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Your search keyword '"Pearson, C. P."' showing total 19 results
Start Over Author "Pearson, C. P." Topic astrophysics::galaxy astrophysics
19 results on '"Pearson, C. P."'

1. Polycyclic aromatic hydrocarbon (PAH) luminous galaxies at z~1

Author

Pearson, C. P., Lee, H. M., Im, M., Lee, M. G., Shim, H., White, G.J., Serjeant, S., Malkan, M., Takagi, Toshinobu, Ohyama, Yoichi, Goto, Tomotsugu, Matsuhara, Hideo, Oyabu, Shinki, Wada, Takehiko, Hanami, Hitoshi, Ishigaki, Takeshi, and Imai, K.

Subjects
Luminous infrared galaxy, Physics, education.field_of_study, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy formation and evolution, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数：17名, Accepted: 2010-02-17, 資料番号: SA1000740000

Published
2010

2. The Herschel Multi-tiered Extragalactic Survey: HerMES

Author

HerMES Collaboration, Oliver, S. J., Bock, J., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Beelen, A., Béthermin, M., Blain, A., Boselli, A., Bridge, C., Brisbin, D., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Chanial, P., Cirasuolo, M., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dubois, E. N., Dwek, E., Dye, S., Eales, S., Elbaz, D., Farrah, D., Feltre, A., Ferrero, P., Fiolet, N., Fox, M., Franceschini, A., Gear, W., Giovannoli, E., Glenn, J., Gong, Y., Solares, E. A. González, Griffin, M., Halpern, M., Harwit, M., Hatziminaoglou, E., Heinis, S., Hurley, P., Hwang, H. S., Hyde, A., Ibar, E., Ilbert, O., Isaak, K., Ivison, R. J., Lagache, G., Floc'h, E. Le, Levenson, L., Faro, B. Lo, Lu, N., Madden, S., Maffei, B., Magdis, G., Mainetti, G., Marchetti, L., Marsden, G., Marshall, J., Mortier, A. M. J., Nguyen, H. T., O'Halloran, B., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Patel, H., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rawlings, J. I., Raymond, G., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sánchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Vigroux, L., Wang, L., Ward, R., Wardlow, J., Wright, G., Xu, C. K., Zemcov, M., Science and Technology Facilities Council (STFC), 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
ULTRALUMINOUS INFRARED GALAXIES, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, infrared: galaxies, surveys, SUBMILLIMETER-SELECTED GALAXIES, LARGE-SCALE STRUCTURE, Astrophysics::Galaxy Astrophysics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 1200-MU-M MAMBO SURVEY, STAR-FORMATION HISTORY, 160 MU-M, POLE TELESCOPE SURVEY, 0201 Astronomical And Space Sciences, QB0495, [SDU]Sciences of the Universe [physics], Physical Sciences, GOODS-N FIELD, astro-ph.CO, DEEP-FIELD-SOUTH, galaxies: evolution, submillimetre: galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Herschel Multi-tiered Extragalactic Survey, HerMES, is a legacy program designed to map a set of nested fields totalling ~380 deg^2. Fields range in size from 0.01 to ~20 deg^2, using Herschel-SPIRE (at 250, 350 and 500 \mu m), and Herschel-PACS (at 100 and 160 \mu m), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the re-processed optical and ultra-violet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multi-wavelength understanding of galaxy formation and evolution. The survey will detect of order 100,000 galaxies at 5\sigma in some of the best studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to: facilitate redshift determination; rapidly identify unusual objects; and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include: the total infrared emission of galaxies; the evolution of the luminosity function; the clustering properties of dusty galaxies; and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results., Comment: 23 pages, 17 figures, 9 Tables, MNRAS accepted

Published
2012
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3. The Herschel Multi-tiered Extragalactic Survey: SPIRE-mm photometric redshifts

Author

Roseboom, I. G., Ivison, R. J., Greve, T. R., Amblard, A., Arumugam, V., Auld, R., Aussel, H., Bethermin, M., Blain, A., Bock, J., Boselli, A., Brisbin, D., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Chanial, P., Chapin, E., Chapman, S., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dunlop, J. S., Dwek, E., Eales, S., Elbaz, D., Farrah, D., Franceschini, A., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Marsden, G., Morrison, G., Mortier, A. M. J., Nguyen, H. T., O’Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rawlings, J. I., Raymond, G., Rigopoulou, D., Rizzo, D., Rodighiero, G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M. P., Vigroux, L., Wardlow, J., Wang, L., Wright, G., Xu, C. K., Zemcov, M., Department of Physics and Astronomy [Brighton] (DPA), University of Sussex, Royal Observatory Edinburgh (ROE), University of Edinburgh, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UCI), University of California-University of California, School of Physics and Astronomy [Cardiff], Cardiff University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), California Institute of Technology (CALTECH), CHANG, Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), Department of Astronomy [Ithaca], Cornell University, Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), University of British Columbia (UBC), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, 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), NASA Goddard Space Flight Center (GSFC), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, Department of Astrophysical and Planetary Sciences [Boulder], European Southern Observatory (ESO), 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), Infrared Processing and Analysis Center (IPAC), School of Physics and Astronomy [Manchester], University of Manchester [Manchester], Visual servoing in robotics, computer vision, and augmented reality (Lagadic), Inria Sophia Antipolis - Méditerranée (CRISAM), Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria)-Inria Rennes – Bretagne Atlantique, Institut National de Recherche en Informatique et en Automatique (Inria)-SIGNAUX ET IMAGES NUMÉRIQUES, ROBOTIQUE (IRISA-D5), Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-CentraleSupélec-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Université de Rennes (UNIV-RENNES)-CentraleSupélec-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Rennes (ENS Rennes)-Télécom Bretagne-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-CentraleSupélec, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), 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), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), 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 Lethbridge, Department of Physics [Oxford], University of Oxford [Oxford], Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, 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), CHANG (CHANG), Laboratoire d'étude des transferts en hydrologie et environnement (LTHE), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), 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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), 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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Cornell University [New York], CentraleSupélec-Télécom Bretagne-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National de Recherche en Informatique et en Automatique (Inria)-École normale supérieure - Rennes (ENS Rennes)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-CentraleSupélec-Télécom Bretagne-Université de Rennes 1 (UR1), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-École normale supérieure - Rennes (ENS Rennes)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Smithsonian Institution-Harvard University [Cambridge], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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 des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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 des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-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), 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), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), University of Oxford, Harvard University-Smithsonian Institution, and California Institute of Technology (CALTECH)-NASA

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the potential of submm-mm and submm-mm-radio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 {\mu}m by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm-sources with reliable radio identifications in the GOODS-N and Lockman Hole North fields 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm-sources are adequately described by a modified blackbody with constant optical depth {\tau} = ({\nu}/{\nu}0)^{\beta} where {\beta} = +1.8 and {\nu}0 = c/100 {\mu}m. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation we derive photometric redshift estimates for the 46 SPIRE detected mm-sources. Testing against the 22 sources with known spectroscopic, or good quality optical/near-IR photometric, redshifts we find submm/mm photometric redshifts offer a redshift accuracy of |z|/(1+z) = 0.16 (< |z| >= 0.51). Including constraints from the radio-far IR correlation the accuracy is improved to |z|/(1 + z) = 0.15 (< |z| >= 0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to ~ 850 {\mu}m selected samples., Comment: 17 pages, 7 figures, accepted for publication in MNRAS

Published
2012
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4. HerMES: detection of cosmic magnification of submillimetre galaxies using angular cross-correlation

Author

Wang, L., Cooray, A., Farrah, D., Amblard, A., Auld, R., Bock, J., Brisbin, D., Burgarella, D., Chanial, P., Clements, D. L., Eales, S., Franceschini, A., Glenn, J., Gong, Y., Griffin, M., Heinis, S., Ibar, E., Ivison, R. J., Mortier, A. M. J., Oliver, S. J., Page, M. J., Papageorgiou, A., Pearson, C. P., P��rez-Fournon, I., Pohlen, M., Rawlings, J. I., Raymond, G., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Scott, Douglas, Serra, P., Seymour, N., Smith, A. J., Symeonidis, M., Tugwell, K. E., Vaccari, M., Vieira, J. D., Vigroux, L., Wright, G., Laboratoire d'Astrophysique de Marseille (LAM), 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), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Cosmic magnification is due to the weak gravitational lensing of sources in the distant Universe by foreground large-scale structure leading to coherent changes in the observed number density of the background sources. Depending on the slope of the background source number counts, cosmic magnification causes a correlation between the background and foreground galaxies, which is unexpected in the absence of lensing if the two populations are spatially disjoint. Previous attempts using submillimetre (sub-mm) sources have been hampered by small number statistics. The large number of sources detected in the {\it Herschel} Multi-tiered Extra-galactic Survey (HerMES) Lockman-SWIRE field enables us to carry out the first robust study of the cross-correlation between sub-mm sources and sources at lower redshifts. Using ancillary data we compile two low-redshift samples from SDSS and SWIRE with ~ 0.2 and 0.4, respectively, and cross-correlate with two sub-mm samples based on flux density and colour criteria, selecting galaxies preferentially at z ~ 2. We detect cross-correlation on angular scales between ~1 and 50 arcmin and find clear evidence that this is primarily due to cosmic magnification. A small, but non-negligible signal from intrinsic clustering is likely to be present due to the tails of the redshift distribution of the sub-mm sources overlapping with those of the foreground samples., Comment: 7 pages, 2 figues, accepted for publication in MNRAS

Published
2011
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5. Modeling of the HERMES J105751.1+573027 submillimeter source lensed by a dark matter dominated foreground group of galaxies

Author

Gavazzi, R., Cooray, A., Conley, A., Aguirre, J. E., Amblard, A., Auld, R., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Fu, H., Glenn, J., Solares, E. A. González, Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Kim, S., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., Matsuhara, H., Mortier, A. M. J., Murphy, E., Naylor, B. J., Neri, R., Nguyen, H. T., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rangwala, N., Rawlings, J. I., Raymond, G., Riechers, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Scott, K. S., Serra, P., Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Tugwell, K. E., Vaccari, M., Valiante, E., Valtchanov, I., Verma, A., Vieira, J. D., Vigroux, L., Wang, L., Wardlow, J., Wiebe, D., Wright, G., Xu, C. K., Zeimann, G., Zemcov, M., and Zmuidzinas, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the results of a gravitational lensing analysis of the bright $\zs=2.957$ sub-millimeter galaxy (SMG), HERMES J105751.1+573027 found in {\it Herschel}/SPIRE Science Demonstration Phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high resolution imaging available in optical and Near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allow us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be $\mu=10.9\pm 0.7$. We measure the half-light radius $R_{\rm eff}$ of the source in the rest-frame Near-UV and $V$ bands that characterize the unobscured light coming from stars and find $R_{\rm eff,*}= [2.0 \pm 0.1]$ kpc, in good agreement with recent studies on the Submillimeter Galaxy population. This lens model is also used to estimate the size of the gas distribution ($R_{\rm eff,gas}= [1.1\pm0.5]$) kpc by mapping back in the source plane the CO (J=5-4) transition line emission. The lens modeling yields a relatively large Einstein radius $R_{\rm Ein}= 4\farcs10 \pm 0\farcs02$, corresponding to a deflector velocity dispersion of [$483\pm 16] \,\kms$. This shows that HERMES J105751.1+573027 is lensed by a {\it galaxy group-size} dark matter halo at redshift $\zl\sim 0.6$. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with $f_{\rm dm}(, Comment: Submitted to ApJ

Published
2011
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6. Cold dust and young starbursts: spectral energy distributions of Herschel SPIRE sources from the HerMES survey

Author

ROWAN ROBINSON, M, Roseboom, I. G., Vaccari, M, Amblard, A, Arumugam, V, Auld, R, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Brisbin, D, Buat, V, Burgarella, D, CASTRO RODRIGUEZ, N, Cava, A, Chanial, P, Clements, D. L., Conley, A, Conversi, L, Cooray, A, Dowell, C. D., Dwek, E, Dye, S, Eales, S, Elbaz, D, Farrah, D, Fox, M, Franceschini, Alberto, Gear, W, Glenn, J, Gonzãlez, SOLARES E. A., Griffin, M, Halpern, M, Hatziminaoglou, E, Huang, J, Ibar, E, Isaak, K, Ivison, R. J., Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, Gabriele, Marchetti, L, Mortier, A. M. J., Nguyen, H. T., O'Halloran, B, Oliver, S. J., Omont, A, Page, M. J., Panuzzo, P, Papageorgiou, A, Patel, H, Pearson, C. P., Perez, FOURNON I., Pohlen, M, Rawlings, J. I., Raymond, G, Rigopoulou, D, Rizzo, D, Schulz, B, Scott, Douglas, Seymour, N, Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M, Trichas, M, Tugwell, K. E., Valtchanov, I, Vigroux, L, Wang, L, Ward, R, Wright, G, C. K., Xu, and Zemcov, M.

Subjects
Astrophysics::Solar and Stellar Astrophysics, galaxies: evolution, galaxies: starburst, galaxies: star formation, cosmology: observations, infrared: galaxies, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present spectral energy distributions (SEDs) for 68 Herschel sources detected at 5σ at 250, 350 and 500 μm in the HerMES SWIRE-Lockman field. We explore whether existing models for starbursts, quiescent star-forming galaxies and active galactic nucleus dust tori are able to model the full range of SEDs measured with Herschel. We find that while many galaxies ( 56 per cent) are well fitted with the templates used to fit IRAS, Infrared Space Observatory (ISO) and Spitzer sources, for about half the galaxies two new templates are required: quiescent ('cirrus') models with colder (10-20 K) dust and a young starburst model with higher optical depth than Arp 220. Predictions of submillimetre fluxes based on model fits to 4.5-24 μm data agree rather poorly with the observed fluxes, but the agreement is better for fits to 4.5-70 μm data. Herschel galaxies detected at 500 μm tend to be those with the highest dust masses. © 2010 The Authors. Journal compilation © 2010 RAS.

Published
2010

7. HerMES: SPIRE detection of high-redshift massive compact galaxies in GOODS-N field

Author

Cava, A., Rodighiero, G., Perez-Fournon, I., Buitrago, F., Trujillo, I., Altieri, B., Amblard, A., Auld, R., Bock, J., Brisbin, D., Burgarella, D., Castro-Rodriguez, N., Chanial, P., Cirasuolo, M., Clements, D. L., Conselice, C. J., Cooray, A., Eales, S., Elbaz, D., Ferrero, P., Franceschini, A., Glenn, J., Solares, E. A. Gonzalez, Griffin, M., Ibar, E., Ivison, R. J., Marchetti, L., Morrison, G. E., Mortier, A. M. J., Oliver, S. J., Page, M. J., Papageorgiou, A., Pearson, C. P., Pohlen, M., Rawlings, J. I., Raymond, G., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Scott, D., Seymour, N., Smith, A. J., Symeonidis, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Vigroux, L., Wang, L., Wright, G., 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), School of Physics and Astronomy [Cardiff], and Cardiff University

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], galaxies: evolution, galaxies: high-redshift, galaxies: star formation, infrared: galaxies, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], Astrophysics::Galaxy Astrophysics, evolution [galaxies], high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have analysed the rest-frame far infrared (FIR) properties of a sample of massive (Mstar > 10^11Msun) galaxies at 2, Comment: 6 pages, 3 figure, 1 table, MNRAS Herschel issue, in V2 added references and corrected typos

Published
2010
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8. The Deep SPIRE HerMES Survey: spectral energy distributions and their astrophysical indications at high redshift

Author

Brisbin, D., Harwit, M., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodriguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Elbaz, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, Guilaine, Levenson, L., Lonsdale, Carol J., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Owen, F. N., Pannella, M., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rizzo, D., Roseboom, I. G., Rowan-Robinson, M., Sanchez Portal, M., Schulz, B., Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Strazzullo, V., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vigroux, L., Wang, L., Ward, R., Wright, Gavin, Xu, C. K., Zemcov, M., 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), Brisbin, D, Harwit, M, Altieri, B, Amblard, A, Arumugam, V, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Buat, V, Castro-Rodriguez, N, Cava, A, Chanial, P, Clements, Dl, Conley, A, Conversi, L, Cooray, A, Dowell, Cd, Dwek, E, Eales, S, Elbaz, D, Fox, M, Franceschini, A, Gear, W, Glenn, J, Griffin, M, Halpern, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, Rj, Lagache, G, Levenson, L, Lonsdale, Cj, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Morrison, Ge, Nguyen, Ht, O'Halloran, B, Oliver, Sj, Omont, A, Owen, Fn, Pannella, M, Panuzzo, P, Papageorgiou, A, Pearson, Cp, Perez-Fournon, I, Pohlen, M, Rizzo, D, Roseboom, Ig, Rowan-Robinson, M, Portal, M, Schulz, B, Seymour, N, Shupe, Dl, Smith, Aj, Stevens, Ja, Strazzullo, V, Symeonidis, M, Trichas, M, Tugwell, Ke, Vaccari, M, Valtchanov, I, Vigroux, L, Wang, L, Ward, R, Wright, G, Xu, Ck, and Zemcov, M

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Spectral and Photometric Imaging Receiver (SPIRE) on Herschel has been carrying out deep extragalactic surveys, one of whose aims is to establish spectral energy distributions (SED)s of individual galaxies spanning the infrared/submillimeter (IR/SMM) wavelength region. We report observations of the (IR/SMM) emission from the Lockman North field (LN) and Great Observatories Origins Deep Survey field North (GOODS-N). Because galaxy images in the wavelength range covered by Herschel generally represent a blend with contributions from neighboring galaxies, we present sets of galaxies in each field especially free of blending at 250, 350, and 500 microns. We identify the cumulative emission of these galaxies and the fraction of the far infrared cosmic background radiation they contribute. Our surveys reveal a number of highly luminous galaxies at redshift z ~< 3 and a novel relationship between infrared and visible emission that shows a dependence on luminosity and redshift., 9 pages, 3 large tables, 2 tables in text, 5 figures Accepted for publication in MNRAS

Published
2010
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9. HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

Author

Glenn, J., Conley, A., Béthermin, M., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodríguez, N., Cava, A., Chanial, P., Clements, D. L., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Elbaz, D., Ellsworth-Bowers, T. P., Fox, M., Franceschini, A., Gear, W., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Laurent, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Marsden, G., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rigopoulou, D., Rizzo, D., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sánchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., Zemcov, M., 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], cosmology: observations, submillimetre: diffuse background, FOS: Physical sciences, cosmology: observations, submillimetre: diffuse background, submillimetre: galaxies, Astrophysics::Cosmology and Extragalactic Astrophysics, submillimetre: galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dusty, star forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-SPIRE images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyze three fields from the HerMES programme in all three SPIRE bands (250, 350, and 500 microns); parameterized galaxy number count models are derived to a depth of ~2 mJy/beam, approximately 4 times the depth of previous analyses at these wavelengths, using a P(D) (probability of deflection) approach for comparison to theoretical number count models. Our fits account for 64, 60, and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number counts models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam., Comment: Accepted for publication in MNRAS

Published
2010
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10. [Letter to the Editor] HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm

Author

Oliver, S, Wang, L, Smith, A J, Altieri, B, Amblard, A, Arumugam, V, Auld, R, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Buat, V, Burgarella, D, Castro-Rodríguez, N, Cava, A, Chanial, P, Clements, D L, Conley, A, Conversi, L, Cooray, A, Dowell, C D, Dwek, E, Eales, S, Elbaz, D, Fox, M, Franceschini, A, Gear, W, Glenn, J, Griffin, M, Halpern, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, R J, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Mitchell-Wynne, K, Mortier, A M J, Nguyen, H T, O'Halloran, B, Omont, A, Page, M J, Panuzzo, P, Papageorgiou, A, Pearson, C P, Pérez-Fournon, I, Pohlen, M, Rawlings, J I, Raymond, G, Rigopoulou, D, Rizzo, D, Roseboom, I, Rowan-Robinson, M, Sánchez Portal, M, Savage, R S, Schulz, B, Scott, D, Seymour-Smith, N, Shupe, D L, Stevens, J A, Symeonidis, M, Trichas, M, Tugwell, K E, Vaccari, M, Valiante, E, Valtchanov, I, Vieira, J D, Vigroux, L, Ward, R, Wright, G, Xu, C K, and Zemcov, M

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy 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\ud 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

Published
2010

11. Evolution of dust temperature of galaxies through cosmic time as seen by Herschel

Author

Cava, A., Cepa, J., Chanial, P., Chapin, E., Chary, R. -R., Cimatti, Alessandro, Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dannerbauer, H., Dickinson, M., Dominguez, H., Dowell, C. D., Dunlop, J. S., Dwek, E., Eales, S., Farrah, D., Schreiber, N. Foerster, Fox, M., Franceschini, A., Gear, W., Genzel, R., Glenn, J., Griffin, M., Gruppioni, C., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Jeong, W. -S., Lagache, Guilaine, Le Borgne, Damien, Le Floc'H, E., Lee, H. M., Lee, J. C., Lee, M. G., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magnelli, B., Mainetti, G., Maiolino, R., Marchetti, L., Mortier, A. M. J., Nguyen, H. T., Nordon, R., O'Halloran, B., Okumura, K., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Perez Garcia, A. M., Poglitsch, A., Pohlen, M., Popesso, P., Pozzi, F., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Saintonge, A., Sanchez Portal, M., Santini, P., Sauvage, M., Schulz, B., Scott, D., Seymour, N., Shao, L., Shupe, D. L., Smith, A. J., Stevens, J. A., Sturm, E., Tacconi, L., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Vigroux, L., Wang, L., Ward, R., Wright, Gavin, Xu, C. K., Zemcov, M., Hwang, H. S., Elbaz, D., Magdis, G., Daddi, Emanuele, Symeonidis, M., Altieri, B., Amblard, A., Andreani, P., Arumugam, V., Auld, R., Aussel, H., Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodriguez, N., H.S. Hwang, D. Elbaz, G. E. Magdi, E. Daddi, M. Symeonidi, B. Altieri, A. Amblard, P. Andreani, V. Arumugam, R. Auld, H. Aussel, T. Babbedge, S. Berta, A. Blain, J. Bock, A. Bongiovanni, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodriguez, A. Cava, J. Cepa, P. Chanial, E. Chapin, R.-R. Chary, A. Cimatti, D.L. Clement, A. Conley, L. Conversi, A. Cooray, H. Dannerbauer, M. Dickinson, H. Dominguez, C.D. Dowell, J.S. Dunlop, E. Dwek, S. Eale, D. Farrah, N. Forster Schreiber, M. Fox, A. Franceschini, W. Gear, R. Genzel, J. Glenn, M. Griffin, C. Gruppioni, M. Halpern, E. Hatziminaoglou, E. Ibar, K. Isaak, R.J. Ivison, W.-S. Jeong, G. Lagache, D. Le Borgne, E. Le Floc'h, H.M. Lee, J.C. Lee, M.G. Lee, L. Levenson, N. Lu, D. Lutz, S. Madden, B. Maffei, B. Magnelli, G. Mainetti, R. Maiolino, L. Marchetti, A.M.J. Mortier, H.T. Nguyen, R. Nordon, B. O'Halloran, K. Okumura, S.J. Oliver, A. Omont, M.J. Page, P. Panuzzo, A. Papageorgiou, C.P. Pearson, I. Perez-Fournon, A.M. Perez Garcia, A. Poglitsch, M. Pohlen, P. Popesso, F. Pozzi, J.I. Rawling, D. Rigopoulou, L. Riguccini, D. Rizzo, G. Rodighiero, I.G. Roseboom, M. Rowan-Robinson, A. Saintonge, M. Sanchez Portal, P. Santini, M. Sauvage, B. Schulz, Douglas Scott, N. Seymour, L. Shao, D.L. Shupe, A.J. Smith, J.A. Steven, E. Sturm, L. Tacconi, M. Tricha, K.E. Tugwell, M. Vaccari, I. Valtchanov, J.D. Vieira, L. Vigroux, L.Wang, R. Ward, G. Wright, C.K. Xu, M. Zemcov, 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), 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), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the dust properties of galaxies in the redshift range 0.10.5 with L_IR>5x10^{10} L_\odot, appears to be 2-5 K colder than that of AKARI-selected local galaxies with similar luminosities; and the dispersion in T_dust for high-z galaxies increases with L_IR due to the existence of cold galaxies that are not seen among local galaxies. We show that this large dispersion of the L_IR-T_dust relation can bridge the gap between local star-forming galaxies and high-z submillimeter galaxies (SMGs). We also find that three SMGs with very low T_dust (, Comment: 9 pages, 6 figures, To appear in MNRAS

Published
2010
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12. Herschel unveils a puzzling uniformity of distant dusty galaxies [Letter]

Author

Elbaz, D., Hwang, H. S., Magnelli, B., Daddi, E., Aussel, H., Altieri, B., Amblard, A., Andreani, P., Arumugam, V., Auld, Robbie Richard, Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodriguez, N., Cava, A., Cepa, J., Chanial, P., Chary, R.-R., Cimatti, A., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dickinson, M., Dominguez, H., Dowell, C. D., Dunlop, J. S., Dwek, E., Eales, Stephen Anthony, Farrah, D., Förster Schreiber, N., Fox, M., Franceschini, A., Gear, Walter Kieran, Genzel, R., Glenn, J., Griffin, Matthew Joseph, Gruppioni, C., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, Kate Gudrun, Ivison, R. J., Lagache, G., Le Borgne, D., Le Floc'h, E., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magdis, G., Mainetti, G., Maiolino, R., Marchetti, L., Mortier, A. M. J., Nguyen, H. T., Nordon, R., O'Halloran, B., Okumura, K., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, Andreas, Pearson, C. P., Perez Fournon, I., Pérez García, A. M., Poglitsch, A., Pohlen, Michael, Popesso, P., Pozzi, F., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Saintonge, A., Sanchez Portal, M., Santini, P., Sauvage, M., Schulz, B., Scott, D., Seymour, N., Shao, L., Shupe, D. L., Smith, A. J., Stevens, J. A., Sturm, E., Symeonidis, M., Tacconi, L., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract

The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved over the last 80% of the age of the Universe. We discuss possible consequences for the determination of star-formation rates (SFR) and any evidence for a major change in their star-formation properties. We use Herschel deep extragalactic surveys from 100 to 500 μm to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and HerMES key programs). An extension to fainter luminosities is done by stacking images on 24 μm prior positions. We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used, e.g. at 24 μm, to identify “isolated” galaxies whose flux is not boosted by bright neighbors. Below z ~ 1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15 dex), therefore similar to z ~ 0 galaxies, over three decades in luminosity below the regime of ultra-luminous IR galaxies (ULIRGs, LIR ≥ 1012 ). This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160 μm, 250 μm or 350 μm bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ~150 μm (rest-frame) before Herschel on those templates. We also note that the dust temperature of luminous IR galaxies (LIRGs, LIR ≥ 1011 ) around z ~ 1 is mildly colder by 10–15% than their local analogs and up to 20% for ULIRGs at z ~ 1.6 (using a single modified blackbody-fit to the peak far-IR emission with an emissivity index of β = 1.5). Above z = 1.5, distant galaxies are found to exhibit a substantially larger mid- over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor coeval star formation at very high SFR and in conditions similar to purely star-forming galaxies.

Published
2010

13. Detection of the Cosmic Far-Infrared Background in the AKARI Deep Field South

Author

Burgarella, D., Clements, D. L., Jeong, W.-S., Khan, S. A., Pearson, C. P., Pollo, A., Serjeant, S., White, G. J., Matsuura, Shuji, Shirahata, Mai, Kawada, Mitsunobu, Takeuchi, Tsutomu, Hanami, Hitoshi, Matsuhara, Hideo, Nakagawa, Takao, Oyabu, Shinki, Takagi, Toshinobu, Laboratoire d'Astrophysique de Marseille (LAM), 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
Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], 01 natural sciences, Sky brightness, diffuse background [infrared], Cosmic infrared background, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, large-scale structure of universe, Physics, Luminous infrared galaxy, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, observations [cosmology], Redshift, Galaxy, diffuse radiation, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 17名, Accepted: 2011-05-09, 資料番号: SA1002997000

Published
2010
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14. The HerMES SPIRE submillimeter local luminosity function [Letter]

Author

Vaccari, M., Marchetti, L., Franceschini, A., Altieri, B., Amblard, A., Arumugam, V., Auld, Robbie Richard, Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Dye, S., Eales, Stephen Anthony, Elbaz, D., Farrah, D., Fox, M., Gear, Walter Kieran, Glenn, J., González Solares, E. A., Griffin, Matthew Joseph, Halpern, M., Hatziminaoglou, E., Huang, J., Ibar, E., Isaak, Kate Gudrun, Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Mortier, A. M. J., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, Andreas, Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rawlings, J. I., Raymond, Gwenifer, Rigopoulou, D., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Sánchez Portal, M., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Valiante, Elisabetta, Valtchanov, I., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing\ud these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric\ud 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\ud several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0 < z < 0.2 local luminosity function\ud and infrared bolometric (8−1000 μm) local luminosity density based on SPIRE data from the HerMES Herschel key program over 14.7 deg2.\ud Flux measurements in the three SPIRE channels at 250, 350 and 500 μm are combined with Spitzer photometry and archival data. We fit the\ud observed optical-to-submillimeter spectral energy distribution of SPIRE sources and use the 1/Vmax estimator to provide the first constraints on\ud the monochromatic 250, 350 and 500 μm as well as on the infrared bolometric (8−1000 μm) local luminosity function based on Herschel data.\ud We compare our results with modeling predictions and find a slightly more abundant local submillimeter population than predicted by a number\ud of models. Our measurement of the infrared bolometric (8−1000 μm) local luminosity function suggests a flat slope at low luminosity, and the\ud inferred local luminosity density, 1.31+0.24\ud −0.21\ud × 108 L� Mpc−3, is consistent with the range of values reported in recent literature.

Published
2010

15. Multi-wavelength analysis of 18um-selected galaxies in the AKARI/IRC monitor field towards the North Ecliptic Pole

Author

Takagi, T., Matsuhara, H., Wada, T., Oyabu, S., Imai, K., Pearson, C. P., Hanami, H., Onaka, T., Fujishiro, N., Ishihara, D., Ita, Y., Kataza, H., Kim, W., Matsumoto, T., Murakami, H., Ohyama, Y., Sakon, I., Tanabe, T., Uemizu, K., Ueno, M., Watarai, H., Usui, F., Lee, H. M., Im, M., Serjeant, S., Savage, R. S., Tange, T., and Nakagawa, T.

Subjects
Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present an initial analysis of AKARI 18um-selected galaxies using all 9 photometric bands at 2-24um available in the InfraRed Camera (IRC), in order to demonstrate new capabilities of AKARI cosmological surveys. We detected 72 sources at 18um in an area of 50.2 arcmin^2 in the AKARI/IRC monitor field towards the North Ecliptic Pole (NEP). From this sample, 25 galaxies with probable redshifts z>~ 0.5 are selected with a single colour cut (N2-N3>0.1) for a detailed SED analysis with ground-based BVRi'z'JK data. Using an SED radiative transfer model of starbursts covering the wavelength range UV -- submm, we derive photometric redshifts from the optical-MIR SEDs of 18um-selected galaxies. From the best-fit SED models, we show that the IRC all-band photometry is capable of tracing the steep rise in flux at the blue side of the PAH 6.2um emission feature. This indicates that the IRC all-band photometry is useful to constrain the redshift of infrared galaxies, specifically for dusty galaxies with a less prominent 4000A break. Also, we find that the flux dip between the PAH 7.7 and 11.2um emission feature is recognizable in the observed SEDs of galaxies at z~1. By using such a colour anomaly due to the PAH and silicate absorption features, unique samples of ULIRGs at z~1, `silicate-break' galaxies, can be constructed from large cosmological surveys of AKARI towards the NEP, i.e. the NEP-Deep and NEP-Wide survey. This pilot study suggests the possibility of detecting many interesting galaxy properties in the NEP-Deep and Wide surveys, such as a systematic difference in SEDs between high- and low-z ULIRGs, and a large variation of the PAH inter-band strength ratio in galaxies at high redshifts. [abridged], Accepted for publication in PASJ, AKARI special issue

Published
2007
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16. Silicate-break galaxies: an efficient selection method of distant ultraluminous infrared galaxies

Author

Takagi, T. and Pearson, C. P.

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present a photometric selection method for ULIRGs in the redshift range of z=1 -- 2. We utilize the most prominent spectral feature of ULIRGs, i.e. the silicate absorption feature at 9.7 micron and an optimized filter system at mid-infrared wavelengths. These `silicate-break' galaxies could be selected by using colour anomalies owing to the silicate absorption feature around 9.7(1+z) micron. Such filter systems are available on the Spitzer Space Telescope but we suggest that the most promising selection criteria would be given with mid-infrared bands of ASTRO-F satellite due to a more comprehensive set of filter bands than that of Spitzer. We study the selection method of silicate-break galaxies with the SED model of both starbursts and quiescent star-forming galaxies, and then verify the method by using the observed spectra of nearby galaxies. We would expect that about 1000 candidates of silicate-break galaxies could be detected per square degree in current and future mid-infrared surveys. The silicate-break selection criteria will break the degeneracy between various galaxy evolution models for extragalactic source counts and place strong limits on the star formation activity at z=1 -- 2. Applying our silicate-break technique to initial Spitzer results we have tentatively identified the first candidate silicate-break galaxy at z=1.6., Comment: 8 pages, 10 figures. Accepted version for publication in MNRAS

Published
2004
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17. Quasars as probes of the submillimetre cosmos at z>5: I. Preliminary SCUBA photometry

Author

Priddey, Robert S., Isaak, Kate G., McMahon, Richard G., Robson, E. I., and Pearson, C. P.

Subjects
Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present submillimetre continuum observations of a sample of some of the highest redshift quasars currently known, made with the SCUBA bolometer array on the JCMT. The median redshift of the sample is 5.3. Two z>5 objects are strong (6 sigma) detections, with S(850um)>10mJy. A firm (5 sigma) detection is obtained for the z=5.7 quasar SDSS J1044-0125; and SDSS J1306+0356, at z=6.0, is detected with a signal-to-noise approx. 4. For the remainder of the sample we have obtained sensitive (sigma=1.5mJy) upper limits. Submm spectral indices measured for two of the sources are consistent with thermal reradiation from dust, rather than from synchrotron emission. Sensitive 450um upper limits imply that the dust is cool,suggesting large dust masses only 1Gyr after the Big Bang., MNRAS Letters, accepted

Published
2003
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18. HerMES: SPIRE galaxy number counts at 250, 350, and 500 μ m

Author

Oliver, S. J., Wang, L., Smith, A. J., Altieri, B., Amblard, A., Arumugam, V., Auld, R., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Elbaz, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Mitchell-Wynne, K., Mortier, A. M. J., Nguyen, H. T., O Halloran, B., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rawlings, J. I., Raymond, G., Rigopoulou, D., Rizzo, D., Roseboom, I. G., Rowan-Robinson, M., Sánchez Portal, M., Savage, R., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Mattia Vaccari, Valiante, E., Valtchanov, I., Vieira, J. D., Vigroux, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
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

19. Herschel unveils a puzzling uniformity of distant dusty galaxies

Author

D. Elbaz, H. S. Hwang, B. Magnelli, E. Daddi, H. Aussel, B. Altieri, A. Amblard, P. Andreani, V. Arumugam, R. Auld, T. Babbedge, S. Berta, A. Blain, J. Bock, A. Bongiovanni, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodriguez, A. Cava, J. Cepa, P. Chanial, R.-R. Chary, A. Cimatti, D. L. Clements, A. Conley, L. Conversi, A. Cooray, M. Dickinson, H. Dominguez, C. D. Dowell, J. S. Dunlop, E. Dwek, S. Eales, D. Farrah, N. Förster Schreiber, M. Fox, A. Franceschini, W. Gear, R. Genzel, J. Glenn, M. Griffin, C. Gruppioni, M. Halpern, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, D. Le Borgne, E. Le Floc'h, L. Levenson, N. Lu, D. Lutz, S. Madden, B. Maffei, G. Magdis, G. Mainetti, R. Maiolino, L. Marchetti, A. M. J. Mortier, H. T. Nguyen, R. Nordon, B. O'Halloran, K. Okumura, S. J. Oliver, A. Omont, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Perez Fournon, A. M. Pérez García, A. Poglitsch, M. Pohlen, P. Popesso, F. Pozzi, J. I. Rawlings, D. Rigopoulou, L. Riguccini, D. Rizzo, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, A. Saintonge, M. Sanchez Portal, P. Santini, M. Sauvage, B. Schulz, D. Scott, N. Seymour, L. Shao, D. L. Shupe, A. J. Smith, J. A. Stevens, E. Sturm, M. Symeonidis, L. Tacconi, M. Trichas, K. E. Tugwell, M. Vaccari, I. Valtchanov, J. Vieira, L. Vigroux, L. Wang, R. Ward, G. Wright, C. K. Xu, M. Zemcov, 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Elbaz D., Hwang H. S., Magnelli B., Daddi E., Aussel H., Altieri B., Amblard A., Andreani P., Arumugam V., Auld R., Babbedge T., Berta S., Blain A., Bock J., Bongiovanni A., Boselli A., Buat V., Burgarella D., Castro-Rodriguez N., Cava A., Cepa J., Chanial P., Chary R.-R., Cimatti A., Clements D. L., Conley A., Conversi L., Cooray A., Dickinson M., Dominguez H., Dowell C. D., Dunlop J. S., Dwek E., Eales S., Farrah D., Förster Schreiber N., Fox M., Franceschini A., Gear W., Genzel R., Glenn J., Griffin M., Gruppioni C., Halpern M., Hatziminaoglou E., Ibar E., Isaak K., Ivison R. J., Lagache G., Le Borgne D., Le Floc'h E., Levenson L., Lu N., Lutz D., Madden S., Maffei B., Magdis G., Mainetti G., Maiolino R., Marchetti L., Mortier A. M. J., Nguyen H. T., Nordon R., O'Halloran B., Okumura K., Oliver S. J., Omont A., Page M. J., Panuzzo P., Papageorgiou A., Pearson C. P., Perez Fournon I., Pérez García A. M., Poglitsch A., Pohlen M., Popesso P., Pozzi F., Rawlings J. I., Rigopoulou D., Riguccini L., Rizzo D., Rodighiero G., Roseboom I. G., Rowan-Robinson M., Saintonge A., Sanchez Portal M., Santini P., Sauvage M., Schulz B., Scott D., Seymour N., Shao L., Shupe D. L., Smith A. J., Stevens J. A., Sturm E., Symeonidis M., Tacconi L., Trichas M., Tugwell K. E., Vaccari M., Valtchanov I., Vieira J., Vigroux L., Wang L., Ward R., Wright G., Xu C. K., and Zemcov M.

Subjects
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, infrared: galaxies, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Bolometer, Astronomy and Astrophysics, Redshift, Space observatory, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved since z~2.5. We use Herschel deep extragalactic surveys from 100 to 500um to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and HerMES key programs). We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used to identify isolated galaxies whose flux is not boosted by bright neighbors. Below z~1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15dex), therefore similar to z~0 galaxies. This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160um, 250um or 350um bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ~150um (rest-frame) on local templates. We also note that the dust temperature of luminous IR galaxies around z~1 is mildly colder by 10-15% than their local analogs and up to 20% for ULIRGs at z~1.6. Above z=1.5, distant galaxies are found to exhibit a substantially larger mid- over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor star formation at very high SFR and in conditions similar to purely star-forming galaxies., Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages

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