": "Eales",
"given_name": "S. A.",
"clpid": "Eales-S-A"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We have carried out two extremely deep surveys with SPIRE, one of the two cameras on Herschel, at 250 \u03bcm, close to the peak of the far-infrared background. We have used the results to investigate the evolution of the rest-frame 250-\u03bcm luminosity function out to z = 2. We find evidence for strong evolution out to z \u2243 1 but evidence for at most weak evolution beyond this redshift. Our results suggest that a significant part of the stars and metals in the universe today were formed at z \u2264 1.4 in spiral galaxies.",
"doi": "10.1051/0004-6361/201014675",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "Art. No. L23"
},
{
"id": "authors:p897d-5ja34",
"collection": "authors",
"collection_id": "p897d-5ja34",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101117-104045678",
"type": "article",
"title": "The Herschel-SPIRE instrument and its in-flight performance",
"author": [
{
"family_name": "Griffin",
"given_name": "M. J.",
"clpid": "Griffin-M-J"
},
{
"family_name": "Hristov",
"given_name": "V.",
"clpid": "Hristov-V-V"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Latter",
"given_name": "W.",
"clpid": "Latter-W"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Schwartz",
"given_name": "A.",
"clpid": "Schwartz-A"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"family_name": "Zhang",
"given_name": "L.",
"orcid": "0000-0002-0898-787X",
"clpid": "Zhang-Liyuan"
}
],
"abstract": "The Spectral and Photometric Imaging REceiver (SPIRE), is the Herschel Space Observatory`s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 \u03bcm, and an imaging Fourier-transform spectrometer (FTS) which covers simultaneously its whole operating range of 194\u2013671 \u03bcm (447\u20131550 GHz). The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4\u00b4\u00d7 8\u00b4, observed simultaneously in the three spectral bands. Its main operating mode is scan-mapping, whereby the field of view is scanned across the sky to achieve full spatial sampling and to cover large areas if desired. The spectrometer has an approximately circular field of view with a diameter of 2.6\u00b4. The spectral resolution can be adjusted between 1.2 and 25 GHz by changing the stroke length of the FTS scan mirror. Its main operating mode involves a fixed telescope pointing with multiple scans of the FTS mirror to acquire spectral data. For extended source measurements, multiple position offsets are implemented by means of an internal beam steering mirror to achieve the desired spatial sampling and by rastering of the telescope pointing to map areas larger than the field of view. The SPIRE instrument consists of a cold focal plane unit located inside the Herschel cryostat and warm electronics units, located on the spacecraft Service Module, for instrument control and data handling. Science data are transmitted to Earth with no on-board data compression, and processed by automatic pipelines to produce calibrated science products. The in-flight performance of the instrument matches or exceeds predictions based on pre-launch testing and modelling: the photometer sensitivity is comparable to or slightly better than estimated pre-launch, and the spectrometer sensitivity is also better by a factor of 1.5\u20132.",
"doi": "10.1051/0004-6361/201014519",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "L3"
},
{
"id": "authors:4d2ya-ktq05",
"collection": "authors",
"collection_id": "4d2ya-ktq05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101122-111936760",
"type": "article",
"title": "HerMES: SPIRE galaxy number counts at 250, 350, and 500 \u03bcm",
"author": [
{
"family_name": "Oliver",
"given_name": "S. J.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ~15% of the infrared extra-galactic background at the wavelength near where it peaks.",
"doi": "10.1051/0004-6361/201014697",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "L21"
},
{
"id": "authors:sm30j-fha12",
"collection": "authors",
"collection_id": "sm30j-fha12",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101124-111407085",
"type": "article",
"title": "In-flight calibration of the Herschel-SPIRE instrument",
"author": [
{
"family_name": "Swinyard",
"given_name": "B. M.",
"clpid": "Swinyard-B-M"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"clpid": "Lu-Nan"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Schwartz",
"given_name": "A.",
"clpid": "Schwartz-A"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zhang",
"given_name": "L.",
"clpid": "Zhang-L"
}
],
"abstract": "SPIRE, the Spectral and Photometric Imaging REceiver, is the Herschel Space Observatory's submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 \u03bcm, and an imaging Fourier-transform spectrometer (FTS) covering 194\u2013671 \u03bcm (447-1550 GHz). In this paper we describe the initial approach taken to the absolute calibration of the SPIRE instrument using a combination of the emission from the Herschel telescope itself and the modelled continuum emission from solar system objects and other astronomical targets. We present the photometric, spectroscopic and spatial accuracy that is obtainable in data processed through the \"standard\" pipelines. The overall photometric accuracy at this stage of the mission is estimated as 15% for the photometer and between 15 and 50% for the spectrometer. However, there remain issues with the photometric accuracy of the spectra of low flux sources in the longest wavelength part of the SPIRE spectrometer band. The spectrometer wavelength accuracy is determined to be better than 1/10th of the line FWHM. The astrometric accuracy in SPIRE maps is found to be 2 arcsec when the latest calibration data are used. The photometric calibration of the SPIRE instrument is currently determined by a combination of uncertainties in the model spectra of the astronomical standards and the data processing methods employed for map and spectrum calibration. Improvements in processing techniques and a better understanding of the instrument performance will lead to the final calibration accuracy of SPIRE being determined only by uncertainties in the models of astronomical standards.",
"doi": "10.1051/0004-6361/201014605",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "L4"
},
{
"id": "authors:xp4jn-t7g17",
"collection": "authors",
"collection_id": "xp4jn-t7g17",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101203-082006802",
"type": "article",
"title": "HerMES: The submillimeter spectral energy distributions of Herschel/SPIRE-detected galaxies",
"author": [
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present colours of sources detected with the Herschel/SPIRE instrument in deep extragalactic surveys of the Lockman Hole, Spitzer-FLS, and GOODS-N fields in three photometric bands at 250, 350 and 500 \u03bcm. We compare these with expectations from the literature and discuss\nassociated uncertainties and biases in the SPIRE data. We identify a 500 \u03bcm flux limited selection of sources from the HerMES point source catalogue that appears free from neighbouring/blended sources in all three SPIRE bands. We compare the colours with redshift tracks of various\ncontemporary models. Based on these spectral templates we show that regions corresponding to specific population types and redshifts can be identified better in colour-flux space. The redshift tracks as well as the colour-flux plots imply a majority of detected objects with redshifts at\n1 < z < 3.5, somewhat depending on the group of model SEDs used. We also find that a population of sources with S_(250)/S_(350) < 0.8 at fluxes above 50 mJy as observed by SPIRE are not well represented by contemporary models and could consist of a mix of cold and lensed galaxies.",
"doi": "10.1051/0004-6361/201014673",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "Art. No. L32"
},
{
"id": "authors:vfyg7-a2f51",
"collection": "authors",
"collection_id": "vfyg7-a2f51",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-081855281",
"type": "article",
"title": "HerMES: Halo occupation number and bias properties of dusty galaxies from angular clustering measurements",
"author": [
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Vieira",
"given_name": "J. D.",
"clpid": "Vieira-J-D"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We measure the angular correlation function, w(\u03b8), from 0.5 to 30 arcmin of detected sources in two wide fields of the Herschel Multi-tiered Extragalactic Survey (HerMES). Our measurements are consistent with the expected clustering shape from a population of sources that trace the\ndark matter density field, including non-linear clustering at arcminute angular scales arising from multiple sources that occupy the same dark matter halos. By making use of the halo model to connect the spatial clustering of sources to the dark matter halo distribution, we estimate source\nbias and halo occupation number for dusty sub-mm galaxies at z ~ 2. We find that sub-mm galaxies with 250 \u03bcm flux densities above 30 mJy reside in dark matter halos with mass above (5 \u00b1 4) \u00d7 10^(12) M_\u2299 while (14 \u00b1 8)% of such sources appear as satellites in more massive halos.",
"doi": "10.1051/0004-6361/201014597",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "Art. No. L22"
},
{
"id": "authors:54sf3-dwk05",
"collection": "authors",
"collection_id": "54sf3-dwk05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101115-102122698",
"type": "article",
"title": "HerMES: Far infrared properties of known AGN in the HerMES fields",
"author": [
{
"family_name": "Hatziminaoglou",
"given_name": "E.",
"clpid": "Hatziminaoglou-E"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Levenson",
"given_name": "L.",
"clpid": "Levenson-L"
},
{
"family_name": "Lu",
"given_name": "N.",
"orcid": "0000-0002-8948-1044",
"clpid": "Lu-Nanyao"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Schulz",
"given_name": "B.",
"clpid": "Schulz-B"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "Nuclear and starburst activity are known to often occur concomitantly. Herschel-SPIRE provides sampling of the far-infrared (FIR) spectral energy distributions (SEDs) of type 1 and type 2 AGN, allowing for the separation between the hot dust (torus) and cold dust (starburst) emission. We study large samples of spectroscopically confirmed type 1 and type 2 AGN lying within the Herschel Multi-tiered Extragalactic Survey (HerMES) fields observed during the science demonstration phase, aiming to understand their FIR colour distributions and constrain their starburst contributions. We find that one third of the spectroscopically confirmed AGN in the HerMES fields have 5\u03c3 detections at 250\u2009\u03bcm, in agreement with previous (sub)mm AGN studies. Their combined Spitzer-MIPS and Herschel-SPIRE colours (specifically S_(250)/S_(70) vs S_(70)/S_(24)) quite clearly separate them from the non-AGN, star forming galaxy population, as their 24 \u03bcm flux is dominated by the hot torus emission. However, their SPIRE colours alone do not differ from those of non-AGN galaxies. SED fitting shows that all those AGN need a starburst component to fully account for their FIR emission. For objects at z > 2 we find a correlation between the infrared luminosity attributed to the starburst component, LSB, and the AGN accretion luminosity, L_(acc), with L_(SB) \u221d L_(acc)^(0.35). Type 2 AGN detected at 250\u2009\u03bcm show on average higher LSB than type 1 objects but their number is still too low to establish whether this trend indicates stronger star formation activity.",
"doi": "10.1051/0004-6361/201014679",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-07",
"volume": "518",
"pages": "L33"
},
{
"id": "authors:12f3h-g5c10",
"collection": "authors",
"collection_id": "12f3h-g5c10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100628-100933554",
"type": "article",
"title": "Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z\u2009~ 2.5",
"author": [
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-G"
},
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Tresse",
"given_name": "L.",
"clpid": "Tresse-L"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-O"
},
{
"family_name": "Le Brun",
"given_name": "V.",
"clpid": "Le-Brun-V"
},
{
"family_name": "Mancini",
"given_name": "C.",
"orcid": "0000-0002-4297-0561",
"clpid": "Mancini-C"
},
{
"family_name": "Matute",
"given_name": "I.",
"orcid": "0000-0003-1177-3896",
"clpid": "Matute-I"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"clpid": "Cimatti-A"
},
{
"family_name": "Marchetti",
"given_name": "L.",
"orcid": "0000-0003-3948-7621",
"clpid": "Marchetti-L"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397",
"clpid": "Ilbert-Olivier"
},
{
"family_name": "Arnouts",
"given_name": "S.",
"clpid": "Arnouts-S"
},
{
"family_name": "Bolzonella",
"given_name": "M.",
"clpid": "Bolzonella-M"
},
{
"family_name": "Zucca",
"given_name": "E.",
"clpid": "Zucca-E"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"clpid": "Bardelli-S"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Garilli",
"given_name": "B.",
"clpid": "Garilli-B"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"clpid": "Zamorani-G"
},
{
"family_name": "Pozzetti",
"given_name": "L.",
"clpid": "Pozzetti-L"
},
{
"family_name": "Bondi",
"given_name": "M.",
"clpid": "Bondi-M"
},
{
"family_name": "de la Torre",
"given_name": "S.",
"orcid": "0000-0002-0839-2884",
"clpid": "de-la-Torre-S"
},
{
"family_name": "Vergani",
"given_name": "D.",
"clpid": "Vergani-D"
},
{
"family_name": "Santini",
"given_name": "P.",
"clpid": "Santini-P"
},
{
"family_name": "Grazian",
"given_name": "A.",
"clpid": "Grazian-A"
},
{
"family_name": "Fontana",
"given_name": "A.",
"clpid": "Fontana-A"
}
],
"abstract": "Context. Studies of the infrared (IR) emission of cosmic sources have proven essential to constraining the evolutionary history of cosmic star formation and the gravitational accretion of nuclear black holes, because many of these events occur inside heavily dust-extinguished environments. \n\nAims. The Spitzer Space Telescope has provided a large amount of data to constrain the nature and cosmological evolution of infrared source populations. In the present paper we exploit a large homogeneous dataset to derive a self-consistent picture of IR emission based on the time-dependent \u03bb_(eff) = 24, 15, 12, and 8 \u03bcm monochromatic and bolometric IR luminosity functions (LF) over the full 0 < z < 2.5 redshift range. \n\nMethods. Our present analysis is based on a combination of data from deep Spitzer surveys of the VIMOS VLT Deep Survey (VVDS-SWIRE) and GOODS fields. To our limiting flux of S_(24) = 400 \u03bcJy, our sample derived from VVDS-SWIRE includes 1494 sources, and 666 and 904 sources brighter than S_(24) = 80 \u03bcJy are catalogued in GOODS-S and GOODS-N, respectively, for a total area of ~0.9 square degrees. Apart from a few galaxies, we obtain reliable optical identifications and redshifts for all these sources, providing a rich and robust dataset for our luminosity function determination. The final combined reliable sample includes 3029 sources, the fraction with photometric redshifts being 72% over all redshifts and almost all galaxies at z > 1.5. Based on the multiwavelength information available in these areas, we constrain the LFs at 8, 12, 15, and 24 \u03bcm. We also infer the total IR luminosities from our best-fit model of the observed SEDs of each source, and use this to derive the bolometric (8\u20131000 \u03bcm) LF and comoving volume emissivity to z ~ 2.5. \n\nResults. In the redshift interval 0 < z < 1, the bolometric IR luminosity density evolves as (1 + z)^(3.8\u00b10.4). Although it is more uncertain at higher-z, our results show a flattening in the IR luminosity density at z > 1. The mean redshift of the peak in the source number density shifts with luminosity: the brightest IR galaxies appear to form stars at earlier cosmic times (z > 1.5), while star formation in the less luminous galaxies continues until more recent epochs (z ~ 1 for L_(IR) < 10^(11)_\u2609), in overall agreement with similar analyses in the literature. \n\nConclusions. Our results are indicative of a rapid increase in the galaxy IR comoving volume emissivity up to z ~ 1 and a constant average emissivity at z > 1. We also appear to measure a difference in the evolutionary rate of the source number densities as a function of luminosity, which is consistent with the downsizing evolutionary patterns reported for other samples of cosmic sources.",
"doi": "10.1051/0004-6361/200912058",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2010-06",
"volume": "515",
"pages": "Art. No. A8"
},
{
"id": "authors:xwgw7-akv63",
"collection": "authors",
"collection_id": "xwgw7-akv63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100526-154509152",
"type": "article",
"title": "The Deep Swire Field. IV. First Properties of the sub-mJy Galaxy Population: Redshift Distribution, AGN Activity, and Star Formation",
"author": [
{
"family_name": "Strazzullo",
"given_name": "Veronica",
"clpid": "Strazzullo-V"
},
{
"family_name": "Pannella",
"given_name": "Maurilio",
"clpid": "Pannella-M"
},
{
"family_name": "Owen",
"given_name": "Frazer N.",
"clpid": "Owen-F-N"
},
{
"family_name": "Bender",
"given_name": "Ralf",
"clpid": "Bender-R"
},
{
"family_name": "Morrison",
"given_name": "Glenn E.",
"clpid": "Morrison-G-E"
},
{
"family_name": "Wang",
"given_name": "Wei-Hao",
"orcid": "0000-0003-2588-1265",
"clpid": "Wang-Wei-Hao"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "We present a study of a 20 cm selected sample in the Deep Spitzer Wide-area InfraRed Extragalactic Legacy Survey Very Large Array Field, reaching a 5\u03c3 limiting flux density at the image center of S_(1.4 GHz) ~ 13.5 \u03bcJy. In a 0.6 \u00d7 0.6 deg^2 field, we are able to assign an optical/IR counterpart to 97% of the radio sources. Up to 11 passbands from the NUV to 4.5 \u03bcm are then used to sample the spectral energy distribution (SED) of these counterparts in order to investigate the nature of the host galaxies. By means of an SED template library and stellar population synthesis models, we estimate photometric redshifts, stellar masses, and stellar population properties, dividing the sample into three sub-classes of quiescent, intermediate, and star-forming galaxies. We focus on the radio sample in the redshift range 0.3 < z < 1.3 where we estimate to have a redshift completeness higher than 90% and study the properties and redshift evolution of these sub-populations. We find that, as expected, the relative contributions of active galactic nuclei (AGNs) and star-forming galaxies to the \u03bcJy population depend on the flux density limit of the sample. At all flux levels, a significant population of \"green-valley\" galaxies is observed. While the actual nature of these sources is not definitely understood, the results of this work may suggest that a significant fraction of faint radio sources might be composite (and possibly transition) objects, thus a simple \"AGN versus star-forming\" classification might not be appropriate to fully understand what faint radio populations really are.",
"doi": "10.1088/0004-637X/714/2/1305",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2010-05-10",
"series_number": "2",
"volume": "714",
"issue": "2",
"pages": "1305-1323"
},
{
"id": "authors:53a6f-rd248",
"collection": "authors",
"collection_id": "53a6f-rd248",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100111-095352567",
"type": "article",
"title": "Multi-wavelength properties of Spitzer selected starbursts at z\u2009~\u20092",
"author": [
{
"family_name": "Fiolet",
"given_name": "N.",
"clpid": "Fiolet-N"
},
{
"family_name": "Omont",
"given_name": "A.",
"orcid": "0000-0002-4721-3922",
"clpid": "Omont-A"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Owen",
"given_name": "F.",
"clpid": "Owen-F-N"
},
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Siana",
"given_name": "B.",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Strazzullo",
"given_name": "V.",
"clpid": "Strazzullo-V"
},
{
"family_name": "Pannella",
"given_name": "M.",
"clpid": "Pannella-M"
},
{
"family_name": "Baker",
"given_name": "A. J.",
"orcid": "0000-0002-7892-396X",
"clpid": "Baker-Andrew-J"
},
{
"family_name": "Beelen",
"given_name": "A.",
"clpid": "Beelen-A"
},
{
"family_name": "Biggs",
"given_name": "A.",
"orcid": "0000-0002-1117-9961",
"clpid": "Biggs-Andrew-D"
},
{
"family_name": "de Breuck",
"given_name": "C.",
"orcid": "0000-0002-6637-3315",
"clpid": "de-Breuck-Carlos"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Ivison",
"given_name": "R.",
"orcid": "0000-0001-5118-1313",
"clpid": "Ivison-Rob-J"
},
{
"family_name": "Lagache",
"given_name": "G.",
"orcid": "0000-0003-1492-2519",
"clpid": "Lagache-Guilaine"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
},
{
"family_name": "Zylka",
"given_name": "R.",
"clpid": "Zylka-Robert"
}
],
"abstract": "Context. Wide-field Spitzer surveys allow identification of thousands of potentially high-z submillimeter galaxies (SMGs) through their bright 24 \u03bcm emission and their mid-IR colors.\nAims. We want to determine the average properties of such z ~ 2 Spitzer-selected SMGs by combining millimeter, radio, and infrared photometry for a representative IR-flux (\u03bb_(rest) ~ 8 \u03bcm) limited sample of SMG candidates.\nMethods. A complete sample of 33 sources believed to be starbursts (\"5.8 \u03bcm-peakers\") was selected in the (0.5 deg^2) J1046+56 field with selection criteria F_(24 \u03bcm) > 400 \u03bcJy, the presence of a redshifted stellar emission peak at 5.8 \u03bcm, and r'_(Vega) > 23. The field, part of the SWIRE Lockman Hole field, benefits from very deep VLA/GMRT 20 cm, 50 cm, and 90 cm radio data (all 33 sources are detected at 50 cm), and deep 160 \u03bcm and 70 \u03bcm Spitzer data. The 33 sources, with photometric redshifts ~1.5\u22122.5, were observed at 1.2mm with IRAM-30m/MAMBO to an rms ~0.7\u20130.8mJy in most cases. Their millimeter, radio, 7-band Spitzer, and near-IR properties were jointly analyzed.\nResults. The entire sample of 33 sources has an average 1.2mm flux density of 1.56 \u00b1 0.22 mJy and a median of 1.61mJy, so the majority of the sources can be considered SMGs. Four sources have confirmed 4\u03c3 detections, and nine were tentatively detected at the 3\u03c3 level. Because of\nits 24 \u03bcm selection, our sample shows systematically lower F_(1.2mm)/F_(24 \u03bcm) flux ratios than classical SMGs, probably because of enhanced PAH emission. A median FIR SED was built by stacking images at the positions of 21 sources in the region of deepest Spitzer coverage. Its parameters\nare T_(dust) = 37 \u00b1 8K, L_(FIR) = 2.5 \u00d7 10^(12) L_\u2609, and SFR = 450 M yr^(\u22121). The FIR-radio correlation provides another estimate of LFIR for each source, with an average value of 4.1 \u00d7 10^(12) L_\u2609; however, this value may be overestimated because of some AGN contribution. Most of our targets are also luminous star-forming BzK galaxies which constitute a significant fraction of weak SMGs at 1.7 \u2272 z \u2272 2.3.\nConclusions. Spitzer 24 \u03bcm-selected starbursts and AGN-dominated ULIRGs can be reliably distinguished using IRAC-24 \u03bcm SEDs. Such \"5.8 \u03bcm-peakers\" with F_(24 \u03bcm) > 400 \u03bcJy have L_(FIR) 10^(12) L_\u2609. They are thus z ~ 2 ULIRGs, and the majority may be considered SMGs. However, they have systematically lower 1.2mm/24 \u03bcm flux density ratios than classical SMGs, warmer dust, comparable or lower IR/mm luminosities, and higher stellar masses. About 2000\u22123000 \"5.8 \u03bcm-peakers\" may be easily identifiable within SWIRE catalogues over 49 deg^2.",
"doi": "10.1051/0004-6361/200912742",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2009-12",
"series_number": "1",
"volume": "508",
"issue": "1",
"pages": "117-132"
},
{
"id": "authors:s8xnj-vek71",
"collection": "authors",
"collection_id": "s8xnj-vek71",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100104-122034465",
"type": "article",
"title": "The SWIRE/Chandra Survey: The X-ray Sources",
"author": [
{
"family_name": "Wilkes",
"given_name": "Belinda J.",
"orcid": "0000-0003-1809-2364",
"clpid": "Wilkes-B-J"
},
{
"family_name": "Kilgard",
"given_name": "Roy",
"clpid": "Kilgard-Roy"
},
{
"family_name": "Kim",
"given_name": "Dong-Woo",
"clpid": "Kim-Dong-Woo"
},
{
"family_name": "Kim",
"given_name": "Minsun",
"clpid": "Kim-Minsun"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Lonsdale",
"given_name": "Carol",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Smith",
"given_name": "Harding E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Owen",
"given_name": "Frazer N.",
"clpid": "Owen-F-N"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Siana",
"given_name": "Brian",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "We report a moderate-depth (70 ks), contiguous 0.7 deg^2 Chandra survey in the Lockman Hole Field of the Spitzer/SWIRE Legacy Survey coincident with a completed, ultra-deep VLA survey with deep optical and near-infrared imaging in-hand. The primary motivation is to distinguish starburst galaxies and active galactic nuclei (AGNs), including the significant, highly obscured (log N_H > 23) subset. Chandra has detected 775 X-ray sources to a limiting broadband (0.3-8 keV) flux ~4 \u00d7 10^(\u201316) erg cm^(\u20132) s^(\u20131). We present the X-ray catalog, fluxes, hardness ratios, and multi-wavelength fluxes. The log N versus log S agrees with those of previous surveys covering similar flux ranges. The Chandra and Spitzer flux limits are well matched: 771 (99%) of the X-ray sources have infrared (IR) or optical counterparts, and 333 have MIPS 24 \u03bcm detections. There are four optical-only X-ray sources and four with no visible optical/IR counterpart. The very deep (~2.7 \u03bcJy rms) VLA data yield 251 (>4\u03c3) radio counterparts, 44% of the X-ray sources in the field. We confirm that the tendency for lower X-ray flux sources to be harder is primarily due to absorption. As expected, there is no correlation between observed IR and X-ray fluxes. Optically bright, type 1, and red AGNs lie in distinct regions of the IR versus X-ray flux plots, demonstrating the wide range of spectral energy distributions in this sample and providing the potential for classification/source selection. Many optically bright sources, which lie outside the AGN region in the optical versus X-ray plots (f_r /f_x >10), lie inside the region predicted for red AGNs in IR versus X-ray plots, consistent with the presence of an active nucleus. More than 40% of the X-ray sources in the VLA field are radio-loud using the classical definition, R_L . The majority of these are red and relatively faint in the optical so that the use of R_L to select those AGNs with the strongest radio emission becomes questionable. Using the 24 \u03bcm to radio flux ratio (q_(24)) instead results in 13 of the 147 AGNs with sufficient data being classified as radio-loud, in good agreement with the ~10% expected for broad-lined AGNs based on optical surveys. We conclude that q_(24) is a more reliable indicator of radio-loudness. Use of R_L should be confined to the optically selected type 1 AGN.",
"doi": "10.1088/0067-0049/185/2/433",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2009-12",
"series_number": "2",
"volume": "185",
"issue": "2",
"pages": "433-450"
},
{
"id": "authors:0tn0d-dv250",
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"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091103-130946829",
"type": "article",
"title": "Spitzer 70 and 160 \u03bcm Observations of the COSMOS Field",
"author": [
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998",
"clpid": "Sanders-D-B"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Aussel",
"given_name": "H.",
"orcid": "0000-0002-1371-5705",
"clpid": "Aussel-Herve"
},
{
"family_name": "Salvato",
"given_name": "M.",
"orcid": "0000-0001-7116-9303",
"clpid": "Salvato-Mara"
},
{
"family_name": "Le Floc'h",
"given_name": "E.",
"clpid": "Le-Floc'h-Emeric"
},
{
"family_name": "Huynh",
"given_name": "M. T.",
"clpid": "Huynh-Minh-T"
},
{
"family_name": "Scoville",
"given_name": "N. Z.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Afonso-Luis",
"given_name": "A.",
"clpid": "Afonso-Luis-A"
},
{
"family_name": "Bhattacharya",
"given_name": "B.",
"clpid": "Bhattacharya-Bidushi"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-P"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Fu",
"given_name": "H.",
"orcid": "0000-0001-9608-6395",
"clpid": "Fu-Hai"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397",
"clpid": "Ilbert-Olivier"
},
{
"family_name": "Kartaltepe",
"given_name": "J. S.",
"orcid": "0000-0001-9187-3605",
"clpid": "Kartaltepe-J"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-A-M"
},
{
"family_name": "Lee",
"given_name": "Nicholas",
"orcid": "0000-0001-5500-1324",
"clpid": "Lee-Nicolas"
},
{
"family_name": "Murphy",
"given_name": "E.",
"orcid": "0000-0001-7089-7325",
"clpid": "Murphy-E-J"
},
{
"family_name": "Sargent",
"given_name": "M. T.",
"orcid": "0000-0003-1033-9684",
"clpid": "Sargent-M-T"
},
{
"family_name": "Schinnerer",
"given_name": "E.",
"orcid": "0000-0002-3933-7677",
"clpid": "Schinnerer-E"
},
{
"family_name": "Sheth",
"given_name": "K.",
"orcid": "0000-0002-5496-4118",
"clpid": "Sheth-K"
},
{
"family_name": "Shopbell",
"given_name": "P. L.",
"clpid": "Shopbell-P-L"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We present Spitzer 70 and 160 \u03bcm observations of the COSMOS Spitzer survey (S-COSMOS). The data processing techniques are discussed for the publicly released products consisting of images and source catalogs. We present accurate 70 and 160 \u03bcm source counts of the COSMOS field and find reasonable agreement with measurements in other fields and with model predictions. The previously reported counts for GOODS-North and the extragalactic First Look Survey are updated with the latest calibration, and counts are measured based on the large area SWIRE survey to constrain the bright source counts. We measure an extragalactic confusion noise level of \u03c3_c = 9.4 \u00b1 3.3 mJy (q = 5) for the MIPS 160 \u03bcm band based on the deep S-COSMOS data and report an updated confusion noise level of \u03c3_c = 0.35 \u00b1 0.15 mJy (q = 5) for the MIPS 70 \u03bcm band.",
"doi": "10.1088/0004-6256/138/5/1261",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2009-11",
"series_number": "5",
"volume": "138",
"issue": "5",
"pages": "1261-1270"
},
{
"id": "authors:t9bz9-gmm46",
"collection": "authors",
"collection_id": "t9bz9-gmm46",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090911-081110058",
"type": "article",
"title": "MAMBO 1.2 mm Observations of Luminous Starbursts at z ~ 2 in the SWIRE Fields",
"author": [
{
"family_name": "Lonsdale",
"given_name": "Carol J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Polletta",
"given_name": "Maria del Carmen",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Omont",
"given_name": "Alain",
"orcid": "0000-0002-4721-3922",
"clpid": "Omont-A"
},
{
"family_name": "Shupe",
"given_name": "Dave",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Berta",
"given_name": "Stefano",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Zylka",
"given_name": "Robert",
"clpid": "Zylka-Robert"
},
{
"family_name": "Siana",
"given_name": "Brian",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Lutz",
"given_name": "Dieter",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Farrah",
"given_name": "Duncan",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Smith",
"given_name": "Harding E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Lagache",
"given_name": "Guilaine",
"orcid": "0000-0003-1492-2519",
"clpid": "Lagache-Guilaine"
},
{
"family_name": "de Breuck",
"given_name": "Carlos",
"orcid": "0000-0002-6637-3315",
"clpid": "de-Breuck-Carlos"
},
{
"family_name": "Owen",
"given_name": "Frazer",
"clpid": "Owen-F-N"
},
{
"family_name": "Beelen",
"given_name": "Alexandre",
"clpid": "Beelen-A"
},
{
"family_name": "Weedman",
"given_name": "Dan",
"clpid": "Weedman-D-W"
},
{
"family_name": "Franceschini",
"given_name": "Alberto",
"clpid": "Franceschini-A"
},
{
"family_name": "Clements",
"given_name": "Dave",
"orcid": "0000-0002-9548-5033",
"clpid": "Clements-D-L"
},
{
"family_name": "Tacconi",
"given_name": "Linda",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
},
{
"family_name": "Afonso-Luis",
"given_name": "Alejandro",
"clpid": "Afonso-Luis-A"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "Ismael",
"clpid": "P\u00e9rez-Fournon-I"
},
{
"family_name": "Cox",
"given_name": "Pierre",
"orcid": "0000-0003-2027-8221",
"clpid": "Cox-Pierre"
},
{
"family_name": "Bertoldi",
"given_name": "Frank",
"orcid": "0000-0002-1707-1775",
"clpid": "Bertoldi-F"
}
],
"abstract": "We report on-off pointed MAMBO observations at 1.2 mm of 61 Spitzer-selected star-forming galaxies from the Spitzer Wide Area Infrared Extragalactic Legacy survey (SWIRE). The sources are selected on the basis of bright 24 \u03bcm fluxes (f _(24\u03bcm) > 0.4 mJy) and of stellar dominated near-infrared spectral energy distributions in order to favor z ~ 2 starburst galaxies. The average 1.2 mm flux for the whole sample is 1.5 \u00b1 0.2 mJy. Our analysis focuses on 29 sources in the Lockman Hole field where the average 1.2 mm flux (1.9 \u00b1 0.3 mJy) is higher than in other fields (1.1 \u00b1 0.2 mJy). The analysis of the multiwavelength spectral energy distributions indicates that these sources are starburst galaxies with far-infrared luminosities from 10^(12) to 10^(13.3)L_\u2609 , and stellar masses of ~0.2-6 \u00d7 10^(11)M_\u2609 . Compared to submillimeter selected galaxies (SMGs), the SWIRE-MAMBO sources are among those with the largest 24 \u03bcm/1.2 mm flux ratios. The origin of such large ratios is investigated by comparing the average mid-infrared spectra and the stacked far-infrared spectral energy distributions of the SWIRE-MAMBO sources and of SMGs. The mid-infrared spectra, available for a handful of sources, exhibit strong polycyclic aromatic hydrocarbon (PAH) features, and a warm dust continuum. The warm dust continuum contributes ~34% of the mid-infrared emission, and is likely associated with an AGN component. This contribution is consistent with what is found in SMGs. The large 24 \u03bcm/1.2 mm flux ratios are thus not due to AGN emission, but rather to enhanced PAH emission compared to SMGs. The analysis of the stacked far-infrared fluxes yields warmer dust temperatures than typically observed in SMGs. Our selection favors warm ultraluminous infrared sources at high-z, a class of objects that is rarely found in SMG samples. Indeed SMGs are not common among bright 24 \u03bcm sources (e.g., only about 20% of SMGs have f_(24 \u03bcm) > 0.4 mJy). Our sample is the largest Spitzer-selected sample detected at millimeter wavelengths currently available.",
"doi": "10.1088/0004-637X/692/1/422",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-02-10",
"series_number": "1",
"volume": "692",
"issue": "1",
"pages": "422-442"
},
{
"id": "authors:1kksd-g4d63",
"collection": "authors",
"collection_id": "1kksd-g4d63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090408-080213990",
"type": "article",
"title": "The contribution of AGNs and star-forming galaxies to the mid-infrared as revealed by their spectral energy distributions",
"author": [
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056",
"clpid": "Gruppioni-C"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"clpid": "Pozzi-F"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"clpid": "Zamorani-G"
},
{
"family_name": "La Franca",
"given_name": "F.",
"clpid": "La-Franca-F"
},
{
"family_name": "Sacchi",
"given_name": "N.",
"clpid": "Sacchi-N"
},
{
"family_name": "Comastri",
"given_name": "A.",
"orcid": "0000-0003-3451-9970",
"clpid": "Comastri-A"
},
{
"family_name": "Pozzetti",
"given_name": "L.",
"clpid": "Pozzetti-L"
},
{
"family_name": "Vignali",
"given_name": "C.",
"orcid": "0000-0002-8853-9611",
"clpid": "Vignali-C"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Matute",
"given_name": "I.",
"orcid": "0000-0003-1177-3896",
"clpid": "Matute-I"
},
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
}
],
"abstract": "We present the broadband SEDs of the largest available highly complete (72%) spectroscopic sample of MIR-selected galaxies and AGNs at intermediate redshift. The sample contains 203 extragalactic sources from the 15 \u03bcm ELAIS-SWIRE survey, all with measured spectroscopic redshift. Most of these sources have full multiwavelength coverage from the FUV (GALEX) to the FIR (Spitzer) and lie in the redshift range 0.1 < z < 1.3. This large sample allows us for the first time to characterize the spectral properties of sources responsible for the strong evolution observed in the MIR. Based on SED-fitting, we have classified the MIR sources, identifying AGN signatures in about 50% of them. This fraction is significantly higher than that derived from optical spectroscopy (~29%) and is due in particular to the identification of AGN activity in objects spectroscopically classified as galaxies (the spectroscopic classification may be somewhat unreliable because of host galaxy dilution in the optical). It is likely that in most of our objects, the AGN is either obscured or low luminosity, and thus dominates the energetic output only in the MIR, showing up just in the range where the host galaxy SED has a minimum. The fraction of AGNs strongly depends on flux density, with that derived through the SED-fitting about 20% at S15\u03bcm ~ 0.5\u20131 mJy and gradually increasing to 100% at S15\u03bcm > 10 mJy, while that obtained from optical spectroscopy is never >30%, even at higher flux densities. Our results will be very useful for updating all models aimed at interpreting the deep IR survey data and in particular for constraining the nature and role of dust-obscured systems in the intermediate/high-redshift universe.",
"doi": "10.1086/589848",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-09-01",
"series_number": "1",
"volume": "684",
"issue": "1",
"pages": "136-152"
},
{
"id": "authors:vb4tc-3g895",
"collection": "authors",
"collection_id": "vb4tc-3g895",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090424-093028091",
"type": "article",
"title": "The SCUBA Half-Degree Extragalactic Survey (SHADES) \u2013 VIII. the nature of faint submillimetre galaxies in SHADES, SWIRE and SXDF surveys",
"author": [
{
"family_name": "Clements",
"given_name": "D. L.",
"orcid": "0000-0002-9548-5033",
"clpid": "Clements-David-L"
},
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Babbedge",
"given_name": "T.",
"clpid": "Babbedge-Thomas-S-R"
},
{
"family_name": "Oliver",
"given_name": "S.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-Michael"
},
{
"family_name": "Davoodi",
"given_name": "P.",
"clpid": "Davoodi-P"
},
{
"family_name": "Ivison",
"given_name": "R.",
"orcid": "0000-0001-5118-1313",
"clpid": "Ivison-Rob-J"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Dunlop",
"given_name": "J.",
"clpid": "Dunlop-J"
},
{
"family_name": "Shupe",
"given_name": "Dave",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Waddington",
"given_name": "I.",
"clpid": "Waddington-Ian"
},
{
"family_name": "Simpson",
"given_name": "C.",
"clpid": "Simpson-C"
},
{
"family_name": "Furusawa",
"given_name": "H.",
"clpid": "Furusawa-H"
},
{
"family_name": "Serjeant",
"given_name": "S.",
"orcid": "0000-0002-0517-7943",
"clpid": "Serjeant-Stephen"
},
{
"family_name": "Afonso-Luis",
"given_name": "A.",
"clpid": "Afonso-Luis-A"
},
{
"family_name": "Alexander",
"given_name": "D. M.",
"orcid": "0000-0002-5896-6313",
"clpid": "Alexander-David-M"
},
{
"family_name": "Aretxaga",
"given_name": "I.",
"orcid": "0000-0002-6590-3994",
"clpid": "Aretxaga-Itziar"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Borys",
"given_name": "C.",
"clpid": "Borys-Colin-J-K"
},
{
"family_name": "Chapman",
"given_name": "S.",
"clpid": "Chapman-Scott-C"
},
{
"family_name": "Coppin",
"given_name": "K.",
"clpid": "Coppin-Kristen-E-K"
},
{
"family_name": "Dunne",
"given_name": "L.",
"clpid": "Dunne-Loretta"
},
{
"family_name": "Dye",
"given_name": "S.",
"clpid": "Dye-Simon"
},
{
"family_name": "Eales",
"given_name": "S. A.",
"clpid": "Eales-Stephen-A"
},
{
"family_name": "Evans",
"given_name": "T.",
"orcid": "0000-0001-5442-1300",
"clpid": "Evans-T-Matthew"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-David-T"
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{
"family_name": "Fox",
"given_name": "M.",
"clpid": "Fox-M"
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{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W"
},
{
"family_name": "Greve",
"given_name": "T.R.",
"orcid": "0000-0002-2554-1837",
"clpid": "Greve-Thomas-R"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-Mark"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-David-H"
},
{
"family_name": "Jennes",
"given_name": "T.",
"clpid": "Jennes-T"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Mortier",
"given_name": "A. M. J.",
"clpid": "Mortier-Angela-M-J"
},
{
"family_name": "Page",
"given_name": "M. J.",
"orcid": "0000-0002-6689-6271",
"clpid": "Page-Mathew-J"
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{
"family_name": "Pope",
"given_name": "A.",
"orcid": "0000-0001-8592-2706",
"clpid": "Pope-Alexandra"
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{
"family_name": "Priddey",
"given_name": "R. S.",
"clpid": "Priddey-Robert-S"
},
{
"family_name": "Rawlings",
"given_name": "S.",
"clpid": "Rawlings-Stephen-L"
},
{
"family_name": "Savage",
"given_name": "R. S.",
"clpid": "Savage-R-S"
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{
"family_name": "Scott",
"given_name": "D.",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
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{
"family_name": "Scott",
"given_name": "S. E.",
"clpid": "Scott-S-E"
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{
"family_name": "Sekiguchi",
"given_name": "K.",
"orcid": "0000-0003-3168-7776",
"clpid": "Sekiguchi-Kazuhiro"
},
{
"family_name": "Smail",
"given_name": "I.",
"orcid": "0000-0003-3037-257X",
"clpid": "Smail-Ian-R"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-Harding-E"
},
{
"family_name": "Stevens",
"given_name": "J. A.",
"clpid": "Stevens-Jason-A"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-Jason-A"
},
{
"family_name": "Takagi",
"given_name": "T.",
"clpid": "Takagi-Toshinobu"
},
{
"family_name": "van Kampen",
"given_name": "E.",
"orcid": "0000-0002-6327-5154",
"clpid": "van-Kampen-Eelco"
}
],
"abstract": "We present the optical-to-submillimetre spectral energy distributions (SEDs) for 33 radio and mid-infrared (mid-IR) identified submillimetre galaxies discovered via the SHADES 850-\u03bcm SCUBA imaging in the Subaru-XMM Deep Field (SXDF). Optical data for the sources come from the SXDF and mid- and far-IR fluxes from SWIRE. We obtain photometric redshift estimates for our sources using optical and IRAC 3.6- and 4.5-\u03bcm fluxes. We then fit SED templates to the longer wavelength data to determine the nature of the far-IR emission that dominates the bolometric luminosity of these sources. The IR template fits are also used to resolve ambiguous identifications and cases of redshift aliasing. The redshift distribution obtained broadly matches previous results for submillimetre sources and on the SHADES SXDF field. Our template fitting finds that active galactic nuclei, while present in about 10 per cent of our sources, do not contribute significantly to their bolometric luminosity. Dust heating by starbursts, with either Arp220 or M82 type SEDs, appears to be responsible for the luminosity in most sources (23/33 are fitted by Arp220 templates, 2/33 by the warmer M82 templates). 8/33 sources, in contrast, are fitted by a cooler cirrus dust template, suggesting that cold dust has a role in some of these highly luminous objects. Three of our sources appear to have multiple identifications or components at the same redshift, but we find no statistical evidence that close associations are common among our SHADES sources. Examination of rest-frame K-band luminosity suggests that 'downsizing' is underway in the submillimetre galaxy population, with lower redshift systems lying in lower mass host galaxies. Of our 33 identifications six are found to be of lower reliability but their exclusion would not significantly alter our conclusions.",
"doi": "10.1111/j.1365-2966.2008.13172.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2008-06-11",
"series_number": "1",
"volume": "387",
"issue": "1",
"pages": "247-267"
},
{
"id": "authors:vd38b-pcx23",
"collection": "authors",
"collection_id": "vd38b-pcx23",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:HATmnras08",
"type": "article",
"title": "Properties of dusty tori in active galactic nuclei \u2013 I. The case of SWIRE/SDSS quasars",
"author": [
{
"family_name": "Hatziminaoglou",
"given_name": "E.",
"clpid": "Hatziminaoglou-E"
},
{
"family_name": "Fritz",
"given_name": "J.",
"clpid": "Fritz-J"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Afonso-Luis",
"given_name": "A.",
"clpid": "Afonso-Luis-A"
},
{
"family_name": "Hern\u00e1n-Caballero",
"given_name": "A.",
"clpid": "Hern\u00e1n-Caballero-A"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "I.",
"clpid": "P\u00e9rez-Fournon-I"
},
{
"family_name": "Serjeant",
"given_name": "S.",
"orcid": "0000-0002-0517-7943",
"clpid": "Serjeant-S"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Oliver",
"given_name": "S. A.",
"clpid": "Oliver-S-A"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
}
],
"abstract": "We derive the properties of dusty tori in active galactic nuclei from the comparison of observed spectral energy distributions (SEDs) of SDSS quasars and a precomputed grid of torus models. The observed SEDs comprise SDSS photometry, Two-Micron All-Sky Survey J, H and K data, whenever available, and mid-infrared (mid-IR) data from the Spitzer Wide-area InfraRed Extragalactic Survey. The adopted model is that of Fritz, Franceschini & Hatziminaoglou. The fit is performed by standard \u03c72 -minimization; the model, however, can be a multicomponent comprising a stellar and a starburst component, whenever necessary. Models with low equatorial optical depth, \u03c49.7, were allowed as well as 'traditional' models with \u03c49.7\u2265 1.0 , corresponding to AV\u2265 22 and the results were compared. Fits using high optical depth tori models only produced dust more compactly distributed than in the configuration where all \u03c49.7 models were permitted. Tori with decreasing dust density with the distance from the centre were favoured while there was no clear preference for models with or without angular variation of the dust density. The computed outer radii of the tori are of some tens of parsecs large but can reach, in a few cases, a few hundreds of parsecs. The mass of dust, MDust, and IR luminosity, LIR, integrated in the wavelength range between 1 and 1000 \u03bcm, do not show significant variations with redshift, once the observational biases are taken into account. Objects with 70-\u03bcm detections, representing 25 per cent of the sample, are studied separately and the starburst contribution (whenever present) to the IR luminosity can reach, in the most extreme but very few cases, 80 per cent.",
"doi": "10.1111/j.1365-2966.2008.13119.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2008-05-21",
"series_number": "3",
"volume": "386",
"issue": "3",
"pages": "1252-1264"
},
{
"id": "authors:jvgf4-pvw66",
"collection": "authors",
"collection_id": "jvgf4-pvw66",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090723-082907868",
"type": "article",
"title": "Photometric redshifts in the SWIRE survey",
"author": [
{
"family_name": "Rowan-Robinson",
"given_name": "Michael",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Babbedge",
"given_name": "Tom",
"clpid": "Babbedge-T-S-R"
},
{
"family_name": "Oliver",
"given_name": "Seb",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Trichas",
"given_name": "Markos",
"clpid": "Trichas-M"
},
{
"family_name": "Berta",
"given_name": "Stefano",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Lonsdale",
"given_name": "Carol",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Smith",
"given_name": "Gene",
"clpid": "Smith-Gene"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Arnouts",
"given_name": "Stephane",
"clpid": "Arnouts-S"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397",
"clpid": "Ilbert-Olivier"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "Olivier",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-O"
},
{
"family_name": "Afonso-Luis",
"given_name": "Alejandro",
"clpid": "Afonso-Luis-A"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "Ismael",
"clpid": "P\u00e9rez-Fournon-I"
},
{
"family_name": "Hatziminaoglou",
"given_name": "Evanthia",
"clpid": "Hatziminaoglou-E"
},
{
"family_name": "Polletta",
"given_name": "Mari",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Farrah",
"given_name": "Duncan",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Vaccari",
"given_name": "Mattia",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
}
],
"abstract": "We present the SWIRE Photometric Redshift Catalogue 1 025 119 redshifts of unprecedented reliability and of accuracy comparable with or better than previous work. Our methodology is based on fixed galaxy and quasi-stellar object templates applied to data at 0.36\u20134.5 \u03bcm, and on a set of four infrared emission templates fitted to infrared excess data at 3.6\u2013170 \u03bcm. The galaxy templates are initially empirical, but are given greater physical validity by fitting star formation histories to them, which also allows us to estimate stellar masses. The code involves two passes through the data, to try to optimize recognition of active galactic nucleus (AGN) dust tori. A few carefully justified priors are used and are the key to supression of outliers. Extinction, A_V , is allowed as a free parameter. The full reduced \u03c7^2_\u03bd (z) distribution is given for each source, so the full error distribution can be used, and aliases investigated.\n\nWe use a set of 5982 spectroscopic redshifts, taken from the literature and from our own spectroscopic surveys, to analyse the performance of our method as a function of the number of photometric bands used in the solution and the reduced \u03c7^2_\u03bd . For seven photometric bands (5 optical + 3.6, 4.5 \u03bcm), the rms value of (z_(phot)\u2212z_(spec)/(1 +z_(spec) is 3.5 per cent, and the percentage of catastrophic outliers [defined as >15 per cent error in (1 +z)], is \u223c1 per cent. These rms values are comparable with the best achieved in other studies, and the outlier fraction is significantly better. The inclusion of the 3.6- and 4.5-\u03bcm IRAC bands is crucial in supression of outliers.\n\nWe discuss the redshift distributions at 3.6 and 24 \u03bcm. In individual fields, structure in the redshift distribution corresponds to clusters which can be seen in the spectroscopic redshift distribution, so the photometric redshifts are a powerful tool for large-scale structure studies. 10 per cent of sources in the SWIRE photometric redshift catalogue have z > 2, and 4 per cent have z > 3, so this catalogue is a huge resource for high-redshift galaxies.\n\nA key parameter for understanding the evolutionary status of infrared galaxies is L_(ir)/L_(opt) . For cirrus galaxies this is a measure of the mean extinction in the interstellar medium of the galaxy. There is a population of ultraluminous galaxies with cool dust and we have shown SEDs for some of the reliable examples. For starbursts, we estimate the specific star formation rate, \u03c6_*/M_* . Although the very highest values of this ratio tend to be associated with Arp220 starbursts, by no means all ultraluminous galaxies are. We discuss an interesting population of galaxies with elliptical-like spectral energy distributions in the optical and luminous starbursts in the infrared.\n\nFor dust tori around type 1 AGN, L_(tor)/L_(opt) is a measure of the torus covering factor and we deduce a mean covering factor of 40 per cent.\n\nOur infrared templates also allow us to estimate dust masses for all galaxies with an infrared excess.",
"doi": "10.1111/j.1365-2966.2008.13109.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2008-05-11",
"series_number": "2",
"volume": "386",
"issue": "2",
"pages": "697-714"
},
{
"id": "authors:j398p-45171",
"collection": "authors",
"collection_id": "j398p-45171",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090427-091319525",
"type": "article",
"title": "High-redshift QSOs in the SWIRE Survey and the z~3 QSO luminosity function",
"author": [
{
"family_name": "Siana",
"given_name": "Brian",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Polletta",
"given_name": "Maria del Carmen",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Smith",
"given_name": "Harding E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Lonsdale",
"given_name": "Carol J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Gonzalez-Solares",
"given_name": "Eduardo",
"clpid": "Gonzalez-Solares-E"
},
{
"family_name": "Farrah",
"given_name": "Duncan",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Babbedge",
"given_name": "Tom S. R.",
"clpid": "Babbedge-T-S-R"
},
{
"family_name": "Rowan-Robinson",
"given_name": "Michael",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "David",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Fang",
"given_name": "Fan",
"clpid": "Fang-Fan"
},
{
"family_name": "Franceschini",
"given_name": "Alberto",
"clpid": "Franceschini-A"
},
{
"family_name": "Oliver",
"given_name": "Seb",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
}
],
"abstract": "We use a simple optical/infrared (IR) photometric selection of high-redshift QSOs that identifies a Lyman break in the optical photometry and requires a red IR color to distinguish QSOs from common interlopers. The search yields 100 z ~ 3 (U-dropout) QSO candidates with 19 < r' < 22 over 11.7 deg^2 in the ELAIS-N1 (EN1) and ELAIS-N2 (EN2) fields of the Spitzer Wide-area Infrared Extragalactic (SWIRE) Legacy Survey. The z ~ 3 selection is reliable, with spectroscopic follow-up of 10 candidates confirming that they are all QSOs at 2.83 < z < 3.44. We find that our z ~ 4 (g'-dropout) sample suffers from both unreliability and incompleteness but present seven previously unidentified QSOs at 3.50 < z < 3.89. Detailed simulations show our z ~ 3 completeness to be ~80%-90% from 3.0 < z < 3.5, significantly better than the ~30%-80% completeness of the SDSS at these redshifts. The resulting luminosity function extends 2 mag fainter than SDSS and has a faint-end slope of \u03b2 = \u2212 1.42 \u00b1 0.15, consistent with values measured at lower redshift. Therefore, we see no evidence for evolution of the faint-end slope of the QSO luminosity function. Including the SDSS QSO sample, we have now directly measured the space density of QSOs responsible for ~70% of the QSO UV luminosity density at z ~ 3. We derive a maximum rate of H I photoionization from QSOs at z ~ 3.2, \u0393 = 4.8 \u00d7 10^(\u221213) s^(\u22121), about half of the total rate inferred through studies of the Ly\u03b1 forest. Therefore, star-forming galaxies and QSOs must contribute comparably to the photoionization of H I in the intergalactic medium at z ~ 3.",
"doi": "10.1086/527025",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-03-01",
"series_number": "1",
"volume": "675",
"issue": "1",
"pages": "49-70"
},
{
"id": "authors:1exvj-51536",
"collection": "authors",
"collection_id": "1exvj-51536",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090428-130122358",
"type": "article",
"title": "Galaxy counts at 24 \u03bcm in the SWIRE fields",
"author": [
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Rowan-Robinson",
"given_name": "Michael",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Lonsdale",
"given_name": "Carol J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Evans",
"given_name": "Tracey",
"clpid": "Evans-Tracey"
},
{
"family_name": "Fang",
"given_name": "Fan",
"clpid": "Fang-Fan"
},
{
"family_name": "Oliver",
"given_name": "Sebastian",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Vaccari",
"given_name": "Mattia",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Rodighiero",
"given_name": "Giulia",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-G"
},
{
"family_name": "Padgett",
"given_name": "Deborah",
"orcid": "0000-0001-5334-5107",
"clpid": "Padgett-D-L"
},
{
"family_name": "Surace",
"given_name": "Jason A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Xu",
"given_name": "C. Kevin",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Berta",
"given_name": "Stefano",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Pozzi",
"given_name": "Francesca",
"orcid": "0000-0002-7412-647X",
"clpid": "Pozzi-F"
},
{
"family_name": "Franceschini",
"given_name": "Alberto",
"orcid": "0000-0002-9979-3383",
"clpid": "Franceschini-A"
},
{
"family_name": "Babbedge",
"given_name": "Thomas",
"clpid": "Babbedge-T"
},
{
"family_name": "Gonzales-Solares",
"given_name": "Eduardo",
"orcid": "0000-0001-9123-0626",
"clpid": "Gonzales-Solares-E-A"
},
{
"family_name": "Siana",
"given_name": "Brian D.",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Farrah",
"given_name": "Duncan",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Frayer",
"given_name": "David T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Polletta",
"given_name": "Maria del Carmen",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Owen",
"given_name": "Frazer",
"clpid": "Owen-F-N"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "Ismael",
"clpid": "P\u00e9rez-Fournon-I"
}
],
"abstract": "This paper presents galaxy source counts at 24 \u03bcm in the six Spitzer Wide-field InfraRed Extragalactic (SWIRE) fields. The source counts are compared to counts in other fields, and to model predictions that have been updated since the launch of Spitzer. This analysis confirms a very steep rise in the Euclidean-normalized differential number counts between 2 mJy and 0.3 mJy. Variations in the counts between fields show the effects of sample variance in the flux range of 0.5-10 mJy, up to 100% larger than Poisson errors. Nonetheless, a \"shoulder\" in the normalized counts persists at around 3 mJy. The peak of the normalized counts at 0.3 mJy is higher and narrower than most models predict. In the ELAIS N1 field, the 24 \u03bcm data are combined with Spitzer-IRAC data and five-band optical imaging, and these band-merged data are fit with photometric redshift templates. Above 1 mJy the counts are dominated by galaxies at z < 0.3. By 300 \u03bcJy, about 25% are between z ~ 0.3 and 0.8, and a significant fraction are at z ~ 1.3-2. At low redshifts the counts are dominated by spirals, and starbursts rise in number density to outnumber the spirals' contribution to the counts below 1 mJy.",
"doi": "10.1088/0004-6256/135/3/1050",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2008-03",
"series_number": "3",
"volume": "135",
"issue": "3",
"pages": "1050-1056"
},
{
"id": "authors:z1mwa-0sr64",
"collection": "authors",
"collection_id": "z1mwa-0sr64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091016-143908375",
"type": "article",
"title": "The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function",
"author": [
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Savage",
"given_name": "R. S.",
"clpid": "Savage-R-S"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Buttery",
"given_name": "H.",
"clpid": "Buttery-H"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"clpid": "Cimatti-A"
},
{
"family_name": "Dias",
"given_name": "J.",
"clpid": "Dias-J-E"
},
{
"family_name": "Feruglio",
"given_name": "C.",
"clpid": "Feruglio-C"
},
{
"family_name": "Fiore",
"given_name": "F.",
"clpid": "Fiore-F"
},
{
"family_name": "Held",
"given_name": "E. V.",
"clpid": "Held-E-V"
},
{
"family_name": "La Franca",
"given_name": "F.",
"clpid": "La-Franca-F"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"clpid": "Maiolino-R"
},
{
"family_name": "Marconi",
"given_name": "A.",
"clpid": "Marconi-A"
},
{
"family_name": "Matute",
"given_name": "I.",
"orcid": "0000-0003-1177-3896",
"clpid": "Matute-I"
},
{
"family_name": "Oliver",
"given_name": "S. J.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Ricciardelli",
"given_name": "E.",
"clpid": "Ricciardelli-E"
},
{
"family_name": "Rubele",
"given_name": "S.",
"clpid": "Rubele-S"
},
{
"family_name": "Sacchi",
"given_name": "N.",
"clpid": "Sacchi-N"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
}
],
"abstract": "Context. In the last couple of years a population of very massive (M_* > 10^(11) M_\u2299), high-redshift (z \u2265 2) galaxies has been identified, but its role in galaxy evolution has not yet been fully understood.\n\nAims. It is necessary to perform a systematic study of high-redshift massive galaxies, in order to determine the shape of the very\nmassive tail of the stellar mass function and determine the epoch of their assembly.\n\nMethods. We selected high-z massive galaxies at 5.8 \u03bcm, in the SWIRE ELAIS-S1 field (1 deg^2). Galaxies with the 1.6 \u03bcm stellar\npeak redshifted into the IRAC bands (z \u2243 1\u22123, called \"IR-peakers\") were identified. Stellar masses were derived by means of spectrophotometric fitting and used to compute the stellar mass function (MF) at z = 1\u22122 and 2\u22123. A parametric fit to the MF was performed, based on a Bayesian formalism, and the stellar mass density of massive galaxies above z = 2 determined.\n\nResults. We present the first systematic study of the very-massive tail of the galaxy stellar mass function at high redshift. A total of 326 sources were selected. The majority of these galaxies have stellar masses in excess of 10^(11) M_\u2299 and lie at z > 1.5. The availability of mid-IR data turned out to be a valuable tool to constrain the contribution of young stars to galaxy SEDs, and thus their M_*/L ratio. The influence of near-IR data and of the chosen stellar library on the SED fitting are also discussed. The z = 2\u22123 stellar mass function between 10^(11) and ~10^(12) M_\u2299 is probed with unprecedented detail. A significant evolution is found not only for galaxies with M ~ 10^(11) M_\u2299, but also in the highest mass bins considered. The comoving number density of these galaxies was lower by more than a factor of 10 at z = 2\u22123, with respect to the local estimate. SWIRE 5.8 \u03bcm peakers more massive than 1.6 \u00d7 10^(11) M_\u2299 provide 30\u221250% of the total stellar mass density in galaxies at z = 2\u22123.",
"doi": "10.1051/0004-6361:20077491",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2007-12",
"series_number": "1",
"volume": "476",
"issue": "1",
"pages": "151-175"
},
{
"id": "authors:b52a4-nt324",
"collection": "authors",
"collection_id": "b52a4-nt324",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091117-111643880",
"type": "article",
"title": "IR and UV Galaxies at z = 0.6: Evolution of Dust Attenuation and Stellar Mass as Revealed by SWIRE and GALEX",
"author": [
{
"family_name": "Xu",
"given_name": "C. Kevin",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Shupe",
"given_name": "David",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Buat",
"given_name": "Veronique",
"clpid": "Buat-V"
},
{
"family_name": "Rowan-Robinson",
"given_name": "Michael",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Babbedge",
"given_name": "Thomas",
"clpid": "Babbedge-T"
},
{
"family_name": "Iglesias-P\u00e1ramo",
"given_name": "Jorge",
"clpid": "Iglesias-P\u00e1ramo-J"
},
{
"family_name": "Takeuchi",
"given_name": "Tsutomu T.",
"clpid": "Takeuchi-Tsutomu-T"
},
{
"family_name": "Barlow",
"given_name": "Tom A.",
"clpid": "Barlow-T-A"
},
{
"family_name": "Conrow",
"given_name": "Tim",
"clpid": "Conrow-T"
},
{
"family_name": "Fang",
"given_name": "Fan",
"clpid": "Fang-Fan"
},
{
"family_name": "Forster",
"given_name": "Karl",
"orcid": "0000-0001-5800-5531",
"clpid": "Forster-K"
},
{
"family_name": "Friedman",
"given_name": "Peter G.",
"clpid": "Friedman-P-G"
},
{
"family_name": "Gonzalez-Solares",
"given_name": "Eduardo",
"clpid": "Gonzalez-Solares-E"
},
{
"family_name": "Lonsdale",
"given_name": "Carol",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Martin",
"given_name": "D. Christopher",
"orcid": "0000-0002-8650-1644",
"clpid": "Martin-D-Christopher"
},
{
"family_name": "Morrissey",
"given_name": "Patrick",
"orcid": "0000-0001-8177-1023",
"clpid": "Morrissey-P"
},
{
"family_name": "Neff",
"given_name": "Susan G.",
"clpid": "Neff-S-G"
},
{
"family_name": "Schiminovich",
"given_name": "David",
"clpid": "Schiminovich-D"
},
{
"family_name": "Seibert",
"given_name": "Mark",
"orcid": "0000-0002-1143-5515",
"clpid": "Seibert-M"
},
{
"family_name": "Small",
"given_name": "Todd",
"clpid": "Small-T"
},
{
"family_name": "Smith",
"given_name": "Gene",
"clpid": "Smith-Gene"
},
{
"family_name": "Surace",
"given_name": "Jason",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Wyder",
"given_name": "Ted K.",
"clpid": "Wyder-T-K"
}
],
"abstract": "We study dust attenuation and stellar mass of z ~ 0.6 star-forming galaxies using new SWIRE observations in IR and GALEX observations in UV. Two samples are selected from the SWIRE and GALEX source catalogs in the SWIRE/GALEX field ELAIS-N1-00 (\u03a9 = 0.8 deg^2). The UV-selected sample has 600 galaxies with photometric redshift (hereafter photo-z) 0.5 \u2264 z \u2264 0.7 and NUV \u2264 23.5 (corresponding to L_(FUV) \u2265 10^(9.6) L_\u2609). The IR-selected sample contains 430 galaxies with f_(24 \u03bcm) \u2265 0.2 mJy (L_(dust) \u2265 10^(10.8) L_\u2609) in the same photo-z range. It is found that the mean L_(dust)/L_(FUV) ratios of the z = 0.6 UV galaxies are consistent with that of their z = 0 counterparts of the same L_(FUV). For IR galaxies, the mean L_(dust)/L_(FUV) ratios of the z = 0.6 LIRGs (L_(dust) ~ 10^(11) L_\u2609) are about a factor of 2 lower than local LIRGs, whereas z = 0.6 ULIRGs (L_(dust) ~ 10^(12) L_\u2609) have the same mean L_(dust)/L_(FUV) ratios as their local counterparts. This is consistent with the hypothesis that the dominant component of LIRG population has changed from large, gas-rich spirals at z > 0.5 to major mergers at z = 0. The stellar mass of z = 0.6 UV galaxies of L_(FUV) \u2264 10^(10.2) L_\u2609 is about a factor of 2 less than their local counterparts of the same luminosity, indicating growth of these galaxies. The mass of z = 0.6 UV luminous galaxies (UVLGs: L_(FUV) > 10^(10.2) L_\u2609) and IR-selected galaxies, which are nearly exclusively LIRGs and ULIRGs, is the same as their local counterparts.",
"doi": "10.1086/516641",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2007-12",
"series_number": "2",
"volume": "173",
"issue": "2",
"pages": "432-440"
},
{
"id": "authors:bd25f-z8615",
"collection": "authors",
"collection_id": "bd25f-z8615",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100222-135706376",
"type": "article",
"title": "UV to IR SEDs of UV-Selected Galaxies in the ELAIS Fields: Evolution of Dust Attenuation and Star Formation Activity from z = 0.7 to 0.2",
"author": [
{
"family_name": "Iglesias-P\u00e1ramo",
"given_name": "J.",
"clpid": "Iglesias-P\u00e1ramo-J"
},
{
"family_name": "Buat",
"given_name": "V.",
"clpid": "Buat-V"
},
{
"family_name": "Hern\u00e1ndez-Fern\u00e1ndez",
"given_name": "J.",
"clpid": "Hern\u00e1ndez-Fern\u00e1ndez-J"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
},
{
"family_name": "Burgarella",
"given_name": "D.",
"clpid": "Burgarella-D"
},
{
"family_name": "Takeuchi",
"given_name": "T. T.",
"clpid": "Takeuchi-Tsutomu-T"
},
{
"family_name": "Boselli",
"given_name": "A.",
"clpid": "Boselli-A"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Babbedge",
"given_name": "T.",
"clpid": "Babbedge-T"
},
{
"family_name": "Conrow",
"given_name": "T.",
"clpid": "Conrow-T"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Gonz\u00e1lez-Solares",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Solares-E"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Smith",
"given_name": "G.",
"clpid": "Smith-Gene"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Barlow",
"given_name": "T. A.",
"clpid": "Barlow-T-A"
},
{
"family_name": "Forster",
"given_name": "K.",
"orcid": "0000-0001-5800-5531",
"clpid": "Forster-K"
},
{
"family_name": "Friedman",
"given_name": "P. G.",
"clpid": "Friedman-P-G"
},
{
"family_name": "Martin",
"given_name": "D. C.",
"orcid": "0000-0002-8650-1644",
"clpid": "Martin-D-Christopher"
},
{
"family_name": "Morrissey",
"given_name": "P.",
"orcid": "0000-0001-8177-1023",
"clpid": "Morrissey-P"
},
{
"family_name": "Neff",
"given_name": "S. G.",
"clpid": "Neff-S-G"
},
{
"family_name": "Schiminovich",
"given_name": "D.",
"clpid": "Schiminovich-D"
},
{
"family_name": "Seibert",
"given_name": "M.",
"orcid": "0000-0002-1143-5515",
"clpid": "Seibert-M"
},
{
"family_name": "Small",
"given_name": "T.",
"clpid": "Small-T"
},
{
"family_name": "Wyder",
"given_name": "T. K.",
"clpid": "Wyder-T-K"
},
{
"family_name": "Bianchi",
"given_name": "L.",
"clpid": "Bianchi-L"
},
{
"family_name": "Donas",
"given_name": "J.",
"clpid": "Donas-J"
},
{
"family_name": "Heckman",
"given_name": "T. M.",
"clpid": "Heckman-T-M"
},
{
"family_name": "Lee",
"given_name": "Y.-W.",
"clpid": "Lee-Young-Wook"
},
{
"family_name": "Madore",
"given_name": "B. F.",
"orcid": "0000-0002-1576-1676",
"clpid": "Madore-B-F"
},
{
"family_name": "Milliard",
"given_name": "B.",
"clpid": "Milliard-B"
},
{
"family_name": "Rich",
"given_name": "R. M.",
"orcid": "0000-0003-0427-8387",
"clpid": "Rich-R-M"
},
{
"family_name": "Szalay",
"given_name": "A. S.",
"clpid": "Szalay-A-S"
},
{
"family_name": "Welsh",
"given_name": "B. Y.",
"clpid": "Welsh-B-Y"
},
{
"family_name": "Yi",
"given_name": "S. K.",
"clpid": "Yi-Sukyoung-K"
}
],
"abstract": "We study the ultraviolet to far-infrared (hereafter UV-to-IR) SEDs of a sample of intermediate-redshift (0.2 \u2264 z \u2264 0.7) UV-selected galaxies from the ELAIS N1 and ELAIS N2 fields by fitting a multi-wavelength data set to a library of GRASIL templates. Star formation related properties of the galaxies are derived from the library of models by using Bayesian statistics. We find a decreasing presence of galaxies with low attenuation and low total luminosity as redshift decreases, which does not hold for high total luminosity galaxies. In addition, the dust attenuation of low-mass galaxies increases as redshift decreases, and this trend seems to disappear for galaxies with M_* \u2265 10^(11) M_\u2299. This result is consistent with a mass-dependent evolution of the dust-to-gas ratio, which could be driven by a mass-dependent efficiency of star formation in star-forming galaxies. The specific star formation rates (SSFR) decrease with increasing stellar mass at all redshifts, and for a given stellar mass the SSFR decreases with decreasing redshift. The differences in the slope of the M^*-SSFR relation found between this work and others at similar redshift could be explained by the adopted selection criteria of the samples, which for a UV-selected sample, favors blue, star-forming galaxies.",
"doi": "10.1086/521867",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2007-11-20",
"series_number": "1",
"volume": "670",
"issue": "1",
"pages": "279-294"
},
{
"id": "authors:whv5s-2x757",
"collection": "authors",
"collection_id": "whv5s-2x757",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091130-115833206",
"type": "article",
"title": "Clustering of galaxies at 3.6 \u03bcm in the Spitzer Wide-area Infrared Extragalactic legacy survey",
"author": [
{
"family_name": "Waddington",
"given_name": "I.",
"clpid": "Waddington-I"
},
{
"family_name": "Oliver",
"given_name": "S. J.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Babbedge",
"given_name": "T. S. R.",
"clpid": "Babbedge-T-S-R"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Gonzalez-Solares",
"given_name": "E. A.",
"clpid": "Gonzalez-Solares-E-A"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-G"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Xu",
"given_name": "C. K.",
"orcid": "0000-0002-1588-6700",
"clpid": "Xu-C-Kevin"
}
],
"abstract": "We investigate the clustering of galaxies selected in the 3.6 \u03bcm band of the Spitzer Wide-area Infrared Extragalactic (SWIRE) legacy survey. The angular two-point correlation function is calculated for 11 samples with flux limits of S_(3.6)\u2265 4\u2013400 \u03bcJy, over an 8 deg^2 field. The angular clustering strength is measured at >5\u03c3 significance at all flux limits, with amplitudes of A = (0.49\u201329) \u00d7 10^(\u22123) at 1\u00b0, for a power-law model, A\u03b8^(\u22120.8). We estimate the redshift distributions of the samples using phenomological models, simulations and photometric redshifts, and so derive the spatial correlation lengths. We compare our results with the Galaxies In Cosmological Simulations (GalICS) models of galaxy evolution and with parametrized models of clustering evolution. The GalICS simulations are consistent with our angular correlation functions, but fail to match the spatial clustering inferred from the phenomological models or the photometric redshifts. We find that the uncertainties in the redshift distributions of our samples dominate the statistical errors in our estimates of the spatial clustering. At low redshifts (median z \u2264 0.5), the comoving correlation length is approximately constant, r_0= 6.1 \u00b1 0.5 h^(\u22121) Mpc, and then decreases with increasing redshift to a value of 2.9 \u00b1 0.3 h^(\u22121) Mpc for the faintest sample, for which the median redshift is z ~ 1. We suggest that this trend can be attributed to a decrease in the average galaxy and halo mass in the fainter flux-limited samples, corresponding to changes in the relative numbers of early- and late-type galaxies. However, we cannot rule out strong evolution of the correlation length over 0.5 < z < 1 .",
"doi": "10.1111/j.1365-2966.2007.12367.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2007-11-11",
"series_number": "4",
"volume": "381",
"issue": "4",
"pages": "1437-1449"
},
{
"id": "authors:zpj90-chp97",
"collection": "authors",
"collection_id": "zpj90-chp97",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091203-110622102",
"type": "article",
"title": "VVDS-SWIRE - Clustering evolution from a spectroscopic sample of galaxies with redshift 0.2 < z < 2.1 selected from Spitzer IRAC 3.6 \u03bcm and 4.5 \u03bcm photometry",
"author": [
{
"family_name": "de la Torre",
"given_name": "S.",
"orcid": "0000-0002-0839-2884",
"clpid": "de-la-Torre-S"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-O"
},
{
"family_name": "Arnouts",
"given_name": "S.",
"clpid": "Arnouts-S"
},
{
"family_name": "Guzzo",
"given_name": "L.",
"clpid": "Guzzo-L"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Iovino",
"given_name": "A.",
"clpid": "Iovino-A"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Meneux",
"given_name": "B.",
"clpid": "Meneux-B"
},
{
"family_name": "Oliver",
"given_name": "S. J.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Pollo",
"given_name": "A.",
"clpid": "Pollo-A"
},
{
"family_name": "Waddington",
"given_name": "I.",
"clpid": "Waddington-I"
},
{
"family_name": "Bottini",
"given_name": "D.",
"clpid": "Bottini-D"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Garilli",
"given_name": "B.",
"clpid": "Garilli-B"
},
{
"family_name": "Le Brun",
"given_name": "V.",
"clpid": "Le-Brun-V"
},
{
"family_name": "Maccagni",
"given_name": "D.",
"clpid": "Maccagni-D"
},
{
"family_name": "Picat",
"given_name": "J. P.",
"clpid": "Picat-J-P"
},
{
"family_name": "Scaramella",
"given_name": "R.",
"clpid": "Scaramella-R"
},
{
"family_name": "Scodeggio",
"given_name": "M.",
"clpid": "Scodeggio-M"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Tresse",
"given_name": "L.",
"clpid": "Tresse-L"
},
{
"family_name": "Vettolani",
"given_name": "G.",
"clpid": "Vettolani-G"
},
{
"family_name": "Zanichelli",
"given_name": "A.",
"clpid": "Zanichelli-A"
},
{
"family_name": "Adami",
"given_name": "C.",
"clpid": "Adami-Christophe-ASTRO-FR"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"clpid": "Bardelli-S"
},
{
"family_name": "Bolzonella",
"given_name": "M.",
"clpid": "Bolzonella-M"
},
{
"family_name": "Cappi",
"given_name": "A.",
"clpid": "Cappi-A"
},
{
"family_name": "Charlot",
"given_name": "S.",
"clpid": "Charlot-S"
},
{
"family_name": "Ciliegi",
"given_name": "P.",
"clpid": "Ciliegi-P"
},
{
"family_name": "Contini",
"given_name": "T.",
"clpid": "Contini-T"
},
{
"family_name": "Foucaud",
"given_name": "S.",
"orcid": "0000-0001-5603-6262",
"clpid": "Foucaud-S"
},
{
"family_name": "Franzetti",
"given_name": "P.",
"clpid": "Franzetti-P"
},
{
"family_name": "Gavignaud",
"given_name": "I.",
"clpid": "Gavignaud-I"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397",
"clpid": "Ilbert-Olivier"
},
{
"family_name": "Lamareille",
"given_name": "F.",
"clpid": "Lamareille-F"
},
{
"family_name": "McCracken",
"given_name": "H. J.",
"orcid": "0000-0002-9489-7765",
"clpid": "McCracken-H-J"
},
{
"family_name": "Marano",
"given_name": "B.",
"clpid": "Marano-B"
},
{
"family_name": "Marinoni",
"given_name": "C.",
"clpid": "Marinoni-C"
},
{
"family_name": "Mazure",
"given_name": "A.",
"clpid": "Mazure-A"
},
{
"family_name": "Merighi",
"given_name": "R.",
"clpid": "Merighi-R"
},
{
"family_name": "Paltani",
"given_name": "S.",
"orcid": "0000-0002-8108-9179",
"clpid": "Paltani-S"
},
{
"family_name": "Pell\u00f2",
"given_name": "R.",
"clpid": "Pell\u00f2-R"
},
{
"family_name": "Pozzetti",
"given_name": "L.",
"clpid": "Pozzetti-L"
},
{
"family_name": "Radovich",
"given_name": "M.",
"clpid": "Radovich-M"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"clpid": "Zamorani-G"
},
{
"family_name": "Zucca",
"given_name": "E.",
"clpid": "Zucca-E"
},
{
"family_name": "Bondi",
"given_name": "M.",
"clpid": "Bondi-M"
},
{
"family_name": "Bongiorno",
"given_name": "A.",
"clpid": "Bongiorno-A"
},
{
"family_name": "Brinchmann",
"given_name": "J.",
"clpid": "Brinchmann-J"
},
{
"family_name": "Cucciati",
"given_name": "O.",
"orcid": "0000-0002-9336-7551",
"clpid": "Cucciati-O"
},
{
"family_name": "Mellier",
"given_name": "Y.",
"clpid": "Mellier-Y"
},
{
"family_name": "Merluzzi",
"given_name": "P.",
"clpid": "Merluzzi-P"
},
{
"family_name": "Temporin",
"given_name": "S.",
"clpid": "Temporin-S"
},
{
"family_name": "Vergani",
"given_name": "D.",
"clpid": "Vergani-D"
},
{
"family_name": "Walcher",
"given_name": "C. J.",
"clpid": "Walcher-C-J"
}
],
"abstract": "Aims. By combining data from the VIMOS VLT Deep Survey (VVDS) with the Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), we have built the currently largest spectroscopic sample of high redshift galaxies selected in the rest-frame near-infrared. We have obtained 2040 spectroscopic redshifts of galaxies with (m_(3.6))_(AB) < 21.5 at 3.6 \u03bcm, and 1255 spectroscopic redshifts of galaxies with (m_(4.5))_(AB) < 21. These allow us to investigate the clustering evolution of galaxies selected via their rest-frame near-infrared luminosity in the redshift range 0.2 < z < 2.1.\nMethods. We use the projected two-point correlation function w_p(r_p) to study the three dimensional clustering properties of galaxies detected at 3.6 \u03bcm and 4.5 \u03bcm with the InfraRed Array Camera (IRAC) in the SWIRE survey with measured spectroscopic redshifts from the first epoch VVDS. We compare these properties to those of a larger sample of 16672 SWIRE galaxies for which we have accurate photometric redshifts in the same field.\nResults. We find that in the 3.6 \u03bcm and 4.5 \u03bcmm flux limited samples, the apparent correlation length does not change from redshift ~2 to the present. The measured correlation lengths have a mean value of r_0 \u2243 3.9 \u00b1 0.5 h^(-1) Mpc for the galaxies selected at 3.6 \u03bcm and a mean value of r_0 \u2243 4.4 \u00b1 0.5 h^(-1) Mpc for the galaxies selected at 4.5 \u03bcm, across the whole redshift range explored. These values are larger than those typicaly found for I-band selected galaxies at I_(AB) < 24, for which r_0 varies from 2.69 h^(-1) Mpc to 3.63 h^(-1) Mpc between z = 0.5 to z = 2.1. We find that the difference in correlation length between I-band and 3.6-4.5 \u03bcm selected samples decreases with increasing redshift, becoming comparable at z \u2243 1.5. We interpret this as evidence that galaxies with older stellar populations and galaxies actively forming stars reside in comparably over-dense environments at epochs earlier than z \u2243 1.5, supporting the recently reported flattening of the color-density relation at high redshift. The increasing difference in correlation length with cosmic time observed between rest-frame UV-optical and near-infrared selected samples could then be an indication that star formation is gradually shifting to lower density regions with decreasing redshift, while the older, passively evolving galaxies remain in the most over-dense peaks.",
"doi": "10.1051/0004-6361:20077161",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2007-11",
"series_number": "2",
"volume": "475",
"issue": "2",
"pages": "443-451"
},
{
"id": "authors:8gsnz-h3480",
"collection": "authors",
"collection_id": "8gsnz-h3480",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ENGpasp07",
"type": "article",
"title": "Absolute Calibration and Characterization of the Multiband Imaging Photometer for Spitzer. I. The Stellar Calibrator Sample and the 24 \u03bcm Calibration",
"author": [
{
"family_name": "Engelbracht",
"given_name": "C. W.",
"clpid": "Engelbracht-C-W"
},
{
"family_name": "Blaylock",
"given_name": "M.",
"clpid": "Blaylock-M"
},
{
"family_name": "Su",
"given_name": "K. Y. L.",
"orcid": "0000-0002-3532-5580",
"clpid": "Su-Katherine-Y-L"
},
{
"family_name": "Rho",
"given_name": "J.",
"orcid": "0000-0003-3643-839X",
"clpid": "Rho-Jeonghee"
},
{
"family_name": "Rieke",
"given_name": "G. H.",
"orcid": "0000-0003-2303-6519",
"clpid": "Rieke-G-H"
},
{
"family_name": "Muzerolle",
"given_name": "J.",
"orcid": "0000-0002-5943-1222",
"clpid": "Muzerolle-J-C"
},
{
"family_name": "Padgett",
"given_name": "D. L.",
"orcid": "0000-0001-5334-5107",
"clpid": "Padgett-D-L"
},
{
"family_name": "Hines",
"given_name": "D. C.",
"orcid": "0000-0003-4653-6161",
"clpid": "Hines-D-C"
},
{
"family_name": "Gordon",
"given_name": "K. D.",
"clpid": "Gordon-K-D"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Noriega-Crespo",
"given_name": "A.",
"orcid": "0000-0002-6296-8960",
"clpid": "Noriega-Crespo-A"
},
{
"family_name": "Kelly",
"given_name": "D. M.",
"clpid": "Kelly-D-M"
},
{
"family_name": "Latter",
"given_name": "W. B.",
"clpid": "Latter-W-B"
},
{
"family_name": "Hinz",
"given_name": "J. L.",
"clpid": "Hinz-J-L"
},
{
"family_name": "Misselt",
"given_name": "K. A.",
"clpid": "Misselt-K-A"
},
{
"family_name": "Morrison",
"given_name": "J. E.",
"clpid": "Morrison-J-E"
},
{
"family_name": "Stansberry",
"given_name": "J. A.",
"clpid": "Stansberry-J-A"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Stolovy",
"given_name": "S.",
"clpid": "Stolovy-S-R"
},
{
"family_name": "Wheaton",
"given_name": "Wm. A.",
"clpid": "Wheaton-W-A"
},
{
"family_name": "Young",
"given_name": "E. T.",
"clpid": "Young-E-T"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
},
{
"family_name": "Wachter",
"given_name": "S.",
"clpid": "Wachter-Stefanie"
},
{
"family_name": "P\u00e9rez-Gonz\u00e1lez",
"given_name": "P. G.",
"orcid": "0000-0003-4528-5639",
"clpid": "P\u00e9rez-Gonz\u00e1lez-P-G"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Marleau",
"given_name": "F. R.",
"clpid": "Marleau-F-R"
}
],
"abstract": "We present the stellar calibrator sample and the conversion from instrumental to physical units for the 24 \u03bcm channel of the Multiband Imaging Photometer for Spitzer (MIPS). The primary calibrators are A stars, and the calibration factor based on those stars is MJy sr^\u22121 (DN s^\u22121)^\u22121, with a nominal uncertainty of 2%. We discuss the data reduction procedures required to attain this accuracy; without these procedures, the calibration factor obtained using the automated pipeline at the Spitzer Science Center is lower. We extend this work to predict 24 \u03bcm flux densities for a sample of 238 stars that covers a larger range of flux densities and spectral types. We present a total of 348 measurements of 141 stars at 24 \u03bcm. This sample covers a factor of 460 in 24 \u03bcm flux density, from 8.6 mJy up to 4.0 Jy. We show that the calibration is linear over that range with respect to target flux and background level. The calibration is based on observations made using 3 s exposures; a preliminary analysis shows that the calibration factor may be 1% and 2% lower for 10 and 30 s exposures, respectively. We also demonstrate that the calibration is very stable: over the course of the mission, repeated measurements of our routine calibrator, HD 159330, show a rms scatter of only 0.4%. Finally, we show that the point-spread function (PSF) is well measured and allows us to calibrate extended sources accurately; Infrared Astronomy Satellite (IRAS) and MIPS measurements of a sample of nearby galaxies are identical within the uncertainties.",
"doi": "10.1086/521881",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2007-09",
"series_number": "9",
"volume": "119",
"issue": "9",
"pages": "994-1018"
},
{
"id": "authors:60he8-3mt34",
"collection": "authors",
"collection_id": "60he8-3mt34",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101018-111256502",
"type": "article",
"title": "Spectral Energy Distributions of Hard X-Ray Selected Active Galactic Nuclei in the XMM-Newton Medium Deep Survey",
"author": [
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Tajer",
"given_name": "M.",
"clpid": "Tajer-M"
},
{
"family_name": "Maraschi",
"given_name": "L.",
"clpid": "Maraschi-L"
},
{
"family_name": "Trinchieri",
"given_name": "G.",
"clpid": "Trinchieri-G"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Chiappetti",
"given_name": "L.",
"clpid": "Chiappetti-L"
},
{
"family_name": "Andreon",
"given_name": "S.",
"clpid": "Andreon-S"
},
{
"family_name": "Pierre",
"given_name": "M.",
"clpid": "Pierre-M"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-O"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"clpid": "Zamorani-G"
},
{
"family_name": "Maccagni",
"given_name": "D.",
"clpid": "Maccagni-D"
},
{
"family_name": "Garcet",
"given_name": "O.",
"clpid": "Garcet-O"
},
{
"family_name": "Surdej",
"given_name": "J.",
"orcid": "0000-0002-7005-1976",
"clpid": "Surdej-J"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Alloin",
"given_name": "D.",
"clpid": "Alloin-D"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Tresse",
"given_name": "L.",
"clpid": "Tresse-L"
}
],
"abstract": "We present the SEDs of a hard X-ray selected sample containing 136 sources with F_(2-10 keV) > 10^(-14) erg cm^(-2) s^(-1); 132 are AGNs. The sources are detected in a 1 deg^2 area of the XMM-Newton Medium Deep Survey where optical data from the VVDS and CFHTLS and infrared data from the SWIRE survey are available. Based on a SED fitting technique we derive photometric redshifts with \u03c3(1 + z) = 0.11 and 6% of outliers and identify AGN signatures in 83% of the objects. This fraction is higher than derived when a spectroscopic classification is available. The remaining 17^(+9)_(-6)% of AGNs show star-forming galaxy SEDs (SF class). The sources with AGN signatures are divided in two classes, AGN1 (33^(+6)_(-1)%) and AGN2 (50^(+6)_(-11)%). The AGN1 and AGN2 classes include sources whose SEDs are fitted by type 1 and type 2 AGN templates, respectively. On average, AGN1s show soft X-ray spectra, consistent with being unabsorbed, while AGN2s and SFs show hard X-ray spectra, consistent with being absorbed. The analysis of the average SEDs as a function of X-ray luminosity shows a reddening of the infrared SEDs, consistent with a decreasing contribution from the host galaxy at higher luminosities. The AGNs in the SF classes are likely obscured in the mid-infrared, as suggested by their low L_(3-20 \u03bcm)/L^(corr)_(0.5-10 keV) ratios. We confirm the previously found correlation for AGNs between the radio luminosity and the X-ray and the mid-infrared luminosities. The X-ray-radio correlation can be used to identify heavily absorbed AGNs. However, the estimated radio fluxes for the missing AGN population responsible for the bulk of the background at E > 10 keV are too faint to be detected even in the deepest current radio surveys.",
"doi": "10.1086/518113",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2007-07-01",
"series_number": "1",
"volume": "663",
"issue": "1",
"pages": "81-102"
},
{
"id": "authors:88d0t-49995",
"collection": "authors",
"collection_id": "88d0t-49995",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100112-113609827",
"type": "article",
"title": "Obscured and unobscured AGN populations in a hard-X-ray selected sample of the XMDS survey",
"author": [
{
"family_name": "Tajer",
"given_name": "M.",
"clpid": "Tajer-M"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Chiappetti",
"given_name": "L.",
"clpid": "Chiappetti-L"
},
{
"family_name": "Maraschi",
"given_name": "L.",
"clpid": "Maraschi-L"
},
{
"family_name": "Trincheri",
"given_name": "G.",
"clpid": "Trincheri-G"
},
{
"family_name": "Maccagni",
"given_name": "D.",
"clpid": "Maccagni-D"
},
{
"family_name": "Andreon",
"given_name": "S.",
"clpid": "Andreon-S"
},
{
"family_name": "Garcet",
"given_name": "O.",
"clpid": "Garcet-O"
},
{
"family_name": "Surdej",
"given_name": "J.",
"orcid": "0000-0002-7005-1976",
"clpid": "Surdej-J"
},
{
"family_name": "Pierre",
"given_name": "M.",
"clpid": "Pierre-M"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-O"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Tresse",
"given_name": "L.",
"clpid": "Tresse-L"
}
],
"abstract": "Aims. Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. \nMethods. We selected a sample of 136 X-ray sources detected at a significance of \u22653\u03c3 in the 2-10 keV band (F_(2-10) \u2273 10^(-14) erg cm^(-2) s^(-1)) in a ~1 deg^2 area in the XMM Medium Deep Survey (XMDS). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.\nResults. 70% of the AGN are fitted by a type 2 AGN or a star forming galaxy template. We group them together in a single class of \"optically obscured\" AGN. These have \"red\" optical colors and in about 60% of cases show significant X-ray absorption (N_H > 10^(22) cm^(-2)). Sources with SEDs typical of type 1 AGN have \"blue\" optical colors and exhibit X-ray absorption in about 30% of cases. The stacked X-ray spectrum of obscured AGN is flatter than that of type 1 AGN and has an average spectral slope of \u0393 = 1.6. The subsample of objects fitted by a star forming galaxy template has an even harder stacked spectrum, with \u0393 ~ 1.2-1.3. The obscured fraction is larger at lower fluxes, lower redshifts and lower luminosities. X-ray absorption is less common than \"optical\" obscuration and its incidence is nearly constant with redshift and luminosity. This implies that at high luminosities X-ray absorption is not necessarily related to optical obscuration. The estimated surface densities of obscured, unobscured AGN and type 2 QSOs are respectively 138, 59 and 35 deg^(-2) at F > 10^(-14) erg cm^(-2) s^(-1).",
"doi": "10.1051/0004-6361:20066667",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2007-05",
"series_number": "1",
"volume": "467",
"issue": "1",
"pages": "73-91"
},
{
"id": "authors:xthts-70e35",
"collection": "authors",
"collection_id": "xthts-70e35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091016-135838249",
"type": "article",
"title": "Keck spectroscopy of z = 1-3 ULIRGs from the Spitzer SWIRE survey",
"author": [
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Siana",
"given_name": "B.",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Fritz",
"given_name": "J.",
"clpid": "Fritz-J"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "I.",
"clpid": "P\u00e9rez-Fournon-I"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
}
],
"abstract": "Context. High-redshift ultra luminous infrared galaxies contribute the bulk of the cosmic IR background and are the best candidates for very massive galaxies in formation at z > 1.5.\n\nAims. It is necessary to identify the energy source for their huge luminosities, starburst or AGN activity, in order to correctly interpret the role of ULIRGs in galaxy evolution, and compute reliable estimates of their star formation rates, stellar masses, and accretion luminosities.\n\nMethods. We present Keck/LRIS optical spectroscopy of 35 z \u2265 1.4 luminous IR galaxies in the Spitzer Wide-area Infra-Red Extragalactic survey (SWIRE) northern fields (Lockman Hole, ELAIS-N1, ELAIS-N2). The primary targets belong to the \"IR-peak\" class of galaxies, having the 1.6 \u03bcm (restframe) stellar feature detected in the IRAC Spitzer channels. The spectral energy distributions of the main targets are thoroughly analyzed, by means of spectro-photometric synthesis and multi-component fits (stars + starburst dust + AGN torus).\n\nResults. The IR-peak selection technique is confirmed to successfully select objects above z = 1.4, though some of the observed sources lie at lower redshift than expected. Among the 16 galaxies with spectroscopic redshift, 62% host an AGN component, two thirds being type-1 and one third type-2 objects. The selection, limited to r' < 24.5, is likely biased to optically-bright AGNs. All IR-peakers without emission lines have a non negligible continuum detection, and are likely to be very powerful starbursts, heavily extinguished by dust (A_V \u2265 5 mag). The SEDs of non-AGN IR-peakers resemble those of starbursts (SFR = 20\u2013500 M_\u2299/yr) hosted in massive (M > 10^(11) M_\u2299) galaxies. The presence of an AGN component provides a plausible explanation for the spectroscopic/photometric redshift discrepancies, as the torus produces an apparent shift of the peak to longer wavelengths. These sources are analyzed in IRAC and optical-IR color spaces. In addition to the IR-peak galaxies, we present redshifts and spectral properties for 150 objects, out of a total of 301 sources on slits.",
"doi": "10.1051/0004-6361:20066795",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2007-05",
"series_number": "2",
"volume": "467",
"issue": "2",
"pages": "565-584"
},
{
"id": "authors:76j1v-ts879",
"collection": "authors",
"collection_id": "76j1v-ts879",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110616-141006266",
"type": "article",
"title": "Active Galactic Nucleus and Starburst Classification from Spitzer Mid-Infrared Spectra for High-Redshift SWIRE Sources",
"author": [
{
"family_name": "Weedman",
"given_name": "D.",
"clpid": "Weedman-D"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Wilkes",
"given_name": "B. J.",
"orcid": "0000-0003-1809-2364",
"clpid": "Wilkes-B-J"
},
{
"family_name": "Siana",
"given_name": "B.",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Houck",
"given_name": "J. R.",
"clpid": "Houck-J-R"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
}
],
"abstract": "Spectra have been obtained with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope for 20 sources in the Lockman Hole field of the SWIRE survey. The sample is divided between sources with indicators of an obscured AGN, based primarily on X-ray detections of optically faint sources, and sources with indicators of a starburst, based on optical and near-infrared spectral energy distributions (SEDs), which show a luminosity peak from stellar photospheric emission. Ten of the 11 AGN sources have IRS spectra that show silicate absorption or are power laws; only one AGN source shows PAH emission features. All nine of the sources showing starburst SEDs in the near-infrared show PAH emission features in the IRS spectra. Redshifts are determined from the IRS spectra for all nine starbursts (1.0 < z < 1.9) and 8 of the 11 AGNs (0.6 < z < 2.5). Classification as AGN because of an X-ray detection, the classification as AGN or starburst derived from the photometric SED, and the IRS spectroscopic classification as AGN (silicate absorption) or starburst (PAH emission) are all consistent in 18 of 20 sources. The surface density for starbursts that are most luminous in the mid-infrared is less than that for the most luminous AGNs within the redshift interval 1.7 \u227e z \u227e 1.9. This result implies that mid-infrared source counts at high redshift are dominated by AGNs for f_\u03bd(24 \u03bcm) \u2273 1.0 mJy.",
"doi": "10.1086/508647",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-12-10",
"series_number": "1",
"volume": "653",
"issue": "1",
"pages": "101-111"
},
{
"id": "authors:c20tv-etm51",
"collection": "authors",
"collection_id": "c20tv-etm51",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110719-112148848",
"type": "article",
"title": "Counting individual galaxies from deep 24-\u03bcm Spitzer surveys",
"author": [
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-G"
},
{
"family_name": "Lari",
"given_name": "C.",
"clpid": "Lari-C"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"clpid": "Pozzi-F"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056",
"clpid": "Gruppioni-C"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"clpid": "Franceschini-A"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
}
],
"abstract": "We address the question of how to deal with confusion-limited surveys in the mid-infrared (MIR) domain by using information from shorter-wavelength observations over the same sky regions. Such information, once applied to apparently extended MIR sources, which are indeed 'blends' of two or more different sources, allow us to disentangle the single counterparts and to split the measured flux density into different components. We present the application of this method to the 24-\u03bcm Spitzer archival data in the Great Observatories Origins Deep Survey ELAIS-N1 (GOODS EN1) test field, where apparently extended, 'blended' sources constitute about 20 per cent of a reliable sample of 983 sources detected above the 5\u03c3 threshold down to 40 \u03bcJy. As a shorter-wavelength data set, we have considered the public Infrared Array Camera (IRAC) images and catalogues of the same field. We show that the 24-\u03bcm sample is almost unbiased down to ~40 \u03bcJy and the careful application of the deblending procedure does not require any statistical completeness correction (at least at the flux level considered). This is probed by direct comparison of our results with results in the literature that analysed the same data set through extensive Monte Carlo simulations. The extrapolation of the source counts down to fainter fluxes suggests that our 24-\u03bcm sample is able to resolve ~62 per cent of the cosmic background down to a flux level of 38 \u03bcJy.",
"doi": "10.1111/j.1365-2966.2006.10844.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2006-10",
"series_number": "4",
"volume": "371",
"issue": "4",
"pages": "1891-1897"
},
{
"id": "authors:w49j2-d8888",
"collection": "authors",
"collection_id": "w49j2-d8888",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:DAVmnras06b",
"type": "article",
"title": "Optical and infrared diagnostics of SDSS galaxies in the SWIRE survey",
"author": [
{
"family_name": "Davoodi",
"given_name": "P.",
"clpid": "Davoodi-P"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"clpid": "Pozzi-F"
},
{
"family_name": "Oliver",
"given_name": "S. A.",
"clpid": "Oliver-S-A"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Afonso-Luis",
"given_name": "A.",
"clpid": "Afonso-Luis-A"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Hatziminaoglou",
"given_name": "E.",
"clpid": "Hatziminaoglou-E"
},
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-G"
},
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Waddington",
"given_name": "I.",
"clpid": "Waddington-I"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Evans",
"given_name": "T.",
"orcid": "0000-0001-5442-1300",
"clpid": "Evans-T-M"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
}
],
"abstract": "We present the rest-frame optical and infrared colours of a complete sample of 1114 z < 0.3 galaxies from the Spitzer Wide-Area Infrared Extragalactic (SWIRE) Legacy Survey and the Sloan Digital Sky Survey (SDSS). We discuss the optical and infrared colours of our sample and analyse in detail the contribution of dusty star-forming galaxies and active galactic nuclei (AGN) to optically selected red sequence galaxies. \n\nWe propose that the optical (g-r) colour and infrared log(L-24/L-3.6) colour of galaxies in our sample are determined primarily by a bulge-to-disc ratio. The (g-r) colour is found to be sensitive to the bulge-to-disc ratio for disc-dominated galaxies, whereas the log (L-24/L-3.6) colour is more sensitive for bulge-dominated systems. \n\nWe identify similar to 18 per cent (195 sources) of our sample as having red optical colours and infrared excess. Typically, the infrared luminosities of these galaxies are found to be at the high end of star-forming galaxies with blue optical colours. Using emission-line diagnostic diagrams, 78 are found to have an AGN contribution and 117 are identified as star-forming systems. The red (g-r) colour of the star-forming galaxies could be explained by extinction. However, their high optical luminosities cannot. We conclude that they have a significant bulge component. \n\nThe number densities of optically red star-forming galaxies are found to correspond to similar to 13 per cent of the total number density of our sample. In addition, these systems contribute similar to 13 per cent of the total optical luminosity density, and 28 per cent of the total infrared luminosity density of our SWIRE/SDSS sample. These objects may reduce the need for 'dry mergers'.",
"doi": "10.1111/j.1365-2966.2006.10793.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2006-09-21",
"series_number": "3",
"volume": "371",
"issue": "3",
"pages": "1113-1124"
},
{
"id": "authors:kyhhp-zjr65",
"collection": "authors",
"collection_id": "kyhhp-zjr65",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BREmnras06",
"type": "article",
"title": "XMM-LSS discovery of a z = 1.22 galaxy cluster",
"author": [
{
"family_name": "Bremer",
"given_name": "M. N.",
"clpid": "Bremer-M-N"
},
{
"family_name": "Valtchanov",
"given_name": "I.",
"orcid": "0000-0001-9930-7886",
"clpid": "Valtchanov-I"
},
{
"family_name": "Willis",
"given_name": "J.",
"clpid": "Willis-J"
},
{
"family_name": "Altieri",
"given_name": "B.",
"clpid": "Altieri-B"
},
{
"family_name": "Andreon",
"given_name": "S.",
"clpid": "Andreon-S"
},
{
"family_name": "Duc",
"given_name": "P. A.",
"clpid": "Duc-P-A"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Jean",
"given_name": "C.",
"clpid": "Jean-C"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Pacaud",
"given_name": "F.",
"clpid": "Pacaud-F"
},
{
"family_name": "Pierre",
"given_name": "M.",
"clpid": "Pierre-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Waddington",
"given_name": "I.",
"clpid": "Waddington-I"
}
],
"abstract": "We present details of the discovery of XLSS J022303.0\u2212043622, a z= 1.2 cluster of galaxies. This cluster was identified from its X-ray properties and selected as a z > 1 candidate from its optical/near-infrared (IR) characteristics in the XMM Large-Scale Structure Survey (XMM-LSS). It is the most distant system discovered in the survey to date. We present ground-based optical and near-IR observations of the system carried out as part of the XMM-LSS survey. The cluster has a bolometric X-ray luminosity of 1.1 \u00b1 0.7 \u00d7 10^44 erg s^\u22121 , fainter than most other known z > 1 X-ray selected clusters. In the optical it has a remarkably compact core, with at least a dozen galaxies inside a 125 kpc radius circle centred on the X-ray position. Most of the galaxies within the core, and those spectroscopically confirmed to be cluster members, have stellar masses similar to those of massive cluster galaxies at low redshift. They have colours comparable to those of galaxies in other z > 1 clusters, consistent with showing little sign of strong ongoing star formation. The bulk of the star formation within the galaxies appears to have ceased at least 1.5 Gyr before the observed epoch. Our results are consistent with massive cluster galaxies forming at z > 1 and passively evolving thereafter. We also show that the system is straightforwardly identified in Spitzer/IRAC 3.6- and 4.5-\u03bcm data obtained by the Spitzer Wide-area Infrared Extragalactic (SWIRE) survey emphasizing the power and utility of joint XMM and Spitzer searches for the most distant clusters.",
"doi": "10.1111/j.1365-2966.2006.10767.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2006-09-21",
"series_number": "3",
"volume": "371",
"issue": "3",
"pages": "1427-1434"
},
{
"id": "authors:wcwma-yp970",
"collection": "authors",
"collection_id": "wcwma-yp970",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110216-083108180",
"type": "article",
"title": "Luminosity functions for galaxies and quasars in the Spitzer Wide-area Infrared Extragalactic Legacy Survey",
"author": [
{
"family_name": "Babbedge",
"given_name": "T. S. R.",
"clpid": "Babbedge-Thomas-S-R"
},
{
"family_name": "Rowan-Robinson",
"given_name": "M.",
"clpid": "Rowan-Robinson-Michael"
},
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577",
"clpid": "Vaccari-Mattia"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-Jason-A"
},
{
"family_name": "Lonsdale",
"given_name": "C. J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Clements",
"given_name": "D. L.",
"orcid": "0000-0002-9548-5033",
"clpid": "Clements-David-L"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Franceschini",
"given_name": "A.",
"orcid": "0000-0002-9979-3383",
"clpid": "Franceschini-Alberto"
},
{
"family_name": "Gonz\u00e1lez-Solares",
"given_name": "E.",
"orcid": "0000-0001-9123-0626",
"clpid": "Gonz\u00e1lez-Solares-Eduardo-A"
},
{
"family_name": "Hatziminaoglou",
"given_name": "E.",
"clpid": "Hatziminaoglou-Evanthia"
},
{
"family_name": "Lacey",
"given_name": "C. G.",
"orcid": "0000-0001-9016-5332",
"clpid": "Lacey-Cedric-G"
},
{
"family_name": "Oliver",
"given_name": "S.",
"orcid": "0000-0001-7862-1032",
"clpid": "Oliver-Sebastian-J"
},
{
"family_name": "Onyett",
"given_name": "N.",
"clpid": "Onyett-N"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "I.",
"orcid": "0000-0002-2807-6459",
"clpid": "P\u00e9rez-Fournon-Ismael"
},
{
"family_name": "Polletta",
"given_name": "M.",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X",
"clpid": "Pozzi-Francesca"
},
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-Giulia"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Siana",
"given_name": "B.",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Smith",
"given_name": "H. E.",
"clpid": "Smith-Harding-E"
}
],
"abstract": "We construct rest-frame luminosity functions (LFs) at 3.6, 4.5, 5.8, 8 and 24 \u03bcm over the redshift range 0 < z < 2 for galaxies and 0 < z < 4 for optical quasi-stellar objects (QSOs), using optical and infrared (IR) data from the Spitzer Wide-area Infrared Extragalactic (SWIRE) Survey. The 3.6- and 4.5-\u03bcm galaxy LFs show evidence for moderate positive luminosity evolution up to z~ 1.5, consistent with the passive ageing of evolved stellar populations. Their comoving luminosity density was found to evolve passively, gradually increasing out to z~ 0.5\u20131 but flattening, or even declining, at higher redshift. Conversely, the 24-\u03bcm galaxy LF, which is more sensitive to obscured star formation and/or active galactic nuclei (AGN) activity, undergoes strong positive evolution, with the derived IR energy density and star formation rate (SFR) density \u221d (1 +z)^\u03b3 with \u03b3= 4.5^(+0.7)_(\u22120.6) and the majority of this evolution occurring since z~ 1. Optical QSOs, however, show positive luminosity evolution in all bands, out to the highest redshifts (3 < z < 4). Modelling as L^* \u221d (1 +z)^\u03b3 gave \u03b3= 1.3^(+0.1)_(\u22120.1) at 3.6 \u03bcm, \u03b3= 1.0^(+0.1)_(\u22120.1) at 4.5 \u03bcm and stronger evolution at the longer wavelengths (5.8, 8 and 24 \u03bcm), of \u03b3~ 3. Comparison of the galaxy LFs to predictions from a semi-analytic model based on cold dark matter (CDM) indicates that an initial mass function (IMF) skewed towards higher mass star formation in bursts compared to locally be preferred. As a result, the currently inferred massive SFRs in distant submm sources may require substantial downwards revision.",
"doi": "10.1111/j.1365-2966.2006.10547.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2006-08",
"series_number": "3",
"volume": "370",
"issue": "3",
"pages": "1159-1180"
},
{
"id": "authors:zhdxa-rgy34",
"collection": "authors",
"collection_id": "zhdxa-rgy34",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:FADaj06",
"type": "article",
"title": "The Spitzer Space Telescope Extragalactic First Look Survey: 24 \u03bcm Data Reduction, Catalog, and Source Identification",
"author": [
{
"family_name": "Fadda",
"given_name": "Dario",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Marleau",
"given_name": "Francine R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "Lisa J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Makozov",
"given_name": "David",
"clpid": "Makozov-D"
},
{
"family_name": "Frayer",
"given_name": "David T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Chapman",
"given_name": "S. C.",
"clpid": "Chapman-S-C"
},
{
"family_name": "Choi",
"given_name": "P. I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Squires",
"given_name": "G. K.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Wilson",
"given_name": "G.",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G"
},
{
"family_name": "Yang",
"given_name": "L.",
"clpid": "Yang-L"
}
],
"abstract": "We present the reduction of the 24 \u03bcm data obtained during the first cosmological survey performed by the Spitzer Space Telescope. Images of a region of sky at moderately high Galactic latitude (l = 88.3\u00b0, b = +34.9\u00b0) were obtained on 2003 December 9-11. The survey consists of a shallow observation of 2.5\u00b0 \u00d7 2\u00b0 centered at 17h18m, +59\u00b030' (main survey) and a deeper observation of 1\u00b0 \u00d7 0.5\u00b0 centered at 17h17m, +59\u00b045' (verification survey). Issues with the reduction of the 24 \u03bcm MIPS data are discussed and solutions to attenuate instrumental effects are proposed and applied to the data. Approximately 17,000 sources are extracted with a signal-to-noise ratio (S/N) greater than 5. The photometry of the point sources is evaluated through point-spread function (PSF) fitting using an empirical PSF derived from the data. Aperture corrections and the absolute calibration have been checked using stars in the field. Astrometric and photometric errors depend on the S/N of the source varying between 0farcs35^-1\" and 5%-15%, respectively, for sources detected at 20-5 \u03c3. The fluxes of the 123 extended sources have been estimated through aperture photometry. The extended sources cover less than 0.3% of the total area of the survey. Based on simulations, the main and verification surveys are 50% complete at 0.3 and 0.15 mJy, respectively. Counterparts have been searched for in optical and radio catalogs. More than 80% of the 24 \u03bcm sources have a reliable optical counterpart down to R = 25.5; 16% of the sources have a 20 cm counterpart down to 0.1 mJy and ~80% of the radio-IR associations have a reliable optical counterpart. A residual map is obtained by subtracting point sources detected at the 3 \u03c3 level and interpolating the regions occupied by extended sources. Several Galactic clouds with low and intermediate velocities are identified by comparison with neutral hydrogen data from this field.",
"doi": "10.1086/504034",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2006-06",
"series_number": "6",
"volume": "131",
"issue": "6",
"pages": "2859-2876"
},
{
"id": "authors:1hx1f-kva19",
"collection": "authors",
"collection_id": "1hx1f-kva19",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110727-102424535",
"type": "article",
"title": "Chandra and Spitzer Unveil Heavily Obscured Quasars in the Chandra/SWIRE Survey",
"author": [
{
"family_name": "Polletta",
"given_name": "Maria del Carmen",
"orcid": "0000-0001-7411-5386",
"clpid": "Polletta-Maria-del-Carmen"
},
{
"family_name": "Wilkes",
"given_name": "Belinda J.",
"orcid": "0000-0003-1809-2364",
"clpid": "Wilkes-B-J"
},
{
"family_name": "Siana",
"given_name": "Brian",
"orcid": "0000-0002-4935-9511",
"clpid": "Siana-Brian-D"
},
{
"family_name": "Lonsdale",
"given_name": "Carol J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Kilgard",
"given_name": "Roy",
"clpid": "Kilgard-Roy"
},
{
"family_name": "Smith",
"given_name": "Harding E.",
"clpid": "Smith-H-E"
},
{
"family_name": "Kim",
"given_name": "Dong-Woo",
"clpid": "Kim-Dong-Woo"
},
{
"family_name": "Owen",
"given_name": "Frazer",
"clpid": "Owen-F-N"
},
{
"family_name": "Efstathiou",
"given_name": "Andreas",
"orcid": "0000-0002-2612-4840",
"clpid": "Efstathiou-Andreas"
},
{
"family_name": "Jarrett",
"given_name": "Tom",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Stacey",
"given_name": "Gordon",
"clpid": "Stacey-G-J"
},
{
"family_name": "Franceschini",
"given_name": "Alberto",
"clpid": "Franceschini-A"
},
{
"family_name": "Rowan-Robinson",
"given_name": "Michael",
"clpid": "Rowan-Robinson-M"
},
{
"family_name": "Babbedge",
"given_name": "Tom S. R.",
"clpid": "Babbedge-T-S-R"
},
{
"family_name": "Berta",
"given_name": "Stefano",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Fang",
"given_name": "Fan",
"clpid": "Fang-Fan"
},
{
"family_name": "Farrah",
"given_name": "Duncan",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Gonzalez-Solares",
"given_name": "Eduardo",
"clpid": "Gonzalez-Solares-E"
},
{
"family_name": "Morrison",
"given_name": "Glenn",
"clpid": "Morrison-G-E"
},
{
"family_name": "Surace",
"given_name": "Jason A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Shupe",
"given_name": "Dave L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "Using the large multiwavelength data set in the Chandra/SWIRE Survey (0.6 deg^2 in the Lockman Hole), we show evidence for the existence of highly obscured (Compton-thick) AGNs, estimate a lower limit to their surface density, and characterize their multiwavelength properties. Two independent selection methods based on the X-ray and infrared spectral properties are presented. The two selected samples contain (1) five X-ray sources with hard X-ray spectra and column densities \u2273 10^(24) cm^(-2) and (2) 120 infrared sources with red and AGN-dominated infrared SEDs. We estimate a surface density of at least 25 Compton-thick AGNs deg^(-2) detected in the infrared in the Chandra/SWIRE field, of which ~40% show distinct AGN signatures in their optical/near-infrared SEDs, the remaining being dominated by the host galaxy emission. Only ~33% of all Compton-thick AGNs are detected in the X-rays at our depth [F(0.3-8 keV) > 10^(-15) ergs cm^(-2) s^(-1)]. We report the discovery of two sources in our sample of Compton-thick AGNs, SWIRE J104409.95+585224.8 (z = 2.54) and SWIRE J104406.30+583954.1 (z = 2.43), which are the most luminous Compton-thick AGNs at high z currently known. The properties of these two sources are discussed in detail with an analysis of their spectra, SEDs, luminosities, and black hole masses.",
"doi": "10.1086/500821",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-05-10",
"series_number": "2",
"volume": "642",
"issue": "2",
"pages": "673-693"
},
{
"id": "authors:h8awm-wkr85",
"collection": "authors",
"collection_id": "h8awm-wkr85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170328-075452484",
"type": "article",
"title": "Spitzer 70 and 160 \u03bcm Observations of the Extragalactic First Look Survey",
"author": [
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Marleau",
"given_name": "F. R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Choi",
"given_name": "P. I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Beck",
"given_name": "R.",
"clpid": "Beck-R"
},
{
"family_name": "Dole",
"given_name": "H.",
"clpid": "Dole-H"
},
{
"family_name": "Engelbracht",
"given_name": "C. W.",
"clpid": "Engelbracht-C-W"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Gordon",
"given_name": "K. D.",
"clpid": "Gordon-K-D"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Henderson",
"given_name": "D.",
"clpid": "Henderson-D"
},
{
"family_name": "Hesselroth",
"given_name": "T.",
"clpid": "Hesselroth-T-D"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Kelly",
"given_name": "D. M.",
"clpid": "Kelly-D-M"
},
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Laine",
"given_name": "S.",
"orcid": "0000-0003-1250-8314",
"clpid": "Laine-S-J"
},
{
"family_name": "Latter",
"given_name": "W. B.",
"clpid": "Latter-W-B"
},
{
"family_name": "Mahoney",
"given_name": "W.",
"clpid": "Mahoney-W-A"
},
{
"family_name": "Makovoz",
"given_name": "D.",
"clpid": "Makovoz-D"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Morrison",
"given_name": "J. E.",
"clpid": "Morrison-J-E"
},
{
"family_name": "Moshir",
"given_name": "M.",
"clpid": "Moshir-M"
},
{
"family_name": "Noriega-Crespo",
"given_name": "A.",
"orcid": "0000-0002-6296-8960",
"clpid": "Noriega-Crespo-A"
},
{
"family_name": "Padgett",
"given_name": "D. L.",
"orcid": "0000-0001-5334-5107",
"clpid": "Padgett-D-L"
},
{
"family_name": "Pesenson",
"given_name": "M.",
"clpid": "Pesenson-M-Z"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Squires",
"given_name": "G. K.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Wilson",
"given_name": "G.",
"clpid": "Wilson-G-W"
}
],
"abstract": "We present 70 and 160 \u03bcm observations from the Spitzer extragalactic First Look Survey (xFLS). The data reduction techniques and the methods for producing co-added mosaics and source catalogs are discussed. Currently, 26% of the 70 \u03bcm sample and 49% of the 160 \u03bcm\u2013selected sources have redshifts. The majority of sources with redshifts are star-forming galaxies at z < 0.5, while about 5% have infrared colors consistent with active galactic nuclei. The observed infrared colors agree with the spectral energy distributions (SEDs) of local galaxies previously determined from IRAS and Infrared Space Observatory data. The average 160 \u03bcm/70 \u03bcm color temperature for the dust is T_d \u2243 30 \u00b1 5 K, and the average 70 \u03bcm/24 \u03bcm spectral index is \u03b1 \u2243 2.4 \u00b1 0.4. The observed infrared-to-radio correlation varies with redshift as expected out to z ~ 1 based on the SEDs of local galaxies. The xFLS number counts at 70 and 160 \u03bcm are consistent within uncertainties with the models of galaxy evolution, but there are indications that the current models may require slight modifications. Deeper 70 \u03bcm observations are needed to constrain the models, and redshifts for the faint sources are required to measure the evolution of the infrared luminosity function.",
"doi": "10.1086/498690",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2006-01",
"series_number": "1",
"volume": "131",
"issue": "1",
"pages": "250-260"
},
{
"id": "authors:m5yj4-vqn92",
"collection": "authors",
"collection_id": "m5yj4-vqn92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-105720718",
"type": "article",
"title": "The Infrared Array Camera Component of the Spitzer Space Telescope Extragalactic First Look Survey",
"author": [
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Wilson",
"given_name": "G.",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G-W"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Chapman",
"given_name": "S. C.",
"clpid": "Chapman-S-C"
},
{
"family_name": "Choi",
"given_name": "P. I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Laine",
"given_name": "S.",
"orcid": "0000-0003-1250-8314",
"clpid": "Laine-S-J"
},
{
"family_name": "Marleau",
"given_name": "F. R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Squires",
"given_name": "G. K.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We present Infrared Array Camera (IRAC) data and source catalogs from the Spitzer Space Telescope Extragalactic First Look Survey. The data were taken in four broad bands centered at nominal wavelengths of 3.6, 4.5, 5.8, and 8.0 \u03bcm. A set of mosaics and catalogs have been produced that are \u224880% complete and \u224899% reliable to their chosen flux density limits. The main field survey covers 3.8 deg^2 and has flux density limits of 20, 25, 100, and 100 \u03bcJy at wavelengths of 3.6, 4.5, 5.8, and 8.0 \u03bcm, respectively. The deeper \"verification\" survey covers 0.25 deg^2 with limits of 10, 10, 30, and 30 \u03bcJy, respectively. We also include deep data in the ELAIS-N1 field, which covers 0.041 deg2 with limits of 4, 3, 10, and 10 \u03bcJy, respectively, but with only two wavelength coverages at a given sky position. The final bandmerged catalogs contain 103,193 objects in the main field, 12,224 in the verification field, and 5239 in ELAIS-N1. Flux densities of high signal-to-noise objects are accurate to about 10%, and the residual systematic error in the absolute flux density scale is ~2%-3%. We have successfully extracted sources at source densities as high as 100,000 deg-2 in our deepest 3.6 and 4.5 \u03bcm data. The mosaics and source catalogs will be made available through the Spitzer Science Center archive and the Infrared Science Archive.",
"doi": "10.1086/432894",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2005-11",
"series_number": "1",
"volume": "161",
"issue": "1",
"pages": "41-52"
},
{
"id": "authors:yx7ef-2n066",
"collection": "authors",
"collection_id": "yx7ef-2n066",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170324-082411883",
"type": "article",
"title": "Spitzer 24 Micron Observations of Optical/Near\u2010Infrared\u2013Selected Extremely Red Galaxies: Evidence for Assembly of Massive Galaxies at z \u223c 1\u20132?",
"author": [
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Choi",
"given_name": "Philip I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Marleau",
"given_name": "F. R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Storrie\u2010Lombardi",
"given_name": "L. J.",
"clpid": "Storrie\u2010Lombardi-L-J"
},
{
"family_name": "Thompson",
"given_name": "D. J.",
"clpid": "Thompson-D-J"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Chapman",
"given_name": "S.",
"clpid": "Chapman-S"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Squires",
"given_name": "G. K.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Wilson",
"given_name": "G.",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G"
}
],
"abstract": "We carried out direct measurement of the fraction of dusty sources in a sample of extremely red galaxies with (R - K_s) \u2265 5.3 mag and K_s < 20.2 mag, using 24 \u03bcm data from the Spitzer Space Telescope. Combining deep 24 \u03bcm Ks- and R-band data over an area of ~64 arcmin^2 in ELAIS N1 of the Spitzer First Look Survey (FLS), we find that 50% \u00b1 6% of our extremely red object (ERO) sample have measurable 24 \u03bcm flux above the 3 \u03c3 flux limit of 40 \u03bcJy. This flux limit corresponds to a star formation rate (SFR) of 12 M_\u2299 yr^(-1) at z ~ 1, much more sensitive than any previous long-wavelength measurement. The 24 \u03bcm-detected EROs have 24 \u03bcm/2.2 \u03bcm and 24 \u03bcm/0.7 \u03bcm flux ratios consistent with infrared luminous, dusty sources at z \u2265 1, and are an order of magnitude too red to be explained by an infrared quiescent spiral or a pure old stellar population at any redshift. Some of these 24 \u03bcm-detected EROs could be active galactic nuclei; however, the fraction among the whole ERO sample is probably small, 10%-20%, as suggested by deep X-ray observations as well as optical spectroscopy. Keck optical spectroscopy of a sample of similarly selected EROs in the FLS field suggests that most of the EROs in ELAIS N1 are probably at z ~ 1. The mean 24 \u03bcm flux (167 \u03bcJy) of the 24 \u03bcm-detected ERO sample roughly corresponds to the rest-frame 12 \u03bcm luminosity, \u03bdL_\u03bd(12 \u03bcm), of 3 \u00d7 10^(10) L_\u2299 at z ~ 1. Using the correlation between IRAS \u03bdL_\u03bd(12 \u03bcm) and infrared luminosity LIR(8-1000 \u03bcm), we infer that the \u3008L_(IR)\u3009 of the 24 \u03bcm-detected EROs is 3 \u00d7 10^(11) and 1 \u00d7 10^(12) L_\u2299 at z = 1.0 and 1.5, respectively, similar to that of local luminous infrared galaxies (LIRGs) and ultraluminous infrared galaxies (ULIRGs). The corresponding SFR would be roughly 50-170 M_\u2299 yr^(-1). If the timescale of this starbursting phase is on the order of 10^8 yr as inferred for the local LIRGs and ULIRGs, the lower limit on the masses of these 24 \u03bcm-detected EROs is 5 \u00d7 10^9 to 2 \u00d7 10^(10) M_\u2299. It is plausible that some of the starburst EROs are in the midst of a violent transformation to become massive early type galaxies at the epoch of z ~ 1-2.",
"doi": "10.1086/422917",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2004-09",
"series_number": "1",
"volume": "154",
"issue": "1",
"pages": "75-79"
},
{
"id": "authors:19yvq-pmb91",
"collection": "authors",
"collection_id": "19yvq-pmb91",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170327-155242177",
"type": "article",
"title": "Obscured and Unobscured Active Galactic Nuclei in the Spitzer Space Telescope First Look Survey",
"author": [
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Sajina",
"given_name": "A.",
"orcid": "0000-0002-1917-1200",
"clpid": "Sajina-Anna"
},
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Chapman",
"given_name": "S. C.",
"clpid": "Chapman-S-C"
},
{
"family_name": "Choi",
"given_name": "P. I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Marleau",
"given_name": "F. R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Wilson",
"given_name": "G.",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G-W"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "Selection of active galactic nuclei (AGNs) in the infrared facilitates the discovery of AGNs whose optical emission is extinguished by dust. In this paper, we use the Spitzer Space Telescope First Look Survey (FLS) to assess the fraction of AGNs with mid-infrared (MIR) luminosities that are comparable to quasars and that are missed in optical quasar surveys because of dust obscuration. We begin by using the Sloan Digital Sky Survey (SDSS) database to identify 54 quasars within the 4 deg^2 extragalactic FLS. These quasars occupy a distinct region in MIR color space by virtue of their strong, red continua. This has allowed us to define an MIR color criterion for selecting AGN candidates. About 2000 FLS objects have colors that are consistent with them being AGNs, but most are much fainter in the MIR than the SDSS quasars, which typically have 8 \u03bcm flux densities S_(8.0) ~ 1 mJy. We have investigated the properties of 43 objects with S_(8.0) \u2265 1 mJy that satisfy our AGN color selection. This sample should contain both unobscured quasars as well as AGNs that are absent from the SDSS survey because of extinction in the optical. After removing 16 known quasars, three probable normal quasars, and eight spurious or confused objects from the initial sample of 43, we are left with 16 objects that are likely to be obscured quasars or luminous Seyfert 2 galaxies. This suggests that the numbers of obscured and unobscured AGNs are similar in samples selected in the MIR at S_(8.0) ~ 1 mJy.",
"doi": "10.1086/422816",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2004-09",
"series_number": "1",
"volume": "154",
"issue": "1",
"pages": "166-169"
},
{
"id": "authors:1mada-kxn61",
"collection": "authors",
"collection_id": "1mada-kxn61",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170327-153742897",
"type": "article",
"title": "Extragalactic Source Counts at 24 Microns in the Spitzer First Look Survey",
"author": [
{
"family_name": "Marleau",
"given_name": "Francine R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Makovoz",
"given_name": "D.",
"clpid": "Makovoz-D"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Chapman",
"given_name": "S.",
"clpid": "Chapman-S-C"
},
{
"family_name": "Choi",
"given_name": "P. I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Squires",
"given_name": "G.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Wilson",
"given_name": "G.",
"clpid": "Wilson-G-W"
}
],
"abstract": "We present the Spitzer Multiband Imaging Photometer 24 \u03bcm source counts in the Extragalactic First Look Survey (FLS) main, verification, and European Large Area ISO Survey N1 fields. Spitzer's increased sensitivity and efficiency in large areal coverage over previous infrared telescopes, coupled with the enhanced sensitivity of the 24 \u03bcm band to sources at intermediate redshift, dramatically improve the quality and statistics of number counts in the mid-infrared. The FLS observations cover areas of 4.4, 0.26, and 0.015 deg^2, respectively, and reach 3 \u03c3 depths of 0.11, 0.08, and 0.03 mJy. The extragalactic counts derived for each survey agree remarkably well. The counts can be fitted by a super-Euclidean power law of index \u03b1 = -2.9 from 0.2 to 0.9 mJy, with a flattening of the counts at fluxes fainter than 0.2 mJy. Comparison with infrared galaxy evolution models reveals a peak's displacement in the 24 \u03bcm counts. This is probably due to the detection of a new population of galaxies with redshift between 1 and 2, previously unseen in the 15 \u03bcm deep counts.",
"doi": "10.1086/422584",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2004-09",
"series_number": "1",
"volume": "154",
"issue": "1",
"pages": "66-69"
},
{
"id": "authors:y0sge-rcx71",
"collection": "authors",
"collection_id": "y0sge-rcx71",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-094800747",
"type": "article",
"title": "Infrared Properties of Radio\u2010selected Submillimeter Galaxies in the Spitzer First Look Survey Verification Field",
"author": [
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Chapman",
"given_name": "S. C.",
"clpid": "Chapman-S-C"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Fadda",
"given_name": "D.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Morganti",
"given_name": "R.",
"clpid": "Morganti-R"
},
{
"family_name": "Garrett",
"given_name": "M. A.",
"clpid": "Garrett-M-A"
},
{
"family_name": "Appleton",
"given_name": "P.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Choi",
"given_name": "P.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Heinrichsen",
"given_name": "I.",
"clpid": "Heinrichsen-I"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Marleau",
"given_name": "F.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Squires",
"given_name": "G. K.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Surace",
"given_name": "J. A.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
},
{
"family_name": "Wilson",
"given_name": "G.",
"clpid": "Wilson-G-W"
}
],
"abstract": "We report on submillimeter and infrared observations of 28 radio-selected galaxies in the Spitzer First Look Survey verification field. All of the radio-selected galaxies that show evidence for emission at 850 \u03bcm with SCUBA have Spitzer counterparts at 24 \u03bcm, while only half of the radio-selected galaxies without 850 \u03bcm emission have detectable counterparts at 24 \u03bcm. The data show a wide range of infrared colors (S_(70 \u03bcm)/S_(24 \u03bcm) < 5-30, S_(8 \u03bcm)/S_(3.6 \u03bcm) < 0.3-4), indicative of a mixture of infrared-warm AGN-dominated and cooler starburst-dominated sources. The galaxies showing 850 \u03bcm emission have Spitzer flux densities and flux density ratios consistent with the range of values expected for high-redshift (z = 1-4) ultraluminous infrared galaxies.",
"doi": "10.1086/423250",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2004-09",
"series_number": "1",
"volume": "154",
"issue": "1",
"pages": "137-141"
},
{
"id": "authors:rqdn8-mj470",
"collection": "authors",
"collection_id": "rqdn8-mj470",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-091729060",
"type": "article",
"title": "The Far- and Mid-Infrared/Radio Correlations in the Spitzer Extragalactic First Look Survey",
"author": [
{
"family_name": "Appleton",
"given_name": "P. N.",
"orcid": "0000-0002-7607-8766",
"clpid": "Appleton-P-N"
},
{
"family_name": "Fadda",
"given_name": "D. T.",
"orcid": "0000-0002-3698-7076",
"clpid": "Fadda-Dario"
},
{
"family_name": "Marleau",
"given_name": "F. R.",
"clpid": "Marleau-F-R"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Condon",
"given_name": "J. J.",
"orcid": "0000-0003-4724-1939",
"clpid": "Condon-J-J"
},
{
"family_name": "Choi",
"given_name": "P. I.",
"clpid": "Choi-Philip-I"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Lacy",
"given_name": "M.",
"orcid": "0000-0002-3032-1783",
"clpid": "Lacy-M"
},
{
"family_name": "Wilson",
"given_name": "G.",
"orcid": "0000-0002-6572-7089",
"clpid": "Wilson-G"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Chapman",
"given_name": "S. C.",
"clpid": "Chapman-S-C"
},
{
"family_name": "Fang",
"given_name": "F.",
"clpid": "Fang-Fan"
},
{
"family_name": "Heinrichson",
"given_name": "I.",
"clpid": "Heinrichson-I"
},
{
"family_name": "Im",
"given_name": "M.",
"orcid": "0000-0002-8537-6714",
"clpid": "Im-Myungshin"
},
{
"family_name": "Jannuzi",
"given_name": "B. T.",
"orcid": "0000-0002-1578-6582",
"clpid": "Jannuzi-B-T"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Squires",
"given_name": "G.",
"orcid": "0000-0002-1977-5717",
"clpid": "Squires-G-K"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-H-I"
}
],
"abstract": "Using the Spitzer Space Telescope and the Very Large Array (VLA), we present the first direct evidence that the well-known far-infrared/radio correlation is valid to cosmologically significant redshift. We also confirm, with improved statistics compared with previous surveys, a similar result for the mid-IR/radio correlation. We explore the dependence of monochromatic q_(24) and q_(70) on z. The results were obtained by matching Spitzer sources at 24 and 70 \u03bcm with VLA 1.4 GHz microjansky radio sources obtained for the Spitzer First Look Survey (FLS). Spectroscopic redshifts have been obtained for over 500 matched IR/radio sources using observations at WIYN and Keck, and archival Sloan Digital Sky Survey (SDSS) data extending out to z > 2. We find that q_(24) shows significantly more dispersion than q_(70). By comparing the observed fluxes at 70, 24, and 4.5 \u03bcm with a library of SED templates, we find that the larger dispersion in q_(24) is predictable in terms of systematic variations in spectral energy distribution (SED) shape throughout the population. Although the models are not able to encompass the full range of observed behavior (both the presence of either extremely flat or extremely steep IR SEDs), the fitting parameters were used to \"k-correct\" the higher z galaxies, which resulted in a reduced scatter in q. For comparison, we also corrected these data using the SED for M82. The results for 24 and 70 \u03bcm provide strong consistent evidence for the universality of the mid- and far-IR/radio correlations out to redshifts of at least z = 1.",
"doi": "10.1086/422425",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2004-09",
"series_number": "1",
"volume": "154",
"issue": "1",
"pages": "147-150"
},
{
"id": "authors:ftsf2-c5v61",
"collection": "authors",
"collection_id": "ftsf2-c5v61",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170322-085802408",
"type": "article",
"title": "The SIRTF First-Look Survey. I. VLA Image and Source Catalog",
"author": [
{
"family_name": "Condon",
"given_name": "J. J.",
"orcid": "0000-0003-4724-1939",
"clpid": "Condon-J-J"
},
{
"family_name": "Cotton",
"given_name": "W. D.",
"clpid": "Cotton-W-D"
},
{
"family_name": "Yin",
"given_name": "Q.-F.",
"clpid": "Yin-Q-F"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Storrie-Lombardi",
"given_name": "L. J.",
"orcid": "0000-0002-5987-5210",
"clpid": "Storrie-Lombardi-L-J"
},
{
"family_name": "Helou",
"given_name": "G.",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Werner",
"given_name": "M. W.",
"clpid": "Werner-M-W"
}
],
"abstract": "The First-Look Survey (FLS) of the Space Infrared Telescope Facility (SIRTF) will cover about 5 deg^2 centered on J2000.0 \u03b1 = 17^h18^m, \u03b4 = +59\u00b030' in order to characterize the extragalactic infrared sky 2 orders of magnitude deeper than the IRAS survey. We expect that most of the FLS far-infrared (\u03bb = 160, 70, and 24 \u03bcm) sources will be star-forming galaxies obeying the very tight far-infrared/radio correlation and will be continuum radio sources with flux densities S \u2273100 \u03bcJy at \u03bd = 1.4 GHz. Conversely, radio sources stronger than 100 \u03bcJy are usually powered by star-forming galaxies, plus some active galactic nuclei, and most should be detectable by the SIRTF FLS. Thus, a sensitive radio survey can be used to select and identify most of the SIRTF FLS source population before launch. We used the B configuration of the VLA to make an image of the FLS area at \u03bd = 1.4 GHz with \u03c3 \u2248 23 \u03bcJy beam^(-1) rms fluctuations, \u03b8 = 5.\"0 resolution, and \u03c3_\u03b1 \u2248 \u03c3\u03b4 \u227e0.\"5 rms uncertainties in right ascension and declination. The resulting radio image and catalog of 3565 radio components with peak flux densities S_p \u2265 5 \u03c3 = 115 \u03bcJy beam^(-1) have been released via the Web to expedite follow-up optical identification and spectroscopy.",
"doi": "10.1086/374633",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2003-05",
"series_number": "5",
"volume": "125",
"issue": "5",
"pages": "2411-2426"
},
{
"id": "authors:bpb6c-3z568",
"collection": "authors",
"collection_id": "bpb6c-3z568",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150605-130416136",
"type": "article",
"title": "An extraordinary cluster of massive stars near the centre of the Milky Way",
"author": [
{
"family_name": "Serabyn",
"given_name": "E.",
"clpid": "Serabyn-E"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Figer",
"given_name": "D. F.",
"clpid": "Figer-D-F"
}
],
"abstract": "The relative numbers of newborn stars of different masses in a galaxy (the initial mass function) determines whether the galaxy's interstellar gas goes mainly into long-lived low-mass stars, as in the disks of normal spiral galaxies, or into short-lived massive stars, as has been proposed for \"starburst\" galaxies. The centre of the Milky Way is not a fully-fledged starburst region, but its star formation rate per unit volume of space is nevertheless roughly a thousand times that of the disk. It is, however, very difficult to study the initial mass function near the centre, because the dust in the gas clouds obscures the starlight, and the relatively rare young stars are mixed with much more numerous older stars. Here we report high-resolution infrared observations of a compact cluster of stars in the central region of our Galaxy. We find approximately 100 young, massive main-sequence stars, several of which seem to be among the most massive in the Galaxy. This cluster may be a weak analogue of the large star clusters in starburst galaxies, which opens the possibility of studying the starburst phenomenon through a local example.",
"doi": "10.1038/28799",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "1998-07-30",
"series_number": "6692",
"volume": "394",
"issue": "6692",
"pages": "448-451"
},
{
"id": "authors:s1fx5-dpa03",
"collection": "authors",
"collection_id": "s1fx5-dpa03",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170213-101148833",
"type": "article",
"title": "Visual and Near-Infrared Imaging of Ultraluminous Infrared Galaxies: The IRAS 2 Jy Sample",
"author": [
{
"family_name": "Murphy",
"given_name": "T. W., Jr.",
"clpid": "Murphy-T-W-Jr"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Matthews",
"given_name": "K.",
"clpid": "Matthews-K"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Mazzarella",
"given_name": "J. M.",
"orcid": "0000-0002-8204-8619",
"clpid": "Mazzarella-J-M"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Strauss",
"given_name": "M. A.",
"orcid": "0000-0002-0106-7755",
"clpid": "Strauss-M-A"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
}
],
"abstract": "New near-infrared and visual images at 2.2 \u03bcm and 6550 \u00c5 are presented for 46 galaxies having infrared luminosities of L_(IR) > 8.5 x 10^(11) L_\u2299, 60 \u03bcm flux densities greater than 1.94 Jy, and declinations greater than -35\u00b0. These galaxies make up a significant fraction of a complete, northern hemisphere sample of ultraluminous infrared galaxies. Visual and/or near-infrared imaging data now exist for 56 ultraluminous infrared galaxies out to nearly 50 000 km s^(-1). Of these 56 galaxies, 53 (95%) show evidence for current or past interactions. Among these systems, there are a large variety of visual morphologies, including strongly interacting pairs with apparent tidal tails, as well as single, distorted galaxies with close double nuclei. There are three galaxies which, to the limits of the imaging data, do not appear to have suffered a recent interaction or merger. Approximately 47% (25/53) of the interacting systems have double nuclei, with projected nuclear separations ranging from 0.3 to 48 kpc. Seven systems have nuclear separations larger than 10 kpc. If the 53 interacting galaxies are viewed as stages in the evolution of pairs of interacting spiral galaxies to a single, luminous AGN or starburst, the present imaging data can be used to estimate the lifetime of the bright infrared phase. Including only those sample galaxies with morphological evidence for interactions, we calculate a lower and an upper limit to the lifetime of the ultraluminous infrared phase of the sample as a whole to be 2 x 10^8 and 2 x 10^9 yr, respectively. Comparison of these dynamical estimates to models of the mergers of gas-rich galaxies and the rates at which fuel is exhausted by starbursts or AGN suggests the lifetime of the ultraluminous phase lies much closer to the smaller of these two values. Selecting galaxies based upon luminous infrared activity clearly biases the sample towards merging galaxies with small physical separations. However, the existence of pairs with large separations indicates that the ultraluminous phase may in some cases start early during the merger process. Alternatively, these systems may contain unresolved third nuclei responsible for triggering the ultraluminous activity. We briefly compare our results to recent models of merging spiral galaxies.",
"doi": "10.1086/117849",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "1996-03",
"series_number": "3",
"volume": "111",
"issue": "3",
"pages": "1025-1052"
},
{
"id": "authors:f65ma-jep54",
"collection": "authors",
"collection_id": "f65ma-jep54",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170213-094321448",
"type": "article",
"title": "Near Infrared Observations of IRAS 09104+4109",
"author": [
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
}
],
"abstract": "Near infrared imaging and grism spectroscopy of the high luminosity infrared bright galaxy IRAS 09104+4109 have been obtained with the W. M. Keck Telescope. The imaging shows 6 \"knots\" of emission projected against the extended stellar envelope of the cD galaxy thought to be the source of the large far infrared luminosity. The luminosities of the knots are consistent with the bulges of galaxies\naccreting onto the central galaxy. In addition, there are 11 companion galaxies seen at radii of 40-150 kpc from the cD nucleus. These objects have colors in the range R\u2014K~ 3.5\u00b10.5 mag, J-H~0.9\u00b10.2 mag H-K ~0.7\u00b10.2 mag, which are consistent with galaxies at a redshift of 0.4. The companion galaxies have luminosities comparable to or less than the characteristic luminosity (L^*) of field galaxies. While the central cD galaxy is identified with the luminous infrared source, it appears to be a quiescent, radio-quiet galaxy, showing no evidence from its near infrared colors for a highly reddened nucleus as seen in other infrared luminous galaxies. The grism spectroscopy shows forbidden lines of low ionization stages of sulfer, iron, and oxygen, as well as hydrogen recombination lines and a strong line of neutral helium. A visual extinction of Av\u20142 mag is derived to the narrow line region surrounding the galaxy nucleus, based on the\nline ratios [S II]1.03 \u00b5m/0.407 \u00b5m and P\u03b4/H\u03b2. The near infrared spectrum is consistent with the optical\nclassification of this system being a Seyfert 2 nucleus.",
"doi": "10.1086/117814",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "1996-02",
"series_number": "2",
"volume": "111",
"issue": "2",
"pages": "649-654"
},
{
"id": "authors:nwvb2-d8f22",
"collection": "authors",
"collection_id": "nwvb2-d8f22",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141029-131913132",
"type": "article",
"title": "Palomar observations of the R impact of comet Shoemaker-Levy 9: II. Spectra",
"author": [
{
"family_name": "Nicholson",
"given_name": "P. D.",
"orcid": "0000-0003-2275-4463",
"clpid": "Nicholson-P-D"
},
{
"family_name": "Gierasch",
"given_name": "P. J.",
"clpid": "Gierasch-P-J"
},
{
"family_name": "Hayward",
"given_name": "T. L.",
"clpid": "Hayward-T-L"
},
{
"family_name": "McGhee",
"given_name": "C. A.",
"clpid": "McGhee-C-A"
},
{
"family_name": "Moersch",
"given_name": "J. E.",
"clpid": "Moersch-J-E"
},
{
"family_name": "Squyres",
"given_name": "S. W.",
"clpid": "Squyres-S-W"
},
{
"family_name": "Van Cleve",
"given_name": "J.",
"clpid": "Van-Cleve-J"
},
{
"family_name": "Matthews",
"given_name": "K.",
"clpid": "Matthews-Keith-Astronomy"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
},
{
"family_name": "Shupe",
"given_name": "D.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Weinberger",
"given_name": "A.",
"orcid": "0000-0001-6654-7859",
"clpid": "Weinberger-A-J"
},
{
"family_name": "Miles",
"given_name": "J. W.",
"clpid": "Miles-J-W"
},
{
"family_name": "Conrath",
"given_name": "B. J.",
"clpid": "Conrath-B-J"
}
],
"abstract": "We present mid-infrared spectroscopic observations from Palomar observatory of the impact of fragment R of comet P/Shoemaker-Levy 9 with Jupiter on 21 July 1994. Low-resolution 8\u201313 \u00b5m spectra taken near the peak of the lightcurve show a broad emission feature that resembles the silicate feature commonly seen in comets and the interstellar medium. We use this feature to estimate the dust content of the impact plume. The overall infrared spectral energy distribution at the time of peak brightness is consistent with emission from an optically-thin layer of small particles at \u223c600 K. Integrating over the spectrum and the lightcurve, we obtain a total radiated energy from the R impact of \u2265 2 \u00d7 10^(25) ergs and a plume mass of \u2265 3 \u00d7 10^(13) g.",
"doi": "10.1029/95GL01067",
"issn": "0094-8276",
"publisher": "American Geophysical Union",
"publication": "Geophysical Research Letters",
"publication_date": "1995-06-15",
"series_number": "12",
"volume": "22",
"issue": "12",
"pages": "1617-1620"
},
{
"id": "authors:vbzvc-qqb04",
"collection": "authors",
"collection_id": "vbzvc-qqb04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170214-134731167",
"type": "article",
"title": "Near-infrared (Fe II) and Pa\u03b2 imaging and spectroscopy of ARP 220",
"author": [
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Matthews",
"given_name": "K.",
"clpid": "Matthews-K"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
}
],
"abstract": "We have imaged the ultraluminous infrared galaxy Arp 220 in light of the near-infrared [Fe II] 1.257 \u03bcm and Pa\u03b2 lines, and have obtained spectra in the J- and H-band atmospheric windows. Arp 220 is a strong source of [Fe II] and Pa\u03b2 emission, with luminosities of 1.3 x 10^(41) and 9.2 x 10^(40) ergs s^(-1), respectively. The [Fe II] and Pa\u03b2 emission are both extended over the central 2\"-3\", but with different morphologies. The Pa\u03b2 line is strongly peaked at the position of the western nucleus seen at 2.2 \u03bcm (Graham et al. 1990) with a fainter \"spur\" in the direction of the eastern nucleus. The [Fe II] emission line shows a weak peak at the western nucleus along with diffuse emission extending to the east, but with no indication of a secondary maximum. The [Fe II] is more extended in the north-south direction than the Pa\u03b2 line. Nearly 75% of the detected [Fe II] emission is spatially resolved. The overall [Fe II]-to-Pa\u03b2 line flux ratio in Arp 220 is consistent with that seen over similar spatial scales in Seyfert 2 galaxies, yet larger than what is measured in galaxies with nuclear starbursts. The [Fe II]-to-Pa\u03b2 line flux ratio is spatially variable being approximately 0.8 at the position of the western nucleus and approximately 2.0 at radii of up to 500 pc. We suggest that the extended [Fe II] emission is produced through the interaction of fast shocks with ambient gas in the ISM at the base of the outflowing, supernovae-driven superwind mapped by Heckman et al. (1987). The bolometric luminosity of the starburst required to power this wind is estimated to be at least 2 x 10^(11) L_\u2609. If the spatially unresolved [Fe II] emission is produced via a large number of supernova remnants, the implied rate is ~0.6 yr^(-1). The overall luminosity of such a starburst could account for a large fraction (1/2-1/3) of the Arp 220 energy budget, but the large deficit of ionizing photons (as counted by the Pa\u03b2 luminosity) requires that the starburst be rapidly declining and/or have a low upper mass cutoff. Alternatively, dust may effectively compete with the\ngas for ionizing photons, or much of the ionizing radiation may escape through \"holes\" in the ISM. It is also possible that a buried AGN produces a large fraction of the unresolved [Fe II] and Pa\u03b2 emission. We briefly discuss these possibilities in light of these new imaging and spectroscopic data.",
"doi": "10.1086/175261",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "1995-02-10",
"series_number": "2",
"volume": "440",
"issue": "2",
"pages": "200-209"
}
]