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Start Over Author "Carollo, M." Topic astrophysics::galaxy astrophysics
25 results on '"Carollo, M."'

1. PHIBSS2: survey design and z = 0.5 – 0.8 results

Author

Freundlich, J., Combes, F., Tacconi, L., Genzel, R., García-Burillo, S., Neri, R., Contini, T., Bolatto, A., Lilly, S., Salomé, P., Bicalho, I., Boissier, J., Boone, F., Bouché, N., Bournaud, F., Burkert, A., Carollo, M., Cooper, M., Cox, P., Feruglio, C., Schreiber, N, Juneau, S., Lippa, M., Lutz, D., Naab, T., Renzini, A., Saintonge, A., Sternberg, A., Walter, F., Weiner, B., Weiß, A., Wuyts, S., Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Observatorio Astronómico Nacional (OAN), oan, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, AUTRES, Biologie et écologie tropicale et méditerranéenne [2007-2010] (BETM), Université de Perpignan Via Domitia (UPVD)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Nanotechnologies Nanosystèmes (LN2 ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-École Centrale de Lyon (ECL), Université de Lyon-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)-Université de Sherbrooke (UdeS)-École supérieure de Chimie Physique Electronique de Lyon (CPE)-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-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Universitätssternwarte der Ludwig-Maximiliansuniversität, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut of Physics - Riga, Latvian Academy of Sciences, Steward observatory, University of Arizona, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Galaxies et cosmologie, Observatorio Astronomico Nacional, Madrid, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Perpignan Via Domitia (UPVD)-École Pratique des Hautes Études (EPHE), Université de Sherbrooke (UdeS)-École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-École Supérieure de Chimie Physique Électronique de Lyon (CPE)-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)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Interactions Hôtes-Pathogènes-Environnements (IHPE), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Perpignan Via Domitia (UPVD), Institut Interdisciplinaire d'Innovation Technologique (3IT), Université de Sherbrooke [Sherbrooke], Ludwig-Maximiliansuniversität, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of São Paulo, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Versuchsanstalt für Wasserbau, Hydrologie und Glaziologie (VAW), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Biologie et écologie tropicale et méditerranéenne (BETM), Université de Perpignan Via Domitia (UPVD)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Nanotechnologies Nanosystèmes (LN2), Université de Sherbrooke [Sherbrooke]-École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-École supérieure de Chimie Physique Electronique de Lyon (CPE)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), and Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Following the success of the Plateau de Bure high-z Blue Sequence Survey (PHIBSS), we present the PHIBSS2 legacy program, a survey of the molecular gas properties of star-forming galaxies on and around the star-formation main sequence (MS) at different redshifts using IRAM's NOrthern Extended Millimeter Array (NOEMA). This survey significantly extends the existing sample of star-forming galaxies with CO molecular gas measurements, probing the peak epoch of star formation (z = 1 − 1.6) as well as its building-up (z = 2 − 3) and winding-down (z = 0.5 − 0.8) phases. The targets are drawn from the well-studied GOODS, COSMOS, and AEGIS cosmological deep fields and uniformly sample the MS in the stellar mass (M)-star formation rate (SFR) plane with log(M /M) = 10 − 11.8 and SFR = 3.5 − 500 M yr −1 without morphological selection, thus providing a statistically meaningful census of star-forming galaxies at different epochs. We describe the survey strategy and sample selection before focusing on the results obtained at redshift z = 0.5 − 0.8, where we report 60 CO(2-1) detections out of 61 targets. We determine molecular gas masses between 2 × 10 9 and 5 × 10 10 M and separately obtain disc sizes and bulge-to-total (B/T) luminosity ratios from HST I-band images. The median molecular gas-to-stellar mass ratio µ gas = 0.28 ± 0.04, gas fraction f gas = 0.22 ± 0.02, and depletion time t depl = 0.84 ± 0.07 Gyr as well as their dependence with stellar mass and offset from the MS follow published scaling relations for a much larger sample of galaxies spanning a significantly wider range of redshifts, the cosmic evolution of the SFR being mainly driven by that of the molecular gas fraction. The galaxy-averaged molecular Kennicutt-Schmidt (KS) relation between molecular gas and SFR surface densities is strikingly linear, pointing towards similar star formation timescales within galaxies at any given epoch. In terms of morphology, the molecular gas content, the SFR, the disc stellar mass, and the disc molecular gas fraction do not seem to correlate with B/T and the stellar surface density, which suggests an ongoing supply of fresh molecular gas to compensate for the build-up of the bulge. Our measurements do not yield any significant variation of the depletion time with B/T and hence no strong evidence for morphological quenching within the scatter of the MS.

Published
2019

2. A catalogue of structural and morphological measurements for DES Y1

Author

Tarsitano, F., Hartley, W.G., Amara, A., Bluck, A., Bruderer, C., Carollo, M., Conselice, C, Melchior, P., Moraes, B., Refregier, A., Sevilla-Noarbe, I., Woo, J., Abbott, T.M.C., Allam, S., Annis, J., Avila, S., Banerji, M., Bertin, E., Brooks, D., Burke, D.L., Carretero, J., Cunha, C.E., Davis, C., Desai, S., Doel, P., Estrada, J., Frieman, J., Gruen, D., Gruendl, R.A., Gutierrez, G., Hollowood, D., Honscheid, K., James, D.J., Jeltema, T., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M.A.G., Menanteau, F., Miquel, R., Plazas, A.A., Romer, A.K., Roodman, A., Sanchez, E., Santiago, B., Schindler, R., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Vikram, V., and Walker, A.R.

Subjects
Galaxy structure, Astronomy and astrophysics, Galaxy evolution, Space and planetary science, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Astrophysics::Galaxy Astrophysics
Abstract

We present a structural and morphological catalogue for 45 million objects selected from the first year data of the Dark Energy Survey (DES). Single Sersic fits and non-parametric measurements are produced for g, r, and i filters. The parameters from the best-fitting Sersic model (total magnitude, half-light radius, S´ersic index, axis ratio, and position angle) are measured with GALFIT; the non-parametric coefficients (concentration, asymmetry, clumpiness, Gini, M20) are provided using the Zurich Estimator of Structural Types (ZEST+). To study the statistical uncertainties, we consider a sample of state-of-the-art image simulations with a realistic distribution in the input parameter space and then process and analyse them as we do with real data: this enables us to quantify the observational biases due to PSF blurring and magnitude effects and correct themeasurements as a function ofmagnitude, galaxy size, Sersic index (concentration for the analysis of the non-parametric measurements) and ellipticity. We present the largest structural catalogue to date: we find that accurate and complete measurements for all the structural parameters are typically obtained for galaxies with SEXTRACTOR MAG AUTO I ≤ 21. Indeed, the parameters in the filters i and r can be overall well recovered up to MAG AUTO ≤ 21.5, corresponding to a fitting completeness of ∼90 per cent below this threshold, for a total of 25million galaxies. The combination of parametric and non-parametric structural measurements makes this catalogue an important instrument to explore and understand how galaxies form and evolve. The catalogue described in this paper will be publicly released alongside the DES collaboration Y1 cosmology data products at the following URL:https://des.ncsa.illinois.edu/releases.

Published
2018

3. The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution:The Absence of Large Clumps in the Interstellar Medium at High-redshift

Author

Novak, Mladen, Sargent, Mark, Herrera-Camus, R., Belli, S., Übler, H., Shimizu, T., Davies, R., Sturm, E., Colina, L., Cunha, E. da, Rybak, M., Venemans, B., Brandt, W., Rivera, G. Calistro, Knudsen, K., Werf, P. van der, Freundlich, J., Combes, F., Tacconi, L., Genzel, R., Garcia-Burillo, S., Bolatto, A., Lilly, S., Salomé, P., Bicalho, I., Boissier, J., Boone, F., Bouché, N., Bournaud, F., Burkert, A., Carollo, M., Cooper, M., Feruglio, C., Förster Schreiber, N., Juneau, S., Lippa, M., Lutz, D., Naab, T., Renzini, A., Saintonge, A., Sternberg, A., Weiner, B., Weiß, A., Wuyts, S., Bouwens, Rychard, Brinchmann, Jarle, Maseda, Michael, Matthee, Jorryt, Schaye, Joop, Schouws, Sander, Pavesi, Riccardo, Le Fèvre, Olivier, Yang, C., Gavazzi, R., Beelen, A., Lehnert, M., Gao, Y., Barcos-Muñoz, L., Neri, R., Fu, H., González-Alfonso, E., Michałowski, M., Nightingale, J., Pérez-Fournon, I., Shao, Yali, Wang, Ran, Li, Jianan, Fan, Xiaohui, Jiang, Linhua, Strauss, Michael, Menten, Karl, Ma, Jingzhe, Cooray, Asantha, Nayyeri, Hooshang, Brown, Arianna, Ghotbi, Noah, Oteo, Ivan, Duivenvoorden, Steven, Greenslade, Joshua, Clements, David, Battisti, Andrew, Ashby, Matthew, Perez-Fournon, Ismael, Oliver, Seb, Eales, Stephen, Negrello, Mattia, Dye, Simon, Dunne, Loretta, Omont, Alain, Serjeant, Stephen, Maddox, Steve, Valiante, Elisabetta, Pillepich, Annalisa, Nelson, Dylan, Cunha, Elisabete da, Diemer, Benedikt, González-López, Jorge, Hernquist, Lars, Marinacci, Federico, Rix, Hans-Walter, Swinbank, Mark, Vogelsberger, Mark, Werf, Paul van der, Yung, L., Aravena, Manuel, Decarli, Roberto, Gónzalez-López, Jorge, Boogaard, Leindert, Carilli, Chris, Popping, Gergö, Assef, Roberto, Bacon, Roland, Bauer, Franz Erik, Bouwens, Richard, Contini, Thierry, Cortes, Paulo, Da Cunha, Elisabete, Daddi, Emanuele, Díaz-Santos, Tanio, Elbaz, David, Inami, Hanae, Fevre, Olivier Le, Magnelli, Benjamin, Oesch, Pascal, Riechers, Dominik, Somerville, Rachel, Uzgil, Bade, Wagg, Jeff, Wisotzki, Lutz, Gullberg, B., Swinbank, A. Mark, Smail, Ian, Biggs, A., Bertoldi, Frank, Breuck, C. De, Chapman, S., Chen, Chian-Chou, Cooke, E., Coppin, K., Cox, Pierre, Dannerbauer, H., Dunlop, J., Edge, A., Farrah, D., Geach, J., GREVE, T., Hodge, Jacqueline, Ibar, E., Ivison, Rob, Karim, A., Schinnerer, E., Scott, Douglas, Simpson, J., Stach, S., Thomson, A., Van Der Werf, Paul, Walter, Fabian, Wardlow, Julie, Weiss, Axel, 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), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Department of Physics, Durham University, Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional [Madrid] (OAN), Instituto Geografico Nacional (IGN), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, AUTRES, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Interactions Hôtes-Pathogènes-Environnements (IHPE), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Perpignan Via Domitia (UPVD), Institut Interdisciplinaire d'Innovation Technologique (3IT), Université de Sherbrooke [Sherbrooke], Universitätssternwarte der Ludwig-Maximiliansuniversität, Ludwig-Maximiliansuniversität, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of São Paulo, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Steward observatory, University of Arizona, Max-Planck-Institut für Extraterrestrische Physik (MPE), Institut of Physics - Riga, Latvian Academy of Sciences, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], 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), Guangzhou Marine Geological Survey, Ministry of Land and Resources (MLR), Physics Department [Santa Barbara], University of California [Santa Barbara] (UCSB), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Universidad de Alcalá - University of Alcalá (UAH), Instituto de Astrofisica de Canarias (IAC), Institute of Plant and Environment Protection, Beijing Academy of Agriculture and Forestry Sciences, Arizona State University [Tempe] (ASU), Max-Planck-Institut für Radioastronomie (MPIFR), California Institute of Technology (CALTECH), Astronomy Centre, University of Sussex, University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires de Marseille (ISM2), Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Max-Planck-Institut für Astronomie (MPIA), Institute for Computational Cosmology (ICC), National Radio Astronomy Observatory [Socorro] (NRAO), National Radio Astronomy Observatory (NRAO), 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), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), 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, Yale Center for Astronomy and Astrophysics (YCAA), Yale University [New Haven], Cornell University, Rutgers University, Astrophysikalisches Institut Potsdam (AIP), Institute of Computational Cosmology, Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Université de Lyon, SUPA, Institute for Astronomy, University of Edinburgh, University of Wales, Department of Physics [Blacksburg], Virginia Tech [Blacksburg], Space Plasma Group, Astronomy Unit [London] (AU), Queen Mary University of London (QMUL)-Queen Mary University of London (QMUL), Royal Observatory Edinburgh (ROE), Interactions et dynamique des environnements de surface (IDES), CLRC Daresbury, SFTC, Centre de Recherches sur la Cognition Animale (CRCA), Institut des sciences du cerveau de Toulouse. (ISCT), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Pacific Northwest National Laboratory (PNNL), Department of Astronomy, University of California [Irvine] (UCI), Centre de Biologie Intégrative (CBI), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut des sciences du cerveau de Toulouse. (ISCT), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse - Jean Jaurès (UT2J)-CHU Toulouse [Toulouse]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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), Université de Perpignan Via Domitia (UPVD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, evolution [galaxies], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], 010308 nuclear & particles physics, Resolution (electron density), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Interstellar medium, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Millimeter, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present deep high resolution (0.03", 200pc) ALMA Band 7 observations covering the dust continuum and [CII] $\lambda157.7\mu$m emission in four $z\sim4.4-4.8$ sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160$\mu$m (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS47.0, displays apparent substructure but this is also consistent with a smooth morphology, as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at high angular resolution (0.03") and depth of these observations ($\sigma_{345\text{GHz}} \sim27-47\mu$Jy beam$^{-1}$). The four SMGs are bright [CII] emitters, and we extract [CII] spectra from the high resolution data, and recover $\sim20-100$% of the [CII] flux and $\sim40-80$% of the dust continuum emission, compared to the previous lower resolution observations. When tapered to 0.2" resolution our maps recover $\sim80-100$% of the continuum emission, indicating that $\sim60$% of the emission is resolved out on $\sim200$pc scales. We find that the [CII] emission in high-redshift galaxies is more spatially extended than the rest-frame 160$\mu$m dust continuum by a factor of $1.6\pm0.4$. By considering the $L_{\text{[CII]}}$/$L_{\text{FIR}}$ ratio as a function of the star-formation rate surface density ($\Sigma_{\text{SFR}}$) we revisit the [CII] deficit, and suggest that the decline in the $L_{\text{[CII]}}$/$L_{\text{FIR}}$ ratio as a function of $\Sigma_{\text{SFR}}$ is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs., Comment: 15 pages, 6 figures, 4 tables, accepted for publication in ApJ

Published
2018

4. The Dark Energy Survey: more than dark energy – an overview

Author

Abbott, T, Abdalla, FB, Aleksić, J, Allam, S, Amara, A, Bacon, D, Balbinot, E, Banerji, M, Bechtol, K, Benoit-Lévy, A, Bernstein, GM, Bertin, E, Blazek, J, Bonnett, C, Bridle, S, Brooks, D, Brunner, RJ, Buckley-Geer, E, Burke, DL, Caminha, GB, Capozzi, D, Carlsen, J, Carnero-Rosell, A, Carollo, M, Carrasco-Kind, M, Carretero, J, Castander, FJ, Clerkin, L, Collett, T, Conselice, C, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Davis, TM, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Estrada, J, Etherington, J, Evrard, AE, Fabbri, J, Finley, DA, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Goldstein, DA, Gruen, D, Gruendl, RA, Guarnieri, P, Gutierrez, G, Hartley, W, Honscheid, K, Jain, B, James, DJ, Jeltema, T, Jouvel, S, Kessler, R, King, A, Kirk, D, Kron, R, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Makler, M, Manera, M, Maraston, C, Marshall, JL, Martini, P, McMahon, RG, Melchior, P, Merson, A, Miller, CJ, Miquel, R, Mohr, JJ, Morice-Atkinson, X, Naidoo, K, Neilsen, E, Nichol, RC, Nord, B, Ogando, R, Ostrovski, F, Palmese, A, Papadopoulos, A, Peiris, HV, Peoples, J, Percival, WJ, and Plazas, AA

Subjects
surveys, general [quasars], astro-ph.GA, minor planets, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, general [supernovae], Astrophysics::Galaxy Astrophysics, general [Galaxy], Astronomical and Space Sciences, general [asteroids], general [galaxies]
Abstract

This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and other transients. The main goals of DES are to characterize dark energy and dark matter, and to test alternative models of gravity; these goals will be pursued by studying large-scale structure, cluster counts, weak gravitational lensing and Type Ia supernovae. However, DES also provides a rich data set which allows us to study many other aspects of astrophysics. In this paper, we focus on additional science with DES, emphasizing areas where the survey makes a difference with respect to other current surveys. The paper illustrates, using early data (from 'Science Verification', and from the first, second and third seasons of observations), what DES can tell us about the Solar system, the Milky Way, galaxy evolution, quasars and other topics. In addition, we show that if the cosmological model is assumed to be Λ+cold dark matter, then important astrophysics can be deduced from the primary DES probes. Highlights from DES early data include the discovery of 34 trans-Neptunian objects, 17 dwarf satellites of the Milky Way, one published z > 6 quasar (and more confirmed) and two published superluminous supernovae (and more confirmed).

Published
2016

5. The Dark Energy Survey: More than dark energy - an overview

Author

Abbott, T, Abdalla, FB, Aleksić, J, Allam, S, Amara, A, Bacon, D, Balbinot, E, Banerji, M, Bechtol, K, Benoit-Lévy, A, Bernstein, GM, Bertin, E, Blazek, J, Bonnett, C, Bridle, S, Brooks, D, Brunner, RJ, Buckley-Geer, E, Burke, DL, Caminha, GB, Capozzi, D, Carlsen, J, Carnero-Rosell, A, Carollo, M, Carrasco-Kind, M, Carretero, J, Castander, FJ, Clerkin, L, Collett, T, Conselice, C, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Davis, TM, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Estrada, J, Etherington, J, Evrard, AE, Fabbri, J, Finley, DA, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Goldstein, DA, Gruen, D, Gruendl, RA, Guarnieri, P, Gutierrez, G, Hartley, W, Honscheid, K, Jain, B, James, DJ, Jeltema, T, Jouvel, S, Kessler, R, King, A, Kirk, D, Kron, R, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, and Lima, M

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and other transients. The main goals of DES are to characterize dark energy and dark matter, and to test alternative models of gravity; these goals will be pursued by studying large-scale structure, cluster counts, weak gravitational lensing and Type Ia supernovae. However, DES also provides a rich data set which allows us to study many other aspects of astrophysics. In this paper, we focus on additional science with DES, emphasizing areas where the survey makes a difference with respect to other current surveys. The paper illustrates, using early data (from 'Science Verification', and from the first, second and third seasons of observations), what DES can tell us about the Solar system, the Milky Way, galaxy evolution, quasars and other topics. In addition, we show that if the cosmological model is assumed to be Λ+cold dark matter, then important astrophysics can be deduced from the primary DES probes. Highlights from DES early data include the discovery of 34 trans-Neptunian objects, 17 dwarf satellites of the Milky Way, one published z > 6 quasar (and more confirmed) and two published superluminous supernovae (and more confirmed).

Published
2016

6. A giant Ly$��$ nebula in the core of an X-ray cluster at $z=1.99$: implications for early energy injection

Author

Valentino, F., Daddi, E., Finoguenov, A., Strazzullo, V., Brun, A. M. C. Le, Vignali, C., Bournaud, F., Dickinson, M., Renzini, A., B��thermin, M., Zanella, A., Gobat, R., Cimatti, A., Elbaz, D., Onodera, M., Pannella, M., Sargent, M. T., Arimoto, N., Carollo, M., and Starck, J-L.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present the discovery of a giant $\gtrsim$100~kpc Ly$��$ nebula detected in the core of the X-ray emitting cluster CL~J1449+0856 at $z=1.99$ through Keck/LRIS narrow-band imaging. This detection extends the known relation between Ly$��$ nebulae and overdense regions of the Universe to the dense core of a $5-7\times10^{13}$ M$_{\odot}$ cluster. The most plausible candidates to power the nebula are two Chandra-detected AGN host cluster members, while cooling from the X-ray phase and cosmological cold flows are disfavored primarily because of the high Ly$��$ to X-ray luminosity ratio ($L_{\mathrm{Ly��}}/L_{\mathrm{X}} \approx0.3$, $\gtrsim10-1000\times$ higher than in local cool-core clusters) and by current modeling. Given the physical conditions of the Ly$��$-emitting gas and the possible interplay with the X-ray phase, we argue that the Ly$��$ nebula would be short-lived ($\lesssim10$ Myr) if not continuously replenished with cold gas at a rate of $\gtrsim1000$ M$_{\odot}$ yr$^{-1}$. We investigate the possibility that cluster galaxies supply the required gas through outflows and we show that their total mass outflow rate matches the replenishment necessary to sustain the nebula. This scenario directly implies the extraction of energy from galaxies and its deposition in the surrounding intracluster medium, as required to explain the thermodynamic properties of local clusters. We estimate an energy injection of the order of $\thickapprox2$ keV per particle in the intracluster medium over a $2$ Gyr interval. In our baseline calculation AGN provide up to $85$% of the injected energy and 2/3 of the mass, while the rest is supplied by supernovae-driven winds., 15 pages, 11 figures, 1 appendix. Accepted for publication in ApJ

Published
2016
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7. DEEP NEAR-INFRARED SPECTROSCOPY OF PASSIVELY EVOLVING GALAXIES AT z greater than or similar to 1.4

Author

Onodera, M, Renzini, A, Carollo, M, Cappellari, M, Mancini, C, Strazzullo, V, Daddi, E, Arimoto, N, Gobat, R, Yamada, Y, McCracken, HJ, Ilbert, O, Capak, P, Cimatti, A, Giavalisco, M, Koekemoer, AM, Kong, X, Lilly, S, Motohara, K, Ohta, K, Sanders, DB, Scoville, N, Tamura, N, Taniguchi, Y, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], 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), National Astronomical Observatory of Japan (NAOJ), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Spitzer Science Center, California Institute of Technology (CALTECH), Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Space Telescope Science Institute (STSci), AUTRES, Institute of Astronomy, The University of Tokyo, Division of Respiratory Medicine and Allergology, Teikyo University School of Medicine, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford-University of Oxford, 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), 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), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), The University of Tokyo (UTokyo), Onodera, M, Renzini, A, Carollo, M, Cappellari, M, Mancini, C, Strazzullo, V, Daddi, E, Arimoto, N, Gobat, R, Yamada, Y, Mccracken, Hj, Ilbert, O, Capak, P, Cimatti, A, Giavalisco, M, Koekemoer, Am, Kong, X, Lilly, S, Motohara, K, Ohta, K, Sanders, Db, Scoville, N, Tamura, N, Taniguchi, Y, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; We present the results of new near-IR spectroscopic observations of passive galaxies at z greater than or similar to 1.4 in a concentration of BzK-selected galaxies in the COSMOS field. The observations have been conducted with Subaru/MOIRCS, and have resulted in absorption lines and/or continuum detection for 18 out of 34 objects. This allows us to measure spectroscopic redshifts for a sample that is almost complete to K-AB = 21. COSMOS photometric redshifts are found in fair agreement overall with the spectroscopic redshifts, with a standard deviation of similar to 0.05; however, similar to 30% of objects have photometric redshifts systematically underestimated by up to similar to 25%. We show that these systematic offsets in photometric redshifts can be removed by using these objects as a training set. All galaxies fall in four distinct redshift spikes at z = 1.43, 1.53, 1.67, and 1.82, with this latter one including seven galaxies. SED fits to broadband fluxes indicate stellar masses in the range of similar to 4-40 x 10(10) M-circle dot and that star formation was quenched similar to 1 Gyr before the cosmoic epoch at which they are observed. the spectra of several individual galaxies have allowed us to measure their H delta(F) indices and the strengths of the 4000 angstrom break, which confirms their identification as passive galaxies, as does a composite spectrum resulting from the co-addition of 17 individual spectra. The effective radii of the galaxies have been measured on the COSMOS HST/ACS i(F814W)-band image, confirming the coexistence at these redshifts of passive galaxies, which are substantially more compact than their local counterparts with others that follow the local effective radius-stellar mass relation. For the galaxy with the best signal-to-noise spectrum we were able to measure a velocity dispersion of 270 +/- 105 km s(-1) (error bar including systematic errors), indicating that this galaxy lies closely on the virial relation given its stellar mass and effective radius.

Published
2012

8. Tracing the cosmic growth of supermassive black holes to z similar to 3 with Herschel*

Author

Delvecchio, I., Gruppioni, C., Pozzi, F., Berta, S., Zamorani, G., Cimatti, Alessandro, Lutz, D., Scott, D., Vignali, C., Cresci, G., Feltre, A., Cooray, A., Vaccari, M., Fritz, J., Le Floc'H, E., Magnelli, B., Popesso, P., Oliver, S., Bock, J., Carollo, M., Contini, T., Le Fevre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and 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)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Galaxies: evolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Infrared: galaxies, Astrophysics::Galaxy Astrophysics, Galaxies: nuclei
Abstract

International audience; We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L1-1000 \textgreater 10(11) L-circle dot) star-forming galaxies at z \textgreater 0.3, becoming about 80 per cent for the brightest (L1-1000 \textgreater 10(12) L-circle dot) infrared (IR) galaxies at z \textgreater= 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z similar to 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z ~ 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency epsilon(rad) (~ 0.07).

Published
2014

9. Deep near-infrared spectroscopy of passively evolving galaxies at z>1.4

Author

Onodera, M., Renzini, A., Carollo, M., Cappellari, M., Mancini, C., Strazzullo, V., Daddi, E., Arimoto, N., Gobat, R., Yamada, Y., McCracken, H. J., Ilbert, O., Capak, P., Cimatti, A., Giavalisco, M., Koekemoer, A. M., Kong, X., Lilly, S., Motohara, K., Ohta, K., Sanders, D. B., Scoville, N., Tamura, N., and Taniguchi, Y.

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

[Abridged] We present the results of new near-IR spectroscopic observations of passive galaxies at z>1.4 in a concentration of BzK-selected galaxies in the COSMOS field. The observations have been conducted with Subaru/MOIRCS, and have resulted in absorption lines and/or continuum detection for 18 out of 34 objects. This allows us to measure spectroscopic redshifts for a sample almost complete to K(AB)=21. COSMOS photometric redshifts are found in fair agreement overall with the spectroscopic redshifts, with a standard deviation of ~0.05; however, ~30% of objects have photometric redshifts systematically underestimated by up to ~25%. We show that these systematic offsets in photometric redshifts can be removed by using these objects as a training set. All galaxies fall in four distinct redshift spikes at z=1.43, 1.53, 1.67 and 1.82, with this latter one including 7 galaxies. SED fits to broad-band fluxes indicate stellar masses in the range of ~4-40x10^10Msun and that star formation was quenched ~1 Gyr before the cosmic epoch at which they are observed. The spectra of several individual galaxies have allowed us to measure their Hdelta_F and Dn4000 indices, which confirms their identification as passive galaxies, as does a composite spectrum resulting from the coaddition of 17 individual spectra. The effective radii of the galaxies have been measured on the HST/ACS F814W image, confirming the coexistence at these redshifts of passive galaxies which are substantially more compact than their local counterparts with others that follow the local size-stellar mass relation. For the galaxy with best S/N spectrum we were able to measure a velocity dispersion of 270+/-105 km/s, indicating that this galaxy lies closely on the virial relation given its stellar mass and effective radius., 26 pages, 24 figures, 5 tables, in emulateapj format; accepted for publication in The Astrophysical Journal

Published
2012
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10. Nuclear properties of a sample of nearby spirals from STIS imaging

Author

Scarlata, C, Stiavelli, M, Hughes, M, Axon, D, Alonso-Herrero, A, Atkinson, J, Batcheldor, D, Binney, J, Capetti, A, Carollo, M, Dressel, L, Gerssen, J, Macchetto, D, Maciejewski, W, Marconi, A, Merrifield, M, Ruiz, M, Sparks, W, Tsvetanov, Z, and Marel, RVD

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

We present surface photometry for the central regions of a sample of 48 spiral galaxies (mostly unbarred and barred of types Sbc or Sc) observed with the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope. Surface brightness profiles were derived and modeled with a Nuker law. We also analyzed archival Wide Field Planetary Camera~2 images with a larger field of view, available for 18 galaxies in our sample. We modeled the extracted bulge surface brightness profiles with an exponential, a de Vaucouleurs or a Sersic profile. In agreement with previous studies, we find that bulges of Sbc galaxies fall into two categories: bulges well described by an exponential profile and those well described by an de Vaucouleurs profile. Only one galaxy requires the use of a more general Sersic profile to properly describe the bulge. Nuclear photometrically distinct components are found in ~55% of the galaxies. For those that we classify as star clusters based on their resolved extent we find absolute magnitudes that are brighter on average than those previously identified in spiral galaxies. This might be due to a bias in our sample toward star forming galaxies, combined with a trend for star forming galaxies to host brighter central clusters., 33 pages, 7 figures. Accepted for publication on the Astronomical Journal

Published
2004

11. Merger-driven star formation activity in Cl J1449+0856 at z = 1.99 as seen by ALMA and JVLA

Author

Masato Onodera, R. T. Coogan, M. Carollo, Alvio Renzini, Helmut Dannerbauer, Evangelia Tremou, Maurilio Pannella, Mark Sargent, Georgios E. Magdis, V. Strazzullo, Andrea Cimatti, R. Gobat, Matthieu Béthermin, Emanuele Daddi, Francesco Valentino, Daizhong Liu, 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), Ludwig-Maximilians-Universität München (LMU), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Max-Planck-Institut für Extraterrestrische Physik (MPE), T Coogan, R, Daddi, E, T Sargent, M, Strazzullo, V, Valentino, F, Gobat, R, Magdis, G, Bethermin, M, Pannella, M, Onodera, M, Liu, D, Cimatti, A, Dannerbauer, H, Carollo, M, Renzini, A, Tremou, E, Coogan, R. T., Daddi, E., Sargent, M. T., Strazzullo, V., Valentino, F., Gobat, R., Magdis, G., Bethermin, M., Pannella, M., Onodera, M., Liu, D., Cimatti, A., Dannerbauer, H., Carollo, M., Renzini, A., Tremou, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)

Subjects
Active galactic nucleus, galaxies: clusters: individual: Cl J1449+0856, galaxies: evolution, galaxies: high-redshift, galaxies: ISM, galaxies: star formation, Astrophysics - Astrophysics of Galaxies, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, Jansky, 0103 physical sciences, Galaxies:high-redshift, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, QB, Physics, ISM [galaxies], 010308 nuclear & particles physics, Star formation, Gas depletion, Astronomy and Astrophysics, Astronomy and Astrophysic, Galaxy, Interstellar medium, Galaxies evolution, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, Excited state, Astrophysics of Galaxies (astro-ph.GA), clusters: individual: Cl J1449+0856 [galaxies], Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], high-redshift [galaxies]
Abstract

We use ALMA and JVLA observations of the galaxy cluster Cl J1449+0856 at z=1.99, in order to study how dust-obscured star-formation, ISM content and AGN activity are linked to environment and galaxy interactions during the crucial phase of high-z cluster assembly. We present detections of multiple transitions of $^{12}$CO, as well as dust continuum emission detections from 11 galaxies in the core of Cl J1449+0856. We measure the gas excitation properties, star-formation rates, gas consumption timescales and gas-to-stellar mass ratios for the galaxies. We find evidence for a large fraction of galaxies with highly-excited molecular gas, contributing $>$50% to the total SFR in the cluster core. We compare these results with expectations for field galaxies, and conclude that environmental influences have strongly enhanced the fraction of excited galaxies in this cluster. We find a dearth of molecular gas in the galaxies' gas reservoirs, implying a high star-formation efficiency (SFE) in the cluster core, and find short gas depletion timescales $��$, 29 pages, 15 figures, 7 tables + Appendix. Accepted for publication in MNRAS

Published
2018

12. Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

Author

David Carton, Leindert Boogaard, Marcella Carollo, Sebastiano Cantalupo, Genevieve Soucail, Stephen Hamer, Peter M. Weilbacher, Thierry Contini, Léo Michel-Dansac, Hayley Finley, R. A. Marino, Johan Richard, Davor Krajnović, Roland Bacon, Benoît Epinat, Adrien Guérou, Wolfram Kollatschny, Jarle Brinchmann, Lutz Wisotzki, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Leiden Observatory [Leiden], Universiteit Leiden, Institut de recherche en astrophysique et planétologie (IRAP), European Southern Observatory (ESO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut für Astrophysik [Göttingen], Georg-August-University = Georg-August-Universität Göttingen, Leibniz-Institut für Astrophysik Potsdam (AIP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden [Leiden], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Georg-August-University [Göttingen], Epinat, B, Contini, T, Finley, H, Boogaard, L, Guerou, A, Brinchmann, J, Carton, D, Michel-Dansac, L, Bacon, R, Cantalupo, S, Carollo, M, Hamer, S, Kollatschny, W, Krajnovic, D, Marino, R, Richard, J, Soucail, G, Weilbacher, P, and Wisotzki, L

Subjects
Active galactic nucleus, Absorption spectroscopy, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Galaxies: kinematics and dynamic, galaxies: groups: general, galaxies: high-redshift, Ionization, Galaxy group, 0103 physical sciences, Tidal force, galaxies: interactions, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Line (formation), Physics, evolution, intergalactic medium, galaxies: high-redshift [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxies: interaction, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution
Abstract

We report the discovery of a 10^4 kpc^2 gaseous structure detected in [OII] in an over-dense region of the COSMOS-Gr30 galaxy group at z~0.725 thanks to deep MUSE Guaranteed Time Observations. We estimate the total amount of diffuse ionised gas to be of the order of (~5+-3)x10^10 Msun and explore its physical properties to understand its origin and the source(s) of the ionisation. The MUSE data allow the identification of a dozen of group members embedded in this structure from emission and absorption lines. We extracted spectra from small apertures defined for both the diffuse ionised gas and the galaxies. We investigated the kinematics and ionisation properties of the various galaxies and extended gas regions thanks to line diagnostics (R23, O32 and [OIII]/H\beta) available within the MUSE wavelength range. We compared these diagnostics to photo-ionisation models and shock models. The structure is divided in two kinematically distinct sub-structures. The most extended sub-structure of ionised gas is likely rotating around a massive galaxy and displays filamentary patterns linking some galaxies. The second sub-structure links another massive galaxy hosting an Active Galactic Nucleus to a low mass galaxy but also extends orthogonally to the AGN host disk over ~35 kpc. This extent is likely ionised by the AGN itself. The location of small diffuse regions in the R23 vs. O32 diagram is compatible with photo-ionisation. However, the location of three of these regions in this diagram (low O32, high R23) can also be explained by shocks, which is supported by their large velocity dispersions. One edge-on galaxy shares the same properties and may be a source of shocks. Whatever the hypothesis, the extended gas seems to be non primordial. We favour a scenario where the gas has been extracted from galaxies by tidal forces and AGN triggered by interactions between at least the two sub-structures., Comment: 21 pages, 12 figures, 3 tables, accepted for publication in A&A (27 October 2017)

Published
2018

13. The MUSE Hubble Ultra Deep Field Survey

Author

Jeremy Blaizot, Mohammad Akhlaghi, Peter D. Mitchell, Hanae Inami, Simon Conseil, Roland Bacon, Sebastiano Cantalupo, Marcella Carollo, Floriane Leclercq, Johan Richard, Anne Verhamme, Joop Schaye, Jarle Brinchmann, Raffaella Anna Marino, Michael V. Maseda, Thierry Contini, Edmund Christian Herenz, Lutz Wisotzki, Takuya Hashimoto, Thibault Garel, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Chimie de Strasbourg, Université de Strasbourg (UNISTRA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Leclercq, F, Bacon, R, Wisotzki, L, Mitchell, P, Garel, T, Verhamme, A, Blaizot, J, Hashimoto, T, Herenz, E, Conseil, S, Cantalupo, S, Inami, H, Contini, T, Richard, J, Maseda, M, Schaye, J, Marino, R, Akhlaghi, M, Brinchmann, J, Carollo, M, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)

Subjects
Physics, 010308 nuclear & particles physics, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Hubble Ultra-Deep Field, 01 natural sciences, Cosmology: observation, Galaxy, Redshift, Accretion (astrophysics), Dark matter halo, 13. Climate action, Space and Planetary Science, galaxies: high-redshift, cosmology: observations, 0103 physical sciences, Satellite galaxy, galaxies: formation, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the detection of extended Lyα haloes around 145 individual star-forming galaxies at redshifts 3 ≤ z ≤ 6 in the Hubble Ultra Deep Field observed with the Multi-Unit Spectroscopic Explorer (MUSE) at ESO-VLT. Our sample consists of continuum-faint (− 15 ≥ MUV ≥ −22) Lyα emitters (LAEs). Using a 2D, two-component (continuum-like and halo) decomposition of Lyα emission assuming circular exponential distributions, we measure scale lengths and luminosities of Lyα haloes. We find that 80% of our objects having reliable Lyα halo measurements show Lyα emission that is significantly more extended than the UV continuum detected by HST (by a factor ≈4 to >20). The median exponential scale length of the Lyα haloes in our sample is ≈4.5 kpc with a few haloes exceeding 10 kpc. By comparing the maximal detected extent of the Lyα emission with the predicted dark matter halo virial radii of simulated galaxies, we show that the detected Lyα emission of our selected sample of Lyα emitters probes a significant portion of the cold circum-galactic medium of these galaxies (>50% in average). This result therefore shows that there must be significant HI reservoirs in the circum-galactic medium and reinforces the idea that Lyα haloes are ubiquitous around high-redshift Lyα emitting galaxies. Our characterization of the Lyα haloes indicates that the majority of the Lyα flux comes from the halo (≈65%) and that their scale lengths seem to be linked to the UV properties of the galaxies (sizes and magnitudes). We do not observe a significant Lyα halo size evolution with redshift, although our sample for z> 5 is very small. We also explore the diversity of the Lyα line profiles in our sample and we find that the Lyα lines cover a large range of full width at half maximum (FWHM) from 118 to 512 km s-1. While the FWHM does not seem to be correlated to the Lyα scale length, most compact Lyα haloes and those that are not detected with high significance tend to have narrower Lyα profiles (-1). Finally, we investigate the origin of the extended Lyα emission but we conclude that our data do not allow us to disentangle the possible processes, i.e. scattering from star-forming regions, fluorescence, cooling radiation from cold gas accretion, and emission from satellite galaxies.

Published
2017

14. The MUSE-Wide survey: A measurement of the Ly$\alpha$ emitting fraction among $z>3$ galaxies

Author

Johan Richard, Thibault Garel, Marcella Carollo, C. Diener, Joseph Caruana, Jarle Brinchmann, J. Kerutt, Kasper B. Schmidt, Tanya Urrutia, Alyssa B. Drake, A. Verhamme, Joop Schaye, Lutz Wisotzki, Edmund Christian Herenz, Sebastiano Cantalupo, R. Saust, R. A. Marino, Rychard Bouwens, Caruana, J, Wisotzki, L, Herenz, E, Kerutt, J, Urrutia, T, Schmidt, K, Bouwens, R, Brinchmann, J, Cantalupo, S, Carollo, M, Diener, C, Drake, A, Garel, T, Marino, R, Richard, J, Saust, R, Schaye, J, Verhamme, A, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: star formation, Galaxies: statistic, 010308 nuclear & particles physics, Galaxies: high-redshift, Astronomy and Astrophysics, Fraction (chemistry), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics
Abstract

We present a measurement of the fraction of Lyman $\alpha$ (Ly$\alpha$) emitters ($X_{\rm{Ly} \alpha}$) amongst HST continuum-selected galaxies at $3, Comment: 10 pages, 5 figures (MNRAS, updated as per version in press)

Published
2017

15. Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel★

Author

Giovanni Cresci, G. Zamorani, Marco Scodeggio, Alessandro Cimatti, A. Feltre, P. Popesso, Ivan Delvecchio, Alvio Renzini, M. Carollo, Benjamin Magnelli, Carlotta Gruppioni, Mattia Vaccari, Douglas Scott, E. Le Floc'h, O. Le Fevre, Francesca Pozzi, Simon J. Lilly, S. Berta, Jacopo Fritz, Asantha Cooray, Dieter Lutz, J. J. Bock, Cristian Vignali, Vincenzo Mainieri, Seb Oliver, Thierry Contini, Delvecchio I., Gruppioni C., Pozzi F., Berta S., Zamorani G., Cimatti A., Lutz D., Scott D., Vignali C., Cresci G., Feltre A., Coorey A., Vaccari M., Fritz J., Le Floch E., Magnelli B., Popesso P., Oliver S., Bock J., Carollo M., Contini T., Le Fevre O., Lilly S., Mainieri V., Renzini A., and Scodeggio M.

Subjects
ULTRALUMINOUS INFRARED GALAXIES, ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, RAY LUMINOSITY FUNCTION, nuclei [galaxies], FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, galaxies [infrared], 01 natural sciences, HIGH-REDSHIFT GALAXIES, infrared: galaxies, QB0460, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), XMM-NEWTON, Luminous infrared galaxy, Physics, Supermassive black hole, 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, STAR-FORMATION HISTORY, Astrophysics - Astrophysics of Galaxies, Galaxy, Black hole, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), X-RAY, DEEP-FIELD-SOUTH, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, galaxies: nuclei, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study a sample of Herschel-PACS selected galaxies within the GOODS-South and the COSMOS fields in the framework of the PACS Evolutionary Probe (PEP) project. Starting from the rich multi-wavelength photometric data-sets available in both fields, we perform a broad-band Spectral Energy Distribution (SED) decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability to reveal AGN activity increases for bright ($L_{\rm 1-1000} > 10^{11} \rm L_{\odot}$) star-forming galaxies at $z>0.3$, becoming about 80 per cent for the brightest ($L_{\rm 1-1000} > 10^{12} \rm L_{\odot}$) infrared (IR) galaxies at $z \geq 1$. Finally, we reconstruct the AGN bolometric luminosity function and the super-massive black hole growth rate across cosmic time up to $z \sim 3$ from a Far-Infrared (FIR) perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at $z \sim 2$ and reproducing the observed local black hole mass density with consistent values of the radiative efficiency $��_{\rm rad}$ ($\sim$0.07)., 20 pages, 14 figures, 1 table, accepted for publication in MNRAS

Published
2014

16. A giant Ly$\alpha$ nebula in the core of an X-ray cluster at $z=1.99$: implications for early energy injection

Author

Matthieu Béthermin, Mark Sargent, Francesco Valentino, Mark Dickinson, Alvio Renzini, Marcella Carollo, V. Strazzullo, Nobuo Arimoto, Cristian Vignali, Masato Onodera, David Elbaz, Raphael Gobat, Maurilio Pannella, Anita Zanella, Andrea Cimatti, Frédéric Bournaud, Amandine Le Brun, Alexis Finoguenov, Emanuele Daddi, Jean-Luc Starck, Valentino, Francesco, Daddi, Emanuele, Finoguenov, Alexi, Strazzullo, Veronica, Brun, Amandine Le, Vignali, Cristian, Bournaud, Frédéric, Dickinson, Mark, Renzini, Alvio, Béthermin, Matthieu, Zanella, Anita, Gobat, Raphaël, Cimatti, Andrea, Elbaz, David, Onodera, Masato, Pannella, Maurilio, Sargent, Mark, Arimoto, Nobuo, Carollo, Marcella, Starck, Jean-Luc, Valentino, F, Daddi, E, Finoguenov, A, Strazzullo, V, Le Brun, A, Vignali, C, Bournaud, F, Dickinson, M, Renzini, A, Bethermin, M, Zanella, A, Gobat, R, Cimatti, A, Elbaz, D, Onodera, M, Pannella, M, Sargent, M, Arimoto, N, Carollo, M, Starck, Jl, and Department of Physics

Subjects
ACTIVE GALACTIC NUCLEI, SIMILAR-TO 2, galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Phase (waves), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, evolution [Galaxy], Luminosity, galaxies: high-redshift, BROAD-BAND SURVEY, Intracluster medium, 0103 physical sciences, STAR-FORMING GALAXIES, Cluster (physics), SINS/ZC-SINF SURVEY, COOLING FLOW, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, Galaxy: evolution, Nebula, 010308 nuclear & particles physics, X-ray, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, MOLECULAR GAS, Galaxy, clusters: individual (CL J1449+0856) [galaxies], Core (optical fiber), DARK-MATTER HALOES, clusters: intracluster medium [galaxies], Space and Planetary Science, galaxies: star formation, galaxies: clusters: individual (CL J1449+0856), active [galaxies], Astrophysics::Earth and Planetary Astrophysics, HIGH-REDSHIFT, star formation [galaxies], SKY SURVEY, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the discovery of a giant $\gtrsim$100~kpc Ly$\alpha$ nebula detected in the core of the X-ray emitting cluster CL~J1449+0856 at $z=1.99$ through Keck/LRIS narrow-band imaging. This detection extends the known relation between Ly$\alpha$ nebulae and overdense regions of the Universe to the dense core of a $5-7\times10^{13}$ M$_{\odot}$ cluster. The most plausible candidates to power the nebula are two Chandra-detected AGN host cluster members, while cooling from the X-ray phase and cosmological cold flows are disfavored primarily because of the high Ly$\alpha$ to X-ray luminosity ratio ($L_{\mathrm{Ly\alpha}}/L_{\mathrm{X}} \approx0.3$, $\gtrsim10-1000\times$ higher than in local cool-core clusters) and by current modeling. Given the physical conditions of the Ly$\alpha$-emitting gas and the possible interplay with the X-ray phase, we argue that the Ly$\alpha$ nebula would be short-lived ($\lesssim10$ Myr) if not continuously replenished with cold gas at a rate of $\gtrsim1000$ M$_{\odot}$ yr$^{-1}$. We investigate the possibility that cluster galaxies supply the required gas through outflows and we show that their total mass outflow rate matches the replenishment necessary to sustain the nebula. This scenario directly implies the extraction of energy from galaxies and its deposition in the surrounding intracluster medium, as required to explain the thermodynamic properties of local clusters. We estimate an energy injection of the order of $\thickapprox2$ keV per particle in the intracluster medium over a $2$ Gyr interval. In our baseline calculation AGN provide up to $85$% of the injected energy and 2/3 of the mass, while the rest is supplied by supernovae-driven winds., Comment: 15 pages, 11 figures, 1 appendix. Accepted for publication in ApJ

Published
2016

17. METAL DEFICIENCY IN CLUSTER STAR-FORMING GALAXIES AT Z=2

Author

Nobuo Arimoto, Marcella Carollo, Stéphanie Juneau, Masato Onodera, Raphael Gobat, Emanuele Daddi, Frédéric Bournaud, Veronica Strazzullo, Alvio Renzini, Francesco Valentino, Anita Zanella, Valentino, F, Daddi, E, Strazzullo, V, Gobat, R, Onodera, M, Bournaud, F, Juneau, S, Renzini, A, Arimoto, N, Carollo, M, and Zanella, A

Subjects
Physics, Active galactic nucleus, 010308 nuclear & particles physics, Star formation, Metallicity, Doubly ionized oxygen, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Star cluster, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Equivalent width, Galaxy cluster, Astrophysics::Galaxy Astrophysics
Abstract

We investigate the environmental effect on the metal enrichment of star-forming galaxies (SFGs) in the farthest spectroscopically confirmed and X-ray detected cluster, CL~J1449+0856 at $z=1.99$. We combined HST/WFC3~G141 slitless spectroscopic data, our 13-band photometry, and a recent Subaru/MOIRCS near infrared spectroscopic follow-up to constrain the physical properties of SFGs in CL~J1449+0856 and in a mass-matched field sample. After a conservative active galactic nuclei (AGN) removal, stacking individual MOIRCS spectra of $6$ ($31$) sources in the cluster (field) in the mass range $10 \leq \mathrm{log(M/M_{\odot}}) \leq 11$, we find a $\sim4\sigma$ significant lower [N II]/H$\alpha$ ratio in the cluster than in the field. Stacking a subsample of $16$ field galaxies with H$\beta$ and [O III] in the observed range, we measure a [O III]/H$\beta$ ratio fully compatible with the cluster value. Converting these ratios into metallicities, we find that the cluster SFGs are up to $0.25\,\mathrm{dex}$ poorer in metals than their field counterparts, depending on adopted calibrations. The low metallicity in cluster sources is confirmed using alternative indicators. Furthermore, we observe a significantly higher H$\alpha$ luminosity and equivalent width in the average cluster spectrum than in the field. This is likely due to enhanced specific star formation rate, even if lower dust reddening and/or an uncertain environmental dependence of the continuum-to-nebular emission differential reddening may play a role. Our findings might be explained by the accretion of pristine gas around galaxies at $z=2$ and from cluster-scale reservoirs, possibly connected with a phase of rapid halo mass assembly at $z>2$ and of high galaxy merging rate., Comment: 19 pages, 19 figures, 2 appendices, accepted by ApJ

Published
2015

18. Galaxy Evolution in Overdense Environments at High Redshift: Passive Early-type Galaxies in a Cluster at z ~ 2

Author

Marcella Carollo, A. Finoguenov, A. Cimatti, Mark Dickinson, Alvio Renzini, Masato Onodera, E. Daddi, V. Strazzullo, Raphael Gobat, R.-R. Chary, Nobuo Arimoto, 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), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), National Optical Astronomy Observatory (NOAO), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), National Astronomical Observatory of Japan (NAOJ), Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Division of Physics, Mathematics and Astronomy [Pasadena], California Institute of Technology (CALTECH), ANR-08-JCJC-0008,UPGAL(2008), European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), 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), Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Strazzullo V., Gobat R., Daddi E., Onodera M., Carollo M., Dickinson M., Renzini A., Arimoto N., Cimatti A., Finoguenov A., Chary R.-R., Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), NOAO, Università di Bologna [Bologna] (UNIBO), and UPGAL

Subjects
galaxies: high redshift, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Cluster (physics), Galaxy formation and evolution, education, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Cosmology: observations, Galaxies: high-redshift, Galaxies: statistics, Large-scale structure of Universe, Astronomy and Astrophysics, Billion years, Redshift, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, galaxies: stellar, galaxies: structure, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: clusters (Cl J1449+0856)
Abstract

We present a study of galaxy populations in the central region of the IRAC-selected, X-ray detected galaxy cluster Cl J1449+0856 at z=2. Based on a sample of spectroscopic and photometric cluster members, we investigate stellar populations and morphological structure of cluster galaxies over an area of ~0.7Mpc^2 around the cluster core. The cluster stands out as a clear overdensity both in redshift space, and in the spatial distribution of galaxies close to the center of the extended X-ray emission. The cluster core region (r, 17 pages, 13 figures, ApJ in press

Published
2013

19. The Early Early Type: Discovery of a Passive Galaxy at $_{Zspec}$ $\sim$ 3

Author

Masato Onodera, Alessandro Cimatti, Mark Dickinson, Marcella Carollo, Matthieu Béthermin, Raphael Gobat, Emanuele Daddi, Alvio Renzini, V. Strazzullo, 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), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), National Optical Astronomy Observatory (NOAO), Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), UPGAL, European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), 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), Gobat R., Strazzullo V., Daddi E., Onodera M., Renzini A., Béthermin M., Dickinson M., Carollo M., and Cimatti A.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, Metallicity, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Photometry (optics), galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, 10. No inequality, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Redshift, Grism, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the discovery of a massive, quiescent galaxy at z=2.99. We have obtained a HST/WFC3 spectrum of this object and measured its redshift from the detection of a deep 4000A break consistent with an old population and a high metallicity. By stellar population modeling of both its grism spectrum and broad-band photometry, we derive an age of ~0.7 Gyr, implying a formation redshift of z>4, and a mass >10^11 Msun. Although this passive galaxy is the most distant confirmed so far, we find that it is slightly less compact than other z>2 early-types of similar mass, being overall more analogous to those z~1.6 field early-type galaxies. The discovery of this object shows that early-type galaxies are detectable to at least z=3 and suggests that the diversity of structural properties found in z=1.4-2 ellipticals to earlier epochs could have its origin in a variety of formation histories among their progenitors., 6 pages, 4 figures, 1 table. Accepted for publication in The Astrophysical Journal Letters

Published
2012

20. The bolometric output and host-galaxy properties of obscured AGN in the XMM-COSMOS survey

Author

Jonathan R. Trump, V. Mainieri, Francesca Civano, M. Carollo, Preethi Nair, Marcella Brusa, Gianni Zamorani, Roberto Gilli, Angela Bongiorno, Cristian Vignali, Anton M. Koekemoer, Ezequiel Treister, Micol Bolzonella, Monique Aller, Andrea Comastri, Andrea Merloni, Elisabeta Lusso, David S Sanders, Lusso E., Comastri A., Vignali C., Zamorani G., Treister E., Sanders D., Bolzonella M., Bongiorno A., Brusa M., Civano F., Gilli R., Mainieri V., Nair P., Aller M.C., Carollo M., Koekemoer A., Merloni A., and Trump J.R.

Subjects
Physics, Solar mass, methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Infrared, GALAXY: GENERAL, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Galaxies: active, Galaxy: general, Methods: statistical, Quasars: general, X-rays: general, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Accretion (astrophysics), Redshift, Galaxy, Luminosity, Black hole, quasars: general, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a study of the multi-wavelength properties, from the mid-infrared to the hard X-rays, of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured the X-ray absorbing column density is determined by either X-ray spectral analyses (for the 45% of the sample), or from hardness ratios. Spectral Energy Distributions (SEDs) are computed for all sources in the sample. The average SEDs in the optical band is dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. We calculate bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using a multi-component modeling to properly disentangle the emission associated to stellar light from that due to black hole accretion. For 90% of the sample we also have the morphological classifications obtained with an upgraded version of the Zurich Estimator of Structural Types (ZEST+). We find that on average Type-2 AGN have lower bolometric corrections than Type-1 AGN. Moreover, we confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these Type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10^10 solar masses., 16 pages, 15 figures, accepted for publication in A&A

Published
2011

21. Black hole accretion and host galaxies of obscured quasars in XMM-COSMOS

Author

Jonathan R. Trump, John D. Silverman, E. Le Floc'h, Günther Hasinger, Daniela Vergani, V. Le Brun, Fabrizio Fiore, S. Bardelli, E. Zucca, Masayuki Tanaka, Chris Impey, Olivier Ilbert, Martin Elvis, Marcella Brusa, Laurence Tresse, Kazushi Iwasawa, F. Lamareille, V. Mainieri, M. Carollo, E. Perez Montero, Karina Caputi, Y. Peng, Jean-Paul Kneib, P. Kampczyk, Lucia Pozzetti, S. de la Torre, Preethi Nair, Yoshiaki Taniguchi, R. Pello, Peter Capak, Roberto Gilli, J. F. Le Borgne, Nico Cappelluti, M. Scodeggio, Anton M. Koekemoer, Andrea Comastri, Christian Maier, Andrea Merloni, P. Franzetti, Angela Bongiorno, C. Knobel, Graziano Coppa, Gianni Zamorani, Olga Cucciati, Elisabeta Lusso, K. Kovac, Herve Aussel, Micol Bolzonella, Lidia Tasca, E. Ricciardelli, L. de Ravel, A. Iovino, Monique Aller, C. Halliday, M. Mignoli, Alvio Renzini, S. J. Lilly, Cristian Vignali, Italo Balestra, Bianca Garilli, Thierry Contini, Mara Salvato, N. Z. Scoville, O. Le Fèvre, Mainieri V., Bongiorno A., Merloni A., Aller M., Carollo M., Iwasawa K., Koekemoer A. M., Mignoli M., Silverman J. D., Bolzonella M., Brusa M., Comastri A., Gilli R., Halliday C., Ilbert O., Lusso E., Salvato M., Vignali C., Zamorani G., Contini T., Kneib J.-P., Le Fevre O., Lilly S., Renzini A., Scodeggio M., Balestra I., Bardelli S., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kovac K., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Nair P., Pello R., Peng Y., Perez Montero E., Pozzetti L., Ricciardelli E., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Aussel H., Capak P., Cappelluti N., Elvis M., Fiore F., Hasinger G., Impey C., Le Floc'h E., Scoville N., Taniguchi Y., Trump J., Astronomy, 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
QSOS, ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, galaxies: active, galaxies: nuclei, galaxies: star formation, quasars: general, X-rays: general, EARLY DATA RELEASE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, 01 natural sciences, POWERFUL RADIO GALAXIES, 0103 physical sciences, Galaxy formation and evolution, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], STELLAR MASS DENSITY, DEEP FIELD-SOUTH, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Quasar, HUBBLE-SPACE-TELESCOPE, Galaxy, Accretion (astrophysics), Redshift, Space and Planetary Science, X-RAY-ABSORPTION, DIGITAL SKY SURVEY, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We explore the connection between black hole growth at the center of obscured quasars selected from the XMM-COSMOS survey and the physical properties of their host galaxies. We study a bolometric regime ( 8 x 10^45 erg/s) where several theoretical models invoke major galaxy mergers as the main fueling channel for black hole accretion. We confirm that obscured quasars mainly reside in massive galaxies (Mstar>10^10 Msun) and that the fraction of galaxies hosting such powerful quasars monotonically increases with the stellar mass. We stress the limitation of the use of rest-frame color-magnitude diagrams as a diagnostic tool for studying galaxy evolution and inferring the influence that AGN activity can have on such a process. We instead use the correlation between star-formation rate and stellar mass found for star-forming galaxies to discuss the physical properties of the hosts. We find that at z ~1, ~62% of Type-2 QSOs hosts are actively forming stars and that their rates are comparable to those measured for normal star-forming galaxies. The fraction of star-forming hosts increases with redshift: ~71% at z ~2, and 100% at z ~3. We also find that the the evolution from z ~1 to z ~3 of the specific star-formation rate of the Type-2 QSO hosts is in excellent agreement with that measured for star-forming galaxies. From the morphological analysis, we conclude that most of the objects are bulge-dominated galaxies, and that only a few of them exhibit signs of recent mergers or disks. Finally, bulge-dominated galaxies tend to host Type-2 QSOs with low Eddington ratios (lambda 0.1)., Accepted by A&A. 20 pages, 16 figures, 2 tables. A version with higher resolution figures and SED fits of Appendix A is available at http://www.eso.org/~vmainier/QSO2/qso2.pdf

Published
2011

22. zCOSMOS 10k-bright spectroscopic sample: exploring mass and environment dependence in early-type galaxies

Author

V. Mainieri, Marcella Carollo, E. Zucca, Michele Moresco, J. F. Le Borgne, Andrea Cimatti, L. de Ravel, A. Cappi, Micol Bolzonella, Lidia Tasca, F. Lamareille, S. Bardelli, Simon J. Lilly, P. Oesch, P. Memeo, U. Abbas, A. Iovino, Alvio Renzini, Cristiano Porciani, Y. Peng, M. Mignoli, E. Ricciardelli, O. Le Fèvre, C. Halliday, Jean-Paul Kneib, D. Maccagni, P. Franzetti, C. Knobel, Graziano Coppa, Gianni Zamorani, Masaomi Tanaka, Anton M. Koekemoer, A. Leauthaud, D. Bottini, Daniela Vergani, Laurence Tresse, Olga Cucciati, Lucia Pozzetti, E. Perez Montero, S. de la Torre, Angela Bongiorno, Bianca Garilli, B. Meneux, Christian Maier, Luigi Guzzo, Christian Marinoni, John D. Silverman, P. Kampczyk, Roberto Scaramella, R. Pello, M. Scodeggio, K. Kovac, Thierry Contini, H. J. McCracken, Preethi Nair, S. Di Cesare, Karina Caputi, Nick Scoville, Claudia Scarlata, V. Le Brun, Paolo Cassata, Moresco M., Pozzetti L., Cimatti A., Zamorani G., Mignoli M., di Cesare S., Bolzonella M., Zucca E., Lilly S., Kova&#269, K., Scodeggio M., Cassata P., Tasca L., Vergani D., Halliday C., Carollo M., Contini T., Kneib J.-P., Le Févre O., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Pellò R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Abbas U., Bottini D., Cappi A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Nair P., Oesch P., Porciani C., Scaramella R., Scarlata C., Scoville N., 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
FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), surveys, 0103 physical sciences, Range (statistics), Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, Sample (graphics), Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Early type, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width
Abstract

We present the analysis of the U-V rest-frame color distribution and some spectral features as a function of mass and environment for two sample of early-type galaxies up to z=1 extracted from the zCOSMOS spectroscopic survey. The first sample ("red galaxies") is defined with a photometric classification, while the second ("ETGs") by combining morphological, photometric, and spectroscopic properties to obtain a more reliable sample. We find that the color distribution of red galaxies is not strongly dependent on environment for all mass bins, with galaxies in overdense regions redder than galaxies in underdense regions with a difference of 0.027\pm0.008 mag. The dependence on mass is far more significant, with average colors of massive galaxies redder by 0.093\pm0.007 mag than low-mass galaxies throughout the entire redshift range. We study the color-mass relation, finding a mean slope 0.12\pm0.005, while the color-environment relation is flatter, with a slope always smaller than 0.04. The spectral analysis that we perform on our ETGs sample is in good agreement with our photometric results: we find for D4000 a dependence on mass between high and low-mass galaxies, and a much weaker dependence on environment (respectively a difference of of 0.11\pm0.02 and of 0.05\pm0.02); for the equivalent width of H{\delta}we measure a difference of 0.28\pm0.08 {\AA}across the same mass range and no significant dependence on environment.By analyzing the lookback time of early-type galaxies, we support the possibility of a downsizing scenario, in which massive galaxies with a stronger D4000 and an almost constant equivalent width of $H\delta$ formed their mass at higher redshift than lower mass ones. We also conclude that the main driver of galaxy evolution is the galaxy mass, the environment playing a subdominant role., Comment: 12 pages, 12 figures, accepted for publication on Astronomy and Astrophysics

Published
2010

23. Ultraluminous X-ray sources out to z ~ 0.3 in the COSMOS field

Author

Angela Bongiorno, O. Le Fèvre, John D. Silverman, N. Z. Scoville, P. Franzetti, Anton M. Koekemoer, Olga Cucciati, E. Zucca, Simonetta Puccetti, C. Knobel, Thierry Contini, S. Bardelli, Bianca Garilli, Giuseppina Fabbiano, G. Zamorani, Antonella Fruscione, L. de Ravel, E. Perez Montero, Jonathan R. Trump, Nico Cappelluti, Andrea Merloni, Mara Salvato, Cristian Vignali, M. Scodeggio, J. P. Kneib, K. Kovac, Alvio Renzini, Lidia Tasca, Y. Peng, S. de la Torre, Peter Capak, Alexis Finoguenov, Graziano Coppa, Francesca Civano, Roberto Gilli, Tom Aldcroft, Fabrizio Fiore, P. Kampczyk, V. Mainieri, F. Lamareille, Monique Aller, Chris Impey, R. Pello, Andrea Comastri, M. Bolzonella, M. Mignoli, Laurence Tresse, Martin Elvis, M. Carollo, Yoshiaki Taniguchi, Simon J. Lilly, Claudia Scarlata, Masayuki Tanaka, Karina Caputi, V. Le Brun, E. Ricciardelli, Christian Maier, Olivier Ilbert, Marcella Brusa, A. Iovino, J. F. Le Borgne, Daniela Vergani, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre 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), Astronomy, Mainieri V., Vignali C., Merloni A., Civano F., Puccetti S., Brusa M., Gilli R., Bolzonella M., Comastri A., Zamorani G., Aller M., Carollo M., Scarlata C., Elvis M., Aldcroft T.L., Cappelluti N., Fabbiano G., Finoguenov A., Fiore F., Fruscione A., Koekemoer A.M., Contini T., Kneib J.P., Le Fevre O., Lilly S., Renzini A., Scodeggio M., Bardelli S., Bongiorno A., Caputi K., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B., Iovino A., Kampczyk P., Knobel C., Kovac K., Lamareille F., Le Borgne J.F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J.D., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Capak P., Ilbert O., Impey C., Salvato M., Scoville S., Taniguchi Y., and Trump L.

Subjects
X-rays: galaxies – X-rays: binaries – X-rays: general – surveys, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, X-rays: binaries, surveys, 0103 physical sciences, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Star formation, X-ray, Astronomy and Astrophysics, Redshift, Galaxy, Early type, X-rays: galaxies, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using Chandra observations we have identified a sample of seven off-nuclear X-ray sources, in the redshift range z=0.072-0.283, located within optically bright galaxies in the COSMOS Survey. Using the multi-wavelength coverage available in the COSMOS field, we study the properties of the host galaxies of these ULXs. In detail, we derived their star formation rate from H_alpha measurements and their stellar masses using SED fitting techniques with the aim to compute the probability to have an off-nuclear source based on the host galaxy properties. We divide the host galaxies in different morphological classes using the available ACS/HST imaging. We find that our ULXs candidates are located in regions of the SFR versus M$_star$ plane where one or more off-nuclear detectable sources are expected. From a morphological analysis of the ACS imaging and the use of rest-frame colours, we find that our ULXs are hosted both in late and early type galaxies. Finally, we find that the fraction of galaxies hosting a ULX ranges from ~0.5% to ~0.2% going from L[0.5-2 keV]=3 x 10^39 erg s^-1 to L[0.5-2 keV]= 2 x 10^40 erg s^-1., Comment: 10 pages, 9 figures, accepted for publication in Astronomy & Astrophysics

Published
2010

24. In and out star formation in z ~ 1.5 quiescent galaxies from rest-frame UV spectroscopy and the far-infrared

Author

Claudia Maraston, Emanuele Daddi, Matthieu Béthermin, Michele Cappellari, Marcella Carollo, Bianca Garilli, Zhibo Ma, Michele Moresco, Lucia Pozzetti, Anita Zanella, Chiara Feruglio, Georgios E. Magdis, M. Mignoli, Veronica Strazzullo, Mark Sargent, Raphael Gobat, Alvio Renzini, Andrea Cimatti, Shuowen Jin, Francesco Valentino, Masato Onodera, Gobat, R, Daddi, E., Strazzullo, V., Garilli, B., Mignoli, M., Ma, Z., Jin, S., Maraston, C., Magdis, G., Béthermin, M., Cappellari, M., Carollo, M., Cimatti, A., Feruglio, C., Moresco, M., Onodera, M., Pozzetti, L., Renzini, A., Sargent, M., Valentino, F., Zanella, A., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Département d'Astrophysique (ex SAP) (DAP), 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, INAF- Milano, Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Institute of cosmology and gravitation, University of Portsmouth, Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford-University of Oxford, 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 and Astronomy [UCLA Los Angeles], University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica e Astronomia [Bologna], Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Padova (OAPD), Astronomy Centre, University of Sussex, 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), University of Oxford [Oxford]-University of Oxford [Oxford], 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), University of California-University of California, Università di Bologna [Bologna] (UNIBO), Daddi, E, Strazzullo, V, Garilli, B, Mignoli, M, Ma, Z, Jin, S, Maraston, C, Magdis, G, Bethermin, M, Cappellari, M, Carollo, M, Cimatti, A, Feruglio, C, Moresco, M, Onodera, M, Pozzetti, L, Renzini, A, Sargent, M, Valentino, F, and Zanella, A

Subjects
formation [galaxies], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, 01 natural sciences, elliptical and lenticular,cD [galaxies], cD, galaxies: high-redshift, galaxies: elliptical and lenticular, galaxies: formation, galaxies: stellar content, galaxies: star formation, Astrophysics - Astrophysics of Galaxies, Ultraviolet visible spectroscopy, Far infrared, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, Galaxies: star formation, 010308 nuclear & particles physics, Star formation, Galaxies: high-redshift, Astronomy and Astrophysics, Rest frame, Astronomy and Astrophysic, stellar content [galaxies], Galaxies: stellar content, Galaxy, Redshift, Galaxies: elliptical and lenticular, cD, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], elliptical and lenticular [galaxies], elliptical and lenticular, cD [galaxies], high-redshift [galaxies]
Abstract

We present a sample of 34 spectroscopically confirmed BzK-selected ~1e11 Msun quiescent galaxies (pBzK) in the COSMOS field. The targets were initially observed with VIMOS on the VLT to facilitate the calibration of the photometric redshifts of massive galaxies at z >~ 1.5. Here we describe the reduction and analysis of the data, and the spectrophotometric properties of these pBzK galaxies. In particular, using a spatially resolved median 2D spectrum, we find that the fraction of stellar populations with ages, 12 pages, 10 figures, accepted for publication in Astronomy & Astrophysics

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25. DEEP NEAR-INFRARED SPECTROSCOPY OF PASSIVELY EVOLVING GALAXIES ATz≳ 1.4

Author

Olivier Ilbert, David B. Sanders, Nobuo Arimoto, Masato Onodera, H. J. McCracken, Emanuele Daddi, S. Lilly, Anton M. Koekemoer, Alessandro Cimatti, Kouji Ohta, Kentaro Motohara, Alvio Renzini, Xu Kong, Michele Cappellari, Yoshiaki Taniguchi, M. Carollo, Yoshihiko Yamada, N. Z. Scoville, Veronica Strazzullo, Peter Capak, C. Mancini, Raphael Gobat, Naoyuki Tamura, Mauro Giavalisco, Onodera M., Renzini A., Carollo M., Cappellari M., Mancini C., Strazzullo V., Daddi E., Arimoto N., Gobat R., Yamada Y., McCracken H. J., Ilbert O., Capak P., Cimatti A., Giavalisco M., Koekemoer A. M., Kong X., Lilly S., Motohara K., Ohta K., Sanders D. B., Scoville N., Tamura N., and Taniguchi Y.

Subjects
Effective radius, Physics, Stellar mass, 010308 nuclear & particles physics, Star formation, Continuum (design consultancy), Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Galaxy, Redshift, galaxies: evolution, galaxies: formation, galaxies: high-redshift, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] We present the results of new near-IR spectroscopic observations of passive galaxies at z>1.4 in a concentration of BzK-selected galaxies in the COSMOS field. The observations have been conducted with Subaru/MOIRCS, and have resulted in absorption lines and/or continuum detection for 18 out of 34 objects. This allows us to measure spectroscopic redshifts for a sample almost complete to K(AB)=21. COSMOS photometric redshifts are found in fair agreement overall with the spectroscopic redshifts, with a standard deviation of ~0.05; however, ~30% of objects have photometric redshifts systematically underestimated by up to ~25%. We show that these systematic offsets in photometric redshifts can be removed by using these objects as a training set. All galaxies fall in four distinct redshift spikes at z=1.43, 1.53, 1.67 and 1.82, with this latter one including 7 galaxies. SED fits to broad-band fluxes indicate stellar masses in the range of ~4-40x10^10Msun and that star formation was quenched ~1 Gyr before the cosmic epoch at which they are observed. The spectra of several individual galaxies have allowed us to measure their Hdelta_F and Dn4000 indices, which confirms their identification as passive galaxies, as does a composite spectrum resulting from the coaddition of 17 individual spectra. The effective radii of the galaxies have been measured on the HST/ACS F814W image, confirming the coexistence at these redshifts of passive galaxies which are substantially more compact than their local counterparts with others that follow the local size-stellar mass relation. For the galaxy with best S/N spectrum we were able to measure a velocity dispersion of 270+/-105 km/s, indicating that this galaxy lies closely on the virial relation given its stellar mass and effective radius., Comment: 26 pages, 24 figures, 5 tables, in emulateapj format; accepted for publication in The Astrophysical Journal

Published
2012

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