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101. The discovery of ERO counterparts to faint submillimetre galaxies

Author: Amy J. Barger, L. L. Cowie, Ian Smail, Frazer N. Owen, Jean-Paul Kneib, G. E. Morrison, Andrew Blain, and Rob Ivison
Subjects: Physics, education.field_of_study, Spiral galaxy, Star formation, media_common.quotation_subject, Spectral properties, Population, Astronomy and Astrophysics, Astrophysics, Universe, Galaxy, Redshift, Space and Planetary Science, Hubble space telescope, education, media_common
Abstract: We have used deep ground-based imaging in the near-infrared to search for counterparts to the luminous submillimeter (submm) sources in the catalog of Smail et al. (1998). For the majority of the submm sources the near-IR imaging supports the counterparts originally selected from deep optical images. However, in two cases (10% of the sample) we find a relatively bright near-IR source close to the submm position, sources that were unidentified in the deep Hubble Space Telescope (HST) and groundbased R-band images used in Smail et al. (1998). We place limits on colours of these sources from deep high-resolution KeckII imaging and find they have 2-� limits of (I K) > � 6.8 and (I K) > 6.0 respectively. Both sources thus class as extremely red objects (EROs). Using the spectral properties of the submm source in the radio and submm we argue that these EROs are probably the source of the submm emission, rather than the bright spiral galaxies previously identified by Smail et al. (1998). This connection provides important insights into the nature of the enigmatic ERO population and faint submm galaxies in general. From the estimated surface density of these submm-bright EROs we suggest that this class accounts for the majority of the reddest members of the ERO population, in good agreement with the preliminary conclusions of pointed submm observations of individual EROs. We conclude that the most extreme EROs represent a population of dusty, ultraluminous galaxies at high redshifts; further study of these will provide useful insights into the nature of star formation in obscured galaxies in the early Universe. The identification of similar counterparts in blank field submm surveys will be extremely difficult owing to their faintness (K � 20.5, I > 26.5). Finally, we discuss the radio and submm properties of the two submm-bright EROs discovered here and suggest that both galaxies lie at z > � 2.
Published: 1999
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102. Molecular Gas in the [CLC][ITAL]z[/ITAL][/CLC] = 2.565 Submillimeter Galaxy SMM J14011+0252

Author: N. Z. Scoville, David T. Frayer, Ian Smail, Jean-Paul Kneib, Andrew Blain, Rob Ivison, Aaron S. Evans, Amy J. Barger, and Min S. Yun
Subjects: High rate, Physics, Space and Planetary Science, Elliptical galaxy, Astronomy and Astrophysics, Optical identification, Astrophysics, Galaxy, Redshift
Abstract: We report the detection of CO(3-2) emission from the submillimeter-selected luminous galaxy SMM J14011+0252. The optical counterpart of the submillimeter source has been identified as a merger system with spectral characteristics consistent with a starburst at z=2.565. The CO emission confirms the optical identification of the submillimeter source and implies a molecular gas mass of 5x10^{10}h_{75}^{-2} M(sun), after correcting for a lensing amplification factor of 2.75. The large molecular gas mass and the radio emission are consistent with the starburst interpretation of the source. These results are similar to those found for SMM J02399-0136, which was the first submillimeter selected CO source found at high redshift. The CO detections of these two high-redshift submillimeter galaxies suggest the presence of massive reservoirs of molecular gas which is consistent with the inferred high rates of star-formation (1000 M(sun)/yr). These two systems appear to be associated with merger events which may evolve into present day luminous elliptical galaxies.
Published: 1999
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103. [Untitled]

Author: Andrew Blain
Subjects: Physics, Luminous infrared galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift survey, Galaxy, Redshift, Cosmology, Luminosity, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, James Clerk Maxwell Telescope, Cosmic dust
Abstract: A class of extremely luminous high-redshift galaxies has recently been detected in unbiased submillimetre-wave surveys using the Submillimetre Common-User Bolometer Array (SCUBA) camera at the James Clerk Maxwell Telescope. Most of the luminosity of these galaxies is emitted from warm interstellar dust grains, and they could be the high-redshift counterparts of the low-redshift ultraluminous infrared galaxies (ULIRGs). Only one - SMM J02399-0136 - has yet been studied in detail. Three other very luminous high-redshift dusty galaxies with well determined spectral energy distributions in the mid-infrared waveband are known - IRAS F10214+4724, H1413+117 and APM 08279+5255. These were detected serendipitously rather than in unbiased surveys, and are all gravitationally lensed by a foreground galaxy. Two - H 1413+117 and APM 08279+5255 - appear to emit a significantly greater fraction of their luminosity in the mid-infrared waveband as compared with both low-redshift ULIRGs and high-redshift submillimetre-selected galaxies. This can be explained by a systematically greater lensing magnification of hotter regions of the source as compared with cooler regions: differential magnification. This effect can confuse the interpretation of the properties of distant ultraluminous galaxies that are lensed by intervening galaxies, but offers a possible way to investigate the temperature distribution of dust in their nuclei on scales of tens of parsecs.
Published: 1999
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104. [Untitled]

Author: Andrew Blain, Ian Smail, Jean-Paul Kneib, and Rob Ivison
Subjects: Physics, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Current (fluid), Cosmology
Published: 1999
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105. [Untitled]

Author: Ian Smail, Jean-Paul Kneib, David T. Frayer, Rob Ivison, and Andrew Blain
Subjects: Physics, Space and Planetary Science, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics, Cosmology, Galaxy, Universe, media_common
Abstract: We discuss observations of the submm-selected galaxy,SMM J02399-0136, and what has been learnt about it during the yearfollowing its discovery. SMM J02399-0136 was the first distantgalaxy detected in surveys with the Submm Common-User Bolometer Array(SCUBA). Its association with a massive, gas-rich starburst/AGN atz = 2.8 has lead to suggestions that the prevalence of AGN in theearly Universe may be high (Ivison et al. 1998) and that these AGNmay account for a significant fraction of the far-IR background (e.g.Fixsen et al. 1998).
Published: 1999
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106. Faint Submillimeter Galaxies: [ITAL]Hubble Space Telescope[/ITAL] Morphologies and Colors

Author: Ian Smail, Rob Ivison, Andrew Blain, and J. P. Kneib
Subjects: Physics, education.field_of_study, Star formation, media_common.quotation_subject, Population, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Universe, Redshift, Space and Planetary Science, Galaxy formation and evolution, education, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We present optical morphologies obtained from deep HST and ground-based images for galaxies selected from the first sub-millimeter survey of the distant Universe. Our sample comprises galaxies detected in deep 850-micron continuum maps of seven massive clusters, obtained using SCUBA, the new bolometer camera on the JCMT. The survey covers a total area of 0.01 square degrees to 1-sigma noise levels of about 2 mJy/beam. We detect a total of 25 sources at 850 microns, of which 17 and 10 are brighter than the respective 50% and 80% completeness limits. Optical counterparts are identified for 14 of the 16 sources in the f(50%) sample and for 9 of the 10 sources in the f(80%) sample that lie within our optical fields. The morphologies of those galaxies for which we have HST imaging fall into three broad categories: faint disturbed galaxies and interactions; faint galaxies too compact to classify reliably; and dusty, star-forming galaxies at intermediate redshifts. The disturbed and interacting galaxies constitute the largest class, which suggests that interactions remain an important mechanism for triggering star formation and the formation of ultraluminous galaxies in the distant Universe. The faint, compact galaxies may represent a later evolutionary stage in these mergers, or more centrally-concentrated starbursts. It is likely that some of these will host AGN. Analysis of the colors of our sample allow us to estimate a crude redshift distribution: >75% have z 50% lie at z
Published: 1998
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107. Molecular Gas in the [CLC][ITAL]z[/ITAL][/CLC] = 2.8 Submillimeter Galaxy SMM 02399−0136

Author: Min S. Yun, Rob Ivison, Ian Smail, Jean-Paul Kneib, N. Z. Scoville, David T. Frayer, Andrew Blain, and Aaron S. Evans
Subjects: Physics, education.field_of_study, Infrared, Star formation, media_common.quotation_subject, Population, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Luminosity, Space and Planetary Science, Sky, Astrophysics::Solar and Stellar Astrophysics, education, Astrophysics::Galaxy Astrophysics, media_common
Abstract: We report the detection of CO(3-2) emission from the submillimeter-selected hyperluminous galaxy SMM 02399-0136. This galaxy is the brightest source detected in the recent SCUBA surveys of the submillimeter sky. The optical counterpart of the submillimeter source has been identified as a narrow-line AGN/starburst galaxy at z=2.8. The CO emission is unresolved, theta < 5 arcsec, and is coincident in redshift and position with the optical counterpart. The molecular gas mass derived from the CO observations is 8x10^{10} h_{75}^{-2} M_{sun}, after correcting for a lensing amplification factor of 2.5. The large CO luminosity suggests that a significant fraction of the infrared luminosity of SMM 02399-0136 arises from star formation. The high inferred star-formation rate of 10^{3} M_{sun}/yr and the large gaseous reservoir may suggest that we are seeing the formation phase of a massive galaxy. Future CO observations of other galaxies detected in deep submillimeter surveys will test the generality of these conclusions for the bulk of the faint submillimeter population.
Published: 1998
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108. Gravitational lensing by spiral galaxies

Author: Andrew Blain and Ole Möller
Subjects: Physics, 010308 nuclear & particles physics, Dark matter, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Dark matter halo, Barred spiral galaxy, Space and Planetary Science, 0103 physical sciences, Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, Interacting galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Galaxy rotation curve
Abstract: We investigate lensing by spiral galaxy disks in dark matter halos and study the effect of the disk on the cross sections for both the formation of multiple images and high magnifications, using a numerical simulation. We present an outline of the methods used and discuss in detail the effect of lens parameters, the inclination angle of the disk and the disk to halo mass ratio.
Published: 1998
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109. A hyperluminous galaxy at z = 2.8 found in a deep submillimetre survey

Author: J. F. Le Borgne, Jean-Paul Kneib, Andrew Blain, Rob Ivison, John K. Davies, Ian Smail, J. Bezecourt, and T. Kerr
Subjects: Physics, Active galactic nucleus, media_common.quotation_subject, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Redshift, Universe, Luminosity, Space and Planetary Science, Emission spectrum, Energy source, Line (formation), media_common
Abstract: We present a detailed study of SMM 02399-0136, a hyperluminous, active galaxy selected from a sub-mm survey of the distant Universe. This galaxy is the brightest source in the fields of seven rich, lensing clusters - total area 0.01 deg^2 - that we have mapped with a sensitivity of ~2 mJy/bm at 850um. We identify a compact optical counterpart with B ~ 23 and a LSB companion 3" away. Our spectroscopy shows that components have the same redshift; z = 2.803 +/- 0.003. The emission lines widths, FWHM ~ 1000-1500 km/s, and line ratios, along with the compact morphology and high luminosity (M_B ~ -24.0) of the galaxy indicate that SMM 02399-0136 contains a rare dust-embedded, narrow-line or type-2 AGN. The source is lensed by the foreground cluster, amplifying its apparent luminosity by a factor of 2.5. Taking this into account, we estimate that SMM 02399-0136 is five times more luminous than F10214+4724. Its far-IR and H-alpha luminosities and LSB radio emission are indicative of an extremely high SFR - several thousand Mo/yr. This assumes that a starburst is the dominant source of energy, but we cannot yet determine the relative contributions of the starburst and the buried AGN. A dust mass of 5-7 x 10^8 Mo is indicated by our data for T(dust) ~ 40-50K, independent of whether the dominant energy source is an AGN or a starburst. We estimate the possible space density of such luminous sub-mm sources and find that while a very large population of these obscured sources could be detected in future wide-field sub-mm surveys, they are unlikely to dominate the faint counts in this waveband. Galaxies such as SMM 02399-0136 and F10214+4724 cannot be easily detected in conventional AGN/QSO surveys, and so estimates of the prevalence of AGN in the early Universe may require significant revision., Comment: 11 pages, 5 figures. Accepted for MNRAS. Full survey discussed briefly
Published: 1998
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110. High-redshift star formation in the Hubble Deep Field revealed by a submillimetre-wavelength survey

Author: Walter Kieran Gear, John A. Peacock, P. Goldschmidt, Steve Serjeant, Robert G. Mann, Rob Ivison, James Dunlop, Andreas Efstathiou, Malcolm S. Longair, Tim Jenness, David P. Hughes, Seb Oliver, Andy Lawrence, Michael Rowan-Robinson, and Andrew Blain
Subjects: Physics, Brightness, Multidisciplinary, Star formation, Hubble Deep Field, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Sky, Source counts, Astrophysics::Galaxy Astrophysics, James Clerk Maxwell Telescope, media_common
Abstract: The advent of sensitive sub-mm array cameras now allows a proper census of dust-enshrouded massive star-formation in very distant galaxies, previously hidden activity to which even the faintest optical images are insensitive. We present the deepest sub-mm survey of the sky to date, taken with the SCUBA camera on the James Clerk Maxwell Telescope and centred on the Hubble Deep Field. The high source density found in this image implies that the survey is confusion-limited below a flux density of 2 mJy. However, within the central 80 arcsec radius independent analyses yield 5 reproducible sources with S(850um) > 2 mJy which simulations indicate can be ascribed to individual galaxies. We give positions and flux densities for these, and furthermore show using multi-frequency photometric data that the brightest sources in our map lie at redshifts z~3. These results lead to integral source counts which are completely inconsistent with a no-evolution model, and imply that massive star-formation activity continues at redshifts > 2. The combined brightness of the 5 most secure sources in our map is sufficient to account for 30 - 50% of the previously unresolved sub-mm background, and we estimate statistically that the entire background is resolved at about the 0.3 mJy level. Finally we discuss possible optical identifications and redshift estimates for the brightest sources. One source appears to be associated with an extreme starburst galaxy at z~1, whilst the remaining four appear to lie in the redshift range 2 < z < 4. This implies a star-formation density over this redshift range that is at least five times higher than that inferred from the ultraviolet output of HDF galaxies.
Published: 1998
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111. The Planck Surveyor mission and gravitational lenses

Author: Andrew Blain
Subjects: Physics, Astrophysics (astro-ph), Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Gravitation, symbols.namesake, Interferometry, Space and Planetary Science, Observational cosmology, Physics::Space Physics, symbols, Millimeter, Planck, Astrophysics::Galaxy Astrophysics
Abstract: An extremely sensitive all-sky survey will be carried out in the millimetre/submillimetre waveband by the forthcoming ESA mission Planck Surveyor. The main scientific goal of the mission is to make very accurate measurements of the spatial power spectrum of primordial anisotropies in the cosmic microwave background radiation; however, hundreds of thousands of distant dusty galaxies and quasars will also be detected. These sources are much more likely to be gravitationally lensed by intervening galaxies as compared with sources discovered in surveys in other wavebands. Here the number of lenses expected in the survey is estimated, and techniques for discriminating between lensed and unlensed sources are discussed. A practical strategy for this discrimination is presented, based on exploiting the remarkable sensitivity and resolving power of large ground-based millimetre/submillimetre-wave interferometer arrays. More than a thousand gravitational lenses could be detected: a sample that would be an extremely valuable resource in observational cosmology., 6 pages, 3 single-frame figures, 2 double-frame figures, to be published in MNRAS
Published: 1998
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112. Rapid growth of black holes in massive star-forming galaxies

Author: Franz E. Bauer, Andrew Blain, Ian Smail, David M. Alexander, Rob Ivison, W. N. Brandt, and Scott Chapman
Subjects: Evolution, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Bright, General Relativity and Quantum Cosmology, Field North Survey, QSO, Binary black hole, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, Active galactic nuclei, Supermassive black hole, Multidisciplinary, Astrophysics (astro-ph), Scuba galaxies, Astronomy, Quasar, Redshift, Intermediate-mass black hole, Elliptical galaxy, Stellar black hole
Abstract: The tight relationship between the masses of black holes and galaxy spheroids in nearby galaxies implies a causal connection between the growth of these two components. Optically luminous quasars host the most prodigious accreting black holes in the Universe and can account for >30% of the total cosmological black-hole growth. As typical quasars are not, however, undergoing intense star formation and already host massive black holes [>10^(8) M(Sun)], there must have been an earlier pre-quasar phase when these black holes grew [mass range ~10^(6)-10^(8) M(Sun)]. The likely signature of this earlier stage is simultaneous black-hole growth and star formation in distant (i.e., z>1; >8 billion light years away) luminous galaxies. Here we report ultra-deep X-ray observations of distant star-forming galaxies that are bright at submillimetre wavelengths. We find that the black holes in these galaxies are growing almost continuously throughout periods of intense star formation. This activity appears to be more tightly associated with these galaxies than any other coeval galaxy populations. We show that the black-hole growth from these galaxies is consistent with that expected for the pre-quasar phase., 5 pages, 2 figures, to appear in Nature on 7th April
Published: 2005
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113. WISE J233237.05–505643.5: A Double-peaked, Broad-lined Active Galactic Nucleus with a Spiral-shaped Radio Morphology

Author: Roberto J. Assef, Christopher W. Stubbs, Dominic J. Benford, Chao-Wei Tsai, Daniel Stern, Kwan-Lok Li, Emonts Bjorn, Jingwen Wu, Thomas H. Jarrett, Albert K. H. Kong, B. Stalder, Carol J. Lonsdale, R. Scott Barrows, Andrew Blain, Peter Eisenhardt, Ray P. Norris, F. William High, Department of Astronomy, and Faculty of Science
Subjects: IMAGING TECHNIQUES, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), WISE J233237.05, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, RED SHIFT, GALAXIES: ACTIVE, GALAXIES: INDIVIDUAL, Primary (astronomy), LINE SPECTRA, OPTICAL MEASUREMENT, CONTINUUMS, CENTROIDS, Spectroscopy, Astrophysics::Galaxy Astrophysics, BLACK HOLES (ASTRONOMY), Physics, Jet (fluid), Supermassive black hole, NEAR INFRARED RADIATION, SPECTROSCOPY, GALACTIC EVOLUTION, Astronomy and Astrophysics, DISK GALAXIES, Redshift, Galaxy, Core (optical fiber), GALAXIES, H ALPHA LINE, Space and Planetary Science, MORPHOLOGY, BLUE SHIFT, INTERSTELLAR MATTER
Abstract: We present radio continuum mapping, optical imaging, and spectroscopy of the newly discovered double-peaked, broad-lined active galactic nucleus (AGN) WISE J233237.05–505643.5 at redshift z = 0.3447. This source exhibits an FR-I and FR-II hybrid morphology, characterized by a bright core, jet, and Doppler-boosted lobe structures in Australian Telescope Compact Array continuum maps at 1.5, 5.6, and 9 GHz. Unlike most FR-II objects, W2332–5056 is hosted by a disk-like galaxy. The core has a projected 5'' linear radio feature that is perpendicular to the curved primary jet, hinting at unusual and complex activity within the inner 25 kpc. The multi-epoch, optical-near-IR photometric measurements indicate significant variability over a 3-20 yr baseline from the AGN component. Gemini South optical data show unusual double-peaked emission-line features: the centroids of the broad-lined components of Hα and Hβ are blueshifted with respect to the narrow lines and host galaxy by ~3800 km s^(–1). We examine possible cases that involve single or double supermassive black holes in the system and discuss the required future investigations to disentangle the mysterious nature of this system.
Published: 2013
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114. An extended Herschel drop-out source in the center of AS1063: a normal dusty galaxy at z = 6.1 or SZ substructures?

Author: Frédéric Boone, Ivan Valtchanov, Alain Omont, D. Schaerer, Kirsten Kraiberg Knudsen, Timothy D. Rawle, Dieter Lutz, Miroslava Dessauges-Zavadsky, Gregory Walth, Ian Smail, Eiichi Egami, Michael Zemcov, P. van der Werf, Andrew Blain, Rob Ivison, Benjamin Clément, Francoise Combes, Scott Chapman, R. Pello, Bruno Altieri, A. M. Swinbank, Pablo G. Pérez-González, A. Weiß, Jean-Paul Kneib, Johan Richard, M. Zamojski, AUTRES, Steward Observatory, University of Arizona, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institute for Computational Cosmology (ICC), Durham University, Department of Physics, Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), Department of Physics and Astronomy [Leicester], University of Leicester, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Royal Observatory Edinburgh (ROE), University of Edinburgh, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Leiden Observatory [Leiden], Universiteit Leiden, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), École normale supérieure - Paris (ENS Paris), European Space Agency (ESA), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Universiteit Leiden [Leiden]
Subjects: Astrofísica, submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High-redshift, FOS: Physical sciences, Astrophysics, star formation [Galaxies], 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Far infrared, galaxies: high-redshift, Drop out, 0103 physical sciences, Brightest cluster galaxy, Formation rate, 010303 astronomy & astrophysics, Reionization, galaxies. [Submillimeter], Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, evolution [Galaxies], Redshift, Galaxy, Astronomía, Space and Planetary Science, galaxies: star formation, Substructure, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In the course of our 870um APEX/LABOCA follow up of the Herschel Lensing Survey we have detected a source in AS1063 (RXC J2248.7-4431), that has no counterparts in any of the Herschel PACS/SPIRE bands, it is a Herschel 'drop-out' with S_870/S_500>0.5. The 870um emission is extended and centered on the brightest cluster galaxy suggesting either a multiply imaged background source or substructure in the Sunyaev-Zel'dovich (SZ) increment due to inhomogeneities in the hot cluster gas of this merging cluster. We discuss both interpretations with emphasis on the putative lensed source. Based on the observed properties and on our lens model we find that this source could be the first SMG with a moderate far infrared luminosity (L_FIR4. In deep HST observations we identified a multiply imaged z~6 source and we measured its spectroscopic redshift z=6.107 with VLT/FORS. This source could be associated with the putative SMG but it is most likely offset spatially by 10-30kpc and they could be interacting galaxies. With a FIR luminosity in the range [5-15]x10^{11} L_sol corresponding to a star formation rate in the range [80-260]M_sol/yr, this SMG would be more representative than the extreme starbursts usually detected at z>4. With a total magnification of ~25 it would open a unique window to the 'normal' dusty galaxies at the end of the epoch of reionization., accepted for publication in A&A
Published: 2013
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115. WISE detections of known QSOs at redshifts greater than six

Author: Roc M. Cutri, Carrie Bridge, Chao-Wei Tsai, Robert Assef, Sara Petty, Thomas H. Jarrett, Dominic J. Benford, Jingwen Wu, Andrew Blain, Daniel Stern, Peter Eisenhardt, Ned Wright, Department of Astronomy, and Faculty of Science
Subjects: QSOS, z quasar survey, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, galaxies: active, FOS: Physical sciences, z-greater-than-5.7 quasars, Astrophysics, Article, infrared: galaxies, additional quasars, midinfrared selection, media_common, Physics, quasars, Astronomy and Astrophysics, z-similar-to-6 quasars, spitzer, Redshift, energy-distributions, observations, Space and Planetary Science, Sky, general, active galactic nuclei, spectral, digital sky survey, galaxies: evolution, host galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
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-micron) band, 16 in W2 (4.6-micron), 3 in W3 (12-micron) and 0 in W4 (22-micron). This is particularly important with Spitzer in its warm-mission phase and no faint follow-up capability at wavelengths longwards of 5 microns until the launch of 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 AGN samples will be a useful tool, and high-redshift QSOs of all types will be easy targets for JWST., 7 pages; 6 figures; in press at ApJ
Published: 2013
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116. 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: Edward L. Wright, James D. Neill, Chao-Wei Tsai, Sara Petty, Frank J. Masci, Duncan Farrah, Dominic J. Benford, Thomas Jarrett, R. M. Rich, Sean E. Lake, Andrew Blain, C. Bridge, Department of Astronomy, and Faculty of Science
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, Metallicity, evolutionary synthesis, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Article, infrared: galaxies, Astrophysics::Solar and Stellar Astrophysics, sauron project, galaxies: elliptical and lenticular, education, disk galaxies, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, galaxies, Star formation, standard stellar library, formation, Astronomy and Astrophysics, initial mass function, elliptic galaxies, ultraviolet-radiation, Horizontal branch, Galaxy, cd, recent star-formation, Stars, Space and Planetary Science, ultraviolet: galaxies, Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, giant branch stars, galaxies: evolution, tp-agb models, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In the local Universe, 10% of massive elliptical galaxies are observed to exhibit a peculiar property: a substantial excess of ultraviolet emission (UVX) over what is expected from their old, red stellar populations. Several origins for the UVX have been proposed, including a population of hot young stars, or 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 ultraviolet excess (UVX) in a selection of 49 nearby E/S0-type galaxies by measuring the extended photometry in the UV-midIR with GALEX, SDSS and WISE. We compare UV/optical and UV/mid-IR colors with the Flexible Stellar Population Synthesis with EHB models (Conroy & Gunn 2010). 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 EHB fraction. There are strong color gradients with the outer radii bluer than the inner half-light radii by ~1 magnitude. This color difference is easily accounted for with a BHB fraction increase of 0.25 with radius. We estimated the average ages for the inner and outer radii are 7.0+/-0.3 Gyr, and 6.2+/-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 ~0.5-2 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, Accepted for publication in the Astronomical Journal: 33 pages, 13 figures, 3 tables, 1 Appendix
Published: 2013
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117. Mid-Infrared Selection of Active Galactic Nuclei with the Wide-Field Infrared Survey Explorer. II. Properties of WISE-Selected Active Galactic Nuclei in the NDWFS Boötes Field

Author: S. Adam Stanford, Christopher S. Kochanek, Chao-Wei Tsai, Mark Brodwin, Andrew Blain, Jingwen Wu, Buell T. Jannuzi, Peter Eisenhardt, Thomas H. Jarrett, Lin Yan, Michael J. I. Brown, Daniel Stern, Roberto J. Assef, and Emilio Donoso
Subjects: Physics, Active galactic nucleus, Statistical methods, Infrared, Ciencias Físicas, Mid infrared, Spectral density, Astronomy and Astrophysics, BOOTES, Torus, Astrophysics, purl.org/becyt/ford/1.3 [https], Wide field, purl.org/becyt/ford/1 [https], Astronomía, Space and Planetary Science, Galactic nuclei, galaxies, WISE, Selection criterion, Quasars, CIENCIAS NATURALES Y EXACTAS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Stern et al.(2012) presented a study of WISE selection of AGN in the 2 deg^2 COSMOS field, finding that a simple criterion W1-W2>=0.8 provides a highly reliable and complete AGN sample for W2, Comment: 34 text pages + 13 Figures + 6 Tables. Accepted for Publication in The Astrophysical Journal. Updated with referee's comments. Minor correction to Tables 1, 2 and 3 regarding an incorrect characterization of the reliability and completeness of the KI and KIM AGN selection criteria
Published: 2013

118. A New Population of High-z, Dusty Lyα Emitters and Blobs Discovered by WISE: Feedback Caught in the Act?

Author: Carrie R. Bridge, Andrew Blain, Colin J. K. Borys, Sara Petty, Dominic Benford, Peter Eisenhardt, Duncan Farrah, Roger L. Griffith, Tom Jarrett, Carol Lonsdale, Spencer A. Stanford, Daniel Stern, Chao-Wei Tsai, Edward L. Wright, and Jingwen Wu
Subjects: Physics, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics, Alpha (navigation), New population, Redshift, Galaxy
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 ≾ z ≾ 4.6 dusty Lyα emitters (LAEs). Of these, at least 37% have emission extended on scales of 30-100 kpc and are considered Lyα "blobs" (LABs). The objects have a surface density of only ~0.1 deg^(–2), 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 ≳ 10^(13)-10^(14) L_☉) 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 Lyα, 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.
Published: 2013

119. The SCUBA-2 Cosmology Legacy Survey: blank-field number counts of 450-mu m-selected galaxies and their contribution to the cosmic infrared background

Author: S. L. Jones, S. J. Oliver, Douglas Scott, Michael Zemcov, Isaac Roseboom, T. A. Targett, David H. Hughes, A. M. Swinbank, Duncan Farrah, David L. Clements, E. I. Robson, G. Marsden, Steve Eales, Antonio Chrysostomou, Ian Smail, David M. Alexander, E. L. Chapin, James Simpson, C. Clarke, Alastair C. Edge, P. van der Werf, D. Rigopoulou, T. Mackenzie, Itziar Aretxaga, Steve Serjeant, John A. Peacock, Scott Chapman, Richard G. McMahon, Chris J. Willott, V. Arumugam, Kristen Coppin, Cedric G. Lacey, Kirsten Kraiberg Knudsen, James Dunlop, James E. Geach, Michał J. Michałowski, Andy Gibb, Mark Halpern, Alexander Karim, Christine D. Wilson, V. Asboth, A. L. R. Danielson, Jamie Stevens, Rowin Meijerink, Philip Best, Tracy Webb, Andrew Blain, M. J. Page, T. Jenness, Marco Spaans, Rob Ivison, C. J. Conselice, Omar Almaini, Kapteyn Astronomical Institute, and Science and Technology Facilities Council (STFC)
Subjects: Absolute magnitude, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, MU-M, High-redshift, FOS: Physical sciences, HERMES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, HUBBLE-DEEP-FIELD, Astronomy & Astrophysics, 01 natural sciences, Cosmology, STAR-FORMATION, HALF, galaxies: high-redshift, SUBMILLIMETER-SELECTED GALAXIES, Cosmic infrared background, 0103 physical sciences, Submillimetre, 010303 astronomy & astrophysics, Observations, James Clerk Maxwell Telescope, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, DEGREE EXTRAGALACTIC SURVEY, Science & Technology, COSMIC cancer database, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, DUSTY, Galaxies, Redshift, Galaxy, EVOLUTION, 0201 Astronomical And Space Sciences, Space and Planetary Science, cosmology: observations, Physical Sciences, astro-ph.CO, HIGH-REDSHIFT, submillimetre: galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The first deep blank-field 450um map (1-sigma~1.3mJy) from the SCUBA-2 Cosmology Legacy Survey (S2CLS), conducted with the James Clerk Maxwell Telescope (JCMT) is presented. Our map covers 140 arcmin^2 of the COSMOS field, in the footprint of the HST CANDELS area. Using 60 submillimetre galaxies (SMGs) detected at >3.75-sigma, we evaluate the number counts of 450um-selected galaxies with flux densities S_450>5mJy. The 8-arcsec JCMT beam and high sensitivity of SCUBA-2 now make it possible to directly resolve a larger fraction of the cosmic infrared background (CIB, peaking at ~200um) into the individual galaxies responsible for its emission than has previously been possible at this wavelength. At S_450>5mJy we resolve (7.4[+/-]0.7)x10^-2 MJy/sr of the CIB at 450um (equivalent to 16[+/-]7% of the absolute brightness measured by COBE at this wavelength) into point sources. A further ~40% of the CIB can be recovered through a statistical stack of 24um emitters in this field, indicating that the majority (~60%) of the CIB at 450um is emitted by galaxies with S_450>2mJy. The average redshift of 450um emitters identified with an optical/near-infrared counterpart is estimated to be =1.3, implying that the galaxies in the sample are in the ultraluminous class (L_IR~1.1x10^12 L_sun). If the galaxies contributing to the statistical stack lie at similar redshifts, then the majority of the CIB at 450um is emitted by galaxies in the LIRG class with L_IR>3.6x10^11 L_sun., 9 pages, 5 figures, submitted to MNRAS
Published: 2013

120. Characterizing the Mid-infrared Extragalactic Sky with WISE and SDSS

Author: Dominik Riechers, S. A. Stanford, Chao-Wei Tsai, Peter Eisenhardt, Carrie Bridge, Emilio Donoso, Lin Yan, Roc M. Cutri, Daniel Stern, Thomas H. Jarrett, Roberto J. Assef, Edward L. Wright, and Andrew Blain
Subjects: QSOS, Physics, Infrared galaxies, Infrared, media_common.quotation_subject, Ciencias Físicas, Flux, Astronomy and Astrophysics, Astrophysics, Galaxies high-redshift, Redshift, Galaxy, Astronomía, Stars, Galaxies evolution, Space and Planetary Science, Sky, galaxies starburst, Spectroscopy, CIENCIAS NATURALES Y EXACTAS, media_common
Abstract: The Wide-ﬁeld Infrared Survey Explorer (WISE) has completed its all-sky survey in four channels at 3.4–22um, detecting hundreds of millions of objects. We merge the WISE mid-infrared data with optical data from the Sloan Digital Sky Survey (SDSS) and provide a phenomenological characterization of WISE extragalactic sources. WISE is most sensitive at 3.4um (W1) and least sensitive at 22um (W4). The W1 band probes massive early-type galaxies out to z~1. This is more distant than SDSS identiﬁed early-type galaxies, consistent with the fact that 28% of 3.4um sources have faint or no r-band counterparts (r > 22.2). In contrast, 92%–95% of 12um and 22um sources have SDSS optical counterparts with r7σ, but only 18.9% at 22um with S/N W4 > 5 sigma. We show that WISE colors alone are effective in isolating stars (or local early-type galaxies), star-forming galaxies, and strong active galactic nuclei (AGNs)/QSOs at z~3. We highlight three major applications of WISE colors: (1) Selection of strong AGNs/QSOs at z~3 using W1−W2>0.8 and W20.8, W2 < 15.2 combined with r−W2>6 (Vega) colors can be used to identify type-2 AGN candidates. The fraction of these type-2 AGN candidates is one-third of all WISE color-selected AGNs. (3) Selection of ultraluminous infrared galaxies (ULIRGs) at z∼2 with extremely red colors, r − W4 > 14 or well-detected 22um sources lacking detections in the 3.4 and 4.6um bands. The surface density of z∼2 ULIRG candidates selected with r −W4 > 14 is 0.9$pm$0.07 deg−2 at S/N W4~5 (the corresponding, lowest ﬂux density of 2.5 mJy), which is consistent with that inferred from smaller area Spitzer surveys. Optical spectroscopy of a small number of these high-redshift ULIRG candidates conﬁrms our selection, and reveals a possible trend that optically fainter or r−W4 redder candidates are at higher redshifts. Fil: Yan, L.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos; Fil: Donoso, Emilio. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos; . Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Cientifico Tecnológico - CONICET - San Juan. Instituto de Ciencias Astronómicas de la Tierra y del Espacio; Argentina Fil: Tsai, Chao Wei. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos; Fil: Stern, D.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos; Fil: Assef, R. J.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos; Fil: Eisenhardt, P.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos; Fil: Blain, A. W.. University of Leicester. Department of Physics & Astronomy; Reino Unido; Fil: Cutri, R.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos; Fil: Jarrett, T. H.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos; Fil: Stanford, S. A.. University of California. Department of Physics; Estados Unidos; Fil: Wright, E.. University of California. Astronomy Department; Estados Unidos; Fil: Bridge, C.. California Institute of Technology. Astronomy Department; Estados Unidos; Fil: Riechers, D. A.. California Institute of Technology. Astronomy Department; Estados Unidos; . Cornell University. Astronomy Department; Estados Unidos
Published: 2013

121. Uncovering obscured luminous AGN with WISE

Author: A. Alonso-Herrero, Francisco J. Carrera, Alessandro Caccianiga, Paola Severgnini, Andrew Blain, Silvia Mateos, Ángel Ruiz, European Commission, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), Universidad de Cantabria, Royal Society (UK), Agenzia Spaziale Italiana, and Inter-University Centre for Astronomy and Astrophysics (India)
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), active [Galaxies], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, general [Quasars], Galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, Public administration, Infrared: galaxies, 01 natural sciences, Quasars: general, galaxies [Infrared], Space and Planetary Science, 0103 physical sciences, media_common.cataloged_instance, Astrophysics::Solar and Stellar Astrophysics, Christian ministry, European union, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mateos et al. presented a highly reliable and efficient mid-infrared (MIR) colour-based selection technique for luminous active galactic nuclei (AGN) using the Wide-field Infrared Survey Explorer (WISE) survey. Here, we evaluate the effectiveness of this technique to identify obscured AGN missed in X-ray surveys. To do so we study the WISE properties of AGN independently selected in hard X-ray and optical surveys. We use the largest catalogue of 887 [O III] λ5007-selected type 2 quasars (QSO2s) at z = 0.83 in the literature from the Sloan Digital Sky Survey (SDSS), and the 258 hard (>4.5 keV) X-ray-selected AGN from the Bright Ultrahard XMM-Newton Survey (BUXS). The fraction of SDSS QSO2s in our infrared AGN selection region (wedge) increases with the AGN luminosity, reaching 66.1+4.5 -4.7 per cent at the highest [OIII] luminosities in the sample. This fraction is substantially lower than for the BUXS type 1 AGN (96.1+3.0 -6.3 per cent), but consistent, within the uncertainties, with that for the BUXS type 2 AGN (75.0+14.1 -19.1 per cent) with the same luminosity. The SDSS QSO2s appear to reside in more luminous (massive) hosts than the BUXS AGN, due to the tight magnitude limits applied in the SDSS spectroscopic target selection. Since host galaxy dilution can reduce substantially the effectiveness of MIR-based techniques, this may explain the lower fraction of SDSS QSO2s in the WISE AGN wedge. The fraction of SDSS QSO2s identified as Compton-thick candidates that fall in the wedge is consistent with the fraction of all SDSS QSO2s in that zone. At the AGN luminosities involved in the comparison, Compton-thick and Compton-thin SDSS QSO2s have similarWISE colour distributions. We conclude that at high luminosities and z = 1 our MIR technique is very effective at identifying both Compton-thin and Compton-thick AGN. ©2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society., SM and FJC acknowledge financial support by the Spanish Ministry of Economy and Competitiveness through grant AYA2010-21490-C02-01. SM, FJC and A.A.-H. acknowledge financial support by the Spanish Ministry of Economy and Competitiveness through grant AYA2012-31447. SM, FJC and A.A.- H. acknowledge financial support from the ARCHES project (7th Framework of the European Union, No. 313146). SM acknowledges financial support from the JAE-Doc program (Consejo Superior de Investigaciones Cientficas, cofunded by FSE). AA-H acknowledges support from the Universidad de Cantabria through the Augusto G. Linares program. AB acknowledges a Royal Society Wolfson Research Merit Award. PS acknowledges financial support from ASI (grant No. I/009/10/0). AR acknowledges support from an IUCAA post-doctoral fellowship.
Published: 2013

122. Mapping the Clumpy Structures within Submillimeter Galaxies using Laser-Guide Star Adaptive Optics Spectroscopy

Author: Mark Swinbank, Ian Smail, Karín Menéndez-Delmestre, Rob Ivison, Thiago S. Gonçalves, Andrew Blain, and Scott C. Chapman
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, Astrophysics::High Energy Astrophysical Phenomena, High-redshift, FOS: Physical sciences, Starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Submillimeter, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, Luminous infrared galaxy, 010308 nuclear & particles physics, Star formation, Kinematics and dynamics, Astronomy and Astrophysics, Galaxies, Nuclei, Galaxy, Redshift, Laser guide star, Space and Planetary Science, Imaging spectroscopy, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first integral-field spectroscopic observations of high-redshift submillimeter-selected galaxies (SMGs) using Laser Guide Star Adaptive Optics (LGS-AO). We target H-alpha emission of three SMGs at redshifts z~1.4-2.4 with the OH-Suppressing Infrared Imaging Spectrograph (OSIRIS) on Keck. The spatially-resolved spectroscopy of these galaxies reveals unresolved broad H-alpha line regions (FWHM>1000 km/s) likely associated with an AGN and regions of diffuse star formation traced by narrow-line H-alpha emission (FWHM, Accepted to ApJ
Published: 2013
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123. The suppression of star formation by powerful active galactic nuclei

Author: Eli Dwek, D. Rigopoulou, James Dunlop, P. Chanial, Michael Zemcov, Michael Pohlen, Stephen Anthony Eales, N. Castro-Rodriguez, Elizabeth Dubois, Rob Ivison, Ivan Valtchanov, Alexandre Amblard, Mark Halpern, M. J. Page, G. Wright, B. O'Halloran, Tom Babbedge, Marco P. Viero, Douglas Scott, Asantha Cooray, Robyn L. Ward, Walter Kieran Gear, Giulia Rodighiero, Alessandro Boselli, C. D. Dowell, K. E. Tugwell, A. J. Smith, Lian-Tao Wang, Alain Omont, Bruno Maffei, Jonathan Rawlings, Antonio Cava, James J. Bock, C. K. Xu, K. G. Isaak, D. Elbaz, Nick Seymour, Lucia Marchetti, Michael Rowan-Robinson, Joaquin Vieira, Matthew Joseph Griffin, M. Fox, S. C. Madden, Jason Glenn, Simon Dye, Bruno Altieri, V. Buat, Chris Pearson, Seb Oliver, Edo Ibar, Andrew Blain, L. R. Levenson, Benjamin L. Schulz, Jamie Stevens, P. Panuzzo, L. Riguccini, Evanthia Hatziminaoglou, Andreas Papageorgiou, Nanyao Y. Lu, M. Symeonidis, V. Arumugam, Alberto Franceschini, Mattia Vaccari, D. Rizzo, L. Vigroux, D. L. Shupe, Isaac Roseboom, Duncan Farrah, Markos Trichas, Hien Nguyen, David L. Clements, G. Mainetti, Luca Conversi, H. Aussel, A. Conley, Guilaine Lagache, Ismael Perez-Fournon, M. Sanchez Portal, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Herschel Science Centre, European Space Agency (ESA), NASA Ames Research Center (ARC), University of Edinburgh, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Blackett Laboratory, Imperial College London, Department of Physics and Astronomy [Leicester], University of Leicester, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), Astronomy Centre, University of Sussex, NASA Goddard Space Flight Center (GSFC), University of Nottingham, UK (UON), Cardiff University, Astronomy Centre, University of Sussex, Astrophysics Group, Imperial College London-Imperial College London, Universita degli Studi di Padova, School of Physics and Astronomy [Cardiff], Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), European Space Research and Technology Centre (ESTEC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Division of Engineering, Colorado School of Mines, University of Manchester [Manchester], Dipartimento di Astronomia [Padova], Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), University of Hertfordshire [Hatfield] (UH), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Università degli Studi di Padova = University of Padua (Unipd), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Harvard University-Smithsonian Institution, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Dipartimento di Astronomia, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), AUTRES, Imagerie et modélisation Vasculaires, Thoraciques et Cérébrales (MOTIVATE), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), and Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)
Subjects: Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Intergalactic star, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Multidisciplinary, 010308 nuclear & particles physics, Star formation, Astronomy, Quasar, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Intermediate-mass black hole, Elliptical galaxy, Stellar black hole, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The old, red stars which constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly from accretion onto black holes. It is widely suspected, but unproven, that the tight correlation in mass of the black hole and stellar components results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, while powerful star-forming galaxies are usually dust-obscured and are brightest at infrared to submillimetre wavelengths. Here we report observations in the submillimetre and X-ray which show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 Gyrs old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10^44 erg/s. This suppression of star formation in the host galaxies of powerful AGN is a key prediction of models in which the AGN drives a powerful outflow, expelling the interstellar medium of its host galaxy and transforming the galaxy's properties in a brief period of cosmic time., Comment: Published in Nature, May 2012. Includes supplementary information
Published: 2013
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124. Submillimeter Follow-up of WISE-Selected Hyperluminous Galaxies

Author: Chao-Wei Tsai, Benjamin J. Weiner, Carol J. Lonsdale, Roger L. Griffith, S. Adam Stanford, Sara Petty, Dominic J. Benford, Neal J. Evans, Shane Bussmann, Thomas H. Jarrett, Jingwen Wu, Daniel Stern, Lin Yan, Roberto J. Assef, Edward L. Wright, Andrew Blain, Sean E. Lake, Peter Eisenhardt, Roc M. Cutri, Jack Sayers, Carrie Bridge, Julia M. Comerford, and Jeonghee Rho
Subjects: Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, Population, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Galaxy, Luminosity, Caltech Submillimeter Observatory, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Millimeter, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of WISE-selected, hyperluminous galaxies, so called W1W2-dropout galaxies. This is a rare (~ 1000 all-sky) population of galaxies at high redshift (peaks at z=2-3), that are faint or undetected by WISE at 3.4 and 4.6 um, yet are clearly detected at 12 and 22 um. The optical spectra of most of these galaxies show significant AGN activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350 to 850 um, with 9 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 um, 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 submm 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 10^{13} Lsun. 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., Will be Published on Sep 1, 2012 by ApJ
Published: 2012

125. The First Hyper-luminous Infrared Galaxy Discovered by WISE

Author: Daniel Stern, Lin Yan, Dominic J. Benford, Michael C. Cushing, Jack Sayers, Chao-Wei Tsai, Roc M. Cutri, Brian Mason, Roberto J. Assef, Frank J. Masci, S. Adam Stanford, Carrie Bridge, J. J. Condon, Jingwen Wu, Neal J. Evans, Roger L. Griffith, Chris Gelino, Peter Eisenhardt, Andrew Blain, Thomas H. Jarrett, Edward L. Wright, Sara Petty, Carol J. Lonsdale, and Carl J. Grillmair
Subjects: Physics, Luminous infrared galaxy, Dwarf star, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Infrared, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Spectral line, Luminosity, Gravitational lens, 13. Climate action, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the discovery by the Wide-field Infrared Survey Explorer 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 microns and well detected at 12 or 22 microns). The WISE data and a 350 micron detection give a minimum bolometric luminosity of 3.7 x 10^13 Lsun, with ~10^14 Lsun plausible. Followup 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 Msun/yr, accounting for < 10% of the bolometric luminosity. Strong 22 micron emission relative to 350 microns 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 ~10x above the far-infrared/radio correlation, indicating an active galactic nucleus 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 M_BH-bulge mass relation, the implied Eddington ratio is >~4. WISE 1814+3412 may be a heavily obscured object where the peak AGN activity occurred prior to the peak era of star formation., Published in 2012 August 20 Astrophysical Journal
Published: 2012

126. Constructing a WISE High Resolution Galaxy Atlas

Author: Kartik Sheth, Roberto J. Assef, Andrew Blain, Spencer A. Stanford, Sara Petty, Dominic J. Benford, John W. Fowler, Frank J. Masci, Chao-Wei Tsai, S. Lake, Edward L. Wright, Carrie Bridge, James D. Neill, Thomas H. Jarrett, Peter Eisenhardt, Mark Seibert, Emilio Donoso, Michelle E. Cluver, and Baerbel Koribalski
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Image (category theory), FOS: Physical sciences, Astronomy and Astrophysics, Image processing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sample (graphics), Galaxy, medicine.anatomical_structure, Space and Planetary Science, Sky, Atlas (anatomy), medicine, Deconvolution, Image resolution, Astrophysics::Galaxy Astrophysics, media_common, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: After eight months of continuous observations, the Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at 3.4 {\mu}m, 4.6 {\mu}m, 12 {\mu}m and 22 {\mu}m. We have begun a dedicated WISE High Resolution Galaxy Atlas (WHRGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalogue. Here we summarize the deconvolution technique 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 super-resolution image processing to that of Spitzer, GALEX and ground-based imaging. The is the first paper in a two part series; results for a much larger sample of nearby galaxies is presented in the second paper., Comment: Published in the AJ (2012, AJ, 144, 68)
Published: 2012

127. THE INFRARED PROPERTIES OF SOURCES MATCHED IN THE WISE ALL-SKY AND HERSCHEL ATLAS SURVEYS

Author: Peter R. Eisenhardt, Simon Dye, Lee S. Kelvin, Jonathan P. Gardner, Carlos D. Hoyos, Gianfranco De Zotti, Edo Ibar, Mark Thompson, S. Fleuren, Jingwen Wu, S. Buttiglione, Maarten Baes, Matt J. Jarvis, Chao-Wei Tsai, Edward L. Wright, Antonio Cava, Carrie Bridge, Rosalind Hopwood, David L. Clements, Nicholas A. Bond, A. Dariush, D. G. Bonfield, Asantha Cooray, Simon P. Driver, Rob Ivison, Dominic J. Benford, Alexandre Amblard, Paul van der Werf, Pasquale Temi, Aaron S. G. Robotham, Stephen Anthony Eales, Loretta Dunne, Andrew Blain, Daniel J. Smith, Lin Yan, Steve Maddox, and Nathan Bourne
Subjects: ACTIVE GALACTIC NUCLEI, SELECTION, Cosmology and Nongalactic Astrophysics (astro-ph.CO), TELESCOPE, Infrared, Terahertz radiation, media_common.quotation_subject, DATA RELEASE, Population, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, infrared: galaxies, surveys, galaxies: high-redshift, STAR-FORMING GALAXIES, education, Astrophysics::Galaxy Astrophysics, galaxies: statistics, POPULATION, media_common, Physics, REDSHIFT SURVEY, education.field_of_study, Science & Technology, Astronomy and Astrophysics, PERFORMANCE, galaxies: general, Galaxy, Redshift, EVOLUTION, 0201 Astronomical And Space Sciences, Space and Planetary Science, Sky, cosmology: observations, Physical Sciences, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, SUBMILLIMETER, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We describe the infrared properties of sources detected over ~36 deg^2 of sky in the GAMA 15-hr equatorial field, using data from both the Herschel Astrophysical Terahertz Large-Area Survey (H-ATLAS) and Wide-field Infrared Survey (WISE). With 5-sigma point-source depths of 34 and 0.048 mJy at 250 micron and 3.4 micron, respectively, we are able to identify 50.6% of the H-ATLAS sources in the WISE survey, corresponding to a surface density of ~630 deg^{-2}. Approximately two-thirds of these sources have measured spectroscopic or optical/near-IR photometric redshifts of z~20.5) have 250-350 micron flux density ratios that suggest either high-redshift galaxies (z>~1.5) or optically faint low-redshift galaxies with unusually low temperatures (T, Comment: 6 pages, 5 figures, accepted to ApJ Letters
Published: 2012

128. A revised asteroid polarization-albedo relationship using WISE/NEOWISE data

Author: Amy Mainzer, Edward L. Wright, Joseph R. Masiero, T. Grav, Robert S. McMillan, Andrew Blain, James Bauer, and David J. Tholen
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Function (mathematics), Astrophysics, Albedo, Polarization (waves), Space and Planetary Science, Asteroid, Coincident, Linear regression, Variation (astronomy), Mathematics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present a reanalysis of the relationship between asteroid albedo and polarization properties using the albedos derived from the Wide-field Infrared Survey Explorer. We find that the function that best describes this relation is a three-dimensional linear fit in the space of log(albedo)-log(polarization slope)-log(minimum polarization). When projected to two dimensions the parameters of the fit are consistent with those found in previous work. We also define p* as the quantity of maximal polarization variation when compared with albedo and present the best fitting albedo-p* relation. Some asteroid taxonomic types stand out in this three-dimensional space, notably the E, B, and M Tholen types, while others cluster in clumps coincident with the S- and C-complex bodies. We note that both low albedo and small (D, 16 pages, Accepted to ApJ
Published: 2012

129. Spitzer Photometry of WISE-Selected Brown Dwarf and Hyper-Luminous Infrared Galaxy Candidates

Author: Daniel Stern, Gregory N. Mace, Dominic J. Benford, Kenneth A. Marsh, Thomas Jarrett, Edward L. Wright, Roc M. Cutri, Michael E. Ressler, Roger L. Griffith, Chao-Wei Tsai, Carol J. Lonsdale, Martin Cohen, J. Davy Kirkpatrick, S. A. Stanford, Peter R. Eisenhardt, Carrie Bridge, Deborah Padgett, Michael F. Skrutskie, Jingwen Wu, A. K. Mainzer, Emilio Donoso, Michael C. Cushing, Christopher R. Gelino, Lin Yan, Sara Petty, and Andrew Blain
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Ciencias Físicas, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, Photometry (optics), Astrophysics::Solar and Stellar Astrophysics, Control sample, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Luminous infrared galaxy, Physics, Brown dwarfs, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Red shift, Astronomía, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, photometry [galaxies], Astrophysics::Earth and Planetary Astrophysics, high-redshift [galaxies], CIENCIAS NATURALES Y EXACTAS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Spitzer 3.6 and 4.5 μm 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 μm ~ 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 × 105 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 μm photometry, along with positionally matched B and R photometry from USNO-B; J, H, and Ks photometry from Two Micron All-Sky Survey; and W1, W2, W3, and W4 photometry from the WISE all-sky catalog. Fil: Griffith, Roger L.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Kirkpatrick, J. Davy. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Eisenhardt, Peter R. M.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos Fil: Gelino, Christopher R.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Cushing, Michael C.. University of Toledo. Department of Physics and Astronomy; Estados Unidos Fil: Benford, Dominic. NASA Goddard Space Flight Center; Estados Unidos Fil: Blain, Andrew. University Of Leicester; Reino Unido Fil: Bridge, Carrie R.. California Instituto Of Technology; Estados Unidos Fil: Cohen, Martin. California Instituto Of Technology; Estados Unidos Fil: Cutri, Roc M.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Donoso, Emilio. Consejo Nacional de Investigaciones Cientificas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Jarrett, Thomas H.. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Lonsdale, Carol. National Radio Astronomy Observatory; Estados Unidos Fil: Mace, Gregory. University of California Los Angeles. Astronomy Department; Estados Unidos Fil: Mainzer, A.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos Fil: Marsh, Ken. Cardiff University. School of Physics and Astronomy; Reino Unido Fil: Padgett, Deborah. NASA Goddard Space Flight Center; Estados Unidos Fil: Petty, Sara. University of California Los Angeles. Astronomy Department; Estados Unidos Fil: Ressler, Michael E.. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos Fil: Skrutskie, Michael F.. University of Virginia. Department of Astronomy; Estados Unidos Fil: Stanford, Spencer A.. University of California Davis. Department of Physics; Estados Unidos Fil: Stern, Daniel. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos Fil: Tsai, Chao Wei. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos Fil: Wright, Edward L.. University of California Los Angeles. Astronomy Department; Estados Unidos Fil: Wu, Jingwen. California Institute of Technology. Jet Propulsion Laboratory; Estados Unidos Fil: Yan, Lin. California Institute of Technology. Infrared Processing and Analysis Center; Estados Unidos
Published: 2012
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130. The redshift and nature of AzTEC/COSMOS 1: A starburst galaxy at z=4.6

Author: S. Berta, H. J. McCracken, David H. Hughes, Giovanni G. Fazio, Kartik Sheth, Mara Salvato, Herve Aussel, Dominik A. Riechers, M. S. Yun, Eric J. Murphy, L. Riguccini, Manuel Aravena, N. Z. Scoville, Bahram Mobasher, Chris Carilli, Eva Schinnerer, Igor Moric, Peter Capak, David B. Sanders, James E. Aguirre, Jean-Paul Kneib, Dieter Lutz, D. Masters, Grant W. Wilson, Vernesa Smolčić, Francesca Civano, Itziar Aretxaga, Andrew Blain, Anton M. Koekemoer, Olivier Ilbert, Mark Sargent, Francesca Pozzi, Yoshiaki Taniguchi, Chris J. Willott, Jeyhan S. Kartaltepe, Kimberly S. Scott, J.-S. Huang, D. Thompson, E. LeFloc'h, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Smol&#269, i&#263, V., Capak P., Ilbert O., Blain A. W., Salvato M., Aretxaga I., Schinnerer E., Masters D., Mori&#263, I., Riechers D. A., Sheth K., Aravena M., Aussel H., Aguirre J., Berta S., Carilli C. L., Civano F., Fazio G., Huang J., Hughes D., Kartaltepe J., Koekemoer A. M., Kneib J.-P., LeFloc'h E., Lutz D., McCracken H., Mobasher B., Murphy E., Pozzi F., Riguccini L., Sanders D. B., Sargent M., Scott K. S., Scoville N. Z., Taniguchi Y., Thompson D., Willott C., Wilson G., Yun M., and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, FOS: Physical sciences, galaxies: starburst, Astrophysics, galaxies: distances and redshifts, galaxies: high-redshift, Photometry (optics), NATURAL SCIENCES. Physics. Astronomy and Astrophysics, galaxies: distances and redshifts – galaxies: high-redshift – galaxies: starburst, Spectroscopy, Line (formation), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], starburst [galaxies], Star formation, Astronomy and Astrophysics, Redshift, Galaxy, Stars, 13. Climate action, Space and Planetary Science, Spectral energy distribution, distances and redshifts [galaxies], high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Based on broad/narrow-band photometry and Keck DEIMOS spectroscopy we report a redshift of z=4.64-0.08+0.06 for AzTEC/COSMOS 1, the brightest sub-mm galaxy in the AzTEC/COSMOS field. In addition to the COSMOS-survey X-ray to radio data, we report observations of the source with Herschel/PACS (100, 160 micron), CSO/SHARC II (350 micron), CARMA and PdBI (3 mm). We do not detect CO(5-4) line emission in the covered redshift ranges, 4.56-4.76 (PdBI/CARMA) and 4.94-5.02 (CARMA). If the line is within this bandwidth, this sets 3sigma upper limits on the gas mass to, Comment: 7 pages, 4 figures, 1 table, accepted for publication in ApJL; one reference corrected
Published: 2011
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131. WISE Discovery of Low Metallicity Blue Compact Dwarf Galaxies

Author: Andrew Blain, S. A. Stanford, Chao-Wei Tsai, Lin Yan, Jingwen Wu, Kristin K. Madsen, Edward L. Wright, Daniel Stern, Peter Eisenhardt, Fiona A. Harrison, Roger L. Griffith, Thomas H. Jarrett, and Yanling Wu
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, Star formation, Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Star (graph theory), Galaxy, First generation, Space and Planetary Science, Spectroscopy, Dwarf galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report two new low metallicity blue compact dwarf galaxies (BCDs), WISEP J080103.93+264053.9 (hereafter W0801+26) and WISEP J170233.53+180306.4 (hereafter W1702+18), discovered using the Wide-field Infrared Survey Explorer (WISE). We identified these two BCDs from their extremely red colors at mid-infrared wavelengths, and obtained follow-up optical spectroscopy using the Low Resolution Imaging Spectrometer on Keck I. The mid-infrared properties of these two sources are similar to the well studied, extremely low metallicity galaxy SBS 0335-052E. We determine metallicities of 12 + log(O/H) = 7.75 and 7.63 for W0801+26 and W1702+18, respectively, placing them amongst a very small group of very metal deficient galaxies (Z < 1/10 Zsun). Their > 300 Angstrom Hbeta equivalent widths, similar to SBS 0335-052E, imply the existence of young (< 5 Myr) star forming regions. We measure star formation rates of 2.6 and 10.9 Msun/yr for W0801+26 and W1702+18, respectively. These BCDs, showing recent star formation activity in extremely low metallicity environments, provide new laboratories for studying star formation in extreme conditions and are low-redshift analogs of the first generation of galaxies to form in the universe. Using the all-sky WISE survey, we discuss a new method to identify similar star forming, low metallicity BCDs., Accepted for publication in ApJL
Published: 2011
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132. Far infrared constraints on the contamination by dust obscured galaxies of high-z dropout searches

Author: Benjamin Magnelli, Ian Smail, Dieter Lutz, Johan Richard, Miroslava Dessauges-Zavadsky, R. Pello, Rob Ivison, M. Zamojski, Andrew Blain, Daniel Schaerer, Raanan Nordon, Karl M. Menten, M. Rex, Jean-Paul Kneib, P. van der Werf, Axel Weiss, Pablo G. Pérez-González, Francoise Combes, Frédéric Boone, Alexandre Beelen, Nicolas Laporte, Benjamin Clément, Bruno Altieri, T. Rawle, Eiichi Egami, Mark Swinbank, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Max-Planck-Institut für Radioastronomie (MPIFR), Steward Observatory, University of Arizona, Institute for Computational Cosmology (ICC), Durham University, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Royal Observatory Edinburgh (ROE), University of Edinburgh, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, California Institute of Technology (CALTECH), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), XMM-Newton Science Operations Centre, Agence Spatiale Européenne = European Space Agency (ESA), Leiden Observatory [Leiden], Universiteit Leiden, Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université de Genève (UNIGE), European Space Agency (ESA), and Universiteit Leiden [Leiden]
Subjects: Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Extinction (astronomy), Gravitational lensing, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], gravitational lensing: weak, Far infrared, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, High-redshift, Weak, distances and redshifts, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, extinction, Near-infrared spectroscopy, Spectral density, Dust, Astronomy and Astrophysics, Extinction, Galaxies, Galaxy, Redshift, Astronomía, Spire, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, dust, galaxies: distances and redshifts, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The spectral energy distributions (SED) of dusty galaxies at intermediate redshift may look similar to very high redshift galaxies in the optical/near infrared (NIR) domain. This can lead to the contamination of high redshift galaxy searches based on broad band optical/NIR photometry by lower redshift dusty galaxies as both kind of galaxies cannot be distinguished. The contamination rate could be as high as 50%. {This work shows how the far infrared (FIR) domain can help to recognize likely low-z interlopers in an optical/NIR search for high-z galaxies.} We analyse the FIR SEDs of two galaxies proposed as very high redshift ($z>7$) dropout candidates based on deep Hawk-I/VLT observations. The FIR SEDs are sampled with PACS/Herschel at 100 and 160\,$��$m, with SPIRE/Herschel at 250, 350 and 500\,$��$m and with LABOCA/APEX at 870\,$��$m. We find that redshifts $>7$ would imply extreme FIR SEDs (with dust temperatures $>100$\,K and FIR luminosities $>10^{13}$\,$L_{\odot}$). At z$\sim$2, instead, the SEDs of both sources would be compatible with that of typical ULIRGs/SMGs. Considering all the data available for these sources from visible to FIR we re-estimate the redshifts and we find $z\sim$1.6--2.5. Due to the strong spectral breaks observed in these galaxies, standard templates from the literature fail to reproduce the visible-near IR part of the SEDs even when additional extinction is included. These sources resemble strongly dust obscured galaxies selected in Spitzer observations with extreme visible-to-FIR colors, and the galaxy GN10 at $z=4$. Galaxies with similar SEDs could contaminate other high redshift surveys., Accepted for publication in A&A
Published: 2011
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133. Millimetre background radiation and galaxy formation

Author: Malcolm S. Longair and Andrew Blain
Subjects: Physics, Dark matter halo, Structure formation, Lyman-alpha emitter, Space and Planetary Science, Protogalaxy, Dark matter, Galaxy formation and evolution, Astronomy, Astronomy and Astrophysics, Dark galaxy, Astrophysics, Background radiation
Published: 1993
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134. Molecular gas content in typical L* galaxies at z ∼ 1.5 − 3

Author: Francoise Combes, Daniel Schaerer, Eiichi Egami, T. D. Rawle, Frédéric Boone, Jean-Paul Kneib, Miroslava Dessauges-Zavadsky, M. Zamojski, A. Mark Swinbank, Panos Sklias, Andrew Blain, and Johan Richard
Subjects: Physics, Space and Planetary Science, Content (measure theory), Astronomy and Astrophysics, Astrophysics, Galaxy
Abstract: To extend the molecular gas measurements to typical L* star-forming galaxies (SFGs) at z ∼ 1.5 − 3, we have observed CO emission for five strongly-lensed galaxies selected from the Herschel Lensing Survey. The combined sample of our L* SFGs with CO-detected SFGs at z >1 from the literature shows a large spread in star formation efficiency (SFE). We find that this spread in SFE is due to variations of several physical parameters, primarily the specific star formation rate, but also stellar mass and redshift. An increase of the molecular gas fraction (fgas) is observed from z ∼ 0.2 to z ∼ 1.2, followed by a quasi non-evolution toward higher redshifts, as found in earlier studies. We provide the first measure of fgas of z >1 SFGs at the low-stellar mass end between 109.4 < M∗/M⊙ < 109.9, which shows a clear fgas upturn.
Published: 2014
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135. Improving the identification of high-z Herschel sources with position priors and optical/NIR and FIR/mm photometric redshifts

Author: Douglas Clowe, Johan Richard, Bruno Altieri, Jean-Paul Kneib, Olivier Ilbert, Benjamin Clément, Eiichi Egami, Néstor Espino-Briones, Giulia Rodighiero, Dario Fadda, Anthony H. Gonzalez, Michael W. Werner, Miroslava Dessauges-Zavadsky, J. G. Cuby, T. D. Rawle, Mathilde Jauzac, Michael Zemcov, Francoise Combes, George H. Rieke, Daniel Johansson, Sun Mi Chung, Andrew Blain, James J. Bock, M. J. Pereira, Marie Rex, Ivan Valtchanov, Frédéric Boone, Graham P. Smith, P. van der Werf, Daniel Schaerer, Gregory Walth, A. K. Fiedler, C. D. Dowell, Carrie Bridge, R. Pello, Rob Ivison, Cathy Horellou, Pablo G. Pérez-González, Dieter Lutz, Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Steward Observatory, University of Arizona, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), AUTRES, XMM-Newton Science Operations Centre, European Space Agency (ESA), Department of Astronomy, California Institute of Technology (CALTECH), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Department of Astronomy [Gainesville] (UF|Astro), University of Florida [Gainesville] (UF), Royal Observatory Edinburgh (ROE), University of Edinburgh, Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Alabama at Birmingham [ Birmingham] (UAB), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université de Genève = University of Geneva (UNIGE), and Universiteit Leiden
Subjects: Astrofísica, submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Noise (electronics), infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, Redshift, Astronomía, Spire, galaxies: photometry, Space and Planetary Science, Millimeter, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
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 um sources as priors. Our catalogs are able to reliably (5 sigma) recover galaxies with fluxes above 6 and 10 mJy in the PACS 100 and 160 um 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., Accepted for publication in Astronomy and Astrophysics (Herschel special issue)
Published: 2010
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136. Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours

Author: Steven P. Bamford, Paolo Serra, Anne E. Sansom, Elizabeth J. Barton, Jochen Liske, E. van Kampen, Antonio Cava, E. Cameron, Alexandre Amblard, James Dunlop, Aprajita Verma, S. Buttiglione, Michael Pohlen, Maarten Baes, Scott M. Croom, H Parkinson, Mattia Negrello, Simon P. Driver, P. Temi, Matthew Prescott, Loretta Dunne, Andrew Blain, James J. Bock, David H. Hughes, Simon Dye, Ivan K. Baldry, S. Serjeant, Stephen Anthony Eales, Rob Ivison, Lee S. Kelvin, Edo Ibar, B. Sibthorpe, Catherine Vlahakis, David L. Clements, David T. Hill, Enzo Pascale, D. Herranz, Rob Sharp, Jon Loveday, David Heath Jones, C. P. Pearson, Jonathan P. Gardner, Joaquin Vieira, John A. Peacock, Robbie Richard Auld, Ivan Valtchanov, P. van der Werf, Cristina Popescu, Jacopo Fritz, Lerothodi Leonard Leeuw, Asantha Cooray, Denis Burgarella, Saumyadip Samui, Mark Thompson, Steve Maddox, Peder Norberg, Michał J. Michałowski, David T. Frayer, Guilaine Lagache, M. López-Caniego, Daniel J. Smith, E. E. Rigby, G. de Zotti, Giulia Rodighiero, D. G. Bonfield, Matt J. Jarvis, Douglas Scott, Aaron S. G. Robotham, Richard J. Tuffs, J. González-Nuevo, Andrew M. Hopkins, Aliakbar Dariush, and Universidad de Cantabria
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, evolution [Galaxy], STAR-FORMATION, high-redshift [Galaxies], galaxies [Submillimeter], Black body, Atlas (anatomy), galaxies: high-redshift, INFRARED GALAXIES, 0103 physical sciences, HISTORY, Emissivity, medicine, Astrophysics::Solar and Stellar Astrophysics, DEEP FIELD SOUTH, COLD DUST, BLAST, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, Photometric redshift, QB, Physics, Galaxy: evolution, DEGREE EXTRAGALACTIC SURVEY, Science & Technology, 010308 nuclear & particles physics, Galaxies: high-redshift, Submillimeter: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Galaxy, Redshift, Spire, 0201 Astronomical And Space Sciences, medicine.anatomical_structure, Physics and Astronomy, Physical Sciences, astro-ph.CO, Spectral energy distribution, SKY SURVEY, UNIVERSE GALAXY SURVEY, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 5 páginas, 4 figuras, 1 tabla.-- Letter to the editor.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.-- et al., We present colour–colour diagrams of detected sources in the Herschel-ATLAS science demonstration field from 100 to 500 μm using both PACS and SPIRE. We fit isothermal modified black bodies to the spectral energy distribution (SED) to extract the dust temperature of sources with counterparts in Galaxy And Mass Assembly (GAMA) or SDSS surveys with either a spectroscopic or a photometric redshift. For a subsample of 330 sources detected in at least three FIR bands with a significance greater than 3σ, we find an average dust temperature of (28±8) K. For sources with no known redshift, we populate the colour–colour diagram with a large number of SEDs generated with a broad range of dust temperatures and emissivity parameters, and compare to colours of observed sources to establish the redshift distribution of this sample. For another subsample of 1686 sources with fluxes above 35 mJy at 350 μm and detected at 250 and 500 μm with a significance greater than 3σ, we find an average redshift of 2.2±0.6., Amblard, Barton, Cooray, Leeuw, Serra and Temi acknowledge support from NASA funds for US participants in Herschel through JPL. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.
Published: 2010
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137. Contribution of Lensed SCUBA Galaxies to the Cosmic Infrared Background

Author: L. R. Levenson, Andrew Blain, Michael Zemcov, and Mark Halpern
Subjects: Physics, Line-of-sight, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Lower limit, Galaxy, Luminosity, Gravitational lens, Space and Planetary Science, Cosmic infrared background, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The surface density of submillimeter (sub-mm) galaxies as a function of flux, usually termed the source number counts, constrains models of the evolution of the density and luminosity of starburst galaxies. At the faint end of the distribution, direct detection and counting of galaxies are not possible. However, gravitational lensing by clusters of galaxies allows detection of sources which would otherwise be too dim to study. We have used the largest catalog of sub-mm-selected sources along the line of sight to galaxy clusters to estimate the faint end of the 850 micron number counts; integrating to S = 0.10 mJy the equivalent flux density at 850 microns is v I_{v} = 0.24 +/- 0.03 nW/m^2/sr. This provides a lower limit to the extragalactic far-infrared background and is consistent with direct estimates of the full intensity from the FIRAS. The results presented here can help to guide strategies for upcoming surveys carried out with single dish sub-mm instruments., v3 matches published manuscript; small grammatical and typographical changes from v2
Published: 2010

138. The Stellar Mass Content of Submillimeter-Selected Galaxies

Author: Lee Armus, Ian Smail, Scott Chapman, Rob Ivison, Laura J. Hainline, David M. Alexander, and Andrew Blain
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Continuum (measurement), Stellar population, Evolution, Astrophysics::High Energy Astrophysical Phenomena, Formation, High-redshift, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Infrared, Power law, Galaxy, Redshift, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a new study of the stellar mass in a sample of ~ 70 submillimeter-selected galaxies (SMGs) with accurate spectroscopic redshifts. We fit combinations of stellar population synthesis models and power laws to the galaxies' observed-frame optical through mid-IR spectral energy distributions to separate stellar emission from non-stellar near-IR continuum. By separating the stellar emission from the non-stellar near-IR continuum, we find that ~ 50% of our sample have non-stellar continuum contributions of less than 10% in rest-frame H-band, but ~ 10% of our sample have non-stellar contributions greater than 50%. We find that the K-band luminosity of the non-stellar continuum emission is correlated with hard X-ray luminosity, indicating an AGN origin of the emission. Upon subtracting this AGN-contributed continuum component from all of the galaxies in our sample, we determine a lower median stellar mass for SMGs than previous studies, ~ 7 x 10^10 M_sun. We use constraints of the starburst time-scale from molecular gas studies to estimate the amount of fading our sample would undergo if they passively evolve after the starburst terminates. The results suggest that typical SMGs, while among the most massive galaxies at z ~ 2, are likely to produce descendants of similar mass and luminosity to L* galaxies in the local universe., accepted to ApJ, significant revisions in new version but conclusions unchanged
Published: 2010

139. HerMES: Halo Occupation Number and Bias Properties of Dusty Galaxies from Angular Clustering Measurements

Author: Duncan Farrah, Matthew Joseph Griffin, Rob Ivison, Hien Nguyen, David L. Clements, A. M. J. Mortier, G. Marsden, Chris Pearson, Denis Burgarella, Bruno Altieri, Jonathan Rawlings, Edo Ibar, L. R. Levenson, Benjamin L. Schulz, Gillian S. Wright, Paolo Serra, Jamie Stevens, N. Castro-Rodriguez, Joaquin Vieira, V. Buat, A. Omont, K. G. Isaak, L. Vigroux, Douglas Scott, K. Mitchell-Wynne, Michael Pohlen, D. Rigopoulou, A. J. Smith, C. K. Xu, Bruno Maffei, Lingyu Wang, Isaac Roseboom, P. Chanial, Ali Ahmad Khostovan, I. Perez-Fournon, S. C. Madden, E. Dwek, K. E. Tugwell, David L. Shupe, A. Amblard, Jason Glenn, D. Rizzo, Walter Kieran Gear, B. O'Halloran, Tom Babbedge, Lucia Marchetti, Antonio Cava, Michael Rowan-Robinson, Andreas Papageorgiou, A. Boselli, J. J. Bock, V. Arumugam, Alberto Franceschini, C. D. Dowell, P. Panuzzo, Mattia Vaccari, Robbie Richard Auld, D. Elbaz, Nick Seymour, Gwenifer Raymond, Mark Halpern, Robyn L. Ward, M. Trichas, M. Sanchez Portal, Asantha Cooray, Ivan Valtchanov, M. Fox, M. J. Page, Stephen Anthony Eales, G. Mainetti, Luca Conversi, H. Aussel, A. Conley, Guilaine Lagache, S. J. Oliver, Evanthia Hatziminaoglou, Michael Zemcov, Nanyao Y. Lu, M. Symeonidis, Andrew Blain, XMM-Newton Science Operations Centre, Agence Spatiale Européenne = European Space Agency (ESA), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Colloïdes et Matériaux Divisés (LCMD), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Division of Engineering, Colorado School of Mines, Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), Centre de recherches Paul Pascal (CRPP), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Institute of Water and Atmospheric Research [Wellington] (NIWA), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, Dark matter, FOS: Physical sciences, Flux, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, education, Cluster analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Angular correlation function, QB, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Dark matter halo, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Halo, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the angular correlation function, w(theta), from 0.5 to 30 arcminutes of detected sources in two wide fields of the Herschel Multi-tiered Extragalactic Survey (HerMES). Our measurements are consistent with the expected clustering shape from a population of sources that trace the dark matter density field, including non-linear clustering at arcminute angular scales arising from multiple sources that occupy the same dark matter halos. By making use of the halo model to connect the spatial clustering of sources to the dark matter halo distribution, we estimate source bias and halo occupation number for dusty sub-mm galaxies at z ~ 2. We find that sub-mm galaxies with 250 micron flux densities above 30 mJy reside in dark matter halos with mass above (5\pm4) x 10^12 M_sun, while (14\pm8)% of such sources appear as satellites in more massive halos., 5 pages; accepted for publication in A&A Special Issue on Herschel First Science Results (July 2010). HerMES information available at http://hermes.sussex.ac.uk/
Published: 2010

140. The HerMES SPIRE submillimeter local luminosity function

Author: T. Babbedge, E. A. González Solares, Eli Dwek, Giulia Rodighiero, B. O'Halloran, Matthew Joseph Griffin, Herve Aussel, L. Vigroux, Bruno Altieri, Mat Page, C. K. Xu, Gillian S. Wright, Stephen Anthony Eales, Evanthia Hatziminaoglou, Walter Kieran Gear, M. Sanchez Portal, Ismael Perez-Fournon, A. Amblard, Asantha Cooray, Alberto Franceschini, N. Lu, M. Symeonidis, N. Castro-Rodríguez, Antonio Cava, Lucia Marchetti, Michael Rowan-Robinson, V. Buat, Mattia Vaccari, Simon Dye, Rob Ivison, Lian-Tao Wang, Markos Trichas, A. J. Smith, Andrew Blain, James J. Bock, David Elbaz, Dimitra Rigopoulou, J. I. Rawlings, Michael Pohlen, V. Arumugam, L. Conversi, David L. Shupe, Isaac Roseboom, Alain Omont, Bruno Maffei, G. Mainetti, Elisabetta Valiante, D. Rizzo, A. Conley, Ivan Valtchanov, Kate Gudrun Isaak, Robyn L. Ward, Andreas Papageorgiou, J.-S. Huang, Suzanne C. Madden, Guilaine Lagache, Michael Zemcov, A. M. J. Mortier, Douglas Scott, Duncan Farrah, Pierre Chanial, M. Fox, Hien Nguyen, David L. Clements, C. D. Dowell, Robbie Richard Auld, Nick Seymour, Gwenifer Raymond, Jason Glenn, P. Panuzzo, Seb Oliver, Edo Ibar, L. R. Levenson, Alessandro Boselli, Benjamin L. Schulz, K. E. Tugwell, Mark Halpern, Chris Pearson, Denis Burgarella, Jamie Stevens, Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire Colloïdes et Matériaux Divisés (LCMD), ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), XMM-Newton Science Operations Centre, European Space Agency (ESA), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Division of Engineering, Colorado School of Mines, Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), Centre de recherches Paul Pascal (CRPP), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California-University of California, National Institute of Water and Atmospheric Research [Wellington] (NIWA), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Photometry (optics), 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Luminosity function (astronomy), Physics, education.field_of_study, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Spire, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric luminosity density in the local Universe, and Herschel offers the first opportunity to do so in an unbiased way by imaging large sky areas at several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0, Comment: Accepted for publication in the A&A Herschel Special Issue
Published: 2010

141. HerMES: The Submillimeter Spectral Energy Distributions of Herschel/SPIRE-Detected Galaxies

Author: Michael Pohlen, Ivan Valtchanov, Chris Pearson, A. Omont, A. J. Smith, Hien Nguyen, M. Fox, David L. Clements, Denis Burgarella, P. Chanial, Walter Kieran Gear, Bruno Maffei, N. Castro-Rodriguez, Jonathan Rawlings, Edo Ibar, K. G. Isaak, L. R. Levenson, Evanthia Hatziminaoglou, E. Giovannoli, Benjamin L. Schulz, Michael Zemcov, Stephen Anthony Eales, Jamie Stevens, Asantha Cooray, Angela M. J. Mortier, Nanyao Y. Lu, C. K. Xu, M. Symeonidis, L. Vigroux, Andrew Blain, I. Perez Fournon, Tom Babbedge, A. Amblard, S. J. Oliver, Jason Glenn, G. Marsden, Gillian S. Wright, B. O'Halloran, P. Panuzzo, D. Rigopoulou, J. J. Bock, Lingyu Wang, Elisabetta Valiante, A. Boselli, K. E. Tugwell, Rob Ivison, Mark Halpern, Robyn L. Ward, Douglas Scott, Bruno Altieri, C. D. Dowell, V. Buat, Robbie Richard Auld, D. Elbaz, Nick Seymour, Gwenifer Raymond, Antonio Cava, S. C. Madden, E. Dwek, David L. Shupe, D. Rizzo, V. Arumugam, Alberto Franceschini, Mattia Vaccari, M. Trichas, M. Sanchez Portal, Andreas Papageorgiou, G. Mainetti, Luca Conversi, H. Aussel, A. Conley, Lucia Marchetti, Michael Rowan-Robinson, Matthew Joseph Griffin, Guilaine Lagache, Mat Page, N. Rangwala, Isaac Roseboom, Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, submillimeter: galaxies, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Point source, Population, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Galaxy, Spire, Space and Planetary Science, galaxies: high-redshift, [SDU]Sciences of the Universe [physics], education, galaxies: evolution, Specific population, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present colours of sources detected with the Herschel/SPIRE instrument in deep extragalactic surveys of the Lockman Hole, Spitzer-FLS, and GOODS-N fields in three photometric bands at 250, 350 and 500 micrometers. We compare these with expectations from the literature and discuss associated uncertainties and biases in the SPIRE data. We identify a 500 micrometer flux limited selection of sources from the HerMES point source catalogue that appears free from neighbouring/blended sources in all three SPIRE bands. We compare the colours with redshift tracks of various contemporary models. Based on these spectral templates we show that regions corresponding to specific population types and redshifts can be identified better in colour-flux space. The redshift tracks as well as the colour-flux plots imply a majority of detected objects with redshifts at 1, Comment: 5 pages, 8 figures, for special Herschel issue
Published: 2010
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142. HerMES: Far-infrared properties of known AGN in the HerMES fields

Author: B. O'Halloran, Alberto Franceschini, Seb Oliver, Mattia Vaccari, Bruno Maffei, Guilaine Lagache, Eli Dwek, D. Rizzo, C. P. Pearson, Andreas Papageorgiou, Stephen Anthony Eales, Lifan Wang, Charles D. Dowell, Jamie Stevens, Kate Gudrun Isaak, Matthew Joseph Griffin, David Elbaz, Alexandre Amblard, Ivan Valtchanov, Michael Pohlen, C. K. Xu, D. L. Shupe, L. Conversi, Michael Zemcov, Isaac Roseboom, Pierre Chanial, V. Arumugam, Asantha Cooray, J. I. Rawlings, N. Castro-Rodriguez, Gillian S. Wright, Edo Ibar, E. A. González Solares, A. M. J. Mortier, Alain Omont, Douglas Scott, Jason Glenn, Markos Trichas, L. R. Levenson, Walter Kieran Gear, Benjamin L. Schulz, Antonio Cava, N. Lu, G. Mainetti, Lucia Marchetti, Michael Rowan-Robinson, Mark Halpern, Rob Ivison, P. Panuzzo, A. Conley, Simon Dye, A. J. Smith, V. Buat, Denis Burgarella, Alessandro Boselli, M. J. Page, Dimitra Rigopoulou, Herve Aussel, Robyn L. Ward, M. Sanchez Portal, K. E. Tugwell, Evanthia Hatziminaoglou, M. Symeonidis, Ismael Perez-Fournon, Robbie Richard Auld, Nick Seymour, M. Fox, Andrew Blain, James J. Bock, Suzanne C. Madden, L. Vigroux, Duncan Farrah, Hien Nguyen, David L. Clements, T. Babbedge, AUTRES, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Colloïdes et Matériaux Divisés (LCMD), ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Division of Engineering, Colorado School of Mines, Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), Centre de recherches Paul Pascal (CRPP), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California-University of California, National Institute of Water and Atmospheric Research [Wellington] (NIWA), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), and University of California (UC)-University of California (UC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, Astrophysics::High Energy Astrophysical Phenomena, Population, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Far infrared, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, Accretion (meteorology), 010308 nuclear & particles physics, Astronomy and Astrophysics, Torus, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Nuclear and starburst activity are known to often occur concomitantly. Herschel-SPIRE provides sampling of the FIR SEDs of type 1 and type 2 AGN, allowing for the separation between the hot dust (torus) and cold dust (starburst) emission. We study large samples of spectroscopically confirmed type 1 and type 2 AGN lying within the Herschel Multi-tiered Extragalactic Survey (HerMES) fields observed during the science demonstration phase, aiming to understand their FIR colour distributions and constrain their starburst contributions. We find that one third of the spectroscopically confirmed AGN in the HerMES fields have 5-sigma detections at 250um, in agreement with previous (sub)mm AGN studies. Their combined Spitzer-MIPS and Herschel-SPIRE colours - specifically S(250)/S(70) vs. S(70)/S(24) - quite clearly separate them from the non-AGN, star-forming galaxy population, as their 24-um flux is dominated by the hot torus emission. However, their SPIRE colours alone do not differ from those of non-AGN galaxies. SED fitting shows that all those AGN need a starburst component to fully account for their FIR emission. For objects at z > 2, we find a correlation between the infrared luminosity attributed to the starburst component, L(SB), and the AGN accretion luminosity, L(acc), with L(SB) propto L(acc)^0.35. Type 2 AGN detected at 250um show on average higher L(SB) than type 1 objects but their number is still too low to establish whether this trend indicates stronger star-formation activity., Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages
Published: 2010

143. HerMES: The SPIRE confusion limit

Author: Mark Halpern, Bruno Maffei, Robyn L. Ward, Jennifer L. Marshall, M. Fox, Dimitra Rigopoulou, Stephen Anthony Eales, G. Mainetti, Luca Conversi, N. Castro-Rodriguez, Hien Nguyen, H. Aussel, A. Conley, David L. Clements, Chris Pearson, Asantha Cooray, Alexandre Amblard, D. V. Wiebe, Mat Page, P. Chanial, Michael Pohlen, Edo Ibar, G. Marsden, Ivan Valtchanov, Gillian S. Wright, Douglas Scott, L. R. Levenson, L. Vigroux, B. O'Halloran, Benjamin L. Schulz, P. Panuzzo, James J. Bock, E. L. Chapin, Jamie Stevens, Walter Kieran Gear, K. E. Tugwell, Tom Babbedge, Michael Zemcov, Rob Ivison, A. Boselli, Lingyu Wang, S. C. Madden, V. Buat, Matthew Joseph Griffin, Andrew Blain, C. K. Xu, Antonio Cava, Evanthia Hatziminaoglou, Nanyao Y. Lu, M. Symeonidis, K. G. Isaak, Jason Glenn, Seb Oliver, Lucia Marchetti, Michael Rowan-Robinson, V. Arumugam, N. Rangwala, C. D. Dowell, D. Elbaz, Nick Seymour, Alberto Franceschini, Markos Trichas, Mattia Vaccari, D. L. Shupe, Isaac Roseboom, A. Omont, A. J. Smith, Andreas Papageorgiou, I. Perez-Fournon, E. Dwek, D. Rizzo, Guilaine Lagache, Centre de recherches Paul Pascal (CRPP), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Colloïdes et Matériaux Divisés (LCMD), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Division of Engineering, Colorado School of Mines, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Institute of Water and Atmospheric Research [Wellington] (NIWA), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of California-University of California, ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), CEA-Direction de l'Energie Nucléaire (CEA-DEN), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN)
Subjects: Time delay and integration, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Measure (physics), FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, law, 0103 physical sciences, medicine, Limit (mathematics), 010303 astronomy & astrophysics, QB, Confusion, media_common, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Photometer, Spire, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], medicine.symptom, Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on the sensitivity of SPIRE photometers on the Herschel Space Observatory. Specifically, we measure the confusion noise from observations taken during the Science Demonstration Phase of the Herschel Multi-tiered Extragalactic Survey. Confusion noise is defined to be the spatial variation of the sky intensity in the limit of infinite integration time, and is found to be consistent among the different fields in our survey at the level of 5.8, 6.3 and 6.8 mJy/beam at 250, 350 and 500 microns, respectively. These results, together with the measured instrument noise, may be used to estimate the integration time required for confusion-limited maps, and provide a noise estimate for maps obtained by SPIRE., Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages
Published: 2010

144. MID-INFRARED SPECTROSCOPY OF CANDIDATE ACTIVE GALACTIC NUCLEI-DOMINATED SUBMILLIMETER GALAXIES

Author: Eiichi Egami, Karín Menéndez-Delmestre, Scott Chapman, Kristen Coppin, J. E. Austermann, Rob Ivison, Edo Ibar, Michael Rowan-Robinson, A. M. Swinbank, Andrew Blain, David H. Hughes, J. Gabor, M. S. Yun, James Dunlop, Duncan Farrah, Mattia Vaccari, Chris Simpson, David L. Clements, Douglas Scott, Ian Smail, Loretta Dunne, A. M. J. Mortier, Simon Dye, David M. Alexander, Mat Page, A. Pope, and Science and Technology Facilities Council (STFC)
Subjects: submillimeter: galaxies, ULTRALUMINOUS INFRARED GALAXIES, Active galactic nucleus, 0306 Physical Chemistry (Incl. Structural), Active, Evolution, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, High-redshift, galaxies: starburst, Starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, LUMINOUS GALAXIES, LOCKMAN HOLE, 01 natural sciences, Mid infrared spectroscopy, 0305 Organic Chemistry, infrared: galaxies, STAR-FORMATION, galaxies: high-redshift, Submillimeter, 0103 physical sciences, Spectroscopy, NUMBER COUNTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, SPITZER-SPACE-TELESCOPE, Physics, DEGREE EXTRAGALACTIC SURVEY, Science & Technology, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies, Galaxy, Redshift, DUST-OBSCURED GALAXIES, 0201 Astronomical And Space Sciences, 13. Climate action, Space and Planetary Science, Physical Sciences, astro-ph.CO, DEEP-FIELD-SOUTH, Astrophysics::Earth and Planetary Astrophysics, HIGH-REDSHIFT, galaxies: evolution, Infrared
Abstract: Spitzer spectroscopy has revealed that ≃80% of submm galaxies (SMGs) are starburst (SB)-dominated in the mid-infrared. Here we focus on the remaining ≃20% that show signs of harboring powerful active galactic nuclei (AGNs). We have obtained Spitzer-InfraRed Spectrograph spectroscopy of a sample of eight SMGs that are candidates for harboring powerful AGNs on the basis of IRAC color selection (S_(8 μm)/S_(4.5 μm) > 2, i.e., likely power-law mid-infrared spectral energy distributions). SMGs with an AGN dominating (≳50%) their mid-infrared emission could represent the "missing link" sources in an evolutionary sequence involving a major merger. First of all, we detect polycyclic aromatic hydrocarbon (PAH) features in all of the SMGs, indicating redshifts from 2.5 to 3.4, demonstrating the power of the mid-infrared to determine redshifts for these optically faint dusty galaxies. Second, we see signs of both star formation (from the PAH features) and AGN activity (from continuum emission) in our sample: 62% of the sample are AGN-dominated in the mid-infrared with a median AGN content of 56%, compared with 1.65 works well at selecting mid-infrared energetically dominant AGNs in SMGs, implying a duty cycle of ~15% if all SMGs go through a subsequent mid-infrared AGN-dominated phase in the proposed evolutionary sequence.
Published: 2010
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145. High-resolution CO and radio imaging of ULIRGs: extended CO structures and implications for the universal star formation law

Author: Robert Beswick, R. Neri, Caitlin M. Casey, T. W. B. Muxlow, R. Genzel, Andrew Blain, Scott Chapman, A. D. Biggs, Rob Ivison, Robert C. Kennicutt, Ian Smail, Linda J. Tacconi, A. Omont, Thomas R. Greve, Frank Bertoldi, Pierre Cox, and Matt Bothwell
Subjects: Luminous infrared galaxy, Physics, Radio galaxy, Star formation, Astronomy and Astrophysics, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, Star (graph theory), Galaxy, Stars, Space and Planetary Science, Law, Astrophysics::Galaxy Astrophysics
Abstract: We present high spatial resolution (0.4", ~3.5 kpc) PdBI interferometric data on three ultra-luminous infrared galaxies (ULIRGs) at z~2: two submillimetre galaxies and one submillimetre faint star forming radio galaxy. The three galaxies have been ro- bustly detected in CO rotational transitions, either 12CO(J=4-3) or 12CO(J=3-2), allowing their sizes and gas masses to be accurately constrained. These are the highest spatial resolution observations observed to date (by a factor of ~2) for intermediate-excitation CO emission in z~2 ULIRGs. The galaxies appear extended over several resolution elements, having a mean radius of 3.7 kpc. High-resolution (0.3") combined MERLIN-VLA observations of their radio continua allow an analysis of the star formation behaviour of these galaxies, on comparable spatial scales to that of the CO observations. This 'matched beam' approach sheds light on the spatial distribution of both molecular gas and star formation, and we can therefore calculate accurate star formation rates and gas surface densities: this allows us to place the three systems in the context of a Kennicutt-Schmidt (KS)-style star formation law. We find a difference in size between the CO and radio emission regions, and as such we suggest that using the spatial extent of the CO emission region to estimate the surface density of star formation may lead to error. This size difference also causes the star formation efficiencies within systems to vary by up to a factor of 5. We also find, with our new accurate sizes, that SMGs lie significantly above the KS relation, indicating that stars are formed more efficiently in these extreme systems than in other high-z star forming galaxies.
Published: 2010
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146. First detection of the Sunyaev Zel'dovich effect increment at λ < 650 μm

Author: G. Rodighiero, Miroslava Dessauges-Zavadsky, C. D. Dowell, Daniel Schaerer, D. Fadda, Dieter Lutz, M. Rex, Eiichi Egami, R. Pello, C. Bridge, George H. Rieke, M. J. Pereira, Gregory Walth, Bruno Altieri, Rob Ivison, O. Ilbert, Francoise Combes, J. P. Kneib, P. van der Werf, T. D. Rawle, P. G. Pérez-González, Graham P. Smith, B. Clement, I. Valtchanov, J. Richard, Mathilde Jauzac, J. J. Bock, Frederic Boone, Michael Zemcov, Andrew Blain, M. W. Werner, AUTRES, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Steward Observatory, University of Arizona, XMM-Newton Science Operations Centre, European Space Agency (ESA), Department of Astronomy, California Institute of Technology (CALTECH), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Royal Observatory Edinburgh (ROE), University of Edinburgh, Max-Planck-Institut für Extraterrestrische Physik (MPE), Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), University of Bristol [Bristol], University of Reading (UOR), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Agence Spatiale Européenne = European Space Agency (ESA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université de Genève = University of Geneva (UNIGE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universiteit Leiden
Subjects: Physics, Astrofísica, 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Astronomy and Astrophysics, Astrophysics, cosmic background radiation, Sunyaev–Zel'dovich effect, Lambda, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomía, Wavelength, Spire, individual: 1E0657-56, Space and Planetary Science, galaxies: clusters, Distortion, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
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 lambda > 1.3 mm, an increment at shorter wavelengths, and small again by lambda ~250 um. As part of the Herschel Lensing Survey (HLS) we have mapped 1E0657-56 (the Bullet cluster) with SPIRE with bands centered at 250, 350 and 500 um and have detected the SZ effect at the two longest wavelengths. The measured SZ effect increment central intensities are Delta I_{0} = 0.097 +- 0.019 MJy sr^{-1} at 350 um and Delta I_{0} = 0.268 +- 0.031 MJy sr^{-1} at 500 um, 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 sigma, 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., Comment: Accepted for publication in Astronomy and Astrophysics (Herschel special issue)
Published: 2010
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147. The Herschel Lensing Survey (HLS): Overview

Author: Michael Zemcov, Miroslava Dessauges-Zavadsky, Dieter Lutz, I. Valtchanov, Eiichi Egami, Giulia Rodighiero, George H. Rieke, A. Omont, M. J. Pereira, Johan Richard, Daniel Schaerer, Gregory Walth, James J. Bock, D. Fadda, Jean-Paul Kneib, Rob Ivison, Pablo G. Pérez-González, P. van der Werf, Andrew Blain, Francoise Combes, T. D. Rawle, Frédéric Boone, M. W. Werner, C. Bridge, Graham P. Smith, M. Rex, L. Metcalfe, Bruno Altieri, G. Tramoy, O. Ilbert, C. D. Dowell, Ian Smail, R. Pello, B. Clement, Mathilde Jauzac, Steward Observatory, University of Arizona, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), XMM-Newton Science Operations Centre, European Space Agency (ESA), AUTRES, Department of Astronomy, California Institute of Technology (CALTECH), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Royal Observatory Edinburgh (ROE), University of Edinburgh, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institute for Computational Cosmology (ICC), Durham University, University of Alabama at Birmingham [ Birmingham] (UAB), University of Bristol [Bristol], University of Reading (UOR), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), École normale supérieure - Paris (ENS-PSL), Université de Genève = University of Geneva (UNIGE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universiteit Leiden
Subjects: Astrofísica, submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Evolution, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Strong gravitational lensing, High-redshift, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Preliminary analysis, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, 0103 physical sciences, medicine, Cluster (physics), Submillimeter, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Confusion, Physics, galaxies, 010308 nuclear & particles physics, Clusters, Astronomy and Astrophysics, Galaxies, Galaxy, Astronomía, Spire, Space and Planetary Science, medicine.symptom, Infrared, galaxies: evolution, clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Herschel Lensing Survey (HLS) will conduct deep PACS and SPIRE imaging of ~40 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 Universe 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, allowing us to study not only the background high-redshift galaxies (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., Accepted for publication in Astronomy and Astrophysics (Herschel special issue)
Published: 2010
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148. The far-infrared/submillimeter properties of galaxies located behind the Bullet cluster

Author: Cathy Horellou, Itziar Aretxaga, Bruno Altieri, Ivan Valtchanov, Carrie Bridge, Graham P. Smith, Michael Zemcov, Eiichi Egami, Kimberly S. Scott, Olivier Ilbert, Ian Smail, Jean-Paul Kneib, T. D. Rawle, Francoise Combes, Pablo G. Pérez-González, Daniel Schaerer, Gregory Walth, P. van der Werf, Dario Fadda, Johan Richard, Hajime Ezawa, David H. Hughes, M. S. Yun, A. K. Fiedler, Giulia Rodighiero, Andrew Blain, James J. Bock, R. Pello, Daniel Johansson, Rob Ivison, Grant W. Wilson, Kotaro Kohno, Alain Omont, Marie Rex, Frédéric Boone, Sun Mi Chung, Jason E. Austermann, Thushara Perera, Dieter Lutz, Ryohei Kawabe, George H. Rieke, M. J. Pereira, Benjamin Clément, Michael W. Werner, Miroslava Dessauges-Zavadsky, Anthony H. Gonzalez, Mathilde Jauzac, C. D. Dowell, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Steward Observatory, University of Arizona, Departamento de Física y Astronomía, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), XMM-Newton Science Operations Centre, Agence Spatiale Européenne = European Space Agency (ESA), Institute for Computational Cosmology (ICC), Durham University, Department of Astronomy, California Institute of Technology (CALTECH), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Royal Observatory Edinburgh (ROE), University of Edinburgh, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), University of Bristol [Bristol], University of Reading (UOR), Leiden Observatory [Leiden], Universiteit Leiden, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), European Space Agency (ESA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Universiteit Leiden [Leiden]
Subjects: submillimeter: galaxies, Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Evolution, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Population, High-redshift, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Far infrared, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Submillimeter, education, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, gravitational lensing: strong, Astronomy and Astrophysics, Galaxies, Galaxy, Astronomía, Gravitational lens, Space and Planetary Science, galaxies: clusters: general, Astrophysics::Earth and Planetary Astrophysics, Infrared, Gravitational lensing, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
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 100-500 micron 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 micron and AzTEC 1.1 mm data we fully constrain the spectral energy distributions of 19 MIPS 24 micron 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., Comment: 8 pages with 4 figures. Accepted for publication in Astronomy and Astrophysics (Herschel special issue)
Published: 2010
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149. A Hubble Space Telescope NICMOS and ACS Morphological Study of z~2 Submillimetre Galaxies

Author: Colin Borys, Mark Swinbank, Andrew Blain, Ian Smail, Laura J. Hainline, Rob Ivison, D. M. Alexander, Christopher J. Conselice, and Scott Chapman
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, Hubble space telescope, 0103 physical sciences, Elliptical galaxy, Astrophysics::Solar and Stellar Astrophysics, Stellar structure, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a quantitative morphological analysis using HST NICMOS H160- and ACS I775- band imaging of 25 spectroscopically confirmed submillimetre galaxies (SMGs) which have redshifts between z=0.7-3.4. Our analysis also employs a comparison sample of more typical star-forming galaxies at similar redshifts (such as LBGs) which have lower far-infrared luminosities. This is the first large-scale study of the morphologies of SMGs in the near-infrared at ~0.1" resolution (, Accepted for publication in MNRAS. 12 pages, 8 figs. High resolution version available at: http://astro.dur.ac.uk/~ams/papers/smg_morph.pdf
Published: 2010
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150. HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

Author: Bruno Maffei, N. Castro-Rodriguez, Asantha Cooray, Angela M. J. Mortier, L. Vigroux, Denis Burgarella, M. J. Page, G. Wright, Chris Pearson, P. Panuzzo, A. Amblard, Joaquin Vieira, B. O'Halloran, Seb Oliver, Walter Kieran Gear, S. C. Madden, P. Chanial, C. K. Xu, Andreas Papageorgiou, Jonathan Rawlings, Tom Babbedge, I. Valtchanov, Mark Halpern, K. G. Isaak, Rob Ivison, Bruno Altieri, V. Buat, Robyn L. Ward, Jason Glenn, V. Arumugam, D. Rigopoulou, D. L. Clements, M. Fox, Alberto Franceschini, K. E. Tugwell, Douglas Scott, Lingyu Wang, Mattia Vaccari, Benjamin L. Schulz, G. Mainetti, A. Boselli, Richard S. Savage, Elisabetta Valiante, Antonio Cava, Luca Conversi, Alex Conley, C. D. Dowell, A. Omont, H. Aussel, I. Perez-Fournon, Jamie Stevens, Robbie Richard Auld, E. Dwek, D. Elbaz, G. Lagache, David L. Shupe, Nick Seymour, Gwenifer Raymond, D. Rizzo, E. Ibar, M. Trichas, M. Sanchez Portal, H. T. Nguyen, Isaac Roseboom, J. J. Bock, Evanthia Hatziminaoglou, Louis Levenson, M. Pohlen, Michael Zemcov, Nanyao Y. Lu, M. Symeonidis, Andrew Blain, Andrew Smith, Lucia Marchetti, Michael Rowan-Robinson, K. Mitchell-Wynne, Steve Eales, Matthew Joseph Griffin, British Antarctic Survey (BAS), Natural Environment Research Council (NERC), XMM-Newton Science Operations Centre, Agence Spatiale Européenne = European Space Agency (ESA), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Colloïdes et Matériaux Divisés (LCMD), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Division of Engineering, Colorado School of Mines, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), Centre de recherches Paul Pascal (CRPP), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Institute of Water and Atmospheric Research [Wellington] (NIWA), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of California-University of California, ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), CEA-Direction de l'Energie Nucléaire (CEA-DEN), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN)
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Age of the universe, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Wavelength, Spire, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Population evolution, Space and Planetary Science, 0103 physical sciences, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, QB
Abstract: Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts at, Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages
Published: 2010
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