[ { "id": "authors:bdpxz-qvr82", "collection": "authors", "collection_id": "bdpxz-qvr82", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150629-075947984", "type": "article", "title": "Co-evolution of black hole growth and star formation from a\n cross-correlation analysis between quasars and the cosmic infrared background", "author": [ { "family_name": "Wang", "given_name": "Lingyu", "clpid": "Wang-Lingyu" }, { "family_name": "Viero", "given_name": "Marco", "clpid": "Viero-M-P" }, { "family_name": "Ross", "given_name": "Nicholas P.", "orcid": "0000-0003-1830-6473", "clpid": "Ross-N-P" }, { "family_name": "Asboth", "given_name": "Viktoria", "clpid": "Asboth-V" }, { "family_name": "B\u00e9thermin", "given_name": "Matthieu", "orcid": "0000-0002-3915-2015", "clpid": "B\u00e9thermin-Matthieu" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Clements", "given_name": "Dave", "orcid": "0000-0002-9548-5033", "clpid": "Clements-D-L" }, { "family_name": "Conley", "given_name": "Alex", "clpid": "Conley-A" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Farrah", "given_name": "Duncan", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-D" }, { "family_name": "Hajian", "given_name": "Amir", "clpid": "Hajian-A" }, { "family_name": "Han", "given_name": "Jiaxin", "orcid": "0000-0002-8010-6715", "clpid": "Han-Jiaxin" }, { "family_name": "Lagache", "given_name": "Guilaine", "orcid": "0000-0003-1492-2519", "clpid": "Lagache-Guilaine" }, { "family_name": "Marsden", "given_name": "Gaelen", "clpid": "Marsden-G" }, { "family_name": "Myers", "given_name": "Adam", "clpid": "Myers-A" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Oliver", "given_name": "Sebastian", "orcid": "0000-0001-7862-1032", "clpid": "Oliver-Sebastian-J" }, { "family_name": "Page", "given_name": "Mat", "orcid": "0000-0002-6689-6271", "clpid": "Page-M-J" }, { "family_name": "Symeonidis", "given_name": "Myrto", "clpid": "Symeonidis-M" }, { "family_name": "Schulz", "given_name": "Bernhard", "clpid": "Schulz-B" }, { "family_name": "Wang", "given_name": "Wenting", "clpid": "Wang-Wenting" }, { "family_name": "Zemcov", "given_name": "Mike", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "We present the first cross-correlation measurement between Sloan Digital Sky Survey type 1 quasars and the cosmic infrared background (CIB) measured by Herschel. The quasars cover the redshift range 0.15 < z < 3.5 where most of the CIB originates. We detect the sub-millimetre emission of the quasars, which dominates on small scales, and correlated emission from dusty star-forming galaxies (DSFGs) dominant on larger scales. The mean flux of the Data Release 7 (DR7) quasars (median redshift \u3008z\u3009 = 1.4) is 11.1, 7.1 and 3.6 mJy at 250, 350 and 500 \u03bcm, respectively, while the mean flux of the DR9 quasars (\u3008z\u3009 = 2.5) is 5.7, 5.0 and 1.8 mJy at 250, 350 and 500 \u03bcm, respectively. Assuming a modified blackbody spectral energy distribution with a power law in the mid-infrared, we infer that the mean infrared luminosity of the DR7 and DR9 quasars is 10^(12.4) and 10^(12.8)\u2009L_\u2299, respectively. The correlated emission arises from DSFGs in the same halo as the quasar (the one-halo term) and DSFGs in separate haloes correlated with the quasar-hosting halo (the two-halo term). Using a simple halo model, we find that most quasars are hosted by central galaxies. The host halo mass scale of the DR7 central and satellite quasars is 10^(12.4 \u00b1 0.9) and 10^(13.6 \u00b1 0.4) M_\u2299, respectively. The host halo mass scale of the DR9 central and satellite quasars is 10^(12.3 \u00b1 0.6) and 10^(12.8 \u00b1 0.4) M_\u2299, respectively. Thus, the halo environment of the central quasars is similar to that of the most actively star-forming galaxies, which supports the view that dusty starburst and quasar activity are evolutionarily linked.", "doi": "10.1093/mnras/stv559", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2015-06-01", "series_number": "4", "volume": "449", "issue": "4", "pages": "4476-4493" }, { "id": "authors:akywc-jzq88", "collection": "authors", "collection_id": "akywc-jzq88", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141222-091108670", "type": "article", "title": "Are Dusty Galaxies Blue? Insights on UV Attenuation from Dust-selected Galaxies", "author": [ { "family_name": "Casey", "given_name": "C. M.", "orcid": "0000-0002-0930-6466", "clpid": "Casey-C-M" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Lee", "given_name": "N.", "clpid": "Lee-Nicholas" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Finkelstein", "given_name": "S. L.", "orcid": "0000-0001-8519-1130", "clpid": "Finkelstein-S-L" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "de Zotti", "given_name": "G.", "orcid": "0000-0003-2868-2595", "clpid": "De-Zotti-G" }, { "family_name": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Fu", "given_name": "H.", "orcid": "0000-0001-9608-6395", "clpid": "Fu-Hai" }, { "family_name": "Le Floc'h", "given_name": "E.", "clpid": "Le-Floc'h-Emeric" }, { "family_name": "Ilbert", "given_name": "O.", "orcid": "0000-0002-7303-4397", "clpid": "Ilbert-Olivier" }, { "family_name": "Ivison", "given_name": "R. J.", "orcid": "0000-0001-5118-1313", "clpid": "Ivison-R-J" }, { "family_name": "Takeuchi", "given_name": "T. T.", "clpid": "Takeuchi-Tsutomu-T" } ], "abstract": "Galaxies' rest-frame ultraviolet (UV) properties are often used to directly infer the degree to which dust obscuration affects the measurement of star formation rates (SFRs). While much recent work has focused on calibrating dust attenuation in galaxies selected at rest-frame ultraviolet wavelengths, locally and at high-z, here we investigate attenuation in dusty, star forming galaxies (DSFGs) selected at far-infrared wavelengths. By combining multiwavelength coverage across 0.15-500 \u03bcm in the COSMOS field, in particular making use of Herschel imaging, and a rich data set on local galaxies, we find an empirical variation in the relationship between the rest-frame UV slope (\u03b2) and the ratio of infrared-to-ultraviolet emission (L_IR/L_UV \u2261 IRX) as a function of infrared luminosity, or total SFR. Both locally and at high-z, galaxies above SFR \u2273 50 M_\u2609 yr^\u20131 deviate from the nominal IRX-\u03b2 relation toward bluer colors by a factor proportional to their increasing IR luminosity. We also estimate contamination rates of DSFGs on high-z dropout searches of \u226a1% at z \u2272 4-10, providing independent verification that contamination from very dusty foreground galaxies is low in Lyman-break galaxy searches. Overall, our results are consistent with the physical interpretation that DSFGs, e.g., galaxies with >50 M_\u2609 yr^\u20131, are dominated at all epochs by short-lived, extreme burst events, producing many young O and B stars that are primarily, yet not entirely, enshrouded in thick dust cocoons. The blue rest-frame UV slopes of DSFGs are inconsistent with the suggestion that most DSFGs at z ~ 2 exhibit steady-state star formation in secular disks.", "doi": "10.1088/0004-637X/796/2/95", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2014-12-01", "series_number": "2", "volume": "796", "issue": "2", "pages": "Art. No. 95" }, { "id": "authors:jj0c8-yb582", "collection": "authors", "collection_id": "jj0c8-yb582", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141121-102020063", "type": "article", "title": "HerMES: point source catalogues from Herschel-SPIRE observations II", "author": [ { "family_name": "Wang", "given_name": "L.", "clpid": "Wang-Lingyu" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Clarke", "given_name": "C.", "clpid": "Clarke-C" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Buat", "given_name": "V.", "clpid": "Buat-V" }, { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Guo", "given_name": "K.", "clpid": "Guo-K" }, { "family_name": "Heinis", "given_name": "S.", "clpid": "Heinis-S" }, { "family_name": "Magdis", "given_name": "G.", "orcid": "0000-0002-4872-2294", "clpid": "Magdis-G-E" }, { "family_name": "Marchetti", "given_name": "L.", "orcid": "0000-0003-3948-7621", "clpid": "Marchetti-L" }, { "family_name": "Marsden", "given_name": "G.", "clpid": "Marsden-G" }, { "family_name": "Norberg", "given_name": "P.", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Oliver", "given_name": "S. J.", "orcid": "0000-0001-7862-1032", "clpid": "Oliver-Sebastian-J" }, { "family_name": "Page", "given_name": "M. J.", "orcid": "0000-0002-6689-6271", "clpid": "Page-M-J" }, { "family_name": "Roehlly", "given_name": "Y.", "clpid": "Roehlly-Y" }, { "family_name": "Roseboom", "given_name": "I. G.", "clpid": "Roseboom-I-G" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Smith", "given_name": "A. J.", "clpid": "Smith-A-J" }, { "family_name": "Vaccari", "given_name": "M.", "orcid": "0000-0002-6748-0577", "clpid": "Vaccari-Mattia" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "The Herschel Multi-tiered Extragalactic Survey (HerMES) is the largest Guaranteed Time Key Programme on the Herschel Space Observatory. With a wedding cake survey strategy, it consists of nested fields with varying depth and area totalling \u223c380 deg^2. In this paper, we present deep point source catalogues extracted from Herschel-Spectral and Photometric Imaging Receiver (SPIRE) observations of all HerMES fields, except for the later addition of the 270 deg^2 HerMES Large-Mode Survey (HeLMS) field. These catalogues constitute the second Data Release (DR2) made in 2013 October. A sub-set of these catalogues, which consists of bright sources extracted from Herschel-SPIRE observations completed by 2010 May\u20091 (covering \u223c74 deg^2) were released earlier in the first extensive data release in 2012 March. Two different methods are used to generate the point source catalogues, the sussextractor point source extractor used in two earlier data releases (EDR and EDR2) and a new source detection and photometry method. The latter combines an iterative source detection algorithm, starfinder, and a De-blended SPIRE Photometry algorithm. We use end-to-end Herschel-SPIRE simulations with realistic number counts and clustering properties to characterize basic properties of the point source catalogues, such as the completeness, reliability, photometric and positional accuracy. Over 500 000 catalogue entries in HerMES fields (except HeLMS) are released to the public through the HeDAM (Herschel Database in Marseille) website (http://hedam.lam.fr/HerMES).", "doi": "10.1093/mnras/stu1569", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2014-11-01", "series_number": "3", "volume": "444", "issue": "3", "pages": "2870-2883" }, { "id": "authors:jy2na-vdq62", "collection": "authors", "collection_id": "jy2na-vdq62", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140617-094634128", "type": "article", "title": "Constraining the Ly\u03b1 Escape Fraction with Far-infrared Observations of Ly\u03b1 Emitters", "author": [ { "family_name": "Wardlow", "given_name": "Julie L.", "orcid": "0000-0003-2376-8971", "clpid": "Wardlow-J-L" }, { "family_name": "Malhotra", "given_name": "S.", "orcid": "0000-0002-9226-5350", "clpid": "Malhotra-S" }, { "family_name": "Zheng", "given_name": "Z.", "clpid": "Zheng-Zheng" }, { "family_name": "Finkelstein", "given_name": "S.", "orcid": "0000-0001-8519-1130", "clpid": "Finkelstein-S-L" }, { "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": "Calanog", "given_name": "J.", "clpid": "Calanog-J-A" }, { "family_name": "Ciardullo", "given_name": "R.", "clpid": "Ciardullo-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": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-D" }, { "family_name": "Gawiser", "given_name": "E.", "clpid": "Gawiser-E" }, { "family_name": "Gronwall", "given_name": "C.", "clpid": "Gronwall-C" }, { "family_name": "Heinis", "given_name": "S.", "clpid": "Heinis-S" }, { "family_name": "Ibar", "given_name": "E.", "clpid": "Ibar-Eduardo" }, { "family_name": "Ivison", "given_name": "R. J.", "orcid": "0000-0001-5118-1313", "clpid": "Ivison-R-J" }, { "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": "Rhoads", "given_name": "J.", "clpid": "Rhoads-J" }, { "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": "Smith", "given_name": "A. J.", "clpid": "Smith-A-J" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Wang", "given_name": "L.", "orcid": "0000-0002-9803-166X", "clpid": "Wang-L" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "We study the far-infrared properties of 498 Ly\u03b1 emitters (LAEs) at z = 2.8, 3.1, and 4.5 in the Extended Chandra Deep Field-South, using 250, 350, and 500 \u03bcm data from the Herschel Multi-tiered Extragalactic Survey and 870 \u03bcm data from the LABOCA ECDFS Submillimeter Survey. None of the 126, 280, or 92 LAEs at z = 2.8, 3.1, and 4.5, respectively, are individually detected in the far-infrared data. We use stacking to probe the average emission to deeper flux limits, reaching 1\u03c3 depths of ~0.1 to 0.4 mJy. The LAEs are also undetected at \u22653\u03c3 in the stacks, although a 2.5\u03c3 signal is observed at 870 \u03bcm for the z = 2.8 sources. We consider a wide range of far-infrared spectral energy distributions (SEDs), including an M82 and an Sd galaxy template, to determine upper limits on the far-infrared luminosities and far-infrared-derived star formation rates of the LAEs. These star formation rates are then combined with those inferred from the Ly\u03b1 and UV emission to determine lower limits on the LAEs' Ly\u03b1 escape fraction (f_(esc)(Ly\u03b1)). For the Sd SED template, the inferred LAEs f_(esc)(Ly\u03b1) are \u227330% (1\u03c3) at z = 2.8, 3.1, and 4.5, which are all significantly higher than the global f_(esc)(Ly\u03b1) at these redshifts. Thus, if the LAEs f_(esc)(Ly\u03b1) follows the global evolution, then they have warmer far-infrared SEDs than the Sd galaxy template. The average and M82 SEDs produce lower limits on the LAE f_(esc)(Ly\u03b1) of ~10%-20% (1\u03c3), all of which are slightly higher than the global evolution of f_(esc)(Ly\u03b1), but consistent with it at the 2\u03c3-3\u03c3 level.", "doi": "10.1088/0004-637X/787/1/9", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2014-05-20", "series_number": "1", "volume": "787", "issue": "1", "pages": "Art. No. 9" }, { "id": "authors:yg9t6-gkj85", "collection": "authors", "collection_id": "yg9t6-gkj85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-091456467", "type": "article", "title": "Herschel Multitiered Extragalactic Survey: clusters of dusty galaxies uncovered by Herschel and Planck", "author": [ { "family_name": "Clements", "given_name": "D. L.", "orcid": "0000-0002-9548-5033", "clpid": "Clements-D-L" }, { "family_name": "Braglia", "given_name": "F. G.", "clpid": "Braglia-F-G" }, { "family_name": "Hyde", "given_name": "A. K.", "clpid": "Hyde-A-K" }, { "family_name": "P\u00e9rez-Fournon", "given_name": "I.", "clpid": "P\u00e9rez-Fournon-I" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Cava", "given_name": "A.", "clpid": "Cava-A" }, { "family_name": "Chapman", "given_name": "S.", "clpid": "Chapman-S-C" }, { "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": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Gonzales Solares", "given_name": "E. A.", "orcid": "0000-0001-9123-0626", "clpid": "Gonzales-Solares-E-A" }, { "family_name": "Marchetti", "given_name": "L.", "orcid": "0000-0003-3948-7621", "clpid": "Marchetti-L" }, { "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": "Roseboom", "given_name": "I. G.", "clpid": "Roseboom-I-G" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Smith", "given_name": "A. J.", "clpid": "Smith-A-J" }, { "family_name": "Vaccari", "given_name": "M.", "orcid": "0000-0002-6748-0577", "clpid": "Vaccari-Mattia" }, { "family_name": "Vieira", "given_name": "J.", "clpid": "Vieira-J" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Wang", "given_name": "L.", "clpid": "Wang-Lingyu" }, { "family_name": "Wardlow", "given_name": "J.", "orcid": "0000-0003-2376-8971", "clpid": "Wardlow-J-L" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "de Zotti", "given_name": "G.", "orcid": "0000-0003-2868-2595", "clpid": "De-Zotti-G" } ], "abstract": "The potential for Planck to detect clusters of dusty, star-forming galaxies at z > 1 is tested by examining the Herschel-SPIRE images of Planck Early Release Compact Source Catalog sources lying in fields observed by the Herschel Multitiered Extragalactic Survey. Of the 16 Planck sources that lie in the \u223c90 sq. deg. examined, we find that 12 are associated with single bright Herschel sources. The remaining four are associated with overdensities of Herschel sources, making them candidate clusters of dusty, star-forming galaxies. We use complementary optical/near-IR data for these 'clumps' to test this idea, and find evidence for the presence of galaxy clusters in all four cases. We use photometric redshifts and red sequence galaxies to estimate the redshifts of these clusters, finding that they range from 0.8 to 2.3. These redshifts imply that the Herschel sources in these clusters, which contribute to the detected Planck flux, are forming stars very rapidly, with typical total cluster star formation rates >1000\u2009M_\u2299\u2009yr^(\u22121). The high-redshift clusters discovered in these observations are used to constrain the epoch of cluster galaxy formation, finding that the galaxies in our clusters are 1\u20131.5 Gyr old at z \u223c 1\u20132. Prospects for the discovery of further clusters of dusty galaxies are discussed, using not only all sky Planck surveys, but also deeper, smaller area, Herschel surveys.", "doi": "10.1093/mnras/stt2253", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2014-04", "series_number": "2", "volume": "439", "issue": "2", "pages": "1193-1211" }, { "id": "authors:7vp5x-kb465", "collection": "authors", "collection_id": "7vp5x-kb465", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140326-101000362", "type": "article", "title": "HerMES: dust attenuation and star formation activity in ultraviolet-selected samples from z \u223c 4 to \u223c 1.5", "author": [ { "family_name": "Heinis", "given_name": "S.", "clpid": "Heinis-S" }, { "family_name": "Buat", "given_name": "V.", "clpid": "Buat-V" }, { "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": "Burgarella", "given_name": "D.", "clpid": "Burgarella-D" }, { "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": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" } ], "abstract": "We study the link between observed ultraviolet (UV) luminosity, stellar mass and dust attenuation within rest-frame UV-selected samples at z \u223c 4,\u2009 \u223c 3 and \u223c1.5. We measure by stacking at 250, 350 and 500\u2009\u03bcm in the Herschel/Spectral and Photometric Imaging Receiver images from the Herschel Multi-Tiered Extragalactic Survey (HerMES) program the average infrared luminosity as a function of stellar mass and UV luminosity. We find that dust attenuation is mostly correlated with stellar mass. There is also a secondary dependence with UV luminosity: at a given UV luminosity, dust attenuation increases with stellar mass, while at a given stellar mass it decreases with UV luminosity. We provide new empirical recipes to correct for dust attenuation given the observed UV luminosity and the stellar mass. Our results also enable us to put new constraints on the average relation between star formation rate (SFR) and stellar mass at z \u223c 4, \u223c3 and \u223c1.5. The SFR\u2013stellar mass relations are well described by power laws (SFR\u221dM^(0.7__\u2217), with the amplitudes being similar at z \u223c 4 and \u223c3, and decreasing by a factor of 4 at z \u223c 1.5 at a given stellar mass. We further investigate the evolution with redshift of the specific SFR. Our results are in the upper range of previous measurements, in particular at z \u223c 3, and are consistent with a plateau at 3 < z < 4. Current model predictions (either analytic, semi-analytic or hydrodynamic) are inconsistent with these values, as they yield lower predictions than the observations in the redshift range we explore. We use these results to discuss the star formation histories of galaxies in the framework of the main sequence of star-forming galaxies. Our results suggest that galaxies at high redshift (2.5 < z < 4) stay around 1 Gyr on the main sequence. With decreasing redshift, this time increases such that z = 1 main-sequence galaxies with 108", "doi": "10.1093/mnras/stt1960", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2014-01-11", "series_number": "2", "volume": "437", "issue": "2", "pages": "1268-1283" }, { "id": "authors:0f1h8-3ps49", "collection": "authors", "collection_id": "0f1h8-3ps49", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131025-085434310", "type": "article", "title": "HerMES: The Far-infrared Emission from Dust-obscured Galaxies", "author": [ { "family_name": "Calanog", "given_name": "J. A.", "clpid": "Calanog-J-A" }, { "family_name": "Wardlow", "given_name": "J.", "orcid": "0000-0003-2376-8971", "clpid": "Wardlow-J-L" }, { "family_name": "Fu", "given_name": "Hai", "orcid": "0000-0001-9608-6395", "clpid": "Fu-Hai" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Assef", "given_name": "R. J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Casey", "given_name": "C. M.", "orcid": "0000-0002-0930-6466", "clpid": "Casey-C-M" }, { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Ibar", "given_name": "E.", "clpid": "Ibar-Eduardo" }, { "family_name": "Kartaltepe", "given_name": "J.", "orcid": "0000-0001-9187-3605", "clpid": "Kartaltepe-J" }, { "family_name": "Magdis", "given_name": "G.", "clpid": "Magdis-G" }, { "family_name": "Marchetti", "given_name": "L.", "orcid": "0000-0003-3948-7621", "clpid": "Marchetti-L" }, { "family_name": "Oliver", "given_name": "S. J.", "orcid": "0000-0001-7862-1032", "clpid": "Oliver-Sebastian-J" }, { "family_name": "P\u00e9rez-Fournon", "given_name": "I.", "clpid": "P\u00e9rez-Fournon-I" }, { "family_name": "Riechers", "given_name": "D.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Rigopoulou", "given_name": "D.", "orcid": "0000-0001-6854-7545", "clpid": "Rigopoulou-D" }, { "family_name": "Roseboom", "given_name": "I. G.", "clpid": "Roseboom-I-G" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Scott", "given_name": "Douglas", "orcid": "0000-0002-6878-9840", "clpid": "Scott-Douglas" }, { "family_name": "Symeonidis", "given_name": "M.", "clpid": "Symeonidis-M" }, { "family_name": "Vaccari", "given_name": "M.", "orcid": "0000-0002-6748-0577", "clpid": "Vaccari-Mattia" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "Dust-obscured galaxies (DOGs) are an ultraviolet-faint, infrared-bright galaxy population that reside at z ~ 2 and are believed to be in a phase of dusty star-forming and active galactic nucleus (AGN) activity. We present far-infrared (far-IR) observations of a complete sample of DOGs in the 2 deg^2 of the Cosmic Evolution Survey. The 3077 DOGs have \u3008z\u3009 = 1.9 \u00b1 0.3 and are selected from 24 \u03bcm and r^+ observations using a color cut of r^+ \u2013 [24] \u2265 7.5 (AB mag) and S_(24) \u2265 100 \u03bcJy. Based on the near-IR spectral energy distributions, 47% are bump DOGs (star formation dominated) and 10% are power-law DOGs (AGN-dominated). We use SPIRE far-IR photometry from the Herschel Multi-tiered Extragalactic Survey to calculate the IR luminosity and characteristic dust temperature for the 1572 (51%) DOGs that are detected at 250 \u03bcm (\u22653\u03c3). For the remaining 1505 (49%) that are undetected, we perform a median stacking analysis to probe fainter luminosities. Herschel-detected and undetected DOGs have average luminosities of (2.8 \u00b1 0.4) \u00d7 10^(12) L_\u2609 and (0.77 \u00b1 0.08) \u00d7 10^(12) L_\u2609, and dust temperatures of (33 \u00b1 7) K and (37 \u00b1 5) K, respectively. The IR luminosity function for DOGs with S_(24) \u2265 100 \u03bcJy is calculated, using far-IR observations and stacking. DOGs contribute 10%-30% to the total star formation rate (SFR) density of the universe at z = 1.5-2.5, dominated by 250 \u03bcm detected and bump DOGs. For comparison, DOGs contribute 30% to the SFR density for all z = 1.5-2.5 galaxies with S_(24) \u2265 100 \u03bcJy. DOGs have a large scatter about the star formation main sequence and their specific SFRs show that the observed phase of star formation could be responsible for their total observed stellar mass at z ~ 2.", "doi": "10.1088/0004-637X/775/1/61", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-09-20", "series_number": "1", "volume": "775", "issue": "1", "pages": "Art. No. 61" }, { "id": "authors:j2zzr-t8803", "collection": "authors", "collection_id": "j2zzr-t8803", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131009-091455399", "type": "article", "title": "Flux calibration of broad-band far-infrared and submillimetre photometric instruments: theory and application to Herschel-SPIRE", "author": [ { "family_name": "Griffin", "given_name": "M. J.", "clpid": "Griffin-M-J" }, { "family_name": "North", "given_name": "C. E.", "clpid": "North-C-E" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Amaral-Rogers", "given_name": "A.", "clpid": "Amaral-Rogers-A" }, { "family_name": "Bendo", "given_name": "G.", "clpid": "Bendo-G-J" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Conversi", "given_name": "L.", "clpid": "Conversi-L" }, { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Ferlet", "given_name": "M.", "clpid": "Ferlet-M-J" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Lim", "given_name": "T.", "clpid": "Lim-Tanya-L" }, { "family_name": "Pearson", "given_name": "C.", "orcid": "0000-0001-6139-649X", "clpid": "Pearson-C-P" }, { "family_name": "Pohlen", "given_name": "M.", "clpid": "Pohlen-M" }, { "family_name": "Sibthorpe", "given_name": "B.", "clpid": "Sibthorpe-B" }, { "family_name": "Spencer", "given_name": "L.", "clpid": "Spencer-L" }, { "family_name": "Swinyard", "given_name": "B.", "clpid": "Swinyard-B" }, { "family_name": "Valtchanov", "given_name": "I.", "orcid": "0000-0001-9930-7886", "clpid": "Valtchanov-I" } ], "abstract": "Photometric instruments operating at far-infrared to millimetre wavelengths often have broad spectral passbands (\u03bb/\u0394\u03bb \u223c 3 or less), especially those operating in space. A broad passband can result in significant variation of the beam profile and aperture efficiency across the passband, effects which thus far have not generally been taken into account in the flux calibration of such instruments. With absolute calibration uncertainties associated with the brightness of primary calibration standards now in the region of 5\u2009per\u2009cent or less, variation of the beam properties across the passband can be a significant contributor to the overall calibration accuracy for extended emission. We present a calibration framework which takes such variations into account for both antenna-coupled and absorber-coupled focal plane architectures. The scheme covers point source and extended source cases, and also the intermediate case of a semi-extended source profile. We apply the new method to the Spectral and Photometric Imaging Receiver (SPIRE) photometer on board the Herschel Space Observatory.", "doi": "10.1093/mnras/stt999", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2013-09", "series_number": "2", "volume": "434", "issue": "2", "pages": "992-1004" }, { "id": "authors:jej8e-7k075", "collection": "authors", "collection_id": "jej8e-7k075", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130606-115901445", "type": "article", "title": "Connecting stellar mass and star-formation rate to dark matter halo mass out to z \u223c 2", "author": [ { "family_name": "Wang", "given_name": "L.", "clpid": "Wang-Lingyu" }, { "family_name": "Farrah", "given_name": "D. G.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Oliver", "given_name": "S. J.", "orcid": "0000-0001-7862-1032", "clpid": "Oliver-Sebastian-J" }, { "family_name": "Amblard", "given_name": "A.", "clpid": "Amblard-A" }, { "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": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Halpern", "given_name": "M.", "orcid": "0000-0002-1760-0868", "clpid": "Halpern-M" }, { "family_name": "Heinis", "given_name": "S.", "clpid": "Heinis-S" }, { "family_name": "Ibar", "given_name": "E.", "clpid": "Ibar-Eduardo" }, { "family_name": "Ilbert", "given_name": "O.", "orcid": "0000-0002-7303-4397", "clpid": "Ilbert-Olivier" }, { "family_name": "Ivison", "given_name": "R. J.", "orcid": "0000-0001-5118-1313", "clpid": "Ivison-R-J" }, { "family_name": "Marsden", "given_name": "G.", "clpid": "Marsden-G" }, { "family_name": "Roseboom", "given_name": "I. G.", "clpid": "Roseboom-I-G" }, { "family_name": "Rowan-Robinson", "given_name": "M.", "clpid": "Rowan-Robinson-M" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Smith", "given_name": "A. J.", "clpid": "Smith-A-J" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "We have constructed an extended halo model (EHM) which relates the total stellar mass and star-formation rate (SFR) to halo mass (M_h). An empirical relation between the distribution functions of total stellar mass of galaxies and host halo mass, tuned to match the spatial density of galaxies over 0 < z < 2 and the clustering properties at z \u223c 0, is extended to include two different scenarios describing the variation of SFR on M_h. We also present new measurements of the redshift evolution of the average SFR for star-forming galaxies of different stellar masses up to z = 2, using data from the Herschel Multi-tiered Extragalactic Survey for infrared bright galaxies. Combining the EHM with the halo accretion histories from numerical simulations, we trace the stellar mass growth and star-formation history in haloes spanning a range of masses. We find that: (1) the intensity of the star-forming activity in haloes in the probed mass range has steadily decreased from z \u223c 2 to 0; (2) at a given epoch, haloes in the mass range between a few times 10^(11)\u2009M_\u2299 and a few times 10^(12)\u2009M_\u2299 are the most efficient at hosting star formation; (3) the peak of SFR density shifts to lower mass haloes over time; and (4) galaxies that are forming stars most actively at z \u223c 2 evolve into quiescent galaxies in today's group environments, strongly supporting previous claims that the most powerful starbursts at z \u223c 2 are progenitors of today's elliptical galaxies.", "doi": "10.1093/mnras/stt190", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2013-05", "series_number": "1", "volume": "431", "issue": "1", "pages": "648-661" }, { "id": "authors:80pgd-kvp22", "collection": "authors", "collection_id": "80pgd-kvp22", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130613-104444434", "type": "article", "title": "HERMES: unveiling obscured star formation \u2013 the far-infrared luminosity function of ultraviolet-selected galaxies at z \u223c 1.5", "author": [ { "family_name": "Heinis", "given_name": "S.", "clpid": "Heinis-S" }, { "family_name": "Buat", "given_name": "V.", "clpid": "Buat-V" }, { "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": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Boselli", "given_name": "A.", "clpid": "Boselli-A" }, { "family_name": "Burgarella", "given_name": "D.", "clpid": "Burgarella-D" }, { "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": "Farrah", "given_name": "D.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Ibar", "given_name": "E.", "clpid": "Ibar-Eduardo" }, { "family_name": "Ilbert", "given_name": "O.", "orcid": "0000-0002-7303-4397", "clpid": "Ilbert-Olivier" }, { "family_name": "Ivison", "given_name": "R. J.", "orcid": "0000-0001-5118-1313", "clpid": "Ivison-R-J" }, { "family_name": "Magdis", "given_name": "G.", "orcid": "0000-0002-4872-2294", "clpid": "Magdis-G-E" }, { "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": "Page", "given_name": "M. J.", "orcid": "0000-0002-6689-6271", "clpid": "Page-M-J" }, { "family_name": "Rodighiero", "given_name": "G.", "orcid": "0000-0002-9415-2296", "clpid": "Rodighiero-G" }, { "family_name": "Roehlly", "given_name": "Y.", "clpid": "Roehlly-Y" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Scott", "given_name": "Douglas", "orcid": "0000-0002-6878-9840", "clpid": "Scott-Douglas" }, { "family_name": "Smith", "given_name": "A. J.", "clpid": "Smith-A-J" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Wang", "given_name": "L.", "clpid": "Wang-Lingyu" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "We study the far-infrared and sub-millimetre properties of a sample of ultraviolet (UV) selected galaxies at z \u223c 1.5. Using stacking at 250, 350 and 500\u2009\u03bcm from Herschel Space Observatory Spectral and Photometric Imaging Receiver (SPIRE) imaging of the Cosmological Evolution Survey (COSMOS) field obtained within the Herschel Multi-tiered Extragalactic Survey (HERMES) key programme, we derive the mean infrared (IR) luminosity as a function of both UV luminosity and slope of the UV continuum \u03b2. The IR to UV luminosity ratio is roughly constant over most of the UV luminosity range we explore. We also find that the IR to UV luminosity ratio is correlated with \u03b2. We observe a correlation that underestimates the correlation derived from low-redshift starburst galaxies, but is in good agreement with the correlation derived from local normal star-forming galaxies. Using these results we reconstruct the IR luminosity function of our UV-selected sample. This luminosity function recovers the IR luminosity functions measured from IR-selected samples at the faintest luminosities (L_(IR) \u223c 10^(11)\u2009L_\u2299), but might underestimate them at the bright-end (L_(IR) \u2273 5 \u00d7 10^(11)\u2009L_\u2299). For galaxies with 10^(11) < L_(IR)/L_\u2299 < 10^(13), the IR luminosity function of an UV selection recovers (given the differences in IR-based estimates) 52\u201365 to 89\u2013112\u2009per\u2009cent of the star formation rate density derived from an IR selection. The cosmic star formation rate density derived from this IR luminosity function is 61\u201376 to 100\u2013133\u2009per\u2009cent of the density derived from IR selections at the same epoch. Assuming the latest Herschel results and conservative stacking measurements, we use a toy model to fully reproduce the far-IR luminosity function from our UV selection at z \u223c 1.5. This suggests that a sample around 4 mag deeper (i.e. reaching u^* \u223c 30\u2009mag) and a large dispersion of the IR to UV luminosity ratio are required.", "doi": "10.1093/mnras/sts397", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2013-02-21", "series_number": "2", "volume": "429", "issue": "2", "pages": "1113-1132" }, { "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: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:1c6q3-ebq87", "collection": "authors", "collection_id": "1c6q3-ebq87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110207-162201734", "type": "article", "title": "Supernova Constraints and Systematic Uncertainties from the First Three Years of the Supernova Legacy Survey", "author": [ { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Ellis", "given_name": "R. S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Neill", "given_name": "J. D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" } ], "abstract": "We combine high-redshift Type Ia supernovae from the first three years of the Supernova Legacy Survey (SNLS) with other supernova (SN) samples, primarily at lower redshifts, to form a high-quality joint sample of 472 SNe (123 low-z, 93 SDSS, 242 SNLS, and 14 Hubble Space Telescope). SN data alone require cosmic acceleration at >99.999% confidence, including systematic effects. For the dark energy equation of state parameter (assumed constant out to at least z = 1.4) in a flat universe, we find w = \u20130.91^(+0.16)_(\u20130.20)(stat)^(+0.07)_(\u20130.14)(sys) from SNe only, consistent with a cosmological constant. Our fits include a correction for the recently discovered relationship between host-galaxy mass and SN absolute brightness. We pay particular attention to systematic uncertainties, characterizing them using a systematic covariance matrix that incorporates the redshift dependence of these effects, as well as the shape-luminosity and color-luminosity relationships. Unlike previous work, we include the effects of systematic terms on the empirical light-curve models. The total systematic uncertainty is dominated by calibration terms. We describe how the systematic uncertainties can be reduced with soon to be available improved nearby and intermediate-redshift samples, particularly those calibrated onto USNO/SDSS-like systems.", "doi": "10.1088/0067-0049/192/1/1", "issn": "0067-0049", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Supplement Series", "publication_date": "2011-01", "volume": "192", "pages": "Art. No. 1" }, { "id": "authors:4y57r-j9v31", "collection": "authors", "collection_id": "4y57r-j9v31", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170424-145706380", "type": "article", "title": "The Local Hosts of Type Ia Supernovae", "author": [ { "family_name": "Neill", "given_name": "J. D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" }, { "family_name": "Sullivan", "given_name": "M.", "orcid": "0000-0001-9053-4820", "clpid": "Sullivan-Mark" }, { "family_name": "Howell", "given_name": "D. A.", "orcid": "0000-0003-4253-656X", "clpid": "Howell-D-A" }, { "family_name": "Conley", "given_name": "Alex", "clpid": "Conley-A" }, { "family_name": "Seibert", "given_name": "Mark", "orcid": "0000-0002-1143-5515", "clpid": "Seibert-M" }, { "family_name": "Martin", "given_name": "D. Christopher", "orcid": "0000-0002-8650-1644", "clpid": "Martin-D-Christopher" }, { "family_name": "Barlow", "given_name": "Tom A.", "clpid": "Barlow-T-A" }, { "family_name": "Foster", "given_name": "Karl", "orcid": "0000-0001-5800-5531", "clpid": "Forster-K" }, { "family_name": "Friedman", "given_name": "Peter G.", "clpid": "Friedman-P-G" }, { "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": "Wyder", "given_name": "Ted K.", "clpid": "Wyder-T-K" }, { "family_name": "Bianchi", "given_name": "Luciana", "orcid": "0000-0001-7746-5461", "clpid": "Bianchi-L-C" }, { "family_name": "Donas", "given_name": "Jos\u00e9", "clpid": "Donas-J" }, { "family_name": "Heckman", "given_name": "Timothy M.", "clpid": "Heckman-T-M" }, { "family_name": "Lee", "given_name": "Young-Wook", "clpid": "Lee-Young-Wook" }, { "family_name": "Madore", "given_name": "Barry F.", "orcid": "0000-0002-1576-1676", "clpid": "Madore-B-F" }, { "family_name": "Milliard", "given_name": "Bruno", "clpid": "Milliard-B" }, { "family_name": "Rich", "given_name": "R. Michael", "orcid": "0000-0003-0427-8387", "clpid": "Rich-R-M" }, { "family_name": "Szalay", "given_name": "Alex S.", "clpid": "Szalay-A-S" } ], "abstract": "We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1 Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^(10) M\u2609, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population. A low host extinction subsample hints at a residual trend in peak luminosity with host age, after correcting for light-curve shape, giving the appearance that older hosts produce less-extincted SNe Ia on average. This has implications for cosmological fitting of SNe Ia, and suggests that host age could be useful as a parameter in the fitting. Converting host mass to metallicity and computing ^(56)Ni mass from the supernova light curves, we find that our local sample is consistent with a model that predicts a shallow trend between stellar metallicity and the ^(56)Ni mass that powers the explosion, but we cannot rule out the absence of a trend. We measure a correlation between ^(56)Ni mass and host age in the local universe that is shallower and not as significant as that seen at higher redshifts. The details of the age-^(56)Ni mass correlations at low and higher redshift imply a luminosity-weighted age threshold of ~3 Gyr for SN Ia hosts, above which they are less likely to produce SNe Ia with ^(56)Ni masses above ~0.5 M\u2609.", "doi": "10.1088/0004-637X/707/2/1449", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-12-20", "series_number": "2", "volume": "707", "issue": "2", "pages": "1449-1465" }, { "id": "authors:y9qwc-r3e44", "collection": "authors", "collection_id": "y9qwc-r3e44", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090617-204752748", "type": "article", "title": "Improved Cosmological Constraints from New, Old, and Combined Supernova Data Sets", "author": [ { "family_name": "Kowalski", "given_name": "M.", "clpid": "Kowalski-M" }, { "family_name": "Rubin", "given_name": "D.", "clpid": "Rubin-D-M" }, { "family_name": "Aldering", "given_name": "G.", "clpid": "Aldering-G-S" }, { "family_name": "Agostinho", "given_name": "R. J.", "clpid": "Agostinho-R-J" }, { "family_name": "Amadon", "given_name": "A.", "clpid": "Amadon-A" }, { "family_name": "Amanullah", "given_name": "R.", "orcid": "0000-0002-5559-9351", "clpid": "Amanullah-R" }, { "family_name": "Balland", "given_name": "C.", "clpid": "Balland-C" }, { "family_name": "Barbary", "given_name": "K.", "clpid": "Barbary-K" }, { "family_name": "Blanc", "given_name": "G.", "clpid": "Blanc-G" }, { "family_name": "Challis", "given_name": "P. J.", "clpid": "Challis-P-J" }, { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Connolly", "given_name": "N. V.", "clpid": "Connolly-N-V" }, { "family_name": "Covarrubias", "given_name": "R.", "clpid": "Covarrubias-R" }, { "family_name": "Dawson", "given_name": "K. S.", "orcid": "0000-0002-0553-3805", "clpid": "Dawson-Kyle-S" }, { "family_name": "Deustua", "given_name": "S. E.", "clpid": "Deustua-S-E" }, { "family_name": "Ellis", "given_name": "R.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Fabbro", "given_name": "S.", "clpid": "Fabbro-S" }, { "family_name": "Fadeyev", "given_name": "V.", "clpid": "Fadeyev-V" }, { "family_name": "Fan", "given_name": "X.", "orcid": "0000-0003-3310-0131", "clpid": "Fan-Xiaohui" }, { "family_name": "Farris", "given_name": "B.", "clpid": "Farris-B" }, { "family_name": "Folatelli", "given_name": "G.", "clpid": "Folatelli-G" }, { "family_name": "Frye", "given_name": "B. L.", "clpid": "Frye-B-L" }, { "family_name": "Garavini", "given_name": "G.", "clpid": "Garavini-G" }, { "family_name": "Gates", "given_name": "E. L.", "orcid": "0000-0002-3739-0423", "clpid": "Gates-E-L" }, { "family_name": "Germany", "given_name": "L.", "clpid": "Germany-L" }, { "family_name": "Goldhaber", "given_name": "G.", "clpid": "Goldhaber-G" }, { "family_name": "Goldman", "given_name": "B.", "clpid": "Goldman-B" }, { "family_name": "Goobar", "given_name": "A.", "orcid": "0000-0002-4163-4996", "clpid": "Goobar-A" }, { "family_name": "Groom", "given_name": "D. E.", "clpid": "Groom-D-E" }, { "family_name": "Haissinski", "given_name": "J.", "clpid": "Haissinski-J" }, { "family_name": "Hardin", "given_name": "D.", "clpid": "Hardin-D" }, { "family_name": "Hook", "given_name": "I.", "orcid": "0000-0002-2960-978X", "clpid": "Hook-I-M" }, { "family_name": "Kent", "given_name": "S.", "clpid": "Kent-S" }, { "family_name": "Kim", "given_name": "A. G.", "clpid": "Kim-Alex-G" }, { "family_name": "Knop", "given_name": "R. A.", "clpid": "Knop-R-A" }, { "family_name": "Lidman", "given_name": "C.", "orcid": "0000-0003-1731-0497", "clpid": "Lidman-C" }, { "family_name": "Linder", "given_name": "E. V.", "clpid": "Linder-E-V" }, { "family_name": "Mendez", "given_name": "J.", "clpid": "Mendez-J" }, { "family_name": "Meyers", "given_name": "J.", "clpid": "Meyers-J" }, { "family_name": "Miller", "given_name": "G. J.", "clpid": "Miller-G-J" }, { "family_name": "Moniez", "given_name": "M.", "clpid": "Moniez-M" }, { "family_name": "Mour\u00e3o", "given_name": "A. M.", "clpid": "Mour\u00e3o-A-M" }, { "family_name": "Newberg", "given_name": "H.", "clpid": "Newberg-H" }, { "family_name": "Nobili", "given_name": "S.", "clpid": "Nobili-S" }, { "family_name": "Nugent", "given_name": "P. E.", "orcid": "0000-0002-3389-0586", "clpid": "Nugent-P-E" }, { "family_name": "Pain", "given_name": "R.", "clpid": "Pain-R" }, { "family_name": "Perdereau", "given_name": "O.", "clpid": "Perdereau-O" }, { "family_name": "Perlmutter", "given_name": "S.", "clpid": "Perlmutter-S" }, { "family_name": "Phillips", "given_name": "M. M.", "orcid": "0000-0003-2734-0796", "clpid": "Phillips-M-M" }, { "family_name": "Prasad", "given_name": "V.", "clpid": "Prasad-V" }, { "family_name": "Quimby", "given_name": "R.", "orcid": "0000-0001-9171-5236", "clpid": "Quimby-R-M" }, { "family_name": "Regnault", "given_name": "N.", "clpid": "Regnault-N" }, { "family_name": "Rich", "given_name": "J.", "clpid": "Rich-J" }, { "family_name": "Rubenstein", "given_name": "E. P.", "clpid": "Rubenstein-E-P" }, { "family_name": "Ruiz-Lapuente", "given_name": "P.", "clpid": "Ruiz-Lapuente-P" }, { "family_name": "Santos", "given_name": "F. D.", "clpid": "Santos-F-D" }, { "family_name": "Schaefer", "given_name": "B. E.", "clpid": "Schaefer-B-E" }, { "family_name": "Schommer", "given_name": "R. A.", "clpid": "Schommer-R-A" }, { "family_name": "Smith", "given_name": "R. C.", "clpid": "Smith-R-C" }, { "family_name": "Soderberg", "given_name": "A. M.", "clpid": "Soderberg-A-M" }, { "family_name": "Spadafora", "given_name": "A. L.", "clpid": "Spadafora-A-L" }, { "family_name": "Strolger", "given_name": "L. G.", "clpid": "Strolger-L-G" }, { "family_name": "Strovink", "given_name": "M.", "clpid": "Strovink-M" }, { "family_name": "Suntzeff", "given_name": "N. B.", "clpid": "Suntzeff-N-B" }, { "family_name": "Suzuki", "given_name": "N.", "clpid": "Suzuki-Naoyuki" }, { "family_name": "Thomas", "given_name": "R. C.", "clpid": "Thomas-R-C" }, { "family_name": "Walton", "given_name": "N. A.", "clpid": "Walton-N-A" }, { "family_name": "Wang", "given_name": "L.", "orcid": "0000-0002-9803-166X", "clpid": "Wang-L" }, { "family_name": "Wood-Vasey", "given_name": "W. M.", "clpid": "Wood-Vasey-W-M" }, { "family_name": "Yun", "given_name": "J. L.", "clpid": "Yun-J-L" } ], "abstract": "We present a new compilation of Type Ia supernovae (SNe Ia), a new data set of low-redshift nearby-Hubble-flow SNe, and new analysis procedures to work with these heterogeneous compilations. This \"Union\" compilation of 414 SNe Ia, which reduces to 307 SNe after selection cuts, includes the recent large samples of SNe Ia from the Supernova Legacy Survey and ESSENCE Survey, the older data sets, as well as the recently extended data set of distant supernovae observed with the Hubble Space Telescope (HST). A single, consistent, and blind analysis procedure is used for all the various SN Ia subsamples, and a new procedure is implemented that consistently weights the heterogeneous data sets and rejects outliers. We present the latest results from this Union compilation and discuss the cosmological constraints from this new compilation and its combination with other cosmological measurements (CMB and BAO). The constraint we obtain from supernovae on the dark energy density is \u03a9_\u039b = 0.713^(+0.027)_(\u22120.029)(stat)^(+ 0.036)_(\u22120.039)(sys), for a flat, \u039bCDM universe. Assuming a constant equation of state parameter, w, the combined constraints from SNe, BAO, and CMB give w = \u2212 0.969^(+ 0.059)_(\u22120.063)(stat)^(+ 0.063)_(\u22120.066)(sys) . While our results are consistent with a cosmological constant, we obtain only relatively weak constraints on a w that varies with redshift. In particular, the current SN data do not yet significantly constrain w at z > 1. With the addition of our new nearby Hubble-flow SNe Ia, these resulting cosmological constraints are currently the tightest available.", "doi": "10.1086/589937", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2008-10-20", "series_number": "2", "volume": "686", "issue": "2", "pages": "749-778" }, { "id": "authors:p8z1c-zdw23", "collection": "authors", "collection_id": "p8z1c-zdw23", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-151408802", "type": "article", "title": "SNLS spectroscopy: testing for evolution in type Ia supernovae", "author": [ { "family_name": "Bronder", "given_name": "T. J.", "clpid": "Bronder-T-J" }, { "family_name": "Hook", "given_name": "I. M.", "orcid": "0000-0002-2960-978X", "clpid": "Hook-I-M" }, { "family_name": "Astier", "given_name": "P.", "clpid": "Astier-P" }, { "family_name": "Balam", "given_name": "D.", "clpid": "Balam-D" }, { "family_name": "Balland", "given_name": "C.", "clpid": "Balland-C" }, { "family_name": "Basa", "given_name": "S.", "clpid": "Basa-S" }, { "family_name": "Carlberg", "given_name": "R. G.", "clpid": "Carlberg-R-G" }, { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Fouchez", "given_name": "D.", "clpid": "Fouchez-D" }, { "family_name": "Guy", "given_name": "J.", "clpid": "Guy-J" }, { "family_name": "Howell", "given_name": "D. A.", "orcid": "0000-0003-4253-656X", "clpid": "Howell-D-A" }, { "family_name": "Neill", "given_name": "J. D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" }, { "family_name": "Pain", "given_name": "R.", "clpid": "Pain-R" }, { "family_name": "Perrett", "given_name": "K.", "clpid": "Perrett-K-M" }, { "family_name": "Pritchet", "given_name": "C. J.", "clpid": "Pritchet-C-J" }, { "family_name": "Regnault", "given_name": "N.", "clpid": "Regnault-N" }, { "family_name": "Sullivan", "given_name": "M.", "orcid": "0000-0001-9053-4820", "clpid": "Sullivan-Mark" }, { "family_name": "Baumont", "given_name": "S.", "clpid": "Baumont-S" }, { "family_name": "Fabbro", "given_name": "S.", "clpid": "Fabbro-S" }, { "family_name": "Filliol", "given_name": "M.", "clpid": "Filliol-M" }, { "family_name": "Perlmutter", "given_name": "S.", "clpid": "Perlmutter-S" }, { "family_name": "Ripoche", "given_name": "P.", "clpid": "Ripoche-P" } ], "abstract": "Aims. We present a quantitative study of a new data set of high redshift Type Ia supernovae spectra, observed at the Gemini telescopes during the first 34 months of the Supernova Legacy Survey. During this time 123 supernovae candidates were observed, of which 87 have been identified as SNe Ia at a median redshift of z=0.720. Spectra from the entire second year of the survey and part of the third year (59 total SNe candidates with 46 confirmed SNe Ia) are published here for the first time. The spectroscopic measurements made on this data set are used determine if these distant SNe comprise a population similar to those observed locally. \n\nMethods. Rest-frame equivalent width and ejection velocity measurements are made on four spectroscopic features. Corresponding measurements are presented for a set of 167 spectra from 24 low-z SNe Ia from the literature. \n\nResults. We show that there exists a sample at high redshift with properties similar to nearby SNe. The high-z measurements are consistent with the range of measurements at low-z and no significant difference was found between the distributions of measurements at low and high redsift for three of the features. The fourth feature displays a possible difference that should be investigated further. Correlations between Type Ia SNe properties and host galaxy morphology were also found to be similar at low and high z, and within each host galaxy class we see no evidence for redshift-evolution in SN properties. A new correlation between SNe Ia peak magnitude and the equivalent width of SiII absorption is presented. Tests on a sub-set of the SNLS SNe demonstrates that this correlation reduces the scatter in SNe Ia luminosity distances in a manner consistent with the lightcurve shape-luminosity corrections that are used for Type Ia SNe cosmology. \n\nConclusions. We show that this new sample of SNLS SNe Ia has spectroscopic properties similar to nearby objects.", "doi": "10.1051/0004-6361:20077655", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2008-01", "series_number": "3", "volume": "477", "issue": "3", "pages": "717-734" }, { "id": "authors:8bns4-3mv73", "collection": "authors", "collection_id": "8bns4-3mv73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100419-103646871", "type": "article", "title": "The Peculiar Velocities of Local Type Ia Supernovae and Their Impact on Cosmology", "author": [ { "family_name": "Neill", "given_name": "James D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" }, { "family_name": "Hudson", "given_name": "Michael J.", "clpid": "Hudson-M-J" }, { "family_name": "Conley", "given_name": "Alex", "clpid": "Conley-A" } ], "abstract": "We quantify the effect of Type Ia supernova (SN Ia) peculiar velocities on the derivation of cosmological parameters. The published distant and local SNe Ia used for the Supernova Legacy Survey first-year cosmology report form the sample for this study. While previous work has assumed that the local SNe are at rest in the CMB frame (the no-flow assumption), we test this assumption by applying peculiar velocity corrections to the local SNe using three different flow models. The models are based on the IRAS PSCz galaxy redshift survey, have varying \u03b2 = \u03a9^(0.6)_m/b, and reproduce the Local Group motion in the CMB frame. These data sets are then fit for w, \u03a9_m, and \u03a9_\u039b using flatness or \u039bCDM and a BAO prior, and the \u03c7^2 statistic is used to examine the effect of the velocity corrections on the quality of the fits. The most favored model is the \u03b2 = 0.5 model, which produces a fit significantly better than the no-flow assumption, consistent with previous peculiar velocity studies. By comparing the no-flow assumption with the favored models, we derive the largest potential systematic error in w caused by ignoring peculiar velocities, \u0394w = +0.04. For \u03a9_\u039b the potential error is \u0394\u03a9_\u039b = -0.04, and for \u03a9_m the potential error is \u0394\u03a9_m < +0.01. The favored flow model (\u03b2 = 0.5) produces the following cosmological parameters: w = -1.08^(+0.09)_(-0.08), \u03a9_m = 0.27^(+0.02)_(-0.02) assuming a flat cosmology, and \u03a9_\u039b = 0.80^(0.08)_(-0.07) and \u03a9_m = 0.27^(+0.02)_(-0.02) for a w = -1 (\u039bCDM) cosmology.", "doi": "10.1086/518808", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2007-06-01", "series_number": "2", "volume": "661", "issue": "2", "pages": "L123-L126" } ]