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2. Herschel deep far-infrared counts through Abell 2218 cluster-lens

Author

G. Rodighiero, Ángel Bongiovanni, Roberto Maiolino, Raanan Nordon, Albrecht Poglitsch, I. Valtchanov, Ekkehard Wieprecht, P. Popesso, Bruno Altieri, Dieter Lutz, J. Cepa, Johan Richard, Eckhard Sturm, Antonio Cava, E. Daddi, P. Andreani, H. Dominguez, A. Cimatti, A. M. Pérez García, J. P. Kneib, Reinhard Genzel, Lijing Shao, Laure Ciesla, D. Elbaz, S. Berta, M. Wetzstein, M. Sánchez-Portal, Carlotta Gruppioni, L. Riguccini, Georgios E. Magdis, Linda J. Tacconi, Francesca Pozzi, H. Aussel, L. Metcalfe, P. Santini, Amelie Saintonge, N. M. Förster Schreiber, Benjamin Magnelli, XMM-Newton Science Operations Centre, European Space Agency (ESA), AUTRES, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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), 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), Station de Pathologie Végétale [Angers], Institut National de la Recherche Agronomique (INRA), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Physics [Berkeley], University of California [Berkeley], University of California-University of California, 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 de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS 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 de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-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), 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), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), B. Altieri, S. Berta, D. Lutz, J.-P. Kneib, L. Metcalfe, P. Andreani, H. Aussel, A. Bongiovanni, A. Cava, J. Cepa, L. Ciesla, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N.M. Forster Schreiber, R. Genzel, C. Gruppioni, B. Magnelli, G. Magdi, R. Maiolino, R. Nordon, A.M. Perez Garcia, A. Poglitsch, P. Popesso, F. Pozzi, J. Richard, L. Riguccini, G. Rodighiero, A. Saintonge, P. Santini, M. Sanchez-Portal, L. Shao, E. Sturm, L.J. Tacconi, I. Valtchanov, M. Wetzstein, E. Wieprecht, Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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), and École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL)

Subjects
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], Strong gravitational lensing, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, galaxies: high-redshift, Cosmic infrared background, 0103 physical sciences, Source counts, Surface brightness, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, Luminous infrared galaxy, Galaxy: evolution, education.field_of_study, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, Gravitational lens, Space and Planetary Science, galaxies: clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitational lensing by massive galaxy clusters allows study of the population of intrinsically faint infrared galaxies that lie below the sensitivity and confusion limits of current infrared and submillimeter telescopes. We present ultra-deep PACS 100 and 160 microns observations toward the cluster lens Abell 2218, to penetrate the Herschel confusion limit. We derive source counts down to a flux density of 1 mJy at 100 microns and 2 mJy at 160 microns, aided by strong gravitational lensing. At these levels, source densities are 20 and 10 beams/source in the two bands, approaching source density confusion at 160 microns. The slope of the counts below the turnover of the Euclidean-normalized differential curve is constrained in both bands and is consistent with most of the recent backwards evolutionary models. By integrating number counts over the flux range accessed by Abell 2218 lensing (0.94-35 mJy at 100 microns and 1.47-35 mJy at 160 microns, we retrieve a cosmic infrared background (CIB) surface brightness of ~8.0 and ~9.9 nW m^-2 sr^-1, in the respective bands. These values correspond to 55% (+/- 24%) and 77% (+/- 31%) of DIRBE direct measurements. Combining Abell 2218 results with wider/shallower fields, these figures increase to 62% (+/- 25%) and 88% (+/- 32%) CIB total fractions, resolved at 100 and 160 microns, disregarding the high uncertainties of DIRBE absolute values., Accepted for publication on the A&A Herschel Special Issue, final version

Published
2016
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3. The Herschel census of infrared SEDs through cosmic time

Author

B. O'Halloran, Mat Page, Michael Pohlen, P. Popesso, David J. Rosario, C. K. Xu, S. J. Lilly, Chris Pearson, Peter Capak, E. Le Floc'h, Matthew Joseph Griffin, E. Giovannoli, Duncan Farrah, D. Rigopoulou, Georgios E. Magdis, Jason Glenn, L. Riguccini, V. Arumugam, Ho Seong Hwang, Ismael Perez-Fournon, Evanthia Hatziminaoglou, Alberto Franceschini, S. Berta, Edo Ibar, Mattia Vaccari, Stijn Wuyts, Lucia Marchetti, Michael Rowan-Robinson, Dieter Lutz, David L. Clements, Lian-Tao Wang, Asantha Cooray, Andreas Papageorgiou, O. Ilbert, Seb Oliver, Benjamin Magnelli, Anthony J. Smith, Benjamin L. Schulz, D. L. Shupe, L. Conversi, Isaac Roseboom, A. Boselli, C. D. Dowell, Douglas Scott, A. Conley, Nick Seymour, Francesca Pozzi, Mara Salvato, Rob Ivison, H. Patel, Herve Aussel, Alain Omont, H. T. Nguyen, Ivan Valtchanov, M. Symeonidis, Michael Zemcov, Raanan Nordon, V. Buat, J. Kartaltepe, James J. Bock, M. Symeonidi, M. Vaccari, S. Berta, M. J. Page, D. Lutz, V. Arumugam, H. Aussel, J. Bock, A. Boselli, V. Buat, P. L. Capak, D. L. Clement, A. Conley, L. Conversi, A. Cooray, C. D. Dowell, D. Farrah, A. Franceschini, E. Giovannoli, J. Glenn, M. Griffin, E. Hatziminaoglou, H.- S. Hwang, E. Ibar, O. Ilbert, R. J. Ivison, E. L. Floc'h, S. Lilly, J. S. Kartaltepe, B. Magnelli, G. Magdi, L. Marchetti, H. T. Nguyen, R. Nordon, B. O'Halloran, S. J. Oliver, A. Omont, A. Papageorgiou, H. Patel, C. P. Pearson, I. Perez-Fournon, M. Pohlen, P. Popesso, F. Pozzi, D. Rigopoulou, L. Riguccini, D. Rosario, I. G. Roseboom, M. Rowan-Robinson, M. Salvato, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, I. Valtchanov, L. Wang, C. K. Xu, M. Zemcov, S. Wuyts, 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
Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Hubble Deep Field, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies [infrared], Luminosity, Spitzer Space Telescope, galaxies: high-redshift, 0103 physical sciences, galaxies [submillimetre], Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], QB, Physics, Luminous infrared galaxy, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, starburst [galaxies], infrared: galaxie, Astronomy, Astronomy and Astrophysics, high redshift [galaxies], Galaxy, Redshift, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, submillimetre: galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS and GOODS (N+S), we examine the dust properties of IR-luminous (L_IR>10^10 L_sun) galaxies at 0.145K) SEDs and cold (T, Comment: 27 pages, 23 figures, 2 tables, accepted for publication in MNRAS

Published
2016
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4. Linking the X-ray and infrared properties of star-forming galaxies at z \textless 1.5

Author

M. Bonzini, M. J. Page, Carolin Villforth, V. Buat, S. J. Oliver, J. J. Bock, M. Symeonidis, Antonis Georgakakis, Georgios E. Magdis, Benjamin Magnelli, Dieter Lutz, Alberto Franceschini, Edo Ibar, Isaac Roseboom, Mattia Vaccari, Duncan Farrah, David J. Rosario, Maurizio Paolillo, Maurilio Pannella, Space Science & Technology Department, Rutheford Appleton Laboratory, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing [Penteli] (IAASARS), National Observatory of Athens (NOA), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), 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), Department of Physics [Blacksburg], Virginia Tech [Blacksburg], AUTRES, 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), Astronomy Centre, University of Sussex, Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), Department of Physics and Astronomy [South Africa], University of the Western Cape (UWC), University of California-University of California, 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), Università degli studi di Napoli Federico II, Universita degli Studi di Padova, University of the Western Cape, M., Symeonidi, A., Georgakaki, M. J., Page, J., Bock, M., Bonzini, V., Buat, D., Farrah, A., Franceschini, E., Ibar, D., Lutz, B., Magnelli, G., Magdi, S. J., Oliver, M., Pannella, Paolillo, Maurizio, D., Rosario, I. G., Roseboom, M., Vaccari, C., Villforth, University of St Andrews. School of Physics and Astronomy, and Dipartimento di Astronomia

Subjects
Infrared, Astrophysics::High Energy Astrophysical Phenomena, Stacking, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), 01 natural sciences, QB0460, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Attenuation, X-ray, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, QC Physics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract

We present the most complete study to date of the X-ray emission from star-formation in high redshift (median z=0.7; z-3 in both hard and soft X-ray bands. From the sources which are star-formation dominated, only a small fraction are individually X-ray detected and for the bulk of the sample we calculate average X-ray luminosities through stacking. We find an average soft X-ray to infrared ratio of log[L_SX/L_IR]=-4.3 and an average hard X-ray to infrared ratio of log[L_HX/L_IR]=-3.8. We report that the X-ray/IR correlation is approximately linear through the entire range of L_IR and z probed and, although broadly consistent with the local (z, Comment: 16 pages, 13 figures, accepted for publication in MNRAS

Published
2014
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5. Herschel reveals the obscured star formation in HiZELS H\alpha\ emitters at z=1.47

Author

M. J. Page, V. Arumugam, S. J. Oliver, Francesca Pozzi, Benjamin Magnelli, Kotaro Kohno, Ian Smail, M. Symeonidis, Duncan Farrah, Dieter Lutz, Nick Seymour, A. Conley, Georgios E. Magdis, James E. Geach, Michael Zemcov, Lingyu Wang, L. Riguccini, Julie Wardlow, S. Berta, Antonio Cava, Rob Ivison, Austin Smith, E. Le Floc'h, J. J. Bock, G. Marsden, David Sobral, Philip Best, Edo Ibar, Matthieu Béthermin, Benjamin L. Schulz, Soh Ikarashi, E. Ibar, D. Sobral, P. N. Best, R. J. Ivison, I. Smail, V. Arumugam, S. Berta, M. Bethermin, J. Bock, A. Cava, A. Conley, D. Farrah, J. Geach, S. Ikarashi, K. Kohno, E. Le Floc'h, D. Lutz, G. Magdi, B. Magnelli, G. Marsden, S. J. Oliver, M. J. Page, F. Pozzi, L. Riguccini, B. Schulz, N. Seymour, A. J. Smith, M. Symeonidi, L. Wang, J. Wardlow, and M. Zemcov

Subjects
Stellar mass, galaxies: starburst, Astrophysics, 01 natural sciences, star formation [Galaxies], Physical cosmology, high-redshift [Galaxies], statistics [Galaxies], galaxies [Infrared], galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, Star formation, infrared: galaxie, Astronomy, Astronomy and Astrophysics, Galaxy, Redshift, Stars, starburst [Galaxies], Space and Planetary Science, galaxies: star formation, galaxies: statistic, submillimetre: galaxies, galaxies. [Submillimetre], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the far-infrared (FIR; rest-frame 8--1000\mu m) properties of a sample of 443 H\alpha-selected star-forming galaxies in the COSMOS and UDS fields detected by the HiZELS imaging survey. Sources are identified using narrow-band filters in combination with broad-band photometry to uniformly select H\alpha\ (and [OII] if available) emitters in a narrow redshift slice at z = 1.47+/-0.02. We use a stacking approach in Spitzer, Herschel (from PEP and HerMES surveys) and AzTEC images to describe their typical FIR properties. We find that HiZELS galaxies with observed H\alpha\ luminosities of ~ 10^{8.1-9.1} Lo have bolometric FIR luminosities of typical LIRGs, L_FIR ~ 10^{11.48+/-0.05} Lo. Combining the H\alpha\ and FIR luminosities, we derive median SFR = 32+/-5 Mo/yr and H\alpha\ extinctions of A(H\alpha) = 1.0+/-0.2 mag. Perhaps surprisingly, little difference is seen in typical HiZELS extinction levels compared to local star-forming galaxies. We confirm previous empirical stellar mass (M*) to A(H\alpha) relations and the little or no evolution up to z = 1.47. For HiZELS galaxies, we provide an empirical parametrisation of the SFR as a function of (u-z)_rest colours and 3.6\mu m photometry. We find that the observed H\alpha\ luminosity is a dominant SFR tracer when (u-z)_rest ~< 0.9 mag or when 3.6\mu m photometry > 22 mag (Vega) or when M* < 10^9.7 Mo. We do not find any correlation between the [OII]/H\alpha\ and FIR luminosity, suggesting that this emission line ratio does not trace the extinction of the most obscured star-forming regions. The luminosity-limited HiZELS sample tends to lie above of the so-called `main sequence' for star-forming galaxies, especially at low M*. This work suggests that obscured star formation is linked to the assembly of M*, with deeper potential wells in massive galaxies providing dense, heavily obscured environments in which stars can form rapidly., Comment: abridged abstract

Published
2013

6. The Complex Physics of Dusty Star-forming Galaxies at High Redshifts as Revealed by Herschel and Spitzer

Author

M. J. Page, Duncan Farrah, David L. Clements, A. Cooray, Isaac Roseboom, Peter Hurley, M. Rowan-Robinson, Lian-Tao Wang, Antonio Cava, Francesca Pozzi, Dimitra Rigopoulou, Seb Oliver, Denis Burgarella, Benjamin Magnelli, M. Symeonidis, Paola Popesso, A. Feltre, V. Buat, Douglas Scott, S. Berta, Giulia Rodighiero, L. Silva, Mattia Vaccari, E. A. González Solares, Georgios E. Magdis, Alberto Franceschini, James J. Bock, Dieter Lutz, Stijn Wuyts, Anthony J. Smith, B. Lo Faro, Lucia Marchetti, 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), B. Lo Faro, A. Franceschini, M. Vaccari, L. Silva, G. Rodighiero, S. Berta, J. Bock, D. Burgarella, V. Buat, A. Cava, D. L. Clement, A. Cooray, D. Farrah, A. Feltre, E. A. González Solare, P. Hurley, D. Lutz, G. Magdi, B. Magnelli, L. Marchetti, S. J. Oliver, M. J. Page, P. Popesso, F. Pozzi, D. Rigopoulou, M. Rowan-Robinson, I. G. Roseboom, Douglas Scott, A. J. Smith, M. Symeonidi, L. Wang, and S. Wuyts

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxy, Redshift, galaxies: evolution, galaxies: general, galaxies: interactions, galaxies: starburst, Stars, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We combine far-infrared photometry from Herschel (PEP/HERMES) with deep mid-infrared spectroscopy from Spitzer to investigate the nature and the mass assembly history of a sample of 31 Luminous and Ultraluminous Infrared Galaxies at z~1 and 2 selected in GOODS-S with 24 $\mu$m fluxes between 0.2 and 0.5 mJy. We model the data with a self-consistent physical model (GRASIL) which includes a state-of-the-art treatment of dust extinction and reprocessing. We find that all of our galaxies appear to require massive populations of old (>1 Gyr) stars and, at the same time, to host a moderate ongoing activity of SF (SFR < 100 M$_{\odot}$/yr). The bulk of the stars appear to have been formed a few Gyr before the observation in essentially all cases. Only five galaxies of the sample require a recent starburst superimposed on a quiescent star formation history (SFH). We also find discrepancies between our results and those based on optical-only SED fitting for the same objects; by fitting their observed Spectral Energy Distributions with our physical model we find higher extinctions (by $\Delta$A_{V} ~ 0.81 and 1.14) and higher stellar masses (by $\Delta$Log(M*) ~ 0.16 and 0.36 dex) for z~1 and z~2 (U)LIRGs, respectively. The stellar mass difference is larger for the most dust obscured objects. We also find lower SFRs than those computed from L_{IR} using the Kennicutt relation due to the significant contribution to the dust heating by intermediate-age stellar populations through 'cirrus' emission (~73% and ~66% of total L_{IR} for z~1 and z~2 (U)LIRGs, respectively)., Comment: 21 pages, 10 figures, 2 tables, accepted for publication in ApJ

Published
2013
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7. The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations

Author

Carlotta Gruppioni, Vassilis Charmandaris, Martin Harwit, David Elbaz, Maurilio Pannella, Linda J. Tacconi, Alessandro Cimatti, Raanan Nordon, Ranga-Ram Chary, David J. Rosario, Ángel Bongiovanni, Herve Aussel, Paola Andreani, Reinhard Genzel, Douglas Scott, Albrecht Poglitsch, Ho Seong Hwang, Georgios E. Magdis, J. Cepa, Matthieu Béthermin, N. M. Förster Schreiber, Dieter Lutz, Paola Santini, Miguel Sánchez-Portal, Emanuele Daddi, Roberto Maiolino, Bruno Altieri, Ivan Valtchanov, Rob Ivison, E. Sturm, Benjamin Magnelli, Mark Dickinson, Paola Popesso, Eric J. Murphy, S. Berta, A. M. Pérez García, Francesca Pozzi, Observatoire de Paris, PSL Research University (PSL), B. Magnelli, P. Popesso, S. Berta, F. Pozzi, D. Elbaz, D. Lutz, M. Dickinson, B. Altieri, P. Andreani, H. Aussel, M. Béthermin, A. Bongiovanni, J. Cepa, V. Charmandari, R.-R. Chary, A. Cimatti, E. Daddi, N. M. Förster Schreiber, R. Genzel, C. Gruppioni, M. Harwit, H. S. Hwang, R. J. Ivison, G. Magdi, R. Maiolino, E. Murphy, R. Nordon, M. Pannella, A. Pérez García, A. Poglitsch, D. Rosario, M. Sanchez-Portal, P. Santini, D. Scott, E. Sturm, L. J. Tacconi, I. Valtchanov, and Université Paris sciences et lettres (PSL)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Infrared, FOS: Physical sciences, Astronomy and Astrophysics, galaxies: starburst, Astrophysics, 01 natural sciences, Galaxy, Redshift, Luminosity, infrared: galaxies, Far infrared, Space and Planetary Science, Cosmic infrared background, 0103 physical sciences, Galaxy formation and evolution, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics - Cosmology and Nongalactic Astrophysics, Luminosity function (astronomy), Galaxies: evolution, Galaxies: starburst, Galaxies: statistics, Infrared: galaxies
Abstract

We present results from the deepest Herschel-PACS (Photodetector Array Camera and Spectrometer) far-infrared blank field extragalactic survey, obtained by combining observations of the GOODS (Great Observatories Origins Deep Survey) fields from the PACS Evolutionary Probe (PEP) and GOODS-Herschel key programmes. We describe data reduction and the construction of images and catalogues. In the deepest parts of the GOODS-S field, the catalogues reach 3-sigma depths of 0.9, 0.6 and 1.3 mJy at 70, 100 and 160 um, respectively, and resolve ~75% of the cosmic infrared background at 100um and 160um into individually detected sources. We use these data to estimate the PACS confusion noise, to derive the PACS number counts down to unprecedented depths and to determine the infrared luminosity function of galaxies down to LIR=10^11 Lsun at z~1 and LIR=10^12 Lsun at z~2, respectively. For the infrared luminosity function of galaxies, our deep Herschel far-infrared observations are fundamental because they provide more accurate infrared luminosity estimates than those previously obtained from mid-infrared observations. Maps and source catalogues (>3-sigma) are now publicly released. Combined with the large wealth of multi-wavelength data available for the GOODS fields, these data provide a powerful new tool for studying galaxy evolution over a broad range of redshifts., Accepted for publication in A&A; 22 pages, 13 figures; V2: updated to match accepted version

Published
2013
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8. Lyman break and ultraviolet-selected galaxies at z ~ 1 - II. PACS 100μm/160μm FIR detections

Author

Tom Broadhurst, I. Matute, S. Berta, Mariano Moles, David Elbaz, Linda J. Tacconi, A. M. Pérez-García, Herve Aussel, Francisco Prada, Francesca Pozzi, I. Oteo, Vicent J. Martínez, Mirjana Pović, Isabel Márquez, M. Sánchez-Portal, Georgios E. Magdis, E. Le Floc'h, Alberto Fernández-Soto, J. M. Quintana, David Cristóbal-Hornillos, Kerttu Viironen, J. Polednikova, I. Pintos-Castro, L. Riguccini, A. del Olmo, Jaime Perea, Paola Andreani, Alessandro Ederoclite, Andrea Cimatti, Eckhard Sturm, Alberto Molino, J. Cepa, Leopoldo Infante, Miguel Cerviño, Francisco J. Castander, J. A. L. Aguerri, Albrecht Poglitsch, T. Aparicio-Villegas, N. M. Foerster Schreiber, B. Cedrés, Ángel Bongiovanni, Narciso Benítez, R. M. Gonzalez-Delgado, Josefa Masegosa, Bruno Altieri, R. Genzel, Jesús Cabrera-Caño, Benjamin Magnelli, Dieter Lutz, Emanuele Daddi, Roberto Maiolino, C. Husillos, I. Valtchanov, P. Popesso, Ricardo Pérez-Martínez, Emilio J. Alfaro, I. Oteo, G. Magdi, A. Bongiovanni, A. M. Perez-Garcia, J. Cepa, B. Cedre, A. Ederoclite, M. Sanchez-Portal, J. A. L. Aguerri, E. J. Alfaro, B. Altieri, P. Andreani, T. Aparicio-Villega, H. Aussel, N. Benitez, S. Berta, T. Broadhurst, J. Cabrera-Cano, F. J. Castander, M. Cervino, A. Cimatti, D. Cristobal-Hornillo, E. Daddi, D. Elbaz, A. Fernandez-Soto, N. F. Schreiber, R. Genzel, R. M. Gonzalez-Delgado, C. Husillo, L. Infante, E. Le Floc'h, D. Lutz, B. Magnelli, R. Maiolino, I. Marquez, V. J. Martinez, J. Masegosa, I. Matute, M. Mole, A. Molino, A. d. Olmo, J. Perea, R. Perez-Martinez, I. Pintos-Castro, A. Poglitsch, J. Polednikova, P. Popesso, M. Povic, F. Pozzi, F. Prada, J. M. Quintana, L. Riguccini, E. Sturm, L. Tacconi, I. Valtchanov, and K. Viironen

Subjects
Stellar population, Astrophysics, galaxies [Radio continuum], medicine.disease_cause, star formation [Galaxies], Physical cosmology, high-redshift [Galaxies], galaxies [Infrared], galaxies: high-redshift, medicine, Luminous infrared galaxy, Physics, Star formation, infrared: galaxie, Astronomy, Astronomy and Astrophysics, evolution [Galaxies], Redshift, Galaxy, galaxies [Ultraviolet], Space and Planetary Science, galaxies: star formation, ultraviolet: galaxies, Spectral energy distribution, radio continuum: galaxie, galaxies: evolution, Ultraviolet
Abstract

In this work, we report the Photodetector Array Camera and Spectrometer (PACS) 100 μm/160 μm detections of a sample of 42 GALEX-selected and far-infrared (FIR)-detected Lyman break galaxies (LBGs) at z ~ 1 located in the Cosmic Evolution Survey (COSMOS) field and analyse their ultraviolet (UV) to FIR properties. The detection of these LBGs in the FIR indicates that they have a dust content high enough so that its emission can be directly detected. According to a spectral energy distribution (SED) fitting with stellar population templates to their UV-to-near-IR observed photometry, PACS-detected LBGs tend to be bigger (Reff ~ 4.1 kpc), more massive [log (M*/M⊙) ~ 10.7], dustier [Es(B - V) ~ 0.40], redder in the UV continuum (β ~ -0.60) and UV-brighter [log (LUV/L⊙) ~ 10.1] than PACSundetected LBGs. PACS-detected LBGs at z ~ 1 are mostly disc-like galaxies and are located over the green valley and red sequence of the colour-magnitude diagram of galaxies at their redshift. By using their UV and IR emission, we find that PACS-detected LBGs tend to be less dusty and have slightly higher total star formation rates (SFRs) than other PACS-detected UV-selected galaxies within the same redshift range. As a consequence of the selection effect due to the depth of the FIR observations employed, all our PACS-detected LBGs have total IR luminosities, LIR, higher than 1011 L⊙ and thus are luminous IR galaxies. However, none of the PACS-detected LBGs are in the ultra-luminous IR galaxy (ULIRG) regime, LIR =1012 L⊙, where the FIR observations are complete. The finding of ULIRGs-LBGs at higher redshifts (z ~ 3) suggests an evolution of the FIR emission of LBGs with cosmic time. In an IRX-β diagram, PACS-detected LBGs at z~1 tend to be located around the relation for local starburst similarly to other UV-selected PACS-detected galaxies at the same redshift. Consequently, the dust-correction factors obtained with theirUVcontinuum slope allowus to determine their total SFR, unlike at higher redshifts. However, the dust attenuation derived from UV to NIR SED fitting overestimates the total SFR for most of our PACS-detected LBGs in an age-dependent way: the overestimation factor is higher in younger galaxies. This is likely due to the typical degeneracy between dust attenuation and age in the SED fitting with synthetic templates and highlights the importance of the FIR measurements in the analysis of star-forming galaxies at intermediate redshifts. Generalitat Valenciana PROMETEO-2008/132 NASA Office of Space Science NNX09AF08G European Southern Observatory LP175.A-0839 Junta de Andalucía TIC-114, P08-TIC-03531 Ministerio de Economía y Competitividad AYA2011- 29517-C03-01, AYA2010-22111-C03-02, AYA2010-15169

Published
2013

9. The far-infrared/radio correlation as probed by Herschel

Author

R. J. Ivison, B. Magnelli, E. Ibar, P. Andreani, D. Elbaz, B. Altieri, A. Amblard, V. Arumugam, R. Auld, H. Aussel, T. Babbedge, S. Berta, A. Blain, J. Bock, A. Bongiovanni, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodríguez, A. Cava, J. Cepa, P. Chanial, A. Cimatti, M. Cirasuolo, D. L. Clements, A. Conley, L. Conversi, A. Cooray, E. Daddi, H. Dominguez, C. D. Dowell, 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, K. Isaak, G. Lagache, L. Levenson, N. Lu, D. Lutz, S. Madden, B. Maffei, G. Magdis, G. Mainetti, R. Maiolino, L. Marchetti, G. E. Morrison, A. M. J. Mortier, H. T. Nguyen, R. Nordon, B. O'Halloran, S. J. Oliver, A. Omont, F. N. Owen, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, A. M. Pérez García, A. Poglitsch, M. Pohlen, P. Popesso, F. Pozzi, J. I. Rawlings, G. Raymond, D. Rigopoulou, L. Riguccini, D. Rizzo, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, A. Saintonge, M. Sanchez Portal, P. Santini, 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, 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), AUTRES, 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), XMM-Newton Science Operations Centre, European Space Agency (ESA), 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, Station de Pathologie Végétale [Angers], Institut National de la Recherche Agronomique (INRA), Laboratoire Colloïdes et Matériaux Divisés (LCMD), 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), Department of Physics [Berkeley], University of California [Berkeley], University of California-University of California, Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, School of Physics and Astronomy [Cardiff], Cardiff University, Division of Engineering, Colorado School of Mines, Max-Planck-Institut für Extraterrestrische Physik (MPE), 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)-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), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), National Radio Astronomy Observatory (NRAO), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), National Institute of Water and Atmospheric Research [Wellington] (NIWA), Laboratoire de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), GoLP/Instituto Plasmas e Fusa˜o Nuclear, Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-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 Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-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)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), 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), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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), R. J. Ivison, B. Magnelli, E. Ibar, P. Andreani, D. Elbaz, B. Altieri, A. Amblard, V. Arumugam, R. Auld, H. Aussel, T. Babbedge, S. Berta, A. Blain, J. Bock, A. Bongiovanni, A. Boselli, V. Buat, D. Burgarella, N. Castro, A. Cava, J. Cepa, P. Chanial, A. Cimatti, M. Cirasuolo, D. L. Clement, A. Conley, L. Conversi, A. Cooray, E. Daddi, H. Dominguez, C. D. Dowell, E. Dwek, S. Eale, D. Farrah, M. Fox, A. Franceschini, W. Gear, R. Genzel, J. Glenn, M. Griffin, C. Gruppioni, M. Halpern, E. Hatziminaoglou, K. Isaak, G. Lagache, L. Levenson, N. Lu, D. Lutz, S. Madden, B. Maffei, G. Magdi, G. Mainetti, R. Maiolino, L. Marchetti, G. E. Morrison, A. M. J. Mortier, H. T. Nguyen, R. Nordon, B. O'Halloran, S. J. Oliver, A. Omont, F. N. Owen, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, A., A. Poglitsch, M. Pohlen, P. Popesso, F. Pozzi, J. I. Rawling, G. Raymond, D. Rigopoulou, L. Riguccini, D. Rizzo, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, A. Saintonge, M. Sanchez Portal, P. Santini, B. Schulz, Douglas Scott, N. Seymour, L. Shao, D. L. Shupe, A. J. Smith, J. A. Steven, E. Sturm, M. Symeonidi, L. Tacconi, M. Tricha, K. E. Tugwell, M. Vaccari, I. Valtchanov, J. Vieira, L. Vigroux, L. Wang, R. Ward, G. Wright, C. K. Xu, and M. Zemcov

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Wavelength, Spire, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Far infrared, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We set out to determine the ratio, q(IR), of rest-frame 8-1000um flux, S(IR), to monochromatic radio flux, S(1.4GHz), for galaxies selected at far-IR and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, and to identify any far-IR-bright outliers - useful laboratories for exploring why the far-IR/radio correlation is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-um and 1.4-GHz samples, obtained in GOODS-N using Herschel (HerMES; PEP) and the VLA. We determine bolometric IR output using ten bands spanning 24-1250um, exploiting data from PACS and SPIRE, as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an L(IR)-matched sample, designed to reveal evolution of q(IR) with z, spanning log L(IR) = 11-12 L(sun) and z=0-2, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies, we see tentative evidence of a break in the flux ratio, q(IR), at L(1.4GHz) ~ 10^22.7 W/Hz, where AGN are starting to dominate the radio power density, and of weaker correlations with z and T(d). From our 250-um-selected sample we identify a small number of far-IR-bright outliers, and see trends of q(IR) with L(1.4GHz), L(IR), T(d) and z, noting that some of these are inter-related. For our L(IR)-matched sample, there is no evidence that q(IR) changes significantly as we move back into the epoch of galaxy formation: we find q(IR) goes as (1+z)^gamma, where gamma = -0.04 +/- 0.03 at z=0-2; however, discounting the least reliable data at z1., A&A Herschel Special Issue, in press as a Letter. 5 pages

Published
2010
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10. A POPULATION OFz> 2 FAR-INFRAREDHERSCHEL-SPIRE-SELECTED STARBURSTS

Author

Francesca Pozzi, E. Le Floc'h, S. Berta, Edward L. Chapin, Dimitra Rigopoulou, James J. Bock, Dieter Lutz, Scott Chapman, Georgios E. Magdis, Benjamin Magnelli, Denis Burgarella, Douglas Scott, Mat Page, Matthieu Béthermin, Julie Wardlow, Caitlin M. Casey, Evanthia Hatziminaoglou, L. Riguccini, David B. Sanders, Seb Oliver, Marco P. Viero, Isaac Roseboom, A. Conley, Nick Seymour, C. Bridge, Rob Ivison, Asantha Cooray, Ivan Valtchanov, Joaquin Vieira, Duncan Farrah, David L. Clements, Christopher J. Conselice, C. M. Casey, S. Berta, M. Béthermin, J. Bock, C. Bridge, D. Burgarella, E. Chapin, S. C. Chapman, D. L. Clement, A. Conley, C. J. Conselice, A. Cooray, D. Farrah, E. Hatziminaoglou, R. J. Ivison, E. le Floc'h, D. Lutz, G. Magdi, B. Magnelli, S. J. Oliver, M. J. Page, F. Pozzi, D. Rigopoulou, L. Riguccini, I. G. Roseboom, D. B. Sander, Douglas Scott, N. Seymour, I. Valtchanov, J. D. Vieira, M. Viero, J. Wardlow, and Science and Technology Facilities Council (STFC)

Subjects
submillimeter: galaxies, Stellar mass, 0306 Physical Chemistry (Incl. Structural), Population, galaxies: starburst, Astrophysics, Astronomy & Astrophysics, 0305 Organic Chemistry, HIGH-REDSHIFT GALAXIES, Lower limit, infrared: galaxies, SCUBA GALAXIES, Far infrared, SUBMILLIMETER-SELECTED GALAXIES, galaxies: high-redshift, STAR-FORMING GALAXIES, SPACE-TELESCOPE, education, PHOTOMETRIC REDSHIFTS, ULTRALUMINOUS GALAXIES, QB, Physics, FORMATION HISTORY, education.field_of_study, Science & Technology, COSMIC cancer database, Star formation, MIDINFRARED SPECTROSCOPY, infrared: galaxie, Astronomy and Astrophysics, Galaxy, 0201 Astronomical And Space Sciences, Spire, 13. Climate action, Space and Planetary Science, Physical Sciences, astro-ph.CO, DEEP-FIELD-SOUTH, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present spectroscopic observations for a sample of 36 Herschel-SPIRE 250-500um selected galaxies (HSGs) at 22 HyLIRGs in the literature which are detected serendipitously or via tailored surveys searching only for high-z HyLIRGs; therefore, we can place lower limits on the contribution of HSGs to the cosmic star formation rate density at (7+-2)x10^(-3)Msun/yr h^3Mpc^(-3) at z~2.5, which is >10% of the estimated total star formation rate density (SFRD) of the Universe from optical surveys. The contribution at z~4 has a lower limit of 3x10^(-3)Msun/yr h^3 Mpc^(-3), ~>20% of the estimated total SFRD. This highlights the importance of extremely infrared-luminous galaxies with high star formation rates to the build-up of stellar mass, even at the earliest epochs., Comment: 25 pages, 10 figures; ApJ accepted

Published
2012
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11. The star-formation rates of 1.5 < z < 2.5 massive galaxies

Author

N. M. Förster Schreiber, S. Berta, H. Dominguez, L. Riguccini, Giulia Rodighiero, Eckhard Sturm, Roberto Maiolino, Georgios E. Magdis, Lijing Shao, D. Elbaz, Benjamin Magnelli, Andrea Cimatti, E. Daddi, Raanan Nordon, Herve Aussel, P. Santini, Paola Andreani, Dieter Lutz, Andrea Grazian, A. M. Pérez García, Amélie Saintonge, Ángel Bongiovanni, I. Valtchanov, Ekkehard Wieprecht, P. Popesso, Linda J. Tacconi, Francesca Pozzi, J. Cepa, M. Wetzstein, M. Sánchez-Portal, Reinhard Genzel, Albrecht Poglitsch, Antonio Cava, Bruno Altieri, R. Nordon, D. Lutz, L. Shao, B. Magnelli, S. Berta, B. Altieri, P. Andreani, H. Aussel, A. Bongiovanni, A. Cava, J. Cepa, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N. M. Förster Schreiber, R. Genzel, A.Grazian, G. Magdi, R. Maiolino R., A. M. Pérez García, A. Poglitsch A., P. Popesso, F. Pozzi, L. Riguccini, and G. Rodighiero

Subjects
Physics, Luminous infrared galaxy, cosmology: observation, Star formation, Extinction (astronomy), Theoretical models, galaxies: starburst, Astronomy and Astrophysics, Astrophysics, Galaxy, Redshift, infrared: galaxies, Space and Planetary Science, Galaxy formation and evolution, galaxies: evolution, galaxies: fundamental parameter
Abstract

The star formation rate (SFR) is a key parameter in the study of galaxy evolution. The accuracy of SFR measurements at z ∼ 2 has been questioned following a disagreement between observations and theoretical models. The latter predict SFRs at this redshift that are typically a factor 4 or more lower than the measurements. We present star-formation rates based on calorimetric measurements of the far-infrared (FIR) luminosities for massive 1.5 < z < 2.5, normal star-forming galaxies (SFGs), which do not depend on extinction corrections and/or extrapolations of spectral energy distributions. The measurements are based on observations in GOODS-N with the Photodetector Array Camera and Spectrometer (PACS) onboard Herschel, as part of the PACS evolutionary probe (PEP) project, that resolve for the first time individual SFGs at these redshifts at FIR wavelengths. We compare FIR-based SFRs to the more commonly used 24 μm and UV SFRs. We find that SFRs from 24 μm alone are higher by a factor of ∼4-7.5 than the true SFRs. This overestimation depends on luminosity: gradually increasing for log L(24 μm) > 12.2 L ⊙. The SFGs and AGNs tend to exhibit the same 24 μm excess. The UV SFRs are in closer agreement with the FIR-based SFRs. Using a Calzetti UV extinction correction results in a mean excess of up to 0.3 dex and a scatter of 0.35 dex from the FIR SFRs. The previous UV SFRs are thus confirmed and the mean excess, while narrowing the gap, is insufficient to explain the discrepancy between the observed SFRs and simulation predictions. © 2010 ESO.

Published
2010
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12. HIV as a risk factor for cardiac disease in Botswana: a cross-sectional study.

Author

Schwartz T, Magdi G, Steen TW, and Sjaastad I

Abstract

The primary objective of this study was to assess how HIV has influenced the spectrum of heart diseases in Botswana and to examine the HIV prevalence among patients with cardiomegaly. The secondary objective was to evaluate the value of the cardiothoracic (CT) ratio on chest radiography (CXR) as a screening tool for cardiac disease. In total, 179 patients (age 14-97 years) with cardiomegaly (all CT ratios >0.53 on CXR) and known HIV status were referred to Botswana's sole hospital-based echocardiographic centre. Clinical examination and echocardiography were performed. Cardiomyopathy (36.9%), pericarditis (21.2%), hypertensive heart disease (14.0%), rheumatic heart disease (8.4%) and right-sided heart failure (6.7%) were the main causes of cardiomegaly; only two patients had a normal echocardiogram. The HIV prevalence was higher than in the general population [59% vs 25%; relative risk (RR) of HIV infection compared with the general population 2.4, 95% CI 2.1-2.7]. HIV infection was strongly associated with pericarditis (RR 3.3, 95% CI 2.8-3.8) and cardiomyopathy (RR 2.9, 95% CI 2.4-3.5). These data suggest an increased risk of non-ischaemic heart disease, in particular pericarditis and cardiomyopathy, among HIV-infected patients. The CT ratio on CXR had high specificity in detecting severe heart disease and can be a useful screening tool in areas with limited resources.

Published
2012
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13. The left ventricular outflow in hypertrophic cardiomyopathy: from structure to function.

Author

Yacoub MH, El-Hamamsy I, Said K, Magdi G, Abul Enein F, George R, Rossi A, Olivotto I, and Cecchi F

Subjects
Cardiomyopathy, Hypertrophic pathology, Cardiomyopathy, Hypertrophic physiopathology, Cardiomyopathy, Hypertrophic therapy, Fibrosis, Humans, Prognosis, Ventricular Outflow Obstruction pathology, Ventricular Outflow Obstruction physiopathology, Ventricular Outflow Obstruction therapy, Cardiomyopathy, Hypertrophic complications, Heart Ventricles pathology, Heart Ventricles physiopathology, Ventricular Function, Left, Ventricular Outflow Obstruction etiology
Abstract

Left ventricular outflow tract obstruction (LVOTO) is one of the defining features of hypertrophic cardiomyopathy (HCM) and one of the main determinants of prognosis. Although the importance of obstruction was recognized since the original description by Teare and Brock, its exact cause and methods for its relief are still being hotly debated. We believe that a rational approach to solving these issues depends on thorough understanding of the specific structure and functions of the left ventricular outflow tract (LVOT) in health and disease. There is now compelling evidence that the LVOT performs a series of vital sophisticated functions which are mediated by the design characteristics, structure, and biological properties of its component parts and that dysregulation of one or more of these functions results in obstruction and other abnormalities. We here review the integrated functions of the LVOT, its structural and functional relationships, with particular reference to its component parts (the major players) and their role in HCM. This knowledge is essential to evolve tailored restorative techniques for treating HCM.

Published
2009
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