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1. Comparison of star formation rates from Hα and infrared luminosity as seen byHerschel

Author

H. Domínguez Sánchez, M. Mignoli, F. Pozzi, F. Calura, A. Cimatti, C. Gruppioni, J. Cepa, M. Sánchez Portal, G. Zamorani, S. Berta, D. Elbaz, E. Le Floc'h, G. L. Granato, D. Lutz, R. Maiolino, F. Matteucci, P. Nair, R. Nordon, L. Pozzetti, L. Silva, J. Silverman, S. Wuyts, C. M. Carollo, T. Contini, J.-P. Kneib, O. Le Fèvre, S. J. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovač, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, B. Magnelli, R. Pelló, Y. Peng, E. Perez-Montero, E. Ricciardelli, L. Riguccini, M. Tanaka, L. A. M. Tasca, L. Tresse, D. Vergani, and E. Zucca

Subjects
Physics, Spiral galaxy, 010504 meteorology & atmospheric sciences, Star formation, Metallicity, Extinction (astronomy), Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

We empirically test the relation between the SFR(LIR) derived from the infrared luminosity, LIR, and the SFR(Ha) derived from the Ha emission line luminosity using simple conversion relations. We use a sample of 474 galaxies at z = 0.06 - 0.46 with both Ha detection (from 20k zCOSMOS survey) and new far-IR Herschel data (100 and 160 {\mu}m). We derive SFR(Ha) from the Ha extinction corrected emission line luminosity. We find a very clear trend between E(B - V) and LIR that allows to estimate extinction values for each galaxy even if the Ha emission line measurement is not reliable. We calculate the LIR by integrating from 8 up to 1000 {\mu}m the SED that is best fitting our data. We compare SFR(Ha) with the SFR(LIR). We find a very good agreement between the two SFR estimates, with a slope of m = 1.01 \pm 0.03 in the SFR(LIR) vs SFR(Ha) diagram, a normalization constant of a = -0.08 \pm 0.03 and a dispersion of sigma = 0.28 dex.We study the effect of some intrinsic properties of the galaxies in the SFR(LIR)-SFR(Ha) relation, such as the redshift, the mass, the SSFR or the metallicity. The metallicity is the parameter that affects most the SFR comparison. The mean ratio of the two SFR estimators log[SFR(LIR)/SFR(Ha)] varies by approx. 0.6 dex from metal-poor to metal-rich galaxies (8.1 < log(O/H) + 12 < 9.2). This effect is consistent with the prediction of a theoretical model for the dust evolution in spiral galaxies. Considering different morphological types, we find a very good agreement between the two SFR indicators for the Sa, Sb and Sc morphologically classified galaxies, both in slope and normalization. For the Sd, irregular sample (Sd/Irr), the formal best-fit slope becomes much steeper (m = 1.62 \pm 0.43), but it is still consistent with 1 at the 1.5 sigma level, because of the reduced statistics of this sub-sample.

Published
2012
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2. 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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3. The evolution of the dust temperatures of galaxies in the SFR\u2013

Author

B. Magnelli, D. Lutz, A. Saintonge, S. Berta, P. Santini, M. Symeonidis, B. Altieri, P. Andreani, H. Aussel, M. Bxe9thermin, J. Bock, A. Bongiovanni, J. Cepa, A. Cimatti, A. Conley, E. Daddi, D. Elbaz, N. M. Fxf6rster Schreiber, R. Genzel, R. J. Ivison, E. Le Floc’h, G. Magdis, R. Maiolino, R. Nordon, S. J. Oliver, M. Page, A. Pxe9rez Garcxeda, A. Poglitsch, P. Popesso, F. Pozzi, and et al (including L. Wang)

Published
2014

5. The effect of environment on star forming galaxies at redshift

Author

P. Popesso, G. Rodighiero, A. Saintonge, P. Santini, A. Grazian, D. Lutz, M. Brusa, B. Altieri, P. Andreani, H. Aussel, S. Berta, A. Bongiovanni, A. Cava, J. Cepa, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N. Förster Schreiber, R. Genzel, C. Gruppioni, G. Magdis, R. Maiolino, B. Magnelli, R. Nordon, A. M. Pérez García, A. Poglitsch, F. Pozzi, L. Riguccini, M. Sanchez-Portal, L. Shao, E. Sturm, L. Tacconi, I. Valtchanov, E. Wieprecht, and M. Wetzstein

Subjects
Physics, Spectrometer, Stellar mass, Star formation, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), Redshift, Universe, Galaxy, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Mass segregation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract

We use deep 70, 100 and 160 μm observations taken with PACS, the Photodetector Array Camera and Spectrometer on board of Herschel, as part of the PACS Evolutionary Probe (PEP) guaranteed time, to study the relation between star formation rate and environment at redshift ~ 1 in the GOODS-S and GOODS-N fields. We use the SDSS spectroscopic catalog to build the local analog and study the evolution of the star formation activity dependence on the environment. At z ∼ 1 we observe a reversal of the relation between star formation rate and local density, confirming the results based on Spitzer 24 μm data. However, due to the high accuracy provided by PACS in measuring the star formation rate also for AGN hosts, we identify in this class of objects the cause for the reversal of the density-SFR relation. Indeed, AGN hosts favor high stellar masses, dense regions and high star formation rates. Without the AGN contribution the relation flattens consistently with respect to the local analog in the same range of star formation rates. As in the local universe, the specific star formation rate anti-correlates with the density. This is due to mass segregation both at high and low redshift. The contribution of AGN hosts does not affect this anti-correlation, since AGN hosts exhibit the same specific star formation rate as star forming galaxies at the same mass. The same global trends and AGN contribution is observed once the relations are studied per morphological type. We study the specific star formation rate vs. stellar mass relation in three density regimes. Our data provides an indication that at M/M⊙ > 1011 the mean specific star formation rate tends to be higher at higher density, while the opposite trend is observed in the local SDSS star forming sample. © 2011 ESO.

Published
2011
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6. Sur deux anciens cours de la Meuse ardennaise

Author

R Nordon

Subjects
Geography, Planning and Development, Earth-Surface Processes
Abstract

Nordon R. Sur deux anciens cours de la Meuse ardennaise. In: Bulletin de l'Association de géographes français, N°23, 5e année,1928. pp. 40-44.

Published
1928

7. 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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8. The Herschel PEP/HerMES Luminosity Function. I: Probing the Evolution of PACS selected Galaxies to z~4

Author

V. Arumugam, Ismael Perez-Fournon, M. Bethermin, Andreas Papageorgiou, Alberto Franceschini, Mattia Vaccari, A. M. Pérez García, Lucia Pozzetti, G. Wright, B. O'Halloran, P. Chanial, Giulia Rodighiero, Pierluigi Monaco, P. Popesso, E. Zucca, Michael Pohlen, Benjamin Magnelli, K. G. Isaak, Lucia Marchetti, Eckhard Sturm, Bruno Maffei, Michael Rowan-Robinson, Matthew Joseph Griffin, Michael Zemcov, Marco Scodeggio, C. K. Xu, Lian-Tao Wang, Antonio Cava, O. Le Fevre, K. E. Tugwell, M. Magliocchetti, Dimitra Rigopoulou, Albrecht Poglitsch, S. C. Madden, Bruno Altieri, Raanan Nordon, M. Carollo, Rob Ivison, Alexandre Amblard, N. Castro-Rodríguez, R. Genzel, James J. Bock, Vincenzo Mainieri, Linda J. Tacconi, Alvio Renzini, Anthony J. Smith, Francesca Pozzi, David J. Rosario, Chris Pearson, Mark Sargent, A. Boselli, Denis Burgarella, G. Mainetti, Edo Ibar, C. D. Dowell, Ivan Delvecchio, H. Aussel, A. Conley, Benjamin L. Schulz, Simon J. Lilly, Jamie Stevens, H. T. Nguyen, V. Buat, Guilaine Lagache, D. Elbaz, Nick Seymour, Asantha Cooray, Alessandro Cimatti, Douglas Scott, M. J. Page, Louis Levenson, M. Sánchez-Portal, Evanthia Hatziminaoglou, David L. Clements, Nanyao Y. Lu, M. Symeonidis, S. Berta, L. Riguccini, L. Vigroux, Ivan Valtchanov, Emanuele Daddi, Roberto Maiolino, Eli Dwek, J. Cepa, Stephen Anthony Eales, H. Dominguez-Sanchez, G. Zamorani, Dieter Lutz, P. Panuzzo, S. Bardelli, D. L. Shupe, Carlotta Gruppioni, E. Le Floc'h, Isaac Roseboom, Seb Oliver, Ángel Bongiovanni, P. Andreani, Alvaro Iribarrem, Thierry Contini, N. M. Foerster Schreiber, Jason Glenn, Markos Trichas, O. Ilbert, C., Gruppioni, F., Pozzi, G., Rodighiero, I., Delvecchio, S., Berta, L., Pozzetti, G., Zamorani, P., Andreani, A., Cimatti, O., Ilbert, E., Le Floc'h, D., Lutz, B., Magnelli, L., Marchetti, Monaco, Pierluigi, R., Nordon, S., Oliver, P., Popesso, L., Riguccini, I., Roseboom, D. J., Rosario, M., Sargent, M., Vaccari, B., Altieri, H., Aussel, A., Bongiovanni, J., Cepa, E., Daddi, H., Dominguez Sanchez, D., Elbaz, N., Forster Schreiber, R., Genzel, A., Iribarrem, M., Magliocchetti, R., Maiolino, A., Poglitsch, A., Perez Garcia, M., Sanchez Portal, E., Sturm, L., Tacconi, I., Valtchanov, A., Amblard, V., Arumugam, M., Bethermin, J., Bock, A., Boselli, V., Buat, D., Burgarella, N., Castro Rodriguez, A., Cava, P., Chanial, D. L., Clement, A., Conley, A., Cooray, C. D., Dowell, E., Dwek, S., Eale, A., Franceschini, J., Glenn, M., Griffin, E., Hatziminaoglou, E., Ibar, K., Isaak, R. J., Ivison, G., Lagache, L., Levenson, N., Lu, S., Madden, B., Maffei, G., Mainetti, H. T., Nguyen, B., O'Halloran, M. J., Page, P., Panuzzo, A., Papageorgiou, C. P., Pearson, I., Perez Fournon, M., Pohlen, D., Rigopoulou, M., Rowan Robinson, B., Schulz, D., Scott, N., Seymour, D. L., Shupe, A. J., Smith, J. A., Steven, M., Symeonidi, M., Tricha, K. E., Tugwell, L., Vigroux, L., Wang, G., Wright, C. K., Xu, M., Zemcov, S., Bardelli, M., Carollo, T., Contini, O., Le Fevre, S., Lilly, V., Mainieri, A., Renzini, M., Scodeggio, E., Zucca, C. Gruppioni, F. Pozzi, G. Rodighiero, I. Delvecchio, S. Berta, L. Pozzetti, G. Zamorani, P. Andreani, A. Cimatti, O. Ilbert, E. Le Floc'h, D. Lutz, B. Magnelli, L. Marchetti, P. Monaco, R. Nordon, S. Oliver, P. Popesso, L. Riguccini, I. Roseboom, D. J. Rosario, M. Sargent, M. Vaccari, B. Altieri, H. Aussel, A. Bongiovanni, J. Cepa, E. Daddi, H. Dominguez-Sanchez, D. Elbaz, N. Forster Schreiber, R. Genzel, A. Iribarrem, M. Magliocchetti, R. Maiolino, A. Poglitsch, A. Perez Garcia, M. Sanchez-Portal, E. Sturm, L. Tacconi, I. Valtchanov, A. Amblard, V. Arumugam, M. Bethermin, J. Bock, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodriguez, A. Cava, P. Chanial, D. L. Clement, A. Conley, A. Cooray, C. D. Dowell, E. Dwek, S. Eale, A. Franceschini, J. Glenn, M. Griffin, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, L. Levenson, N. Lu, S. Madden, B. Maffei, G. Mainetti, H. T. Nguyen, B. O'Halloran, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Perez-Fournon, M. Pohlen, D. Rigopoulou, M. Rowan-Robinson, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, J. A. Steven, M. Symeonidi, M. Tricha, K. E. Tugwell, L. Vigroux, L. Wang, G. Wright, C. K. Xu, M. Zemcov, S. Bardelli, M. Carollo, T. Contini, O. Le Fevre, S. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, and E. Zucca

Subjects
Astrofísica, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: active, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, galaxies: evolution, galaxies: luminosity function, mass function, cosmology: observations, infrared: galaxies, 01 natural sciences, galaxies [infrared], Luminosity, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], QB, Luminosity function (astronomy), luminosity function [galaxies], Physics, Luminous infrared galaxy, Supermassive black hole, cosmology: observation, Spiral galaxy, 010308 nuclear & particles physics, starburst [galaxies], Astronomy, Astronomy and Astrophysics, Galaxy, Astronomía, Space and Planetary Science, active [galaxies], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology]
Abstract

We exploit the deep and extended far infrared data sets (at 70, 100 and 160 um) of the Herschel GTO PACS Evolutionary Probe (PEP) Survey, in combination with the HERschel Multi tiered Extragalactic Survey (HerMES) data at 250, 350 and 500 um, to derive the evolution of the restframe 35 um, 60 um, 90 um, and total infrared (IR) luminosity functions (LFs) up to z~4. We detect very strong luminosity evolution for the total IR LF combined with a density evolution. In agreement with previous findings, the IR luminosity density increases steeply to z~1, then flattens between z~1 and z~3 to decrease at z greater than 3. Galaxies with different SEDs, masses and sSFRs evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to the IR luminosity density. Galaxies occupying the well established SFR/stellar mass main sequence (MS) are found to dominate both the total IR LF and luminosity density at all redshifts, with the contribution from off MS sources (0.6 dex above MS) being nearly constant (~20% of the total IR luminosity density) and showing no significant signs of increase with increasing z over the whole 0.8, Comment: 32 pages, 20 figures, 9 tables. Published in MNRAS. Replaced Fig. 8 (small scaling bug in the previous version)

Published
2013
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9. The Herschel-PEP survey: evidence for downsizing in the hosts of dusty star-forming systems

Author

Eckhard Sturm, L. Riguccini, David J. Rosario, I. Valtchanov, P. Popesso, Linda J. Tacconi, Francesca Pozzi, P. Andreani, Dieter Lutz, N. M. Förster Schreiber, D. Elbaz, H. Aussel, J. Cepa, Roberto Maiolino, Raanan Nordon, Andrea Cimatti, S. Berta, Héctor O. Castañeda, E. Le Floc'h, M. Magliocchetti, M. Sánchez-Portal, P. Santini, Reinhard Genzel, Benjamin Magnelli, Giulia Rodighiero, Bruno Altieri, Albrecht Poglitsch, Carlotta Gruppioni, O. Ilbert, Andrea Grazian, M. Magliocchetti, P. Popesso, D. Rosario, D. Lutz, H. Aussel, S. Berta, B. Altieri, P. Andreani, J. Cepa, H. Castaneda, A. Cimatti, D. Elbaz, R. Genzel, A. Grazian, C. Gruppioni, O. Ilbert, E. Le Floc'h, B. Magnelli, R. Maiolino, R. Nordon, A. Poglitsch, F. Pozzi, L. Riguccini, G. Rodighiero, M. Sanchez-Portal, P. Santini, N. M. Forster Schreiber, E. Sturm, L. Tacconi, and I. Valtchanov

Subjects
large-scale structure of the Universe, Luminous infrared galaxy, Physics, cosmology: observation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Limiting, Astrophysics, Star (graph theory), Correlation function (astronomy), Cosmology, infrared: galaxies, Extended Groth Strip, Space and Planetary Science, cosmology: theory, galaxies: statistic, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Cluster analysis, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

By making use of Herschel-PEP observations of the COSMOS and Extended Groth Strip fields, we have estimated the dependence of the clustering properties of FIR-selected sources on their 100um fluxes. Our analysis shows a tendency for the clustering strength to decrease with limiting fluxes: r0(S100um >8 mJy)~4.3 Mpc and r0(S100um >5 mJy)~5.8 Mpc. These values convert into minimum halo masses Mmin~10^{11.6} Msun for sources brighter than 8 mJy and Mmin~10^{12.4} Msun for S100um > 5 mJy galaxies. We show such an increase of the clustering strength to be due to an intervening population of z~2 sources, which are very strongly clustered and whose relative contribution, equal to about 10% of the total counts at S100um > 2 mJy, rapidly decreases for brighter flux cuts. By removing such a contribution, we find that z ~100 Msun/yr). Our analysis shows that the same amount of (intense) star forming activity takes place in extremely different environments at the different cosmological epochs. For z, Comment: 12 pages, 8 figures, to appear in MNRAS

Published
2013
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10. 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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11. 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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12. The Mean Star-Forming Properties of QSO Host Galaxies

Author

David J. Rosario, Marcella Brusa, Natascha M. Förster-Schreiber, Jonathan R. Trump, Paola Santini, Andrea Merloni, Roberto Maiolino, Elisabeta Lusso, Simon J. Lilly, Benny Trakhtenbrot, M. Mignoli, Paola Popesso, Benjamin Magnelli, Angela Bongiorno, Mara Salvato, Linda J. Tacconi, M. Schramm, G. Zamorani, V. Mainieri, S. Berta, Dieter Lutz, Hagai Netzer, Raanan Nordon, Reinhard Genzel, John D. Silverman, D. J. Rosario, B. Trakhtenbrot, D. Lutz, H. Netzer, J. R. Trump, J. D. Silverman, M. Schramm, E. Lusso, S. Berta, A. Bongiorno, M. Brusa, N. M. Förster-Schreiber, R. Genzel, S. Lilly, B. Magnelli, V. Mainieri, R. Maiolino, A. Merloni, M. Mignoli, R. Nordon, P. Popesso, M. Salvato, P. Santini, L. J. Tacconi, and G. Zamorani

Subjects
Physics, QSOS, Luminous infrared galaxy, Supermassive black hole, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, infrared: galaxie, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: active, Galaxies: high-redshift, Galaxies: star formation, Infrared: galaxies, Quasars: general, Surveys, Accretion (astrophysics), Redshift, Galaxy, Black hole, Space and Planetary Science, galaxies: high-redshift, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Quasi-stellar objects (QSOs) occur in galaxies in which supermassive black holes (SMBHs) are growing substantially through rapid accretion of gas. Many popular models of the co-evolutionary growth of galaxies and SMBHs predict that QSOs are also sites of substantial recent star formation, mediated by important processes, such as major mergers, which rapidly transform the nature of galaxies. A detailed study of the star-forming properties of QSOs is a critical test of such models. We present a far-infrared Herschel/PACS study of the mean star formation rate (SFR) of a sample of spectroscopically observed QSOs to z~2 from the COSMOS extragalactic survey. This is the largest sample to date of moderately luminous AGNs studied using uniform, deep far-infrared photometry. We study trends of the mean SFR with redshift, black hole mass, nuclear bolometric luminosity and specific accretion rate (Eddington ratio). To minimize systematics, we have undertaken a uniform determination of SMBH properties, as well as an analysis of important selection effects within spectroscopic QSO samples that influence the interpretation of SFR trends. We find that the mean SFRs of these QSOs are consistent with those of normal massive star-forming galaxies with a fixed scaling between SMBH and galaxy mass at all redshifts. No strong enhancement in SFR is found even among the most rapidly accreting systems, at odds with several co-evolutionary models. Finally, we consider the qualitative effects on mean SFR trends from different assumptions about the star-forming properties of QSO hosts and redshift evolution of the SMBH-galaxy relationship. While limited currently by uncertainties, valuable constraints on AGN-galaxy co-evolution can emerge from our approach., 10 figures, 1 table; accepted for publication in Astronomy & Astrophysics

Published
2013

13. The lack of star formation gradients in galaxy groups up to z tilde 1.6

Author

Mara Salvato, D. Fadda, Andrea Biviano, H. Aussel, R. Genzel, W. N. Brandt, E. Le Floc'h, Dieter Lutz, Kirpal Nandra, M. C. Cooper, Franz E. Bauer, D. Elbaz, Raanan Nordon, Benjamin Magnelli, A. Cimatti, Alexis Finoguenov, Linda J. Tacconi, M. Sanchez Portal, Bruno Altieri, Francesca Pozzi, P. Popesso, Albrecht Poglitsch, Nico Cappelluti, D. Wilman, S. Berta, Masayuki Tanaka, O. Ilbert, John S. Mulchaey, Mark Dickinson, F. Ziparo, Stijn Wuyts, F. Ziparo, P. Popesso, A. Biviano, A. Finoguenov, S. Wuyt, D. Wilman, M. Salvato, M. Tanaka, O. Ilbert, K. Nandra, D. Lutz, D. Elbaz, M. Dickinson, B. Altieri, H. Aussel, S. Berta, A. Cimatti, D. Fadda, R. Genzel, E. Le Flo'ch, B. Magnelli, R. Nordon, A. Poglitsch, F. Pozzi, M. S. Portal, L. Tacconi, F. E. Bauer, W. N. Brandt, N. Cappelluti, M. C. Cooper, and J. S. Mulchaey

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Astronomy & Astrophysics, galaxies [infrared], Peculiar galaxy, galaxies: groups: general, Galaxy group, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, clusters, Interacting galaxy, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, [galaxies], evolution [galaxies], Luminous infrared galaxy, Physics, groups: general [galaxies], general [groups], infrared: galaxie, Astronomy, Astronomy and Astrophysics, stellar content [galaxies], X-rays: galaxies: cluster, galaxies [X-rays], Space and Planetary Science, galaxies: star formation, Elliptical galaxy, astro-ph.CO, galaxies: stellar content, galaxies: clusters [X-rays], star formation [galaxies], galaxies: evolution, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In the local Universe, galaxy properties show a strong dependence on environment. In cluster cores, early type galaxies dominate, whereas star-forming galaxies are more and more common in the outskirts. At higher redshifts and in somewhat less dense environments (e.g. galaxy groups), the situation is less clear. One open issue is that of whether and how the star formation rate (SFR) of galaxies in groups depends on the distance from the centre of mass. To shed light on this topic, we have built a sample of X-ray selected galaxy groups at 010^10.3 M_sun in order to have a high spectroscopic completeness. As we use only spectroscopic redshifts, our results are not affected by uncertainties due to projection effects. We use several SFR indicators to link the star formation (SF) activity to the galaxy environment. Taking advantage of the extremely deep mid-infrared Spitzer MIPS and far-infrared Herschel PACS observations, we have an accurate, broad-band measure of the SFR for the bulk of the star-forming galaxies. We use multi-wavelength SED fitting techniques to estimate the stellar masses of all objects and the SFR of the MIPS and PACS undetected galaxies. We analyse the dependence of the SF activity, stellar mass and specific SFR on the group-centric distance, up to z~1.6, for the first time. We do not find any correlation between the mean SFR and group-centric distance at any redshift. We do not observe any strong mass segregation either, in agreement with predictions from simulations. Our results suggest that either groups have a much smaller spread in accretion times with respect to the clusters and that the relaxation time is longer than the group crossing time., Comment: Accepted for publication in MNRAS

Published
2013
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14. Cosmological model dependence of the galaxy luminosity function: far-infrared results in the Lemaître-Tolman-Bondi model

Author

L. Riguccini, Benjamin Magnelli, Alvaro Iribarrem, Sean February, Marcelo B. Ribeiro, Paola Popesso, E. Le Floc'h, S. Berta, Raanan Nordon, Carlotta Gruppioni, Paola Andreani, Francesca Pozzi, European Southern Observatory (ESO), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, A. Iribarrem, P. Andreani, C. Gruppioni, S. February, M. B. Ribeiro, S. Berta, E. Le Floc’h, B. Magnelli, R. Nordon, P. Popesso, F. Pozzi, L. Riguccini, Department of Astronomy, and Faculty of Science

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, infrared: galaxies, General Relativity and Quantum Cosmology, cosmology: theory, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, infrared: galaxie, Estimator, Astronomy and Astrophysics, Redshift, Galaxy, galaxies: distances and redshift, Supernova, galaxies: luminosity function, Space and Planetary Science, mass function, galaxies: luminosity function, mass function, galaxies: distances and redshifts, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This is the first paper of a series aiming at investigating galaxy formation and evolution in the giant-void class of the Lemaitre-Tolman-Bondi (LTB) models that best fits current cosmological observations. Here we investigate the Luminosity Function (LF) methodology, and how its estimates would be affected by a change on the cosmological model assumed in its computation. Are the current observational constraints on the allowed Cosmology enough to yield robust LF results? We use the far-infrared source catalogues built on the observations performed with the Herschel/PACS instrument, and selected as part of the PACS evolutionary probe (PEP) survey. Schechter profiles are obtained in redshift bins up to z approximately 4, assuming comoving volumes in both the standard model, that is, Friedmann-Lemaitre-Robertson-Walker metric with a perfect fluid energy-momentum tensor, and non-homogeneous LTB dust models, parametrized to fit the current combination of results stemming from the observations of supernovae Ia, the cosmic microwave background, and baryonic acoustic oscillations. We find that the luminosity functions computed assuming both the standard model and LTB void models show in general good agreement. However, the faint-end slope in the void models shows a significant departure from the standard model up to redshift 0.4. We demonstrate that this result is not artificially caused by the used LF estimator which turns out to be robust under the differences in matter-energy density profiles of the models. The differences found in the LF slopes at the faint end are due to variation in the luminosities of the sources, which depend on the geometrical part of the model. It follows that either the standard model is over-estimating the number density of faint sources or the void models are under-estimating it., 23 pages, 11 figures. Accepted for publication in A&A

Published
2013
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15. 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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16. Panchromatic spectral energy distributions of Herschel sources

Author

Alberto Franceschini, Ho Seong Hwang, Giulia Rodighiero, L. Riguccini, David J. Rosario, Paola Santini, Raanan Nordon, S. Berta, Francesca Pozzi, A. Cooray, Drew Brisbin, Paola Popesso, Benjamin Magnelli, Marco P. Viero, E. Le Floc'h, Lucia Pozzetti, Dieter Lutz, Carlotta Gruppioni, Isaac Roseboom, S. J. Oliver, Douglas Scott, Stijn Wuyts, Ivan Valtchanov, Lian-Tao Wang, Evanthia Hatziminaoglou, M. Symeonidis, M. J. Page, S. Berta, D. Lutz, P. Santini, S. Wuyt, D. Rosario, D. Brisbin, A. Cooray, A. Franceschini, C. Gruppioni, E. Hatziminaoglou, H. S. Hwang, E. Le Floc’h, B. Magnelli, R. Nordon, S. Oliver, M. J. Page, P. Popesso, L. Pozzetti, F. Pozzi, L. Riguccini, G. Rodighiero, I. Roseboom, D. Scott, M. Symeonidi, I. Valtchanov, M. Viero, and L. Wang

Subjects
statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Infrared, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], Luminosity, infrared: galaxies, Photometry (optics), Astrophysics::Solar and Stellar Astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, galaxies: statistics, Physics, Luminous infrared galaxy, Star formation, Astronomy and Astrophysics, infrared: galaxies – galaxies: statistics – galaxies: star formation – galaxies: active – galaxies: evolution, Galaxy, Stars, Space and Planetary Science, galaxies: star formation, active [galaxies], Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(abridged) Far-infrared Herschel photometry from the PEP and HerMES programs is combined with ancillary datasets in the GOODS-N, GOODS-S, and COSMOS fields. Based on this rich dataset, we reproduce the restframe UV to FIR ten-colors distribution of galaxies using a superposition of multi-variate Gaussian modes. The median SED of each mode is then fitted with a modified version of the MAGPHYS code that combines stellar light, emission from dust heated by stars and a possible warm dust contribution heated by an AGN. The defined Gaussian grouping is also used to identify rare sources. The zoology of outliers includes Herschel-detected ellipticals, very blue z~1 Ly-break galaxies, quiescent spirals, and torus-dominated AGN with star formation. Out of these groups and outliers, a new template library is assembled, consisting of 32 SEDs describing the intrinsic scatter in the restframe UV-to-submm colors of infrared galaxies. This library is tested against L(IR) estimates with and without Herschel data included, and compared to eight other popular methods often adopted in the literature. When implementing Herschel photometry, these approaches produce L(IR) values consistent with each other within a median absolute deviation of 10-20%, the scatter being dominated more by fine tuning of the codes, rather than by the choice of SED templates. Finally, the library is used to classify 24 micron detected sources in PEP GOODS fields. AGN appear to be distributed in the stellar mass (M*) vs. star formation rate (SFR) space along with all other galaxies, regardless of the amount of infrared luminosity they are powering, with the tendency to lie on the high SFR side of the "main sequence". The incidence of warmer star-forming sources grows for objects with higher specific star formation rates (sSFR), and they tend to populate the "off-sequence" region of the M*-SFR-z space., Comment: Accepted for publication in A&A. Some figures are presented in low resolution. The new galaxy templates are available for download at the address http://www.mpe.mpg.de/ir/Research/PEP/uvfir_templ

Published
2013
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17. Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density

Author

V. Buat, Duncan Farrah, M. J. Page, Francesca Pozzi, Asantha Cooray, Raanan Nordon, James Dunlop, S. J. Oliver, Benjamin Magnelli, Denis Burgarella, S. Berta, E. Le Floc'h, D. Lutz, Sebastien Heinis, P. Popesso, L. Riguccini, Marco Viero, Carlotta Gruppioni, Alberto Franceschini, Mattia Vaccari, O. Cucciati, M. Bethermin, J. J. Bock, 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), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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), D. Burgarella, V. Buat, C. Gruppioni, O. Cucciati, S. Heini, S. Berta, M. Béthermin, J. Bock, A. Cooray, J. S. Dunlop, D. Farrah, A. Franceschini, E. Le Floc’h, D. Lutz, B. Magnelli, R. Nordon, S. J. Oliver, M. J. Page, P. Popesso, F. Pozzi, L. Riguccini, M. Vaccari, M. Viero, 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)), and 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)

Subjects
Stellar mass, media_common.quotation_subject, galaxies: starburst, Astrophysics, Plateau (mathematics), 01 natural sciences, infrared: galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, media_common, Physics, cosmology: observation, 010308 nuclear & particles physics, Star formation, Attenuation, infrared: galaxie, Astronomy and Astrophysics, early Universe, Redshift, Galaxy, Universe, Space and Planetary Science, Homogeneous, galaxies: star formation, cosmology: observations, ultraviolet: galaxies, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Using new homogeneous luminosity functions (LFs) in the far-ultraviolet (FUV) from VVDS and in the far-infrared (FIR) from Herschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we were able to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRDTOT). By integrating SFRDTOT, we followed the mass building and analyzed the redshift evolution of the stellar mass density (SMD). This article aims at providing a complete view of star formation from the local Universe to z ~ 4 and, using assumptions on earlier star formation history, compares this evolution with previously published data in an attempt to draw a homogeneous picture of the global evolution of star formation in galaxies. Our main conclusions are that: 1) the dust attenuation AFUV is found to increase from z = 0 to z ~ 1.2 and then starts to decrease until our last data point at z = 3.6; 2) the estimated SFRD confirms published results to z ~ 2. At z > 2, we observe either a plateau or a small increase up to z ~ 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect to the plateau of SFRDTOT and a probable origin might be found in the evolution of the bright ends of the FUV and FIR LFs; 4) using assumptions (exponential rise and linear rise with time) for the evolution of the star formation density from z = 3.6 to zform = 10, we integrated SFRDTOT and obtained a good agreement with the published SMDs.

Published
2013
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18. 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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19. 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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20. Donor T cells for CAR T cell therapy.

Author

Tang TCY, Xu N, Nordon R, Haber M, Micklethwaite K, and Dolnikov A

Abstract

Adoptive cell therapy using patient-derived chimeric receptor antigen (CAR) T cells redirected against tumor cells has shown remarkable success in treating hematologic cancers. However, wider accessibility of cellular therapies for all patients is needed. Manufacture of patient-derived CAR T cells is limited by prolonged lymphopenia in heavily pre-treated patients and risk of contamination with tumor cells when isolating T cells from patient blood rich in malignant blasts. Donor T cells provide a good source of immune cells for adoptive immunotherapy and can be used to generate universal off-the-shelf CAR T cells that are readily available for administration into patients as required. Genome editing tools such as TALENs and CRISPR-Cas9 and non-gene editing methods such as short hairpin RNA and blockade of protein expression are currently used to enhance CAR T cell safety and efficacy by abrogating non-specific toxicity in the form of graft versus host disease (GVHD) and preventing CAR T cell rejection by the host., (© 2022. The Author(s).)

Published
2022
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22. Positioning a Scientific Community on Unproven Cellular Therapies: The 2015 International Society for Cellular Therapy Perspective.

Author

Dominici M, Nichols K, Srivastava A, Weiss DJ, Eldridge P, Cuende N, Deans RJ, Rasko JE, Levine AD, Turner L, Griffin DL, O'Donnell L, Forte M, Mason C, Wagena E, Janssen W, Nordon R, Wall D, Ho HN, Ruiz MA, Wilton S, Horwitz EM, and Gunter KC

Subjects
Humans, Societies, Medical, Cell- and Tissue-Based Therapy standards, Evidence-Based Medicine, Patient Safety standards
Published
2015
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23. Ex vivo expansion of cord blood progenitors impairs their short-term and long-term repopulating activity associated with transcriptional dysregulation of signalling networks.

Author

Holmes T, Yan F, Ko KH, Nordon R, Song E, O'Brien TA, and Dolnikov A

Subjects
Animals, Antigens, CD34 metabolism, Cell Cycle Proteins genetics, Cell Cycle Proteins metabolism, Cell Differentiation, Cell Proliferation, Cells, Cultured, Flow Cytometry, Gene Expression Regulation, Hematopoietic Stem Cell Transplantation, Hematopoietic Stem Cells cytology, Humans, Immunophenotyping, Mice, Time Factors, Transplantation, Heterologous, Fetal Blood cytology, Hematopoietic Stem Cells metabolism, Signal Transduction
Abstract

Objectives: Cord blood (CB) has been established to be an alternative source of haematopoietic stem/progenitor cells (HPC) for transplantation. The number of HPC per CB unit is limited, which results in engraftment delay. Ex vivo expansion of HPC improvement must overcome this., Materials and Methods: Flow cytometry was used to extensively phenotype HPC pre- and post-expansion and CFDA-SE staining was used to track cell divisions. The NSG mouse model was employed in transplantation studies to determine long and short term repopulation in human cells. Gene array analysis was used to evaluate signalling pathways regulated following ex vivo expansion of HPC., Results: expansion of CD34(+) HPC impaired their regenerative function. In this xenograft transplantation model we showed that repopulating activity of CB cells declined following expansion. Expanded HPC had delayed engraftment at early and late stages post-transplant. High resolution division tracking revealed that the cultured HPC had reduced expansion and self-renewal probability and increased differentiation rate compared to non-expanded cells. Gene expression analysis exposed significant modulation of a complex network of genes and pathways that normally maintain HPC proliferation and limit their differentiation., Conclusions: The decline in short-term engraftment is consistent with the loss of rapid SCID repopulating ability r(SRA) by expanded CD34(+) CD38(+) cells recently reported. Our data raise concerns for future clinical applications of expanded HPC alone in transplantation., (© 2012 Blackwell Publishing Ltd.)

Published
2012
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24. GSK-3β inhibition promotes engraftment of ex vivo-expanded hematopoietic stem cells and modulates gene expression.

Author

Ko KH, Holmes T, Palladinetti P, Song E, Nordon R, O'Brien TA, and Dolnikov A

Subjects
Animals, Cell Cycle drug effects, Cell Cycle genetics, Cell Proliferation drug effects, Cells, Cultured, Chimerism drug effects, Cyclin D1 metabolism, Cyclin-Dependent Kinase Inhibitor p57 metabolism, Fetal Blood cytology, Flow Cytometry, Glycogen Synthase Kinase 3 beta, Hematopoietic Stem Cells enzymology, Hematopoietic Stem Cells physiology, Humans, Mice, Mice, Inbred NOD, Mice, SCID, Signal Transduction genetics, Gene Expression drug effects, Glycogen Synthase Kinase 3 antagonists & inhibitors, Hematopoietic Stem Cell Transplantation methods, Hematopoietic Stem Cells drug effects, Indoles pharmacology, Oximes pharmacology, Wnt Proteins metabolism
Abstract

Glycogen synthase kinase-3β (GSK-3β) has been identified as an important regulator of stem cell function acting through activation of the wingless (Wnt) pathway. Here, we report that treatment with an inhibitor of GSK-3β, 6-bromoindirubin 3'-oxime (BIO) delayed cell cycle progression by increasing cell cycle time. BIO treatment resulted in the accumulation of late dividing cells enriched with primitive progenitor cells retaining the ability for sustained proliferation. In vivo analysis using a Non-obese diabetic/severe combined immunodeficient (NOD/SCID) transplantation model has demonstrated that pretreatment with BIO promotes engraftment of ex vivo-expanded hematopoietic stem cells. BIO enhanced the engraftment of myeloid, lymphoid and primitive stem cell compartments. Limiting dilution analysis of SCID repopulating cells (SRC) revealed that BIO treatment increased human chimerism without increasing SRC frequency. Clonogenic analysis of human cells derived from the bone marrow of transplant recipient mice demonstrated that a higher level of human chimerism and cellularity was related to increased regeneration per SRC unit. Gene expression analysis showed that treatment with BIO did not modulate the expression of canonical Wnt target genes upregulated during cytokine-induced cell proliferation. BIO increased the expression of several genes regulating Notch and Tie2 signaling downregulated during ex vivo expansion, suggesting a role in improving stem cell engraftment. In addition, treatment with BIO upregulated CDK inhibitor p57 and downregulated cyclin D1, providing a possible mechanism for the delay seen in cell cycle progression. We conclude that transient, pharmacologic inhibition of GSK-3β provides a novel approach to improve engraftment of expanded HSC after stem cell transplantation., (Copyright © 2010 AlphaMed Press.)

Published
2011
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25. Chimeric protein for selective cell attachment onto cellulosic substrates.

Author

Craig SJ, Shu A, Xu Y, Foong FC, and Nordon R

Subjects
Animals, Antigens, CD34 chemistry, Cell Separation, Cloning, Molecular, Humans, Immunoglobulin G chemistry, Ligands, Mice, Protein Structure, Tertiary, Rabbits, Rats, Recombinant Fusion Proteins biosynthesis, Recombinant Fusion Proteins genetics, Substrate Specificity, Antibodies chemistry, Cell Adhesion, Cellulose chemistry, Protein Engineering, Recombinant Fusion Proteins chemistry
Abstract

We have developed a fusion protein (CBD-LG) incorporating a cellulose-binding domain and an antibody binding domain, protein LG, to provide an adaptor molecule for cell separation with regenerated cellulose hollow fiber arrays. A single hollow fiber cell adhesion assay utilizing a CD34+ cell line, KG1a, was used to investigate whether ligand affinity interactions were strong enough for cell attachment and separation. CBD-LG efficiently captured CD34+ cells labeled with the mouse IgG2a monoclonal antibody MHCD3400. However, it was not possible to bind CD34+ cells labeled with an IgG1 antibody (HPCA-2). The low affinity of HPCA-2 for LG was overcome by secondary antibodies: KG1a cells that were dual labeled with HPCA-2 followed by rat anti-mouse IgG1 adhered inside hollow fibers coated with CBD-LG. Alternatively, immobilized rabbit polyclonal anti-mouse IgG1 captured cells labeled with HPCA-2. The development of an adaptor molecule to display recombinant domains at the surface of hollow fibers will be an effective tool to investigate cellular ligand-receptor interactions, a necessary step in the development of hollow fiber bioreactors for manufacture of human cellular products.

Published
2007
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26. Engineered proteins containing the cohesin and dockerin domains from Clostridium thermocellum provides a reversible, high affinity interaction for biotechnology applications.

Author

Craig SJ, Foong FC, and Nordon R

Subjects
Bacterial Proteins chemistry, Carrier Proteins chemistry, Cell Cycle Proteins chemistry, Chromosomal Proteins, Non-Histone chemistry, Clostridium thermocellum chemistry, Nuclear Proteins chemistry, Protein Structure, Tertiary genetics, Recombinant Fusion Proteins chemistry, Cohesins, Bacterial Proteins genetics, Carrier Proteins genetics, Cell Cycle Proteins genetics, Chromosomal Proteins, Non-Histone genetics, Clostridium thermocellum genetics, Nuclear Proteins genetics, Protein Engineering methods, Recombinant Fusion Proteins genetics
Abstract

The cohesin-dockerin interaction, which is responsible for the formation of the cellulosome complex of cellulolytic bacteria, is a calcium-dependent, high affinity interaction. In this study, the cohesin (Cip7) and dockerin (Doc) domains of Clostridium thermocellum were fused to the cellulose-binding domain (CBD) of C. cellulovorans and the antibody-binding domain, protein LG, respectively, to form CBD-Cip7 and LG-Doc. Immobilised CBD-Cip7 was able to bind LG-Doc and subsequently antibody as determined using surface plasmon resonance. Binding was reversed by the removal of Ca2+ with EDTA. The dockerin containing fusion protein was affinity purified using an immobilised cohesin domain. Elution of the LG-Doc from the cohesin column was with EDTA. This affinity chromatography was repeated using an LG-dockerin column for the purification of cohesin fusion protein. The fusion proteins created in this report have shown that the properties of the cohesin and dockerin domains can be transferred to other protein domains and that the interaction between the cohesin and dockerin is specific, Ca2+ -dependent and reversible. We have shown that the cohesin-dockerin interaction has several properties making it suitable for use in recombinant fusion protein production and purification.

Published
2006
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27. Susceptibility of cell populations to transduction by retroviral vectors.

Author

Wotherspoon S, Dolnikov A, Symonds G, and Nordon R

Subjects
Antigens, CD34 blood, Cells, Cultured, Fetal Blood cytology, Fetal Blood metabolism, Hematopoietic Stem Cells metabolism, Humans, Receptor, Nerve Growth Factor analysis, Genetic Vectors, Retroviridae genetics, Transduction, Genetic
Abstract

Retroviral transduction efficiency is related to the multiplicity of infection and the physiological state of the target cells. It is generally not known what proportion of a cell population is susceptible to transduction. We used coinfection with two retroviral vectors containing the marker genes for green fluorescent protein and the truncated human nerve growth factor receptor. In the CD34+ cell line TF-1 or human primary CD34+ hematopoietic progenitor cells, it was found that cells transduced with one vector had a better than random chance of transduction by the other vector. A probability model was developed to estimate target cell susceptibility; susceptibility was calculated as the product of the proportions of transgene-positive cells divided by the proportion of double-positive cells. By using this relationship, it was found that susceptibility was related to the target cell type and culture conditions but not the retroviral titer or the retroviral packaging envelope protein used in this study. Cotransduction with two vectors is a relatively simple procedure that provides a means to assess the maximum transduction level possible in a given cell population.

Published
2004
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