[ { "id": "authors:481ec-8re78", "collection": "authors", "collection_id": "481ec-8re78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160205-102129138", "type": "article", "title": "A Mature Galaxy Cluster at z = 1.58 around the Radio Galaxy 7C 1753+6311", "author": [ { "family_name": "Cooke", "given_name": "E. A.", "orcid": "0000-0003-3843-8393", "clpid": "Cooke-E-A" }, { "family_name": "Hatch", "given_name": "N. A.", "clpid": "Hatch-N-A" }, { "family_name": "Stern", "given_name": "D.", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Rettura", "given_name": "A.", "orcid": "0000-0002-5615-256X", "clpid": "Rettura-A" }, { "family_name": "Brodwin", "given_name": "M.", "orcid": "0000-0002-4208-798X", "clpid": "Brodwin-M" }, { "family_name": "Galametz", "given_name": "A.", "orcid": "0000-0002-1504-8117", "clpid": "Galametz-A" }, { "family_name": "Wylezalek", "given_name": "D.", "orcid": "0000-0003-2212-6045", "clpid": "Wylezalek-D" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Conselice", "given_name": "C. J.", "orcid": "0000-0003-1949-7638", "clpid": "Conselice-C-J" }, { "family_name": "de Breuck", "given_name": "C.", "orcid": "0000-0002-6637-3315", "clpid": "de-Breuck-Carlos" }, { "family_name": "Gonzalez", "given_name": "A. H.", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-A-H" }, { "family_name": "Jarvis", "given_name": "M.", "orcid": "0000-0001-7039-9078", "clpid": "Jarvis-M-J" } ], "abstract": "We report on the discovery of a z = 1.58 mature cluster around the high-redshift radio galaxy 7C 1753+6311, first identified in the Clusters Around Radio-loud active galactic nuclei survey. Two-thirds of the excess galaxies within the central 1 Mpc lie on a red sequence with a color that is consistent with an average formation redshift of z_f ~ 3. We show that 80 \u00b1 6% of the red sequence galaxies in the cluster core are quiescent, while the remaining 20% are red due to dusty star formation. We demonstrate that the cluster has an enhanced quiescent galaxy fraction that is three times that of the control field. We also show that this enhancement is mass dependent: 91 \u00b1 9% of the M_* > 10^(10.5) M_\u2299 cluster galaxies are quiescent, compared to only 36 \u00b1 2% of field galaxies, whereas the fraction of quiescent galaxies with lower masses is the same in the cluster and field environments. The presence of a dense core and a well-formed, quiescent red sequence suggest that this is a mature cluster. This means that distant radio galaxies do not solely reside in young, uncollapsed protoclusters, rather they can be found in clusters in a wide range of evolutionary states.", "doi": "10.3847/0004-637X/816/2/83", "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. 83" }, { "id": "authors:4tthm-4qd56", "collection": "authors", "collection_id": "4tthm-4qd56", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151218-121638912", "type": "article", "title": "Radio Jet Feedback and Star Formation in Heavily Obscured, Hyperluminous Quasars at Redshifts ~ 0.5\u20133. I. ALMA Observations", "author": [ { "family_name": "Lonsdale", "given_name": "Carol J.", "orcid": "0000-0003-0898-406X", "clpid": "Lonsdale-Carol-J" }, { "family_name": "Lacy", "given_name": "M.", "orcid": "0000-0002-3032-1783", "clpid": "Lacy-M" }, { "family_name": "Kimball", "given_name": "A. E.", "clpid": "Kimball-A-E" }, { "family_name": "Blain", "given_name": "A.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Whittle", "given_name": "M.", "clpid": "Whittle-M" }, { "family_name": "Wilkes", "given_name": "B.", "orcid": "0000-0003-1809-2364", "clpid": "Wilkes-B-J" }, { "family_name": "Stern", "given_name": "D.", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Condon", "given_name": "J.", "orcid": "0000-0003-4724-1939", "clpid": "Condon-J-J" }, { "family_name": "Kim", "given_name": "M.", "clpid": "Kim-M" }, { "family_name": "Assef", "given_name": "R. J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Tsai", "given_name": "C.-W.", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Efstathiou", "given_name": "A.", "orcid": "0000-0002-2612-4840", "clpid": "Efstathiou-Andreas" }, { "family_name": "Jones", "given_name": "S.", "clpid": "Jones-S" }, { "family_name": "Eisenhardt", "given_name": "P.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Wu", "given_name": "J.", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Lonsdale", "given_name": "Colin J.", "orcid": "0000-0003-4062-4654", "clpid": "Lonsdale-Colin-J" }, { "family_name": "Jones", "given_name": "K.", "clpid": "Jones-K" }, { "family_name": "Jarrett", "given_name": "T.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Smith", "given_name": "R.", "clpid": "Smith-R" } ], "abstract": "We present Atacama Large Millimeter/submillimeter Array (ALMA) 870 \u03bcm (345 GHz) data for 49 high-redshift (0.47 < z < 2.85), luminous 11.7 < log (L_(bol/L_\u2299) < 14.2) radio-powerful active galactic nuclei (AGNs), obtained to constrain cool dust emission from starbursts concurrent with highly obscured radiative-mode black hole (BH) accretion in massive galaxies that possess a small radio jet. The sample was selected from the Wide-field Infrared Survey Explorer with extremely steep (red) mid-infrared colors and with compact radio emission from NVSS/FIRST. Twenty-six sources are detected at 870 \u03bcm, and we find that the sample has large mid- to far-infrared luminosity ratios, consistent with a dominant and highly obscured quasar. The rest-frame 3 GHz radio powers are 24.7 < log (P_(3.0 GHz)/W Hz^(-1)) and all sources are radio-intermediate or radio-loud. BH mass estimates are 7.7 < log(M_(BH)/M_\u2299) < 10.2. The rest-frame 1\u20135 \u03bcm spectral energy distributions are very similar to the \"Hot DOGs\" (hot dust-obscured galaxies), and steeper (redder) than almost any other known extragalactic sources. ISM masses estimated for the ALMA-detected sources are 9.9 < log (M_(ISM)/M_\u2299) < 11.75 assuming a dust temperature of 30 K. The cool dust emission is consistent with star formation rates reaching several thousand M_\u2299 yr^(\u22121), depending on the assumed dust temperature, but we cannot rule out the alternative that the AGN powers all the emission in some cases. Our best constrained source has radiative transfer solutions with approximately equal contributions from an obscured AGN and a young (10\u201315 Myr) compact starburst.", "doi": "10.1088/0004-637X/813/1/45", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-11-01", "series_number": "1", "volume": "813", "issue": "1", "pages": "Art. No. 45" }, { "id": "authors:0ef20-g4n92", "collection": "authors", "collection_id": "0ef20-g4n92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150722-104921866", "type": "article", "title": "The Most Luminous Galaxies Discovered by WISE", "author": [ { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Sayers", "given_name": "Jack", "orcid": "0000-0002-8213-3784", "clpid": "Sayers-Jack" }, { "family_name": "Cutri", "given_name": "Roc M.", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" }, { "family_name": "Masci", "given_name": "Frank J.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-F-J" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" }, { "family_name": "Gelino", "given_name": "Christopher R.", "clpid": "Gelino-C-R" }, { "family_name": "Beichman", "given_name": "Charles A.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" } ], "abstract": "

We present 20 Wide-field Infrared Survey Explorer (WISE)-selected galaxies with bolometric luminosities Lbol > 1014 L\u2609, including five with infrared luminosities LIR ≡ L(rest 8–1000 μm) > 1014 L\u2609. These \"extremely luminous infrared galaxies,\" or ELIRGs, were discovered using the \"W1W2-dropout\" selection criteria which requires marginal or non-detections at 3.4 and 4.6 μm (W1 and W2, respectively) but strong detections at 12 and 22 μm in the WISE survey. Their spectral energy distributions are dominated by emission at rest-frame 4–10 μm, suggesting that hot dust with Td ∼ 450 K is responsible for the high luminosities. These galaxies are likely powered by highly obscured active galactic nuclei (AGNs), and there is no evidence suggesting these systems are beamed or lensed. We compare this WISE-selected sample with 116 optically selected quasars that reach the same Lbol level, corresponding to the most luminous unobscured quasars in the literature. We find that the rest-frame 5.8 and 7.8 μm luminosities of the WISE-selected ELIRGs can be 30%–80% higher than that of the unobscured quasars. The existence of AGNs with Lbol > 1014 L\u2609 at z > 3 suggests that these supermassive black holes are born with large mass, or have very rapid mass assembly. For black hole seed masses ∼103 M\u2609, either sustained super-Eddington accretion is needed, or the radiative efficiency must be <15%, implying a black hole with slow spin, possibly due to chaotic accretion.

", "doi": "10.1088/0004-637X/805/2/90", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-06-01", "series_number": "2", "volume": "805", "issue": "2", "pages": "Art. No. 90" }, { "id": "authors:3svcb-n5a73", "collection": "authors", "collection_id": "3svcb-n5a73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150608-072844799", "type": "article", "title": "Half of the Most Luminous Quasars May Be Obscured: Investigating the Nature of WISE-Selected Hot Dust-Obscured Galaxies", "author": [ { "family_name": "Assef", "given_name": "R. J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Einsenhardt", "given_name": "P. R. M.", "clpid": "Einsenhardt-P-R-M" }, { "family_name": "Stern", "given_name": "D.", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Tsai", "given_name": "C.-W.", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Wu", "given_name": "J.", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Wylezalek", "given_name": "D.", "orcid": "0000-0003-2212-6045", "clpid": "Wylezalek-D" }, { "family_name": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Donoso", "given_name": "E.", "clpid": "Donoso-E" }, { "family_name": "Gonzales", "given_name": "A.", "clpid": "Gonzales-A" }, { "family_name": "Griffith", "given_name": "R. L.", "clpid": "Griffith-R-L" }, { "family_name": "Jarrett", "given_name": "T. H.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" } ], "abstract": "The Wide-field Infrared Survey Explorer mission has unveiled a rare population of high-redshift (z = 1\u20134.6), dusty, hyper-luminous galaxies, with infrared luminosities L_(IR) > 10^(13)L_\u2609, and sometimes exceeding 10^(14)L_\u2609. Previous work has shown that their dust temperatures and overall far-infrared spectral energy distributions (SEDs) are significantly hotter than expected to be powered by star formation. We present here an analysis of the rest-frame optical through mid-infrared SEDs for a large sample of these so-called \"hot, dust-obscured galaxies\" (Hot DOGs). We find that the SEDs of Hot DOGs are generally well modeled by the combination of a luminous, yet obscured active galactic nuclei (AGNs) that dominates the rest-frame emission at \u03bb > 1 \u00b5m and the bolometric luminosity output, and a less luminous host galaxy that is responsible for the bulk of the rest optical/UV emission. Even though the stellar mass of the host galaxies may be as large as 10^(11)\u201310^(12) M_\u2299, the AGN emission, with a range of luminosities comparable to those of the most luminous QSOs known, require that either Hot DOGs have black hole masses significantly in excess of the local relations, or that they radiate significantly above the Eddington limit, at a level at least 10 times more efficiently than z ~ 2 QSOs. We show that, while rare, the number density of Hot DOGs is comparable to that of equally luminous but unobscured (i.e., Type 1) QSOs. This may be at odds with the trend suggested at lower luminosities for the fraction of obscured AGNs to decrease with increasing luminosity. That trend may, instead, reverse at higher luminosities. Alternatively, Hot DOGs may not be the torus-obscured counterparts of the known optically selected, largely unobscured, hyper-luminous QSOs, and may represent a new component of the galaxy evolution paradigm. Finally, we discuss the environments of Hot DOGs and statistically show that these objects are in regions as dense as those of known high-redshift proto-clusters.", "doi": "10.1088/0004-637X/804/1/27", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-05-01", "series_number": "1", "volume": "804", "issue": "1", "pages": "Art. No. 27" }, { "id": "authors:bdv16-5nt36", "collection": "authors", "collection_id": "bdv16-5nt36", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150311-182729941", "type": "article", "title": "A Deep Hubble Space Telescope and Keck Search for Definitive Identification of Lyman Continuum Emitters at z ~ 3.1", "author": [ { "family_name": "Siana", "given_name": "Brian", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Shapley", "given_name": "Alice E.", "orcid": "0000-0003-3509-4855", "clpid": "Shapley-A-E" }, { "family_name": "Kulas", "given_name": "Kristin R.", "clpid": "Kulas-K-R" }, { "family_name": "Nestor", "given_name": "Daniel B.", "clpid": "Nestor-D-B" }, { "family_name": "Steidel", "given_name": "Charles C.", "orcid": "0000-0002-4834-7260", "clpid": "Steidel-C-C" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Alavi", "given_name": "Anahita", "orcid": "0000-0002-8630-6435", "clpid": "Alavi-A" }, { "family_name": "Brown", "given_name": "Thomas M.", "orcid": "0000-0002-1793-9968", "clpid": "Brown-T-M" }, { "family_name": "Conselice", "given_name": "Christopher J.", "orcid": "0000-0003-1949-7638", "clpid": "Conselice-C-J" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Dickinson", "given_name": "Mark", "orcid": "0000-0001-5414-5131", "clpid": "Dickinson-Mark-E" }, { "family_name": "Giavalisco", "given_name": "Mauro", "orcid": "0000-0002-7831-8751", "clpid": "Giavalisco-M" }, { "family_name": "Colbert", "given_name": "James W.", "clpid": "Colbert-J-W" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Gardner", "given_name": "Jonathan P.", "clpid": "Gardner-J-P" }, { "family_name": "de Mello", "given_name": "Duilia F.", "clpid": "de-Mello-D-F" } ], "abstract": "Narrowband imaging of the rest-frame Lyman continuum (LyC) of galaxies at z ~ 3.1 has produced a large number of candidate LyC-emitting galaxies. These samples are contaminated by galaxies at lower redshift. To better understand LyC escape, we need an uncontaminated sample of galaxies that emit strongly in the LyC. Here we present deep Hubble Space Telescope imaging of five bright galaxies at z ~ 3.1 that had previously been identified as candidate LyC emitters with ground-based images. The WFC3 F336W images probe the LyC of galaxies at z > 3.06 and provide an order-of-magnitude increase in spatial resolution over ground-based imaging. The non-ionizing UV images often show multiple galaxies (or components) within ~ 1\" of the candidate LyC emission seen from the ground. In each case, only one of the components is emitting light in the F336W filter, which would indicate LyC escape if that component is at z > 3.06. We use Keck/NIRSPEC near-IR spectroscopy to measure redshifts of these components to distinguish LyC emitters from foreground contamination. We find that two candidates are low-redshift contaminants, one candidate had a previously misidentified redshift, and the other two cannot be confirmed as LyC emitters. The level of contamination is consistent with previous estimates. For the galaxies with z > 3.06, we derive strong l\u03c3 limits on the relative escape fraction between 0.07 and 0.09. We still do not have a sample of definitive LyC emitters, and a much larger study of low-luminosity galaxies is required. The combination of high-resolution imaging and deep spectroscopy is critical for distinguishing LyC emitters from foreground contaminants.", "doi": "10.1088/0004-637X/804/1/17", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-05-01", "series_number": "1", "volume": "804", "issue": "1", "pages": "Art. No. 17" }, { "id": "authors:m1dtb-k6x32", "collection": "authors", "collection_id": "m1dtb-k6x32", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150424-145449611", "type": "article", "title": "Submillimetre observations of WISE/radio-selected AGN and their environments", "author": [ { "family_name": "Jones", "given_name": "Suzy F.", "clpid": "Jones-Suzy-F" }, { "family_name": "Blain", "given_name": "Andrew W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Lonsdale", "given_name": "Carol", "orcid": "0000-0003-0898-406X", "clpid": "Lonsdale-C-J" }, { "family_name": "Condon", "given_name": "James", "orcid": "0000-0003-4724-1939", "clpid": "Condon-J-J" }, { "family_name": "Farrah", "given_name": "Duncan", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Assef", "given_name": "Roberto J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Kimball", "given_name": "Amy", "clpid": "Kimball-A" }, { "family_name": "Lacy", "given_name": "Mark", "orcid": "0000-0002-3032-1783", "clpid": "Lacy-M" }, { "family_name": "Eisenhardt", "given_name": "Peter", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Jarrett", "given_name": "Tom", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" } ], "abstract": "We present JCMT SCUBA-2 850 \u03bcm submillimetre (submm) observations of 30 mid-infrared (mid-IR) luminous active galactic nuclei (AGNs), detected jointly by the Wide-field Infrared Survey Explorer (WISE) all-sky IR survey and the NVSS/FIRST radio survey. These rare sources are selected by their extremely red mid-IR spectral energy distributions (SEDs) and compact radio counterparts. Further investigations show that they are highly obscured, have abundant warm AGN-heated dust and are thought to be experiencing intense AGN feedback. These galaxies appear to be consistent with a later AGN-dominated phase of merging galaxies, while hot, dust-obscured galaxies are an earlier starburst-dominated phase. When comparing the number of submm galaxies detected serendipitously in the surrounding 1.5 arcmin to those in blank-field submm surveys, there is a very significant overdensity, of order 5, but no sign of radial clustering centred at our primary objects. The WISE/radio-selected AGN thus reside in 10-Mpc-scale overdense environments that could be forming in pre-viralized clusters of galaxies. WISE/radio-selected AGNs appear to be the strongest signposts of high-density regions of active, luminous and dusty galaxies. SCUBA-2 850 \u03bcm observations indicate that their submm fluxes are low compared to many popular AGN SED templates, hence the WISE/radio-selected AGNs have either less cold and/or more warm dust emission than normally assumed for typical AGN. Most of the targets are not detected, only four targets are detected at SCUBA-2 850 \u03bcm, and have total IR luminosities \u226510^(13) L\u2299, if their redshifts are consistent with the subset of the 10 SCUBA-2 undetected targets with known redshifts, z \u223c 0.44\u20132.86.", "doi": "10.1093/mnras/stv214", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2015-04-21", "series_number": "4", "volume": "448", "issue": "4", "pages": "3325-3338" }, { "id": "authors:kxckt-c4055", "collection": "authors", "collection_id": "kxckt-c4055", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141209-153059756", "type": "article", "title": "The FUV to Near-IR Morphologies of Luminous Infrared Galaxies in the Goals Sample", "author": [ { "family_name": "Petty", "given_name": "S. M.", "clpid": "Petty-S-M" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Charmandaris", "given_name": "V.", "orcid": "0000-0002-2688-1956", "clpid": "Charmandaris-V" }, { "family_name": "Evans", "given_name": "A. S.", "orcid": "0000-0003-2638-1334", "clpid": "Evans-A-S" }, { "family_name": "Le Floc'h", "given_name": "E.", "clpid": "Le-Floc'h-Emeric" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "D\u00edaz-Santos", "given_name": "T.", "orcid": "0000-0003-0699-6083", "clpid": "D\u00edaz-Santos-T" }, { "family_name": "Howell", "given_name": "J. H.", "clpid": "Howell-J-H" }, { "family_name": "Inami", "given_name": "H.", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" }, { "family_name": "Psychogyios", "given_name": "A.", "clpid": "Psychogyios-A" }, { "family_name": "Stierwalt", "given_name": "S.", "orcid": "0000-0002-2596-8531", "clpid": "Stierwalt-S" }, { "family_name": "Surace", "given_name": "J. A.", "orcid": "0000-0001-7291-0087", "clpid": "Surace-J-A" } ], "abstract": "We compare the morphologies of a sample of 20 luminous infrared galaxies (LIRGs) from the Great Observatories All-sky LIRG Survey (GOALS) in the FUV, B, I, and H bands, using the Gini (G) and M_(20) parameters to quantitatively estimate the distribution and concentration of flux as a function of wavelength. Hubble Space Telescope (HST) images provide an average spatial resolution of ~80pc. While our LIRGs can be reliably classified as mergers across the entire range of wavelengths studied here, there is a clear shift toward more negative M_(20) (more bulge-dominated) and a less significant decrease in G values at longer wavelengths. We find no correlation between the derived FUV G-M_(20) parameters and the global measures of the IR to FUV flux ratio (IRX). Given the fine resolution in our HST data, this suggests either that the UV morphology and IRX are correlated on very small scales, or that the regions emitting the bulk of the IR emission emit almost no FUV light. We use our multi-wavelength data to simulate how merging LIRGs would appear from z~0.5\u20133 in deep optical and near-infrared images such as the Hubble Ultra-Deep Field, and use these simulations to measure the G-M_(20) at these redshifts. Our simulations indicate a noticeable decrease in G, which flattens at z \u2265 2 by as much as 40%, resulting in mis-classifying our LIRGs as disk-like, even in the rest-frame FUV. The higher redshift values of M_(20) for the GOALS sources do not appear to change more than about 10% from the values at $z\\sim 0$. The change in G-M_(20) is caused by the surface brightness dimming of extended tidal features and asymmetries, and also the decreased spatial resolution which reduced the number of individual clumps identified. This effect, seen as early as z~0.5, could easily lead to an underestimate of the number of merging galaxies at high-redshift in the rest-frame FUV.", "doi": "10.1088/0004-6256/148/6/111", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2014-12", "series_number": "6", "volume": "148", "issue": "6", "pages": "Art. No. 111" }, { "id": "authors:62afg-gk992", "collection": "authors", "collection_id": "62afg-gk992", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160824-144504856", "type": "article", "title": "NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-selected Quasars at z ~ 2", "author": [ { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Lansbury", "given_name": "G. B.", "orcid": "0000-0002-5328-9827", "clpid": "Lansbury-G-B" }, { "family_name": "Assef", "given_name": "R. J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Brandt", "given_name": "W. N.", "orcid": "0000-0002-0167-2453", "clpid": "Brandt-W-N" }, { "family_name": "Alexander", "given_name": "D. M.", "orcid": "0000-0002-5896-6313", "clpid": "Alexander-D-M" }, { "family_name": "Ballantyne", "given_name": "D. R.", "orcid": "0000-0001-8128-6976", "clpid": "Ballantyne-D-R" }, { "family_name": "Balokovi\u0107", "given_name": "M.", "orcid": "0000-0003-0476-6647", "clpid": "Balokovi\u0107-M" }, { "family_name": "Bauer", "given_name": "F. E.", "orcid": "0000-0002-8686-8737", "clpid": "Bauer-F-E" }, { "family_name": "Benford", "given_name": "D. J.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Blain", "given_name": "A.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Boggs", "given_name": "S. E.", "orcid": "0000-0001-9567-4224", "clpid": "Boggs-S-E" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Brightman", "given_name": "M.", "orcid": "0000-0002-8147-2602", "clpid": "Brightman-M" }, { "family_name": "Christensen", "given_name": "F. E.", "orcid": "0000-0001-5679-1946", "clpid": "Christensen-F-E" }, { "family_name": "Comastri", "given_name": "Andrea", "orcid": "0000-0003-3451-9970", "clpid": "Comastri-A" }, { "family_name": "Craig", "given_name": "William W.", "clpid": "Craig-W-W" }, { "family_name": "Del Moro", "given_name": "A.", "clpid": "Del-Moro-A" }, { "family_name": "Eisenhardt", "given_name": "Peter R. M.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Gandhi", "given_name": "P.", "orcid": "0000-0003-3105-2615", "clpid": "Gandhi-Poshak" }, { "family_name": "Griffith", "given_name": "R. L.", "clpid": "Griffith-R-L" }, { "family_name": "Hailey", "given_name": "C. J.", "clpid": "Hailey-C-J" }, { "family_name": "Harrison", "given_name": "F. A.", "orcid": "0000-0002-4226-8959", "clpid": "Harrison-F-A" }, { "family_name": "Hickox", "given_name": "R. C.", "orcid": "0000-0003-1468-9526", "clpid": "Hickox-R-C" }, { "family_name": "Jarrett", "given_name": "T. H.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Koss", "given_name": "M.", "orcid": "0000-0002-7998-9581", "clpid": "Koss-M-J" }, { "family_name": "Lake", "given_name": "S.", "clpid": "Lake-S-E" }, { "family_name": "LaMassa", "given_name": "S. M.", "orcid": "0000-0002-5907-3330", "clpid": "LaMassa-S-M" }, { "family_name": "Luo", "given_name": "B.", "orcid": "0000-0002-9036-0063", "clpid": "Luo-Bin" }, { "family_name": "Tsai", "given_name": "C. W.", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Urry", "given_name": "C. M.", "orcid": "0000-0002-0745-9792", "clpid": "Urry-C-M" }, { "family_name": "Walton", "given_name": "D. J.", "orcid": "0000-0001-5819-3552", "clpid": "Walton-D-J" }, { "family_name": "Wright", "given_name": "D. J.", "clpid": "Wright-D-J" }, { "family_name": "Wu", "given_name": "J.", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Yan", "given_name": "L.", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" }, { "family_name": "Zhang", "given_name": "W. W.", "orcid": "0000-0002-1426-9698", "clpid": "Zhang-W-W" } ], "abstract": "We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected active galactic nuclei (AGNs) at z ~ 2 across a broad X-ray band (0.1 - 79 keV). The parent sample, selected to be faint or undetected in the WISE 3.4 \u03bcm (W1) and 4.6 \u03bcm (W2) bands but bright at 12 \u03bcm (W3) and 22 \u03bcm (W4), are extremely rare, with only ~1000 so-called \"W1W2-dropouts\" across the extragalactic sky. Optical spectroscopy reveals typical redshifts of z ~ 2 for this population, implying rest-frame mid-IR luminosities of \u03bdL \u03bd(6 \u03bcm) ~ 6 \u00d7 1046 erg s^-1 and bolometric luminosities that can exceed L bol ~ 1014 L_\u2299. The corresponding intrinsic, unobscured hard X-ray luminosities are L(2-10 keV) ~ 4 \u00d7 1045 erg s-1 for typical quasar templates. These are among the most AGNs known, though the optical spectra rarely show evidence of a broad-line region and the selection criteria imply heavy obscuration even at rest-frame 1.5 \u03bcm. We designed our X-ray observations to obtain robust detections for gas column densities N H <= 1024 cm-2. In fact, the sources prove to be fainter than these predictions. Two of the sources were observed by both NuSTAR and XMM-Newton, with neither being detected by NuSTAR (f 3-24 keV <~ 10-13 erg cm^(-2)s^(-1), and one being faintly detected by XMM-Newton (f 0.5-10 keV ~ 5 \u00d7 10-15 erg cm-2 s-1). A third source was observed only with XMM-Newton, yielding a faint detection (f 0.5-10 keV ~ 7 \u00d7 10-15 erg cm-2 s-1). The X-ray data imply these sources are either X-ray weak, or are heavily obscured by column densities N H >~ 1024 cm-2. The combined X-ray and mid-IR analysis seems to favor this second possibility, implying the sources are extremely obscured, consistent with Compton-thick, luminous quasars. The discovery of a significant population of heavily obscured, extremely luminous AGNs would not conform to the standard paradigm of a receding torus, in which more luminous quasars are less likely to be obscured, and instead suggests that an additional source of obscuration is present in these extreme sources.", "doi": "10.1088/0004-637X/794/2/102", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2014-10", "series_number": "2", "volume": "79", "issue": "2", "pages": "Art No.102" }, { "id": "authors:s2vze-efp27", "collection": "authors", "collection_id": "s2vze-efp27", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141002-141208452", "type": "article", "title": "Interferometric Follow-up of WISE Hyper-luminous Hot, Dust-obscured Galaxies", "author": [ { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Bussmann", "given_name": "R. Shane", "clpid": "Bussmann-R-S" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Petric", "given_name": "Andreea", "orcid": "0000-0003-4030-3455", "clpid": "Petric-A-O" }, { "family_name": "Blain", "given_name": "Andrew", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Eisenhardt", "given_name": "Peter R. M.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Benford", "given_name": "Dominic J.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Assef", "given_name": "Roberto J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Gelino", "given_name": "Christopher R.", "clpid": "Gelino-C-R" }, { "family_name": "Moustakas", "given_name": "Leonidas", "orcid": "0000-0003-3030-2360", "clpid": "Moustakas-L-A" }, { "family_name": "Wright", "given_name": "Edward L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" } ], "abstract": "The Wide-field Infrared Survey Explorer (WISE) has discovered an extraordinary population of hyper-luminous dusty galaxies that are faint in the two bluer passbands (3.4 \u03bcm and 4.6 \u03bcm) but are bright in the two redder passbands of WISE (12 \u03bcm and 22 \u03bcm). We report on initial follow-up observations of three of these hot, dust-obscured galaxies, or Hot DOGs, using the Combined Array for Research in Millimeter-wave Astronomy and the Submillimeter Array interferometer arrays at submillimeter/millimeter wavelengths. We report continuum detections at ~1.3 mm of two sources (WISE J014946.17+235014.5 and WISE J223810.20+265319.7, hereafter W0149+2350 and W2238+2653, respectively), and upper limits to CO line emission at 3 mm in the observed frame for two sources (W0149+2350 and WISE J181417.29+341224.8, hereafter W1814+3412). The 1.3 mm continuum images have a resolution of 1\"-2\" and are consistent with single point sources. We estimate the masses of cold dust are 2.0 \u00d7 10^8 M_\u2609 for W0149+2350 and 3.9 \u00d7 10^8 M_\u2609 for W2238+2653, comparable to cold dust masses of luminous quasars. We obtain 2\u03c3 upper limits to the molecular gas masses traced by CO, which are 3.3 \u00d7 10^(10) M_\u2609 and 2.3 \u00d7 10^(10) M_\u2609 for W0149+2350 and W1814+3412, respectively. We also present high-resolution, near-IR imaging with the WFC3 on the Hubble Space Telescope for W0149+2653 and with NIRC2 on Keck for W2238+2653. The near-IR images show morphological structure dominated by a single, centrally condensed source with effective radius less than 4 kpc. No signs of gravitational lensing are evident.", "doi": "10.1088/0004-637X/793/1/8", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2014-09-20", "series_number": "1", "volume": "793", "issue": "1", "pages": "Art. No. 8" }, { "id": "authors:cmqtc-pgz41", "collection": "authors", "collection_id": "cmqtc-pgz41", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140904-152428097", "type": "article", "title": "Submillimetre observations of WISE-selected high-redshift, luminous, dusty galaxies", "author": [ { "family_name": "Jones", "given_name": "Suzy F.", "clpid": "Jones-S-F" }, { "family_name": "Blain", "given_name": "Andrew W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Assef", "given_name": "Roberto J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Eisenhardt", "given_name": "Peter", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Petty", "given_name": "Sara", "clpid": "Petty-S" }, { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Cutri", "given_name": "Roc", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" }, { "family_name": "Wright", "given_name": "Edward L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "We present SCUBA-2 (Submillimetre Common-User Bolometer Array) 850\u2009\u03bcm submillimetre (submm) observations of the fields of 10 dusty, luminous galaxies at z \u223c 1.7\u20134.6, detected at 12 and/or 22\u2009\u03bcm by the Wide-field Infrared Survey Explorer (WISE) all-sky survey, but faint or undetected at 3.4 and 4.6\u2009\u03bcm; dubbed hot, dust-obscured galaxies (Hot DOGs). The six detected targets all have total infrared luminosities greater than 10^(13)\u2009L_\u2299, with one greater than 10^(14)\u2009L_\u2299. Their spectral energy distributions (SEDs) are very blue from mid-infrared to submm wavelengths and not well fitted by standard active galactic nuclei (AGN) SED templates, without adding extra dust extinction to fit the WISE 3.4 and 4.6\u2009\u03bcm data. The SCUBA-2 850\u2009\u03bcm observations confirm that the Hot DOGs have less cold and/or more warm dust emission than standard AGN templates, and limit an underlying extended spiral or ULIRG-type galaxy to contribute less than about 2 or 55\u2009per\u2009cent of the typical total Hot DOG IR luminosity, respectively. The two most distant and luminous targets have similar observed submm to mid-infrared ratios to the rest, and thus appear to have even hotter SEDs. The number of serendipitous submm galaxies detected in the 1.5-arcmin-radius SCUBA-2 850\u2009\u03bcm maps indicates there is a significant overdensity of serendipitous sources around Hot DOGs. These submm observations confirm that the WISE-selected ultraluminous galaxies have very blue mid-infrared to submm SEDs, suggesting that they contain very powerful AGN, and are apparently located in unusual arcmin-scale overdensities of very luminous dusty galaxies.", "doi": "10.1093/mnras/stu1157", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2014-09-01", "series_number": "1", "volume": "443", "issue": "1", "pages": "146-157" }, { "id": "authors:pnkas-cn822", "collection": "authors", "collection_id": "pnkas-cn822", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-100322157", "type": "article", "title": "HST/WFC3 Near-Infrared spectroscopy of quenched galaxies at z ~ 1.5 from the WISP Survey: Stellar population properties", "author": [ { "family_name": "Bedregal", "given_name": "A. G.", "clpid": "Bedregal-A-G" }, { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Henry", "given_name": "A. L.", "orcid": "0000-0002-6586-4446", "clpid": "Henry-A-L" }, { "family_name": "Atek", "given_name": "H.", "orcid": "0000-0002-7570-0824", "clpid": "Atek-H" }, { "family_name": "Rafelski", "given_name": "M.", "orcid": "0000-0002-9946-4731", "clpid": "Rafelski-M" }, { "family_name": "Teplitz", "given_name": "H. I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Dominguez", "given_name": "A.", "clpid": "Dominguez-A" }, { "family_name": "Siana", "given_name": "Brian", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Colbert", "given_name": "J. W.", "clpid": "Colbert-J-W" }, { "family_name": "Malkan", "given_name": "M.", "orcid": "0000-0001-6919-1237", "clpid": "Malkan-M-A" }, { "family_name": "Ross", "given_name": "N. R.", "clpid": "Ross-N-R" }, { "family_name": "Martin", "given_name": "C. L.", "clpid": "Martin-C-L" }, { "family_name": "Dressler", "given_name": "A.", "clpid": "Dressler-A" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Hathi", "given_name": "N. P.", "orcid": "0000-0001-6145-5090", "clpid": "Hathi-N-P" }, { "family_name": "Masters", "given_name": "D.", "orcid": "0000-0001-5382-6138", "clpid": "Masters-D-C" }, { "family_name": "McCarthy", "given_name": "P. J.", "clpid": "McCarthy-P-J" }, { "family_name": "Rutkowski", "given_name": "M. J.", "clpid": "Rutkowski-M-J" } ], "abstract": "We combine Hubble Space Telescope (HST) G102 and G141 near-IR (NIR) grism spectroscopy with HST/WFC3-UVIS, HST/WFC3-IR, and Spitzer/IRAC [3.6 \u03bcm] photometry to assemble a sample of massive (log (M_(star)/M_\u2609) ~ 11.0) and quenched (specific star formation rate <0.01 Gyr^(\u20131)) galaxies at z ~ 1.5. Our sample of 41 galaxies is the largest with G102+G141 NIR spectroscopy for quenched sources at these redshifts. In contrast to the local universe, z ~ 1.5 quenched galaxies in the high-mass range have a wide range of stellar population properties. We find that their spectral energy distributions (SEDs) are well fitted with exponentially decreasing star formation histories and short star formation timescales (\u03c4 \u2264 100 Myr). Quenched galaxies also show a wide distribution in ages, between 1 and 4 Gyr. In the (u \u2013 r)_0-versus-mass space quenched galaxies have a large spread in rest-frame color at a given mass. Most quenched galaxies populate the z ~ 1.5 red sequence (RS), but an important fraction of them (32%) have substantially bluer colors. Although with a large spread, we find that the quenched galaxies on the RS have older median ages (3.1 Gyr) than the quenched galaxies off the RS (1.5 Gyr). We also show that a rejuvenated SED cannot reproduce the observed stacked spectra of (the bluer) quenched galaxies off the RS. We derive the upper limit on the fraction of massive galaxies on the RS at z ~ 1.5 to be <43%. We speculate that the young quenched galaxies off the RS are in a transition phase between vigorous star formation at z > 2 and the z ~ 1.5 RS. According to their estimated ages, the time required for quenched galaxies off the RS to join their counterparts on the z ~ 1.5 RS is of the order of ~1 Gyr.", "doi": "10.1088/0004-637X/778/2/126", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-12-01", "series_number": "2", "volume": "778", "issue": "2", "pages": "Art. No. 126" }, { "id": "authors:y5kxj-g4897", "collection": "authors", "collection_id": "y5kxj-g4897", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-094902432", "type": "article", "title": "WISE detections of known QSOs at redshifts greater than six", "author": [ { "family_name": "Blain", "given_name": "Andrew W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Assef", "given_name": "Roberto", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Eisenhardt", "given_name": "Peter", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Benford", "given_name": "Dominic", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Jarrett", "given_name": "Tom", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Cutri", "given_name": "Roc", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" }, { "family_name": "Petty", "given_name": "Sara", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Wright", "given_name": "Edward L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" } ], "abstract": "We present WISE All-Sky mid-infrared (IR) survey detections of 55% (17/31) of the known QSOs at z > 6 from a range of surveys: the SDSS, the CFHT-LS, FIRST, Spitzer, and UKIDSS. The WISE catalog thus provides a substantial increase in the quantity of IR data available for these sources: 17 are detected in the WISE W1 (3.4 \u03bcm) band, 16 in W2 (4.6 \u03bcm), 3 in W3 (12 \u03bcm), and 0 in W4 (22 \u03bcm). This is particularly important with Spitzer in its warm-mission phase and no faint follow-up capability at wavelengths longward of 5 \u03bcm until the launch of James Webb Space Telescope (JWST). WISE thus provides a useful tool for understanding QSOs found in forthcoming large-area optical/IR sky surveys using PanSTARRS, SkyMapper, VISTA, DES, and LSST. The rest-UV properties of the WISE-detected and the WISE-non-detected samples differ: the detections have brighter i/z-band magnitudes and redder rest-UV colors. This suggests that a more aggressive hunt for very high redshift QSOs by combining WISE W1 and W2 data with red, observed optical colors could be effective at least for a subset of dusty candidate QSOs. Stacking the WISE images of the WISE-non-detected QSOs indicates that they are, on average, significantly fainter than the WISE-detected examples, and are thus not narrowly missing detection in the WISE catalog. The WISE catalog detection of three of our sample in the W3 band indicates that their mid-IR flux can be detected individually, although there is no stacked W3 detection of sources detected in W1 but not W3. Stacking analyses of WISE data for large active galactic nucleus samples will be a useful tool, and high-redshift QSOs of all types will be easy targets for JWST.", "doi": "10.1088/0004-637X/778/2/113", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-12-01", "series_number": "2", "volume": "778", "issue": "2", "pages": "Art. No. 113" }, { "id": "authors:p8hmn-b3584", "collection": "authors", "collection_id": "p8hmn-b3584", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131011-105108149", "type": "article", "title": "UV-bright Nearby Early-type Galaxies Observed in the Mid-infrared: Evidence for a Multi-stage Formation History by Way of WISE and GALEX Imaging", "author": [ { "family_name": "Petty", "given_name": "S. M.", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Neill", "given_name": "J. D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" }, { "family_name": "Jarrett", "given_name": "T. H.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Farrah", "given_name": "D. G.", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-D" }, { "family_name": "Rich", "given_name": "R. M.", "orcid": "0000-0003-0427-8387", "clpid": "Rich-R-M" }, { "family_name": "Tsai", "given_name": "C.-W.", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Benford", "given_name": "D. J.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Lake", "given_name": "S. E.", "clpid": "Lake-S-E" }, { "family_name": "Masci", "given_name": "F. J.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-F-J" }, { "family_name": "Wright", "given_name": "E. L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" } ], "abstract": "In the local universe, 10% of massive elliptical galaxies are observed to exhibit a peculiar property: a substantial excess of ultraviolet emission than what is expected from their old, red stellar populations. Several origins for this ultraviolet excess (UVX) have been proposed including a population of hot young stars and a population of old, blue horizontal branch or extended horizontal branch (BHB or EHB) stars that have undergone substantial mass loss from their outer atmospheres. We explore the radial distribution of UVX in a selection of 49 nearby E/S0-type galaxies by measuring their extended photometry in the UV through mid-infrared (mid-IR) with the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the Wide-field Infrared Survey Explorer (WISE). We compare UV/optical and UV/mid-IR colors with the Flexible Stellar Population Synthesis models, which allow for the inclusion of EHB stars. We find that combined WISE mid-IR and GALEX UV colors are more effective in distinguishing models than optical colors, and that the UV/mid-IR combination is sensitive to the EHB fraction. There are strong color gradients, with the outer radii bluer than the inner half-light radii by ~1 mag. This color difference is easily accounted for with an increase in the BHB fraction of 0.25 with radius. We estimated that the average ages for the inner and outer radii are 7.0 \u00b1 0.3 Gyr, and 6.2 \u00b1 0.2 Gyr, respectively, with the implication that the outer regions are likely to have formed ~1 Gyr after the inner regions. Additionally, we find that metallicity gradients are likely not a significant factor in the color difference. The separation of color between the inner and outer regions, which agrees with a specific stellar population difference (e.g., higher EHB populations), and the ~0.5\u20132 Gyr age difference suggests multi-stage formation. Our results are best explained by inside-out formation: rapid star formation within the core at early epochs (>4 Gyr ago) and at least one later stage starburst event coinciding with z ~ 1.", "doi": "10.1088/0004-6256/146/4/77", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2013-10", "series_number": "4", "volume": "146", "issue": "4", "pages": "Art. No. 77" }, { "id": "authors:m4zt4-5rj38", "collection": "authors", "collection_id": "m4zt4-5rj38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131004-114331470", "type": "article", "title": "The build-up of nuclear stellar cusps in extreme starburst galaxies and major mergers", "author": [ { "family_name": "Haan", "given_name": "S.", "clpid": "Haan-S" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Surace", "given_name": "J. A.", "orcid": "0000-0001-7291-0087", "clpid": "Surace-J-A" }, { "family_name": "Charmandaris", "given_name": "V.", "orcid": "0000-0002-2688-1956", "clpid": "Charmandaris-V" }, { "family_name": "Evans", "given_name": "A. S.", "orcid": "0000-0003-2638-1334", "clpid": "Evans-A-S" }, { "family_name": "D\u00edaz-Santos", "given_name": "T.", "orcid": "0000-0003-0699-6083", "clpid": "D\u00edaz-Santos-T" }, { "family_name": "Melbourne", "given_name": "J. L.", "clpid": "Melbourne-J-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": "Stierwalt", "given_name": "S.", "orcid": "0000-0002-2596-8531", "clpid": "Stierwalt-S" }, { "family_name": "Kim", "given_name": "D. C.", "clpid": "Kim-D-C" }, { "family_name": "Vavilkin", "given_name": "T.", "clpid": "Vavilkin-T" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Petric", "given_name": "A.", "orcid": "0000-0003-4030-3455", "clpid": "Petric-A-O" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Braun", "given_name": "R.", "orcid": "0000-0002-9353-9923", "clpid": "Braun-R-A" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Inami", "given_name": "H.", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" } ], "abstract": "Nuclear stellar cusps are defined as central excess light component in the stellar light profiles of galaxies and are suggested to be stellar relics of intense compact starbursts in the central \u223c100\u2013500\u2009pc region of gas-rich major mergers. Here, we probe the build-up of nuclear cusps during the actual starburst phase for a complete sample of luminous infrared galaxy (LIRG) systems (85 LIRGs, with 11.4 < log\u2009[LIR/L_\u2299] < 12.5) in the Great Observatories All-sky LIRG Survey sample. Cusp properties are derived via 2D fitting of the nuclear stellar light imaged in the near-infrared (NIR) by the Hubble Space Telescope and have been combined with mid-infrared (IR) diagnostics for active galactic nucleus (AGN)/starburst characterization. We find that nuclear stellar cusps are resolved in 76\u2009per\u2009cent of LIRGs (merger and non-interacting galaxies). The cusp strength and luminosity increase with far-IR luminosity (excluding AGN) and merger stage, confirming theoretical models that starburst activity is associated with the build-up of nuclear stellar cusps. Evidence for ultracompact nuclear starbursts is found in \u223c13\u2009per\u2009cent of LIRGs, which have a strong unresolved central NIR light component but no significant contribution of an AGN. The nuclear NIR surface density (measured within 1\u2009kpc radius) increases by a factor of \u223c5 towards late merger stages. A careful comparison to local early-type galaxies with comparable masses reveals (a) that local (U)LIRGs have a significantly larger cusp fraction and (b) that the majority of the cusp LIRGs have host galaxy luminosities (H band) similar to core ellipticals which are roughly one order in magnitude larger than those for cusp ellipticals.", "doi": "10.1093/mnras/stt1087", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2013-09-11", "series_number": "2", "volume": "434", "issue": "2", "pages": "1264-1286" }, { "id": "authors:wyvnz-xzb48", "collection": "authors", "collection_id": "wyvnz-xzb48", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130923-094035250", "type": "article", "title": "The NuSTAR Extragalactic Survey: A First Sensitive Look at the High-energy Cosmic X-Ray Background Population", "author": [ { "family_name": "Alexander", "given_name": "D. M.", "orcid": "0000-0002-5896-6313", "clpid": "Alexander-D-M" }, { "family_name": "Grefenstette", "given_name": "B. W.", "orcid": "0000-0002-1984-2932", "clpid": "Grefenstette-B-W" }, { "family_name": "Harrison", "given_name": "F. A.", "orcid": "0000-0002-4226-8959", "clpid": "Harrison-F-A" }, { "family_name": "Madsen", "given_name": "K. K.", "orcid": "0000-0003-1252-4891", "clpid": "Madsen-K-K" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Miller", "given_name": "S. H.", "clpid": "Miller-S-H" } ], "abstract": "We report on the first 10 identifications of sources serendipitously detected by the Nuclear Spectroscopic Telescope Array (NuSTAR) to provide the first sensitive census of the cosmic X-ray background source population at \u227310 keV. We find that these NuSTAR-detected sources are \u2248100 times fainter than those previously detected at \u227310 keV and have a broad range in redshift and luminosity (z = 0.020-2.923 and L_(10-40 keV) \u2248 4 \u00d7 10^(41)-5 \u00d7 10^(45) erg s^(\u20131)); the median redshift and luminosity are z \u2248 0.7 and L_(10-40 keV) \u2248 3 \u00d7 10^(44) erg s^(\u20131), respectively. We characterize these sources on the basis of broad-band \u22480.5-32 keV spectroscopy, optical spectroscopy, and broad-band ultraviolet-to-mid-infrared spectral energy distribution analyses. We find that the dominant source population is quasars with L_(10-40 keV) > 10^(44) erg s^(\u20131), of which \u224850% are obscured with N_H \u2273 10^(22) cm^(\u20132). However, none of the 10 NuSTAR sources are Compton thick (N_H \u2273 10^(24) cm^(\u20132)) and we place a 90% confidence upper limit on the fraction of Compton-thick quasars (L_(10-40 keV) > 10^(44) erg s^(\u20131)) selected at \u227310 keV of \u227e33% over the redshift range z = 0.5-1.1. We jointly fitted the rest-frame \u224810-40 keV data for all of the non-beamed sources with L_(10-40 keV) > 10^(43) erg s^(\u20131) to constrain the average strength of reflection; we find R < 1.4 for \u0393 = 1.8, broadly consistent with that found for local active galactic nuclei (AGNs) observed at \u227310 keV. We also constrain the host-galaxy masses and find a median stellar mass of \u224810^(11) M_\u2609, a factor \u22485 times higher than the median stellar mass of nearby high-energy selected AGNs, which may be at least partially driven by the order of magnitude higher X-ray luminosities of the NuSTAR sources. Within the low source-statistic limitations of our study, our results suggest that the overall properties of the NuSTAR sources are broadly similar to those of nearby high-energy selected AGNs but scaled up in luminosity and mass.", "doi": "10.1088/0004-637X/773/2/125", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-08-20", "series_number": "2", "volume": "773", "issue": "2", "pages": "Art. No. 125" }, { "id": "authors:6wazf-6sy97", "collection": "authors", "collection_id": "6wazf-6sy97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130729-100444888", "type": "article", "title": "The rapid assembly of an elliptical galaxy of 400 billion solar masses at a redshift of 2.3", "author": [ { "family_name": "Fu", "given_name": "Hai", "orcid": "0000-0001-9608-6395", "clpid": "Fu-Hai" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" } ], "abstract": "Stellar archaeology shows that massive elliptical galaxies formed rapidly about ten billion years ago with star-formation rates of above several hundred solar masses per year. Their progenitors are probably the submillimetre bright galaxies at redshifts z greater than 2. Although the mean molecular gas mass (5\u2009\u00d7\u200910^(10) solar masses) of the submillimetre bright galaxies can explain the formation of typical elliptical galaxies, it is inadequate to form elliptical galaxies4 that already have stellar masses above 2\u2009\u00d7\u200910^(11) solar masses at z\u2009\u2248\u20092. Here we report multi-wavelength high-resolution observations of a rare merger of two massive submillimetre bright galaxies at z = 2.3. The system is seen to be forming stars at a rate of 2,000 solar masses per year. The star-formation efficiency is an order of magnitude greater than that of normal galaxies, so the gas reservoir will be exhausted and star formation will be quenched in only around 200 million years. At a projected separation of 19\u2009 kiloparsecs, the two massive starbursts are about to merge and form a passive elliptical galaxy with a stellar mass of about 4\u2009\u00d7\u200910^(11) solar masses. We conclude that gas-rich major galaxy mergers with intense star formation can form the most massive elliptical galaxies by z\u2009\u2248\u20091.5.", "doi": "10.1038/nature12184", "issn": "0028-0836", "publisher": "Nature Publishing Group", "publication": "Nature", "publication_date": "2013-06-20", "series_number": "7454", "volume": "498", "issue": "7454", "pages": "338-341" }, { "id": "authors:t8x5r-vej40", "collection": "authors", "collection_id": "t8x5r-vej40", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120604-084501850", "type": "article", "title": "A New Population of High-z, Dusty Ly\u03b1 Emitters and Blobs Discovered by WISE: Feedback Caught in the Act?", "author": [ { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Blain", "given_name": "Andrew", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Borys", "given_name": "Colin J. K.", "clpid": "Borys-C-J-K" }, { "family_name": "Petty", "given_name": "Sara M.", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Benford", "given_name": "Dominic J.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Eisenhardt", "given_name": "Peter", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Farrah", "given_name": "Duncan", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Griffith", "given_name": "Roger L.", "clpid": "Griffith-R-L" }, { "family_name": "Jarrett", "given_name": "Tom", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Lonsdale", "given_name": "Carol", "orcid": "0000-0003-0898-406X", "clpid": "Lonsdale-Carol-J" }, { "family_name": "Stanford", "given_name": "Spencer A.", "clpid": "Stanford-S-A" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Wright", "given_name": "Edward L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" }, { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" } ], "abstract": "By combining data from the NASA Wide-field Infrared Survey Explorer (WISE) mission with optical spectroscopy from the W. M. Keck telescope, we discover a mid-IR color criterion that yields a 78% success rate in identifying rare, typically radio-quiet, 1.6 \u227e z \u227e 4.6 dusty Ly\u03b1 emitters (LAEs). Of these, at least 37% have emission extended on scales of 30-100 kpc and are considered Ly\u03b1 \"blobs\" (LABs). The objects have a surface density of only ~0.1 deg^(\u20132), making them rare enough that they have been largely missed in deep, small area surveys. We measured spectroscopic redshifts for 92 of these galaxies, and find that the LAEs (LABs) have a median redshift of 2.3 (2.5). The WISE photometry coupled with data from Herschel (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) reveals that these galaxies are in the Hyper Luminous IR galaxy regime (L IR \u2273 10^(13)-10^(14) L_\u2609) and have warm colors. They are typically more luminous and warmer than other dusty, z ~ 2 populations such as submillimeter-selected galaxies and dust-obscured galaxies. These traits are commonly associated with the dust being illuminated by intense active galactic nucleus activity. We hypothesize that the combination of spatially extended Ly\u03b1, large amounts of warm IR-luminous dust, and rarity (implying a short-lived phase) can be explained if the galaxies are undergoing brief, intense \"feedback\" transforming them from an extreme dusty starburst/QSO into a mature galaxy.", "doi": "10.1088/0004-637X/769/2/91", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-06-01", "series_number": "2", "volume": "769", "issue": "2", "pages": "Art. No. 91" }, { "id": "authors:mpzth-c0h34", "collection": "authors", "collection_id": "mpzth-c0h34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130408-102147094", "type": "article", "title": "Mid-infrared Properties of Nearby Luminous Infrared Galaxies. I. Spitzer Infrared Spectrograph Spectra for the GOALS Sample", "author": [ { "family_name": "Stierwalt", "given_name": "S.", "orcid": "0000-0002-2596-8531", "clpid": "Stierwalt-S" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Surace", "given_name": "J. A.", "orcid": "0000-0001-7291-0087", "clpid": "Surace-J-A" }, { "family_name": "Inami", "given_name": "H.", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" }, { "family_name": "Petric", "given_name": "A. O.", "orcid": "0000-0003-4030-3455", "clpid": "Petric-A-O" }, { "family_name": "D\u00edaz-Santos", "given_name": "T.", "orcid": "0000-0003-0699-6083", "clpid": "D\u00edaz-Santos-T" }, { "family_name": "Haan", "given_name": "S.", "clpid": "Haan-S" }, { "family_name": "Howell", "given_name": "J.", "clpid": "Howell-J-H" }, { "family_name": "Marshall", "given_name": "J.", "clpid": "Marshall-J" }, { "family_name": "Mazzarella", "given_name": "J. M.", "orcid": "0000-0002-8204-8619", "clpid": "Mazzarella-J-M" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Melbourne", "given_name": "J. E.", "clpid": "Melbourne-J-E" }, { "family_name": "Chan", "given_name": "B.", "clpid": "Chan-Ben-Hiu-Pan" }, { "family_name": "Lord", "given_name": "S.", "clpid": "Lord-S" }, { "family_name": "Xu", "given_name": "K.", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" }, { "family_name": "Appleton", "given_name": "P.", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" } ], "abstract": "The Great Observatories All-Sky LIRG Survey (GOALS) is a comprehensive, multiwavelength study of luminous infrared galaxies (LIRGs) in the local universe. Here we present low resolution Spitzer Infrared Spectrograph spectra covering 5-38 \u03bcm and provide a basic analysis of the mid-IR spectral properties observed for nearby LIRGs. In a companion paper, we discuss detailed fits to the spectra and compare the LIRGs to other classes of galaxies. The GOALS sample of 244 nuclei in 180 luminous (10^(11) \u2264 L_(IR)/L_\u2609 < 10^(12)) and 22 ultraluminous (L_(IR)/L_\u2609 \u2265 10^(12)) IR galaxies represents a complete subset of the IRAS Revised Bright Galaxy Sample and covers a range of merger stages, morphologies, and spectral types. The majority (>60%) of the GOALS LIRGs have high 6.2 \u03bcm polycyclic aromatic hydrocarbon (PAH) equivalent widths (EQW_(6.2 \u03bcm) > 0.4 \u03bcm) and low levels of silicate absorption (s 9.7 \u03bcm > \u20131.0). There is a general trend among the U/LIRGs for both silicate depth and mid-infrared (MIR) slope to increase with increasing L_(IR). U/LIRGs in the late to final stages of a merger also have, on average, steeper MIR slopes and higher levels of dust obscuration. Together, these trends suggest that as gas and dust is funneled toward the center of a coalescing merger, the nuclei become more compact and more obscured. As a result, the dust temperature increases also leading to a steeper MIR slope. The sources that depart from these correlations have very low PAH equivalent width (EQW_(6.2 \u03bcm) < 0.1 \u03bcm) consistent with their emission being dominated by an active galactic nucleus (AGN) in the MIR. These extremely low PAH EQW sources separate into two distinct types: relatively unobscured sources with a very hot dust component (and thus very shallow MIR slopes) and heavily dust obscured nuclei with a steep temperature gradient. The most heavily dust obscured sources are also the most compact in their MIR emission, suggesting that the obscuring (cool) dust is associated with the outer regions of the starburst and not simply a measure of the dust along the line of sight through a large, dusty disk. A marked decline is seen for the fraction of high EQW (star formation dominated) sources as the merger progresses. The decline is accompanied by an increase in the fraction of composite sources while the fraction of sources where an AGN dominates the MIR emission remains low. When compared to the MIR spectra of submillimeter galaxies (SMGs) at z ~ 2, both the average GOALS LIRG and ULIRG spectra are more absorbed at 9.7 \u03bcm and the average GOALS LIRG has more PAH emission. However, when the AGN contributions to both the local GOALS LIRGs and the high-z SMGs are removed, the average local starbursting LIRG closely resembles the starburst-dominated SMGs.", "doi": "10.1088/0067-0049/206/1/1", "issn": "0067-0049", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Supplement Series", "publication_date": "2013-05", "series_number": "1", "volume": "206", "issue": "1", "pages": "Art. No. 1" }, { "id": "authors:vkj8x-hp913", "collection": "authors", "collection_id": "vkj8x-hp913", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-090532935", "type": "article", "title": "Extending the Nearby Galaxy Heritage with WISE: First Results from the WISE Enhanced Resolution Galaxy Atlas", "author": [ { "family_name": "Jarrett", "given_name": "T. H.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Masci", "given_name": "F.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-F-J" }, { "family_name": "Tsai", "given_name": "C. W.", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Petty", "given_name": "S.", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Cluver", "given_name": "M. E.", "orcid": "0000-0002-9871-6490", "clpid": "Cluver-M-E" }, { "family_name": "Assef", "given_name": "Roberto J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Benford", "given_name": "D. J.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-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-R" }, { "family_name": "Donoso", "given_name": "E.", "clpid": "Donoso-E" }, { "family_name": "Eisenhardt", "given_name": "P.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Koribalski", "given_name": "B.", "clpid": "Koribalski-B-S" }, { "family_name": "Lake", "given_name": "S.", "clpid": "Lake-S" }, { "family_name": "Neill", "given_name": "James D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" }, { "family_name": "Seibert", "given_name": "M.", "orcid": "0000-0002-1143-5515", "clpid": "Seibert-M" }, { "family_name": "Sheth", "given_name": "K.", "orcid": "0000-0002-5496-4118", "clpid": "Sheth-K" }, { "family_name": "Stanford", "given_name": "S. Adam", "clpid": "Stanford-S-A" }, { "family_name": "Wright", "given_name": "E.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" } ], "abstract": "The Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at mid-infrared wavelengths 3.4 \u03bcm, 4.6 \u03bcm, 12 \u03bcm, and 22 \u03bcm. The mission was primarily designed to extract point sources, leaving resolved and extended sources, for the most part, unexplored. Accordingly, we have begun a dedicated WISE Enhanced Resolution Galaxy Atlas (WERGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we demonstrate the first results of the WERGA project for a sample of 17 galaxies, chosen to be of large angular size, diverse morphology, and covering a range in color, stellar mass, and star formation. It includes many well-studied galaxies, such as M 51, M 81, M 87, M 83, M 101, and IC 342. Photometry and surface brightness decomposition is carried out after special super-resolution processing, achieving spatial resolutions similar to that of Spitzer Infrared Array Camera. The enhanced resolution method is summarized in the first paper of this two-part series. In this second work, we present WISE, Spitzer, and Galaxy Evolution Explorer (GALEX) photometric and characterization measurements for the sample galaxies, combining the measurements to study the global properties. We derive star formation rates using the polycyclic aromatic hydrocarbon sensitive 12 \u03bcm (W3) fluxes, warm-dust sensitive 22 \u03bcm (W4) fluxes, and young massive-star sensitive ultraviolet (UV) fluxes. Stellar masses are estimated using the 3.4 \u03bcm (W1) and 4.6 \u03bcm (W2) measurements that trace the dominant stellar mass content. We highlight and showcase the detailed results of M 83, comparing the WISE/Spitzer results with the Australia Telescope Compact Array H I gas distribution and GALEX UV emission, tracing the evolution from gas to stars. In addition to the enhanced images, WISE's all-sky coverage provides a tremendous advantage over Spitzer for building a complete nearby galaxy catalog, tracing both stellar mass and star formation histories. We discuss the construction of a complete mid-infrared catalog of galaxies and its complementary role of studying the assembly and evolution of galaxies in the local universe.", "doi": "10.1088/0004-6256/145/1/6", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2013-01", "series_number": "1", "volume": "145", "issue": "1", "pages": "Art. No. 6" }, { "id": "authors:56cst-bxz13", "collection": "authors", "collection_id": "56cst-bxz13", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121219-122507868", "type": "article", "title": "A Close-pair Analysis of Damp Mergers at Intermediate Redshifts", "author": [ { "family_name": "Chou", "given_name": "Richard C. Y.", "clpid": "Chou-Richard-C-Y" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Abraham", "given_name": "Roberto G.", "orcid": "0000-0002-4542-921X", "clpid": "Abraham-R-G" } ], "abstract": "We have studied the kinematics of ~2800 candidate close-pair galaxies at 0.1 < z < 1.2 identified from the Canada-France-Hawaii Telescope Legacy Survey fields. Spectra of these systems were obtained using spectrometers on the 6.5 m Magellan and 5 m Hale telescopes. These data allow us to constrain the rate of dry mergers at intermediate redshifts and to test the \"hot halo\" model for quenching of star formation. Using virial radii estimated from the correlation between dynamical and stellar masses published by Leauthaud et al., we find that around 1/5 of our candidate pairs are likely to share a common dark matter halo (our metric for close physical association). These pairs are divided into red-red, blue-red, and blue-blue systems using the rest-frame colors classification method introduced in Chou et al.. Galaxies classified as red in our sample have very low star formation rates, but they need not be totally quiescent, and hence we refer to them as \"damp,\" rather than \"dry,\" systems. After correcting for known selection effects, the fraction of blue-blue pairs is significantly greater than that of red-red and blue-red pairs. Red-red pairs are almost entirely absent from our sample, suggesting that damp mergers are rare at z ~ 0.5. Our data support models with a short merging timescale (<0.5 Gyr) in which star formation is enhanced in the early phase of mergers, but quenched in the late phase. Hot halo models may explain this behavior, but only if virial shocks that heat gas are inefficient until major mergers are nearly complete.", "doi": "10.1088/0004-637X/760/2/113", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-12-01", "series_number": "2", "volume": "760", "issue": "2", "pages": "Art. No. 113" }, { "id": "authors:vc4sk-qfw98", "collection": "authors", "collection_id": "vc4sk-qfw98", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-142950078", "type": "article", "title": "The dominant role of mergers in the size evolution of massive\n early-type galaxies since z \u223c 1", "author": [ { "family_name": "L\u00f3pez-Sanjuan", "given_name": "C.", "clpid": "L\u00f3pez-Sanjuan-C" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Xu", "given_name": "C. K.", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Salvato", "given_name": "M.", "orcid": "0000-0001-7116-9303", "clpid": "Salvato-Mara" } ], "abstract": "Aims. The role of galaxy mergers in massive galaxy evolution, and in particular to mass assembly and size growth, remains an open question. In this paper we measure the merger fraction and rate, both minor and major, of massive early-type galaxies (M_\u22c6 \u2265 10^(11) M_\u2299) in the COSMOS field, and study their role in mass and size evolution.\nMethods. We used the 30-band photometric catalogue in COSMOS, complemented with the spectroscopy of the zCOSMOS survey, to define close pairs with a separation on the sky plane 10 h^(-1) kpc \u2264 r_p \u2264 30 h^(-1) kpc and a relative velocity \u0394v \u2264 500 km s^(-1) in redshift space. We measured both major (stellar mass ratio \u03bc \u2261 M_(\u22c6,2)/M_(\u22c6,1) \u2265 1/4) and minor (1/10 \u2264 \u03bc < 1/4) merger fractions of massive galaxies, and studied their dependence on redshift and on morphology (early types vs. late types).\nResults. The merger fraction and rate of massive galaxies evolves as a power-law (1 + z)^n, with major mergers increasing with redshift, n_(MM) = 1.4, and minor mergers showing little evolution, n_(mm) ~ 0. When split by their morphology, the minor merger fraction for early-type galaxies (ETGs) is higher by a factor of three than that for late-type galaxies (LTGs), and both are nearly constant with redshift. The fraction of major mergers for massive LTGs evolves faster (n_(MM)^(LT) ~ 4 ) than for ETGs (n_(MM)^(ET)= 1.8).\nConclusions. Our results show that massive ETGs have undergone 0.89 mergers (0.43 major and 0.46 minor) since z ~ 1, leading to a mass growth of ~30%. We find that \u03bc \u2265 1/10 mergers can explain ~55% of the observed size evolution of these galaxies since z ~ 1. Another ~20% is due to the progenitor bias (younger galaxies are more extended) and we estimate that very minor mergers (\u03bc < 1/10) could contribute with an extra ~20%. The remaining ~5% should come from other processes (e.g., adiabatic expansion or observational effects). This picture also reproduces the mass growth and the velocity dispersion evolution of these galaxies. We conclude from these results, and after exploring all the possible uncertainties in our picture, that merging is the main contributor to the size evolution of massive ETGs at z \u2272 1, accounting for ~50\u221275% of that evolution in the last 8 Gyr. Nearly half of the evolution due to mergers is related to minor (\u03bc < 1/4) events.", "doi": "10.1051/0004-6361/201219085", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2012-12", "volume": "548", "pages": "Art. No. A7" }, { "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:pznd8-jed85", "collection": "authors", "collection_id": "pznd8-jed85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121204-104158528", "type": "article", "title": "Spitzer Photometry of WISE-selected Brown Dwarf and Hyper-luminous Infrared Galaxy Candidates", "author": [ { "family_name": "Griffith", "given_name": "Roger L.", "clpid": "Griffith-R-L" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Gelino", "given_name": "Christopher R.", "clpid": "Gelino-C-R" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Cohen", "given_name": "Martin", "clpid": "Cohen-Martin" }, { "family_name": "Cutri", "given_name": "Roc M.", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" }, { "family_name": "Donoso", "given_name": "Emilio", "clpid": "Donoso-E" }, { "family_name": "Jarrett", "given_name": "Thomas H.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "We present Spitzer 3.6 and 4.5 \u03bcm photometry and positions for a sample of 1510 brown dwarf candidates identified by the Wide-field Infrared Survey Explorer (WISE) all-sky survey. Of these, 166 have been spectroscopically classified as objects with spectral types M(1), L(7), T(146), and Y(12). Sixteen other objects are non-(sub)stellar in nature. The remainder are most likely distant L and T dwarfs lacking spectroscopic verification, other Y dwarf candidates still awaiting follow-up, and assorted other objects whose Spitzer photometry reveals them to be background sources. We present a catalog of Spitzer photometry for all astrophysical sources identified in these fields and use this catalog to identify seven fainter (4.5 \u03bcm ~ 17.0 mag) brown dwarf candidates, which are possibly wide-field companions to the original WISE sources. To test this hypothesis, we use a sample of 919 Spitzer observations around WISE-selected high-redshift hyper-luminous infrared galaxy candidates. For this control sample, we find another six brown dwarf candidates, suggesting that the seven companion candidates are not physically associated. In fact, only one of these seven Spitzer brown dwarf candidates has a photometric distance estimate consistent with being a companion to the WISE brown dwarf candidate. Other than this, there is no evidence for any widely separated (>20 AU) ultra-cool binaries. As an adjunct to this paper, we make available a source catalog of ~7.33 \u00d7 10^5 objects detected in all of these Spitzer follow-up fields for use by the astronomical community. The complete catalog includes the Spitzer 3.6 and 4.5 \u03bcm photometry, along with positionally matched B and R photometry from USNO-B; J, H, and K_s photometry from Two Micron All-Sky Survey; and W1, W2, W3, and W4 photometry from the WISE all-sky catalog.", "doi": "10.1088/0004-6256/144/5/148", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2012-11", "series_number": "5", "volume": "144", "issue": "5", "pages": "Art. No. 148" }, { "id": "authors:x5876-ezy31", "collection": "authors", "collection_id": "x5876-ezy31", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121031-103418816", "type": "article", "title": "Submillimeter Follow-up of WISE-selected Hyperluminous Galaxies", "author": [ { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Sayers", "given_name": "Jack", "orcid": "0000-0002-8213-3784", "clpid": "Sayers-Jack" }, { "family_name": "Benford", "given_name": "Dominic", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Blain", "given_name": "Andrew", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Eisenhardt", "given_name": "Peter R. M.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Petty", "given_name": "Sara", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Assef", "given_name": "Roberto", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Bussmann", "given_name": "Shane", "clpid": "Bussmann-S" }, { "family_name": "Comerford", "given_name": "Julia M.", "orcid": "0000-0001-8627-4907", "clpid": "Comerford-J-M" }, { "family_name": "Cutri", "given_name": "Roc", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" }, { "family_name": "Evans", "given_name": "Neal J., II", "orcid": "0000-0001-5175-1777", "clpid": "Evans-N-J-II" }, { "family_name": "Griffith", "given_name": "Roger", "clpid": "Griffith-R-L" }, { "family_name": "Jarrett", "given_name": "Thomas", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Lake", "given_name": "Sean", "clpid": "Lake-S" }, { "family_name": "Lonsdale", "given_name": "Carol", "orcid": "0000-0003-0898-406X", "clpid": "Lonsdale-Carol-J" }, { "family_name": "Rho", "given_name": "Jeonghee", "orcid": "0000-0003-3643-839X", "clpid": "Rho-Jeonghee" }, { "family_name": "Stanford", "given_name": "S. Adam", "clpid": "Stanford-S-A" }, { "family_name": "Weiner", "given_name": "Benjamin", "clpid": "Weiner-B-J" }, { "family_name": "Wright", "given_name": "Edward L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "

We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (∼1000 all-sky) population of galaxies at high redshift (peaks at z = 2–3), which are faint or undetected by WISE at 3.4 and 4.6 μm, yet are clearly detected at 12 and 22 μm. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350–850 μm, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 μm, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60–120 K using a single-temperature model. Their infrared luminosities are well over 1013 L\u2609. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.

", "doi": "10.1088/0004-637X/756/1/96", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-09-01", "series_number": "1", "volume": "756", "issue": "1", "pages": "Art. No. 96" }, { "id": "authors:r0etj-a9w74", "collection": "authors", "collection_id": "r0etj-a9w74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121030-134258087", "type": "article", "title": "The First Hyper-luminous Infrared Galaxy Discovered by WISE", "author": [ { "family_name": "Eisenhardt", "given_name": "Peter R. M.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Wu", "given_name": "Jingwen", "orcid": "0000-0001-7808-3756", "clpid": "Wu-Jingwen" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Assef", "given_name": "Roberto", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Benford", "given_name": "Dominic", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-J" }, { "family_name": "Blain", "given_name": "Andrew", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Condon", "given_name": "J. J.", "orcid": "0000-0003-4724-1939", "clpid": "Condon-J-J" }, { "family_name": "Cushing", "given_name": "Michael C.", "orcid": "0000-0001-7780-3352", "clpid": "Cushing-M-C" }, { "family_name": "Cutri", "given_name": "Roc", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" }, { "family_name": "Evans", "given_name": "Neal J., II", "orcid": "0000-0001-5175-1777", "clpid": "Evans-N-J-II" }, { "family_name": "Gelino", "given_name": "Chris", "clpid": "Gelino-C-R" }, { "family_name": "Griffith", "given_name": "Roger L.", "clpid": "Griffith-R-L" }, { "family_name": "Grillmair", "given_name": "Carl J.", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Jarrett", "given_name": "Tom", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "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": "Mason", "given_name": "Brian S.", "clpid": "Mason-B-S" }, { "family_name": "Petty", "given_name": "Sara", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Sayers", "given_name": "Jack", "orcid": "0000-0002-8213-3784", "clpid": "Sayers-Jack" }, { "family_name": "Stanford", "given_name": "S. A.", "clpid": "Stanford-S-A" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Wright", "given_name": "Edward L.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "

We report the discovery by the Wide-field Infrared Survey Explorer (WISE) of the z = 2.452 source WISE J181417.29+341224.9, the first hyperluminous source found in the WISE survey. WISE 1814+3412 is also the prototype for an all-sky sample of ∼1000 extremely luminous \"W1W2-dropouts\" (sources faint or undetected by WISE at 3.4 and 4.6 μm and well detected at 12 or 22 μm). The WISE data and a 350 μm detection give a minimum bolometric luminosity of 3.7 × 1013 L\u2609, with ∼1014 L\u2609 plausible. Follow-up images reveal four nearby sources: a QSO and two Lyman break galaxies (LBGs) at z = 2.45, and an M dwarf star. The brighter LBG dominates the bolometric emission. Gravitational lensing is unlikely given the source locations and their different spectra and colors. The dominant LBG spectrum indicates a star formation rate ∼300 M\u2609 yr−1, accounting for \u2272 10% of the bolometric luminosity. Strong 22 μm emission relative to 350 μm implies that warm dust contributes significantly to the luminosity, while cooler dust normally associated with starbursts is constrained by an upper limit at 1.1 mm. Radio emission is ∼10 times above the far-infrared/radio correlation, indicating an active galactic nucleus (AGN) is present. An obscured AGN combined with starburst and evolved stellar components can account for the observations. If the black hole mass follows the local MBH–bulge mass relation, the implied Eddington ratio is \u2273 4. WISE 1814+3412 may be a heavily obscured object where the peak AGN activity occurred prior to the peak era of star formation.

", "doi": "10.1088/0004-637X/755/2/173", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-08-20", "series_number": "2", "volume": "755", "issue": "2", "pages": "Art. No. 173" }, { "id": "authors:8gckr-m6b29", "collection": "authors", "collection_id": "8gckr-m6b29", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120827-101936774", "type": "article", "title": "Constructing a WISE High Resolution Galaxy Atlas", "author": [ { "family_name": "Jarrett", "given_name": "T. H.", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Masci", "given_name": "F.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-F-J" }, { "family_name": "Tsai", "given_name": "C. W.", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Petty", "given_name": "S.", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" }, { "family_name": "Cluver", "given_name": "M.", "orcid": "0000-0002-9871-6490", "clpid": "Cluver-M-E" }, { "family_name": "Assef", "given_name": "Roberto J.", "orcid": "0000-0002-9508-3667", "clpid": "Assef-R-J" }, { "family_name": "Benford", "given_name": "D. J.", "orcid": "0000-0002-9884-4206", "clpid": "Benford-D-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-R" }, { "family_name": "Donoso", "given_name": "E.", "clpid": "Donoso-E" }, { "family_name": "Eisenhardt", "given_name": "P.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Fowler", "given_name": "J.", "clpid": "Fowler-J" }, { "family_name": "Koribalski", "given_name": "B.", "clpid": "Koribalski-B-S" }, { "family_name": "Lake", "given_name": "S.", "clpid": "Lake-S" }, { "family_name": "Neill", "given_name": "James D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-J-D" }, { "family_name": "Seibert", "given_name": "M.", "orcid": "0000-0002-1143-5515", "clpid": "Seibert-M" }, { "family_name": "Sheth", "given_name": "K.", "orcid": "0000-0002-5496-4118", "clpid": "Sheth-K" }, { "family_name": "Stanford", "given_name": "S.", "clpid": "Stanford-S" }, { "family_name": "Wright", "given_name": "E.", "orcid": "0000-0001-5058-1593", "clpid": "Wright-E-L" } ], "abstract": "After eight months of continuous observations, the Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at 3.4 \u03bcm, 4.6 \u03bcm, 12 \u03bcm, and 22 \u03bcm. We have begun a dedicated WISE High Resolution Galaxy Atlas project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we summarize the deconvolution techniques used to significantly improve the spatial resolution of WISE imaging, specifically designed to study the internal anatomy of nearby galaxies. As a case study, we present results for the galaxy NGC 1566, comparing the WISE enhanced-resolution image processing to that of Spitzer, Galaxy Evolution Explorer, and ground-based imaging. This is the first paper in a two-part series; results for a larger sample of nearby galaxies are presented in the second paper.", "doi": "10.1088/0004-6256/144/2/68", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2012-08", "series_number": "2", "volume": "144", "issue": "2", "pages": "Art. No. 68" }, { "id": "authors:h92mr-xj498", "collection": "authors", "collection_id": "h92mr-xj498", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120319-112743267", "type": "article", "title": "Direct Evidence for Termination of Obscured Star Formation by Radiatively Driven Outflows in Reddened QSOs", "author": [ { "family_name": "Farrah", "given_name": "Duncan", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-Duncan" }, { "family_name": "Urrutia", "given_name": "Tanya", "orcid": "0000-0001-6746-9936", "clpid": "Urrutia-T" }, { "family_name": "Lacy", "given_name": "Mark", "orcid": "0000-0002-3032-1783", "clpid": "Lacy-M" }, { "family_name": "Efstathiou", "given_name": "Andreas", "orcid": "0000-0002-2612-4840", "clpid": "Efstathiou-Andreas" }, { "family_name": "Afonso", "given_name": "Jos\u00e9", "orcid": "0000-0002-9149-2973", "clpid": "Afonso-J" }, { "family_name": "Coppin", "given_name": "Kristen", "clpid": "Coppin-K-E-K" }, { "family_name": "Hall", "given_name": "Patrick B.", "clpid": "Hall-P-B" }, { "family_name": "Lonsdale", "given_name": "Carol", "orcid": "0000-0003-0898-406X", "clpid": "Lonsdale-Carol-J" }, { "family_name": "Jarrett", "given_name": "Tom", "orcid": "0000-0002-4939-734X", "clpid": "Jarrett-T-H" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Borys", "given_name": "Colin", "clpid": "Borys-C-J-K" }, { "family_name": "Petty", "given_name": "Sara M.", "orcid": "0000-0003-0624-3276", "clpid": "Petty-Sara-M" } ], "abstract": "We present optical to far-infrared photometry of 31 reddened QSOs that show evidence for radiatively driven outflows originating from active galactic nuclei (AGNs) in their rest-frame UV spectra. We use these data to study the relationships between the AGN-driven outflows, and the AGN and starburst infrared luminosities. We find that FeLoBAL QSOs are invariably IR-luminous, with IR luminosities exceeding 10^(12) L_\u2609 in all cases. The AGN supplies 76% of the total IR emission, on average, but with a range from 20% to 100%. We find no evidence that the absolute luminosity of obscured star formation is affected by the AGN-driven outflows. Conversely, we find an anticorrelation between the strength of AGN-driven outflows, as measured from the range of outflow velocities over which absorption exceeds a minimal threshold, and the contribution from star formation to the total IR luminosity, with a much higher chance of seeing a starburst contribution in excess of 25% in systems with weak outflows than in systems with strong outflows. Moreover, we find no convincing evidence that this effect is driven by the IR luminosity of the AGN. We conclude that radiatively driven outflows from AGNs can have a dramatic, negative impact on luminous star formation in their host galaxies. We find that such outflows act to curtail star formation such that star formation contributes less than ~25% of the total IR luminosity. We also propose that the degree to which termination of star formation takes place is not deducible from the IR luminosity of the AGN.", "doi": "10.1088/0004-637X/745/2/178", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-02", "series_number": "2", "volume": "745", "issue": "2", "pages": "Art. No. 178" }, { "id": "authors:0w75b-st056", "collection": "authors", "collection_id": "0w75b-st056", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120201-083615093", "type": "article", "title": "Very Strong Emission-line Galaxies in the WFC3 Infrared Spectroscopic Parallel Survey and Implications for High-redshift Galaxies", "author": [ { "family_name": "Atek", "given_name": "H.", "orcid": "0000-0002-7570-0824", "clpid": "Atek-H" }, { "family_name": "Siana", "given_name": "B.", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Malkan", "given_name": "M.", "orcid": "0000-0001-6919-1237", "clpid": "Malkan-M-A" }, { "family_name": "McCarthy", "given_name": "P.", "clpid": "McCarthy-P-J" }, { "family_name": "Teplitz", "given_name": "H.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Henry", "given_name": "A. L.", "orcid": "0000-0002-6586-4446", "clpid": "Henry-A-L" }, { "family_name": "Colbert", "given_name": "J.", "clpid": "Colbert-J-W" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Bunker", "given_name": "A. J.", "clpid": "Bunker-A-J" }, { "family_name": "Dressler", "given_name": "A.", "clpid": "Dressler-A" }, { "family_name": "Fosbury", "given_name": "R. A. E.", "clpid": "Fosbury-R-A-E" }, { "family_name": "Hathi", "given_name": "N. P.", "orcid": "0000-0001-6145-5090", "clpid": "Hathi-N-P" }, { "family_name": "Martin", "given_name": "C.", "clpid": "Martin-Crystal-L" }, { "family_name": "Ross", "given_name": "N. R.", "clpid": "Ross-N-R" }, { "family_name": "Shim", "given_name": "H.", "clpid": "Shim-H" } ], "abstract": "The WFC3 Infrared Spectroscopic Parallel Survey uses the Hubble Space Telescope (HST) infrared grism capabilities to obtain slitless spectra of thousands of galaxies over a wide redshift range including the peak of star formation history of the universe. We select a population of very strong emission-line galaxies with rest-frame equivalent widths (EWs) higher than 200 \u00c5. A total of 176 objects are found over the redshift range 0.35 < z < 2.3 in the 180 arcmin^2 area that we have analyzed so far. This population consists of young and low-mass starbursts with high specific star formation rates (sSFR). After spectroscopic follow-up of one of these galaxies with Keck/Low Resolution Imaging Spectrometer, we report the detection at z = 0.7 of an extremely metal-poor galaxy with 12 + log(O/H) =7.47 \u00b1 0.11. After estimating the active galactic nucleus fraction in the sample, we show that the high-EW galaxies have higher sSFR than normal star-forming galaxies at any redshift. We find that the nebular emission lines can substantially affect the total broadband flux density with a median brightening of 0.3 mag, with some examples of line contamination producing brightening of up to 1 mag. We show that the presence of strong emission lines in low-z galaxies can mimic the color-selection criteria used in the z ~ 8 dropout surveys. In order to effectively remove low-redshift interlopers, deep optical imaging is needed, at least 1 mag deeper than the bands in which the objects are detected. Without deep optical data, most of the interlopers cannot be ruled out in the wide shallow HST imaging surveys. Finally, we empirically demonstrate that strong nebular lines can lead to an overestimation of the mass and the age of galaxies derived from fitting of their spectral energy distribution (SED). Without removing emission lines, the age and the stellar mass estimates are overestimated by a factor of 2 on average and up to a factor of 10 for the high-EW galaxies. Therefore, the contribution of emission lines should be systematically taken into account in SED fitting of star-forming galaxies at all redshifts.", "doi": "10.1088/0004-637X/743/2/121", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2011-12-20", "series_number": "2", "volume": "743", "issue": "2", "pages": "Art. No. 121" }, { "id": "authors:b0cqk-a0592", "collection": "authors", "collection_id": "b0cqk-a0592", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120125-151623435", "type": "article", "title": "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)", "author": [ { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Gelino", "given_name": "Christopher R.", "clpid": "Gelino-C-R" }, { "family_name": "Griffith", "given_name": "Roger L.", "clpid": "Griffith-R-L" }, { "family_name": "Marsh", "given_name": "Kenneth A.", "orcid": "0000-0003-0107-7803", "clpid": "Marsh-K-A" }, { "family_name": "Tsai", "given_name": "Chao-Wei", "orcid": "0000-0002-9390-9672", "clpid": "Tsai-Chao-Wei" }, { "family_name": "Beichman", "given_name": "Charles A.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Capak", "given_name": "Peter L.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Morales-Calder\u00f3n", "given_name": "Mar\u00eda", "clpid": "Morales-Calder\u00f3n-M" }, { "family_name": "Manohar", "given_name": "Swarnima", "clpid": "Manohar-S" }, { "family_name": "Scoville", "given_name": "Nicholas Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Schurr", "given_name": "Steven D.", "clpid": "Schurr-S-D" } ], "abstract": "We present ground-based spectroscopic verification of 6 Y dwarfs (see also Cushing et al.), 89 T dwarfs, 8 L dwarfs, and 1 M dwarf identified by the Wide-field Infrared Survey Explorer (WISE). Eighty of these are cold brown dwarfs with spectral types \u2265T6, six of which have been announced earlier by Mainzer et al. and Burgasser et al. We present color-color and color-type diagrams showing the locus of M, L, T, and Y dwarfs in WISE color space. Near-infrared and, in a few cases, optical spectra are presented for these discoveries. Near-infrared classifications as late as early Y are presented and objects with peculiar spectra are discussed. Using these new discoveries, we are also able to extend the optical T dwarf classification scheme from T8 to T9. After deriving an absolute WISE 4.6 \u03bcm (W2) magnitude versus spectral type relation, we estimate spectrophotometric distances to our discoveries. We also use available astrometric measurements to provide preliminary trigonometric parallaxes to four of our discoveries, which have types of L9 pec (red), T8, T9, and Y0; all of these lie within 10 pc of the Sun. The Y0 dwarf, WISE 1541\u20132250, is the closest at 2.8^(+1.3)_(\u20130.6) pc; if this 2.8 pc value persists after continued monitoring, WISE 1541\u20132250 will become the seventh closest stellar system to the Sun. Another 10 objects, with types between T6 and >Y0, have spectrophotometric distance estimates also placing them within 10 pc. The closest of these, the T6 dwarf WISE 1506+7027, is believed to fall at a distance of ~4.9 pc. WISE multi-epoch positions supplemented with positional info primarily from the Spitzer/Infrared Array Camera allow us to calculate proper motions and tangential velocities for roughly one-half of the new discoveries. This work represents the first step by WISE to complete a full-sky, volume-limited census of late-T and Y dwarfs. Using early results from this census, we present preliminary, lower limits to the space density of these objects and discuss constraints on both the functional form of the mass function and the low-mass limit of star formation.", "doi": "10.1088/0067-0049/197/2/19", "issn": "0067-0049", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Supplement Series", "publication_date": "2011-12", "series_number": "2", "volume": "197", "issue": "2", "pages": "19" }, { "id": "authors:rtnf2-3sq78", "collection": "authors", "collection_id": "rtnf2-3sq78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110315-152141116", "type": "article", "title": "The Space Density Evolution of Wet and Dry Mergers in the Canada-France-Hawaii Telescope Legacy Survey", "author": [ { "family_name": "Chou", "given_name": "Richard C. Y.", "clpid": "Chou-Richard-C-Y" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Abraham", "given_name": "Roberto G.", "orcid": "0000-0002-4542-921X", "clpid": "Abraham-R-G" } ], "abstract": "We analyze 1298 merging galaxies with redshifts up to z = 0.7 from the Canada-France-Hawaii Telescope Legacy Survey, taken from the catalog presented in the work of Bridge et al. By analyzing the internal colors of these systems, we show that the so-called wet and dry mergers evolve in different senses, and quantify the space densities of these systems. The local space density of wet mergers is essentially identical to the local space density of dry mergers. The evolution in the total merger rate is modest out to z ~ 0.7, although the wet and dry populations have different evolutionary trends. At higher redshifts, dry mergers make a smaller contribution to the total merging galaxy population, but this is offset by a roughly equivalent increase in the contribution from wet mergers. By comparing the mass density function of early-type galaxies to the corresponding mass density function for merging systems, we show that not all the major mergers with the highest masses (M_(stellar) > 10^(11) M_\u2299) will end up with the most massive early-type galaxies, unless the merging timescale is dramatically longer than that usually assumed. On the other hand, the usually assumed merging timescale of ~0.5-1 Gyr is quite consistent with the data if we suppose that only less massive early-type galaxies form via mergers. Since low-intermediate-mass ellipticals are 10-100 times more common than their most massive counterparts, the hierarchical explanation for the origin of early-type galaxies may be correct for the vast majority of early types, even if incorrect for the most massive ones.", "doi": "10.1088/0004-6256/141/3/87", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2011-03", "series_number": "3", "volume": "141", "issue": "3", "pages": "Art. No. 87" }, { "id": "authors:v455w-7jy63", "collection": "authors", "collection_id": "v455w-7jy63", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110125-143537643", "type": "article", "title": "Spitzer infrared spectrometer 16\u03bcm observations of the GOODS fields", "author": [ { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Chary", "given_name": "Ranga", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Elbaz", "given_name": "David", "orcid": "0000-0002-7631-647X", "clpid": "Elbaz-David" }, { "family_name": "Dickinson", "given_name": "Mark", "orcid": "0000-0001-5414-5131", "clpid": "Dickinson-Mark-E" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Colbert", "given_name": "James", "clpid": "Colbert-J-W" }, { "family_name": "Le Floc'h", "given_name": "Emeric", "clpid": "Le-Floc'h-Emeric" }, { "family_name": "Frayer", "given_name": "David T.", "orcid": "0000-0003-1924-1122", "clpid": "Frayer-D-T" }, { "family_name": "Howell", "given_name": "Justin H.", "clpid": "Howell-J-H" }, { "family_name": "Koo", "given_name": "David C.", "orcid": "0000-0003-3385-6799", "clpid": "Koo-David-C" }, { "family_name": "Papovich", "given_name": "Casey", "orcid": "0000-0001-7503-8482", "clpid": "Papovich-C" }, { "family_name": "Phillips", "given_name": "Andrew C.", "clpid": "Phillips-A-C" }, { "family_name": "Scarlata", "given_name": "Claudia", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Siana", "given_name": "Brian", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Spinrad", "given_name": "Hyron", "clpid": "Spinrad-H" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" } ], "abstract": "We present Spitzer 16\u03bcm imaging of the Great Observatories Origins Deep Survey (GOODS) fields. We survey\n150 arcmin^2 in each of the two GOODS fields (North and South), to an average 3\u03c3 depth of 40 and 65 \u03bcJy,\nrespectively. We detect ~1300 sources in both fields combined. We validate the photometry using the 3\u201324\u03bcm\nspectral energy distribution of stars in the fields compared to Spitzer spectroscopic templates. Comparison with\nISOCAM and AKARI observations in the same fields shows reasonable agreement, though the uncertainties are\nlarge. We provide a catalog of photometry, with sources cross-correlated with available Spitzer, Chandra, and\nHubble Space Telescope data. Galaxy number counts show good agreement with previous results from ISOCAM\nand AKARI with improved uncertainties. We examine the 16\u201324\u03bcm flux ratio and find that for most sources it\nlies within the expected locus for starbursts and infrared luminous galaxies. A color cut of S_(16)/S_(24) > 1.4 selects\nmostly sources which lie at 1.1 < z < 1.6, where the 24\u03bcm passband contains both the redshifted 9.7 \u03bcm silicate\nabsorption and the minimum between polycyclic aromatic hydrocarbon emission peaks. We measure the integrated\ngalaxy light of 16\u03bcm sources and find a lower limit on the galaxy contribution to the extragalactic background\nlight at this wavelength to be 2.2 \u00b1 0.2 nW m^(\u22122) sr^(\u22121).", "doi": "10.1088/0004-6256/141/1/1", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2011-01", "series_number": "1", "volume": "141", "issue": "1", "pages": "Art. No. 1" }, { "id": "authors:qyzze-m2659", "collection": "authors", "collection_id": "qyzze-m2659", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101208-091910540", "type": "article", "title": "The WFC3 infrared spectroscopic parallel (WISP) survey", "author": [ { "family_name": "Atek", "given_name": "H.", "orcid": "0000-0002-7570-0824", "clpid": "Atek-H" }, { "family_name": "Malkan", "given_name": "M.", "orcid": "0000-0001-6919-1237", "clpid": "Malkan-M-A" }, { "family_name": "McCarthy", "given_name": "P.", "clpid": "McCarthy-P-J" }, { "family_name": "Teplitz", "given_name": "H. I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Siana", "given_name": "B.", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Henry", "given_name": "A. L.", "orcid": "0000-0002-6586-4446", "clpid": "Henry-A-L" }, { "family_name": "Colbert", "given_name": "J. W.", "clpid": "Colbert-J-W" }, { "family_name": "Ross", "given_name": "N. R.", "clpid": "Ross-N-R" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Bunker", "given_name": "A. J.", "clpid": "Bunker-A-J" }, { "family_name": "Dressler", "given_name": "A.", "clpid": "Dressler-A" }, { "family_name": "Fosbury", "given_name": "R. A. E.", "clpid": "Fosbury-R-A-E" }, { "family_name": "Martin", "given_name": "C.", "clpid": "Martin-Crystal-L" }, { "family_name": "Shim", "given_name": "H.", "clpid": "Shim-H" } ], "abstract": "We present the WFC3 Infrared Spectroscopic Parallel (WISP) Survey. WISP is obtaining slitless, near-infrared grism spectroscopy of ~90 independent, high-latitude fields by observing in the pure-parallel mode with the Wide Field Camera Three on the Hubble Space Telescope for a total of ~250 orbits. Spectra are obtained with the G_(102) (\u03bb = 0.8\u20131.17 \u03bcm, R ~ 210) and G_(141) grisms (\u03bb = 1.11\u20131.67 \u03bcm, R ~ 130), together with direct imaging in the J and H bands (F110W and F140W, respectively). In the present paper, we present the first results from 19 WISP fields, covering approximately 63 arcmin^2. For typical exposure times (~6400 s in G_(102) and ~2700 s in G_(141)), we reach 5\u03c3 detection limits for emission lines of f ~ 5 \u00d7 10^(\u221217) erg s^(\u22121) cm^(\u22122) for compact objects. Typical direct imaging 5\u03c3 limits are 26.3 and 26.1 mag. (AB) in F110W and F140W, respectively. Restricting ourselves to the lines measured with the highest confidence, we present a list of 328 emission lines, in 229 objects, in a redshift range 0.3 < z < 3. The single-line emitters are likely to be a mix of H\u03b1 and [O_III]5007,4959 \u00c5, with H\u03b1 predominating. The overall surface density of high-confidence emission-line objects in our sample is approximately 4 per arcmin^2. These first fields show high equivalent width sources, active galactic nucleus, and post-starburst galaxies. The median observed star formation rate (SFR) of our H\u03b1-selected sample is 4M_\u2299 yr^(\u22121). At intermediate redshifts, we detect emission lines in galaxies as faint as H_(140) ~ 25, or M_R < \u221219, and are sensitive to SFRs down to less than 1M_\u2299 yr^(\u22121). The slitless grisms on WFC3 provide a unique opportunity to study the spectral properties of galaxies much fainter than L^* at the peak of the galaxy assembly epoch.", "doi": "10.1088/0004-637X/723/1/104", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-11-01", "series_number": "1", "volume": "723", "issue": "1", "pages": "104-115" }, { "id": "authors:gp5bc-gg232", "collection": "authors", "collection_id": "gp5bc-gg232", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101217-094158383", "type": "article", "title": "A deep hubble space telescope search for escaping lymna continuum flux at z ~ 1.3: evidence for an evolving ionizing emissivity", "author": [ { "family_name": "Siana", "given_name": "Brian", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Brown", "given_name": "Thomas M.", "orcid": "0000-0002-1793-9968", "clpid": "Brown-T-M" }, { "family_name": "Giavalisco", "given_name": "Mauro", "orcid": "0000-0002-7831-8751", "clpid": "Giavalisco-M" }, { "family_name": "Dickinson", "given_name": "Mark", "orcid": "0000-0001-5414-5131", "clpid": "Dickinson-Mark-E" }, { "family_name": "Chary", "given_name": "Ranga-Ram", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "de Mello", "given_name": "Duilia F.", "clpid": "de-Mello-D-F" }, { "family_name": "Conselice", "given_name": "Christopher J.", "orcid": "0000-0003-1949-7638", "clpid": "Conselice-C-J" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Gardner", "given_name": "Jonathan P.", "clpid": "Gardner-J-P" }, { "family_name": "Colbert", "given_name": "James W.", "clpid": "Colbert-J-W" }, { "family_name": "Scarlata", "given_name": "Claudia", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" } ], "abstract": "We have obtained deep Hubble Space Telescope far-UV images of 15 starburst galaxies at z ~ 1.3 in the GOODS fields to search for escaping Lyman continuum (LyC) photons. These are the deepest far-UV images (m_(AB) = 28.7, 3\u03c3, 1\" diameter) over this large an area (4.83 arcmin^2) and provide some of the best escape fraction constraints\nfor any galaxies at any redshift. We do not detect any individual galaxies, with 3\u03c3 limits to the LyC (~700 \u00c5)\nflux 50\u2013149 times fainter (in f_\u03bd) than the rest-frame UV (1500 \u00c5) continuum fluxes. Correcting for the mean\nintergalactic medium (IGM) attenuation (factor ~2), as well as an intrinsic stellar Lyman break (factor ~3), these\nlimits translate to relative escape fraction limits of f_(esc,rel) < [0.03, 0.21]. The stacked limit is f_(esc,rel)(3\u03c3) < 0.02. We use a Monte Carlo simulation to properly account for the expected distribution of line-of-sight IGM opacities. When including constraints from previous surveys at z ~ 1.3 we find that, at the 95% confidence level, no more than 8% of star-forming galaxies at z ~ 1.3 can have relative escape fractions greater than 0.50. Alternatively, if the majority of galaxies have low, but non-zero, escaping LyC, the escape fraction cannot be more than 0.04. In light of some evidence for strong LyC emission from UV-faint regions of Lyman break galaxies (LBGs) at z ~ 3, we also stack sub-regions of our galaxies with different surface brightnesses and detect no significant LyC flux at the f_(esc,rel) < 0.03 level. Both the stacked limits and the limits from the Monte Carlo simulation suggest that the average ionizing emissivity (relative to non-ionizing UV emissivity) at z ~ 1.3 is significantly lower than has been observed in LBGs at z ~ 3. If the ionizing emissivity of star-forming galaxies is in fact increasing with redshift, it would help to explain the high photoionization rates seen in the IGM at z > 4 and reionization of the IGM at z > 6.", "doi": "10.1088/0004-637X/723/1/241", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-11-01", "series_number": "1", "volume": "723", "issue": "1", "pages": "241-250" }, { "id": "authors:batg1-rw577", "collection": "authors", "collection_id": "batg1-rw577", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100928-121612208", "type": "article", "title": "A Spectroscopic Search for Leaking Lyman Continuum at z ~ 0.7", "author": [ { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Siana", "given_name": "Brian", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Scarlata", "given_name": "Claudia", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Conselice", "given_name": "Christopher J.", "orcid": "0000-0003-1949-7638", "clpid": "Conselice-C-J" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Brown", "given_name": "Thomas M.", "orcid": "0000-0002-1793-9968", "clpid": "Brown-T-M" }, { "family_name": "Salvato", "given_name": "Mara", "orcid": "0000-0001-7116-9303", "clpid": "Salvato-Mara" }, { "family_name": "Rudie", "given_name": "Gwen C.", "orcid": "0000-0002-8459-5413", "clpid": "Rudie-G-C" }, { "family_name": "de Mello", "given_name": "Duilia F.", "clpid": "de-Mello-D-F" }, { "family_name": "Colbert", "given_name": "James", "clpid": "Colbert-J-W" }, { "family_name": "Gardner", "given_name": "Jonathan P.", "clpid": "Gardner-J-P" }, { "family_name": "Giavalisco", "given_name": "Mauro", "orcid": "0000-0002-7831-8751", "clpid": "Giavalisco-M" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" } ], "abstract": "We present the results of rest-frame, UV slitless spectroscopic observations of a sample of 32 z ~ 0.7 Lyman break galaxy (LBG) analogs in the COSMOS field. The spectroscopic search was performed with the Solar Blind Channel on the Hubble Space Telescope. We report the detection of leaking Lyman continuum (LyC) radiation from an active galactic nucleus-starburst composite. While we find no direct detections of LyC emission in the remainder of our sample, we achieve individual lower limits (3\u03c3) of the observed non-ionizing UV-to-LyC flux density ratios, f -\u03bd (1500 \u00c5)/f _\u03bd(830 \u00c5) of 20 to 204 (median of 73.5) and 378.7 for the stack. Assuming an intrinsic Lyman break of 3.4 and an intergalactic medium transmission of LyC photons along the line of sight to the galaxy of 85%, we report an upper limit for the relative escape fraction in individual galaxies of 0.02-0.19 and a stacked 3\u03c3 upper limit of 0.01. We find no indication of a relative escape fraction near unity as seen in some LBGs at z ~ 3. Our UV spectra achieve the deepest limits to date at any redshift for the escape fraction in individual sources. The contrast between these z ~ 0.7 low escape fraction LBG analogs with z ~ 3 LBGs suggests that either the processes conducive to high f esc are not being selected for in the z 1 samples or the average escape fraction is decreasing from z ~ 3 to z ~ 1. We discuss possible mechanisms that could affect the escape of LyC photons", "doi": "10.1088/0004-637X/720/1/465", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-09-01", "series_number": "1", "volume": "720", "issue": "1", "pages": "465-479" }, { "id": "authors:pqp6y-b2w73", "collection": "authors", "collection_id": "pqp6y-b2w73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101123-094918178", "type": "article", "title": "Deep Herschel view of obscured star formation in the Bullet cluster", "author": [ { "family_name": "Rawle", "given_name": "T. D.", "clpid": "Rawle-T-D" }, { "family_name": "Fadda", "given_name": "D.", "orcid": "0000-0002-3698-7076", "clpid": "Fadda-D" }, { "family_name": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "Appleton", "given_name": "P. N.", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "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" } ], "abstract": "We use deep, five band (100\u2013500 \u03bcm) data from the Herschel Lensing Survey (HLS) to fully constrain the obscured star formation rate, SFR_(FIR), of galaxies in the Bullet cluster (z = 0.296), and a smaller background system (z = 0.35) in the same field. Herschel detects 23 Bullet cluster members with a total SFRFIR = 144\u00b114 M_\u2609 yr^(-1). On average, the background system contains brighter far-infrared (FIR) galaxies, with ~50% higher SFRFIR (21 galaxies; 207 \u00b1 9 M_\u2609 yr^(-1)). SFRs extrapolated from 24 \u03bcm flux via recent templates (SFR_(24 \u00b5m)) agree well with SFRFIR for ~60% of the cluster galaxies. In the remaining ~40%, SFR24 \u00b5m underestimates SFR_(FIR) due to a significant excess in observed S_(100)/S_(24) (rest frame S_(75)/S_(18)) compared to templates of the same FIR luminosity.", "doi": "10.1051/0004-6361/201014681", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2010-07-16", "volume": "518", "pages": "L14" }, { "id": "authors:sdd7g-wxj62", "collection": "authors", "collection_id": "sdd7g-wxj62", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-114942947", "type": "article", "title": "The Herschel Lensing Survey (HLS): Overview", "author": [ { "family_name": "Egami", "given_name": "E.", "clpid": "Egami-Eichi" }, { "family_name": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Fadda", "given_name": "D.", "orcid": "0000-0002-3698-7076", "clpid": "Fadda-D" }, { "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": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" } ], "abstract": "The Herschel Lensing Survey (HLS) will conduct deep PACS and SPIRE imaging of \u223c40 massive clusters of galaxies. The strong gravitational lensing power of these clusters will enable us to penetrate through the confusion noise, which sets the ultimate limit on our ability to probe the\nUniverse with Herschel. Here we present an overview of our survey and a summary of the major results from our science demonstration phase (SDP) observations of the Bullet cluster (z = 0.297). The SDP data are rich and allow us to study not only the background high-redshift galaxies\n(e.g., strongly lensed and distorted galaxies at z = 2.8 and 3.2) but also the properties of cluster-member galaxies. Our preliminary analysis shows a great diversity of far-infrared/submillimeter spectral energy distributions (SEDs), indicating that we have much to learn with Herschel about the properties of galaxy SEDs. We have also detected the Sunyaev-Zel'dovich (SZ) effect increment with the SPIRE data. The success of this SDP program demonstrates the great potential of the Herschel Lensing Survey to produce exciting results in a variety of science areas.", "doi": "10.1051/0004-6361/201014696", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2010-07", "volume": "518", "pages": "Art. No. L12" }, { "id": "authors:daxbh-8df73", "collection": "authors", "collection_id": "daxbh-8df73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-100758912", "type": "article", "title": "Improving the identification of high-z Herschel sources with position priors and optical/NIR and FIR/mm photometric redshifts", "author": [ { "family_name": "P\u00e9rez-Gonz\u00e1lez", "given_name": "P. G.", "orcid": "0000-0003-4528-5639", "clpid": "P\u00e9rez-Gonz\u00e1lez-P-G" }, { "family_name": "Blain", "given_name": "A. W.", "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": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Fadda", "given_name": "D.", "orcid": "0000-0002-3698-7076", "clpid": "Fadda-D" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "We present preliminary results about the detection of high redshift (U)LIRGs in the Bullet cluster field by the PACS and SPIRE instruments within the Herschel Lensing Survey (HLS) Program. We describe in detail a photometric procedure designed to recover robust fluxes and deblend faint Herschel sources near the confusion noise. The method is based on the use of the positions of Spitzer/MIPS 24 \u03bcm sources as priors. Our catalogs are able to reliably (5\u03c3) recover galaxies with fluxes above 6 and 10 mJy in the PACS 100 and 160 \u03bcm channels, respectively, and 12 to 18 mJy in the SPIRE bands. We also obtain spectral energy distributions covering the optical through the far-infrared/millimeter spectral ranges of all the Herschel detected sources, and analyze them to obtain independent estimations of the photometric redshift based on either stellar population or dust emission models. We exemplify the potential of the combined use of Spitzer position priors plus independent optical and IR photometric redshifts to robustly assign optical/NIR counterparts to the sources detected by Herschel and other (sub-)mm instruments.", "doi": "10.1051/0004-6361/201014593", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2010-07", "volume": "518", "pages": "L15" }, { "id": "authors:3635g-n3876", "collection": "authors", "collection_id": "3635g-n3876", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100706-101351253", "type": "article", "title": "The Buried Starburst in the Interacting Galaxy II Zw 096 as Revealed by the Spitzer Space Telescope", "author": [ { "family_name": "Inami", "given_name": "H.", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Surace", "given_name": "J. A.", "orcid": "0000-0001-7291-0087", "clpid": "Surace-J-A" }, { "family_name": "Mazzarella", "given_name": "J. M.", "orcid": "0000-0002-8204-8619", "clpid": "Mazzarella-J-M" }, { "family_name": "Evans", "given_name": "A. S.", "orcid": "0000-0003-2638-1334", "clpid": "Evans-A-S" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Howell", "given_name": "J. H.", "clpid": "Howell-J-H" }, { "family_name": "Petric", "given_name": "A.", "orcid": "0000-0003-4030-3455", "clpid": "Petric-A-O" }, { "family_name": "Vavilkin", "given_name": "T.", "clpid": "Vavilkin-T" }, { "family_name": "Iwasawa", "given_name": "K.", "orcid": "0000-0002-4923-3281", "clpid": "Iwasawa-Kazushi" }, { "family_name": "Haan", "given_name": "S.", "clpid": "Haan-S" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Stierwalt", "given_name": "S.", "orcid": "0000-0002-2596-8531", "clpid": "Stierwalt-S" }, { "family_name": "Appleton", "given_name": "P. N.", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Barnes", "given_name": "J. E.", "clpid": "Barnes-J-E" }, { "family_name": "Bothun", "given_name": "G.", "clpid": "Bothus-G" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Chan", "given_name": "B.", "clpid": "Chan-Ben-Hiu-Pan" }, { "family_name": "Charmandaris", "given_name": "V.", "orcid": "0000-0002-2688-1956", "clpid": "Charmandaris-V" }, { "family_name": "Frayer", "given_name": "D. T.", "orcid": "0000-0003-1924-1122", "clpid": "Frayer-D-T" }, { "family_name": "Kewley", "given_name": "L. J.", "orcid": "0000-0001-8152-3943", "clpid": "Kewley-L-J" }, { "family_name": "Kim", "given_name": "D. C.", "clpid": "Kim-D-C" }, { "family_name": "Lord", "given_name": "S.", "clpid": "Lord-S" }, { "family_name": "Madore", "given_name": "B. F.", "orcid": "0000-0002-1576-1676", "clpid": "Madore-B-F" }, { "family_name": "Marshall", "given_name": "J. A.", "orcid": "0000-0001-7712-8465", "clpid": "Marshall-J-A" }, { "family_name": "Matsuhara", "given_name": "H.", "clpid": "Matsuhara-Hideo" }, { "family_name": "Melbourne", "given_name": "J. E.", "clpid": "Melbourne-J-E" }, { "family_name": "Rich", "given_name": "J.", "clpid": "Rich-J" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Spoon", "given_name": "H. W. W.", "orcid": "0000-0002-8712-369X", "clpid": "Spoon-H-W-W" }, { "family_name": "Sturm", "given_name": "E.", "clpid": "Sturm-E" }, { "family_name": "U", "given_name": "V.", "orcid": "0000-0002-1912-0024", "clpid": "U-Vivian" }, { "family_name": "Veilleux", "given_name": "S.", "orcid": "0000-0002-3158-6820", "clpid": "Veilleux-S" }, { "family_name": "Xu", "given_name": "K.", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" } ], "abstract": "An analysis of data from the Spitzer Space Telescope, Hubble Space Telescope, Chandra X-ray Observatory, and AKARI Infrared Astronomy Satellite is presented for the z = 0.036 merging galaxy system II Zw 096 (CGCG 448-020). Because II Zw 096 has an infrared luminosity of log(L_(IR)/L_\u2609) = 11.94, it is classified as a Luminous Infrared Galaxy (LIRG), and was observed as part of the Great Observatories All-sky LIRG Survey (GOALS). The Spitzer data suggest that 80% of the total infrared luminosity comes from an extremely compact, red source not associated with the nuclei of the merging galaxies. The Spitzer mid-infrared spectra indicate no high-ionization lines from a buried active galactic nucleus in this source. The strong detection of the 3.3 \u03bcm and 6.2 \u03bcm polycyclic aromatic hydrocarbon emission features in the AKARI and Spitzer spectra also implies that the energy source of II Zw 096 is a starburst. Based on Spitzer infrared imaging and AKARI near-infrared spectroscopy, the star formation rate is estimated to be 120 M_\u2609 yr^(-1) and >45 M_\u2609 yr^(-1), respectively. Finally, the high-resolution B-, I-, and H-band images show many star clusters in the interacting system. The colors of these clusters suggest at least two populations\u2014one with an age of 1-5 Myr and one with an age of 20-500 Myr, reddened by 0-2 mag of visual extinction. The masses of these clusters span a range between 10^6 and 10^8 M_\u2609. This starburst source is reminiscent of the extranuclear starburst seen in NGC 4038/9 (the Antennae Galaxies) and Arp 299 but approximately an order of magnitude more luminous than the Antennae. The source is remarkable in that the off-nuclear infrared luminosity dominates the entire system.", "doi": "10.1088/0004-6256/140/1/63", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2010-07", "series_number": "1", "volume": "140", "issue": "1", "pages": "63-74" }, { "id": "authors:6b71g-an727", "collection": "authors", "collection_id": "6b71g-an727", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101115-102053323", "type": "article", "title": "First detection of the Sunyaev Zel'dovich effect increment at \u03bb < 650 \u03bcm", "author": [ { "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": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Fadda", "given_name": "D.", "orcid": "0000-0002-3698-7076", "clpid": "Fadda-D" } ], "abstract": "The Sunyaev-Zel'dovich (SZ) effect is a spectral distortion of the cosmic microwave background as observed through the hot plasma in galaxy clusters. This distortion is a decrement in the CMB intensity for \u03bb > 1.3 mm, an increment at shorter wavelengths, and small again by \u03bb ~ 250 \u03bcm. As part of the Herschel Lensing Survey (HLS) we have mapped 1E0657\u201356 (the Bullet cluster) with SPIRE with bands centered at 250, 350 and 500 \u03bcm and have detected the SZ effect at the two longest wavelengths. The measured SZ effect increment central intensities are \u0394I_0 = 0.097 \u00b1 0.019 MJy\u2009sr^(-1) at 350 \u03bcm and \u0394I_0 = 0.268 \u00b1 0.031 MJy\u2009sr^(-1) at 500 \u03bcm, consistent with the SZ effect spectrum derived from previous measurements at 2 mm. No other diffuse emission is detected. The presence of the finite temperature SZ effect correction is preferred by the SPIRE data at a significance of 2.1\u03c3, opening the possibility that the relativistic SZ effect correction can be constrained by SPIRE in a sample of clusters. The results presented here have important ramifications for both sub-mm measurements of galaxy clusters and blank field surveys with SPIRE.", "doi": "10.1051/0004-6361/201014685", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2010-07", "volume": "518", "pages": "Art. No. L16" }, { "id": "authors:3kmgg-b9731", "collection": "authors", "collection_id": "3kmgg-b9731", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101118-114636998", "type": "article", "title": "The far-infrared/submillimeter properties of galaxies located behind the Bullet cluster", "author": [ { "family_name": "Rex", "given_name": "M.", "clpid": "Rex-M" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "Fadda", "given_name": "D.", "orcid": "0000-0002-3698-7076", "clpid": "Fadda-D" }, { "family_name": "Blain", "given_name": "A. W.", "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": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" } ], "abstract": "The Herschel Lensing Survey (HLS) takes advantage of gravitational lensing by massive galaxy clusters to sample a population of high-redshift galaxies which are too faint to be detected above the confusion limit of current far-infrared/submillimeter telescopes. Measurements from 100\u2013500 \u03bcm bracket the peaks of the far-infrared spectral energy distributions of these galaxies, characterizing their infrared luminosities and star formation rates. We introduce initial results from our science demonstration phase observations, directed toward the Bullet cluster (1E0657-56). By combining our observations with LABOCA 870 \u03bcm and AzTEC 1.1 mm data we fully constrain the spectral energy distributions of 19 MIPS 24 \u03bcm-selected galaxies which are located behind the cluster. We find that their colors are best fit using templates based on local galaxies with systematically lower infrared luminosities. This suggests that our sources are not like local ultra-luminous infrared galaxies in which vigorous star formation is contained in a compact highly dust-obscured region. Instead, they appear to be scaled up versions of lower luminosity local galaxies with star formation occurring on larger physical scales.", "doi": "10.1051/0004-6361/201014693", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2010-07", "volume": "518", "pages": "L13" }, { "id": "authors:4qw15-jhb97", "collection": "authors", "collection_id": "4qw15-jhb97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100527-152554021", "type": "article", "title": "The Great Observatories All-sky LIRG Survey: Comparison of Ultraviolet and Far-infrared Properties", "author": [ { "family_name": "Howell", "given_name": "Justin H.", "clpid": "Howell-J-H" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Mazzarella", "given_name": "Joseph M.", "orcid": "0000-0002-8204-8619", "clpid": "Mazzarella-J-M" }, { "family_name": "Evans", "given_name": "Aaron S.", "orcid": "0000-0003-2638-1334", "clpid": "Evans-A-S" }, { "family_name": "Surace", "given_name": "Jason A.", "orcid": "0000-0001-7291-0087", "clpid": "Surace-J-A" }, { "family_name": "Sanders", "given_name": "David B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Petric", "given_name": "Andreea", "orcid": "0000-0003-4030-3455", "clpid": "Petric-A-O" }, { "family_name": "Appleton", "given_name": "Philip", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Bothun", "given_name": "Greg", "clpid": "Bothun-G" }, { "family_name": "Bridge", "given_name": "Carrie", "clpid": "Bridge-C-R" }, { "family_name": "Chan", "given_name": "Ben H. P.", "clpid": "Chan-Ben-Hiu-Pan" }, { "family_name": "Charmandaris", "given_name": "Vassilis", "orcid": "0000-0002-2688-1956", "clpid": "Charmandaris-V" }, { "family_name": "Frayer", "given_name": "David T.", "orcid": "0000-0003-1924-1122", "clpid": "Frayer-D-T" }, { "family_name": "Haan", "given_name": "Sebastian", "clpid": "Haan-S" }, { "family_name": "Inami", "given_name": "Hanae", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" }, { "family_name": "Kim", "given_name": "Dong-Chan", "clpid": "Kim-Dong-Chan" }, { "family_name": "Lord", "given_name": "Steven D.", "clpid": "Lord-S-D" }, { "family_name": "Madore", "given_name": "Barry F.", "orcid": "0000-0002-1576-1676", "clpid": "Madore-B-F" }, { "family_name": "Melbourne", "given_name": "Jason", "clpid": "Melbourne-J-L" }, { "family_name": "Schulz", "given_name": "Bernhard", "clpid": "Schulz-B" }, { "family_name": "U", "given_name": "Vivian", "orcid": "0000-0002-1912-0024", "clpid": "U-Vivian" }, { "family_name": "Vavilkin", "given_name": "Tatjana", "clpid": "Vavilkin-T" }, { "family_name": "Veilleux", "given_name": "Sylvain", "orcid": "0000-0002-3158-6820", "clpid": "Veilleux-S" }, { "family_name": "Xu", "given_name": "Kevin", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" } ], "abstract": "The Great Observatories All-sky LIRG Survey (GOALS) consists of a complete sample of 202 luminous infrared galaxies (LIRGs) selected from the IRAS Revised Bright Galaxy Sample (RBGS). The galaxies span the full range of interaction stages, from isolated galaxies to interacting pairs to late stage mergers. We present a comparison of the UV and infrared properties of 135 galaxies in GOALS observed by GALEX and Spitzer. For interacting galaxies with separations greater than the resolution of GALEX and Spitzer (~2\"-6\"), we assess the UV and IR properties of each galaxy individually. The contribution of the FUV to the measured star formation rate (SFR) ranges from 0.2% to 17.9%, with a median of 2.8% and a mean of 4.0% \u00b1 0.4%. The specific star formation rate (SSFR) of the GOALS sample is extremely high, with a median value (3.9 \u00d7 10^(\u201310) yr^(\u20131)) that is comparable to the highest SSFRs seen in the Spitzer Infrared Nearby Galaxies Survey sample. We examine the position of each galaxy on the IR excess-UV slope (IRX-\u03b2) diagram as a function of galaxy properties, including IR luminosity and interaction stage. The LIRGs on average have greater IR excesses than would be expected based on their UV colors if they obeyed the same relations as starbursts with L_(IR) < 10^(11) L_\u2609 or normal late-type galaxies. The ratio of L_(IR) to the value one would estimate from the IRX-\u03b2 relation published for lower luminosity starburst galaxies ranges from 0.2 to 68, with a median value of 2.7. A minimum of 19% of the total IR luminosity in the RBGS is produced in LIRGs and ultraluminous infrared galaxies with red UV colors (\u03b2>0). Among resolved interacting systems, 32% contain one galaxy which dominates the IR emission while the companion dominates the UV emission. Only 21% of the resolved systems contain a single galaxy which dominates both wavelengths.", "doi": "10.1088/0004-637X/715/1/572", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-05-20", "series_number": "1", "volume": "715", "issue": "1", "pages": "572-588" }, { "id": "authors:w3ahs-m0b11", "collection": "authors", "collection_id": "w3ahs-m0b11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100210-104549065", "type": "article", "title": "The CFHTLS-Deep Catalog of Interacting Galaxies. I. Merger Rate Evolution to z = 1.2", "author": [ { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Carlberg", "given_name": "R. G.", "clpid": "Carlberg-R-G" }, { "family_name": "Sullivan", "given_name": "M.", "orcid": "0000-0001-9053-4820", "clpid": "Sullivan-Mark" } ], "abstract": "We present the rest-frame optical galaxy merger fraction between 0.2 < z < 1.2, as a function of stellar mass and optical luminosity, as observed by the Canada-France-Hawaii Telescope Legacy Deep Survey (CFHTLS-Deep). We developed a new classification scheme to identify major galaxy-galaxy mergers based on the presence of tidal tails and bridges. These morphological features are signposts of recent and ongoing merger activity. Through the visual classification of all galaxies, down to i_(vega) \u2264 22.2 (\u224827,000 galaxies) over 2 square degrees, we have compiled the CFHTLS-Deep Catalog of Interacting Galaxies, with \u22481600 merging galaxies. We find the merger fraction to be 4.3% \u00b1 0.3% at z ~ 0.3 and 19.0% \u00b1 2.5% at z ~ 1, implying evolution of the merger fraction going as (1 + z)^m , with m = 2.25 \u00b1 0.24. This result is inconsistent with a mild or non-evolving (m < 1.5) scenario at a \u22734\u03c3 level of confidence. A mild trend, where by massive galaxies with M_*>10^(10.7) M_\u2609 are undergoing fewer mergers than less massive systems (M_* ~ 10^(10) M_\u2609), consistent with the expectations of galaxy assembly downsizing is observed. Our results also show that interacting galaxies have on average SFRs double that found in non-interacting field galaxies. We conclude that (1) the optical galaxy merger fraction does evolve with redshift, (2) the merger fraction depends mildly on stellar mass, with lower mass galaxies having higher merger fractions at z < 1, and (3) star formation is triggered at all phases of a merger, with larger enhancements at later stages, consistent with N-body simulations.", "doi": "10.1088/0004-637X/709/2/1067", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-02-01", "series_number": "2", "volume": "709", "issue": "2", "pages": "1076-1082" }, { "id": "authors:w2ffa-c9510", "collection": "authors", "collection_id": "w2ffa-c9510", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091209-113002302", "type": "article", "title": "He II Emission in Ly\u03b1 Nebulae: Active Galactic Nucleus or Cooling Radiation?", "author": [ { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Colbert", "given_name": "J.", "clpid": "Colbert-J-W" }, { "family_name": "Teplitz", "given_name": "H. I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" }, { "family_name": "Francis", "given_name": "P.", "clpid": "Francis-Paul-J" }, { "family_name": "Palunas", "given_name": "P.", "clpid": "Palunas-Povilas" }, { "family_name": "Siana", "given_name": "B.", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Williger", "given_name": "G. M.", "clpid": "Williger-G-M" }, { "family_name": "Woodgate", "given_name": "B.", "clpid": "Woodgate-Bruce-E" } ], "abstract": "We present a study of an extended Ly\u03b1 nebula located in a known overdensity at z ~ 2.38. The data include multiwavelength photometry covering the rest-frame spectral range from 0.1 to 250 \u03bcm, and deep optical spectra of the sources associated with the extended emission. Two galaxies are associated with the Ly\u03b1 nebula. One of them is a dust enshrouded active galactic nucleus (AGN), while the other is a powerful starburst, forming stars at \u2273400 M_\u2609 yr^(\u20131). We detect the He II emission line at 1640 \u00c5 in the spectrum of the obscured AGN, but detect no emission from other highly ionized metals (C IV or N V) as is expected from an AGN. One scenario that simultaneously reproduces the width of the detected emission lines, the lack of C IV emission, and the geometry of the emitting gas, is that the He II and the Ly\u03b1 emission are the result of cooling gas that is being accreted on the dark matter halo of the two galaxies, Ly1 and Ly2. Given the complexity of the environment associated with our Ly\u03b1 nebula it is possible that various mechanisms of excitation are at work simultaneously.", "doi": "10.1088/0004-637X/706/2/1241", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-12-01", "series_number": "2", "volume": "706", "issue": "2", "pages": "1241-1252" }, { "id": "authors:5zntm-nrk26", "collection": "authors", "collection_id": "5zntm-nrk26", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091104-113041493", "type": "article", "title": "The Effect of Dust Geometry on the Ly\u03b1 Output of Galaxies", "author": [ { "family_name": "Scarlata", "given_name": "C.", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-C-M" }, { "family_name": "Colbert", "given_name": "J.", "clpid": "Colbert-J-W" }, { "family_name": "Teplitz", "given_name": "H. I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Panagia", "given_name": "N.", "clpid": "Panagia-N" }, { "family_name": "Hayes", "given_name": "M.", "clpid": "Hayes-M" }, { "family_name": "Siana", "given_name": "B.", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Rau", "given_name": "A.", "orcid": "0000-0001-5990-6243", "clpid": "Rau-A" }, { "family_name": "Francis", "given_name": "P.", "clpid": "Francis-Paul-J" }, { "family_name": "Caon", "given_name": "A.", "clpid": "Caon-A" }, { "family_name": "Pizzella", "given_name": "A.", "clpid": "Pizzella-A" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C-R" } ], "abstract": "We present the optical spectroscopic follow-up of 31 z = 0.3 Ly\u03b1 emitters, previously identified by Deharveng et al. We find that 17% of the Ly\u03b1 emitters have line ratios that require the hard ionizing continuum produced by an active galactic nucleus. The uniform dust screen geometry traditionally used in studies similar to ours is not able to simultaneously reproduce the observed high Ly\u03b1/H\u03b1 and H\u03b1/H\u03b2 line ratios. We consider different possibilities for the geometry of the dust around the emitting sources. We find that also a uniform mixture of sources and dust does not reproduce the observed line ratios. Instead, these are well reproduced by a clumpy dust screen. This more realistic treatment of the geometry results in extinction corrected (Ly\u03b1/H\u03b1) C values consistent with case B recombination theory, whereas a uniform dust screen model would imply values (Ly\u03b1/H\u03b1) C higher than 8.7. Our analysis shows that there is no need to invoke ad hoc multiphase media in which the Ly\u03b1 photons only scatter between the dusty clouds and eventually escape", "doi": "10.1088/0004-637X/704/2/L98", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2009-10-20", "series_number": "2", "volume": "704", "issue": "2", "pages": "L98-L102" }, { "id": "authors:1fn5m-06447", "collection": "authors", "collection_id": "1fn5m-06447", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090828-145425289", "type": "article", "title": "Expanding the Search for Galaxies at z ~ 7-10 with New NICMOS Parallel Fields", "author": [ { "family_name": "Henry", "given_name": "Alaina L.", "orcid": "0000-0002-6586-4446", "clpid": "Henry-A-L" }, { "family_name": "Siana", "given_name": "Brian", "orcid": "0000-0002-4935-9511", "clpid": "Siana-Brian-D" }, { "family_name": "Malkan", "given_name": "Matthew A.", "orcid": "0000-0001-6919-1237", "clpid": "Malkan-M-A" }, { "family_name": "Ashby", "given_name": "Matthew L. N.", "orcid": "0000-0002-3993-0745", "clpid": "Ashby-M-L-N" }, { "family_name": "Bridge", "given_name": "Carrie R.", "clpid": "Bridge-C-R" }, { "family_name": "Chary", "given_name": "Ranga-Ram", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Colbert", "given_name": "James W.", "clpid": "Colbert-J-W" }, { "family_name": "Giavalisco", "given_name": "Mauro", "orcid": "0000-0002-7831-8751", "clpid": "Giavalisco-M" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "McCarthy", "given_name": "Patrick J.", "clpid": "McCarthy-P-J" } ], "abstract": "We have carried out a search for galaxies at z ~ 7-10 in ~14.4 arcmin^2 of new NICMOS parallel imaging taken in the Great Observatories Origins Deep Survey (5.9 arcmin^2), the Cosmic Origins Survey (7.2 arcmin^2), and SSA22 (1.3 arcmin^2). These images reach 5\u03c3 sensitivities of J_(110) = 26.0-27.5 (AB), and combined they increase the amount of deep near-infrared data by more than 60% in fields where the investment in deep optical data has already been made. We find no z > 7 candidates in our survey area, consistent with the Bouwens et al. measurements at z ~ 7 and 9 (over 23 arcmin^2), which predict 0.7 galaxies at z ~ 7 and <0.03 galaxies at z ~ 9. We estimate that 10%-20% of z > 7 galaxies are missed by this survey, due to incompleteness from foreground contamination by faint sources. For the case of luminosity evolution, assuming a Schecter parameterization with a typical \u03a6_* = 10^(\u20133) Mpc^(\u20133), we find M^*> \u2013 20.0 for z ~ 7 and M^*> \u2013 20.7 for z ~ 9 (68% confidence). This suggests that the downward luminosity evolution of Lyman break galaxies continues to z ~ 7, although our result is marginally consistent with the z ~ 6 luminosity function of Bouwens et al. In addition, we present newly acquired deep MMT/Megacam imaging of the z ~ 9 candidate JD2325+1433, first presented in Henry et al. The resulting weak but significant detection at i' indicates that this galaxy is most likely an interloper at z ~ 2.7.", "doi": "10.1088/0004-637X/697/2/1128", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-06-01", "series_number": "2", "volume": "697", "issue": "2", "pages": "1128-1137" }, { "id": "authors:svwjs-8ey12", "collection": "authors", "collection_id": "svwjs-8ey12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091026-143517879", "type": "article", "title": "The Role of Galaxy Interactions and Mergers in Star Formation at z \u2264 1.3: Mid-Infrared Properties in the Spitzer First Look Survey", "author": [ { "family_name": "Bridge", "given_name": "C. R.", "clpid": "Bridge-C-R" }, { "family_name": "Appleton", "given_name": "P. N.", "orcid": "0000-0002-7607-8766", "clpid": "Appleton-P-N" }, { "family_name": "Conselice", "given_name": "C. J.", "orcid": "0000-0003-1949-7638", "clpid": "Conselice-C-J" }, { "family_name": "Choi", "given_name": "P. I.", "clpid": "Choi-Philip-I" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Fadda", "given_name": "D.", "orcid": "0000-0002-3698-7076", "clpid": "Fadda-Dario" }, { "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": "Carlberg", "given_name": "R. G.", "clpid": "Carlberg-R-G" }, { "family_name": "Helou", "given_name": "G.", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Yan", "given_name": "L.", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "By combining the 0.12 deg2 F814W Hubble Space Telescope (HST) and Spitzer MIPS 24 \u03bcm imaging in the First Look Survey (FLS), we investigate the properties of interacting and merging mid-infrared bright and faint sources at 0.2 \u2264 z \u2264 1.3. We find a marginally significant increase in the pair fraction for MIPS 24 \u03bcm detected, optically selected close pairs, with a pair fraction of 0.25 \u00b1 0.10 at z ~ 1, in contrast to 0.11 \u00b1 0.08 at z ~ 0.4, while galaxies below our 24 \u03bcm MIPS detection limit show a pair fraction consistent with zero at all redshifts. In addition, 24 \u03bcm detected galaxies with fluxes \u2265 0.1 mJy are on average 5 times more likely to be in a close galaxy pair in the range 0.2 \u2264 z \u2264 1.3 than galaxies below this flux limit. Using the 24 \u03bcm flux to derive the total far-IR luminosity, we find that paired galaxies (early-stage mergers) are responsible for 27% \u00b1 9% of the IR luminosity density resulting from star formation at z ~ 1, while morphologically classified (late stage) mergers make up 34% \u00b1 11%. This implies that 61% \u00b1 14% of the infrared luminosity density and, in turn, ~40% of the star formation rate density at z ~ 1 can be attributed to galaxies at some stage of a major merger or interaction. We argue that close pairs/mergers in a LIRG/ULIRG phase become increasingly important contributors to the IR luminosity and star formation rate density of the universe at z > 0.7.", "doi": "10.1086/512029", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2007-04-20", "series_number": "2", "volume": "659", "issue": "2", "pages": "931-940" } ]