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18 results on '"evolution survey cosmos"'

1. Euclid: the selection of quiescent and star-forming galaxies using observed colours

Author

F. J. Castander, Rafael Toledo-Moreo, L. Bisigello, Marc Sauvage, M. Poncet, Ulrike Kuchner, H. Israel, R. Cledassou, S. Kermiche, Crescenzo Tortora, F. Sureau, Sebastiano Ligori, R. Kohley, Sandrine Pires, Jarle Brinchmann, Mauro Roncarelli, Michele Moresco, G. Zamorani, Andy Taylor, G. Meylan, Andrea Cimatti, Natalia Auricchio, J. Carretero, B. Kubik, M. Wetzstein, Lucia Pozzetti, Thomas D. Kitching, Felix Hormuth, Stefano Andreon, E. Franceschi, Claudia Maraston, M. Bolzonella, Roberto P. Saglia, Martin Kunz, Simona Mei, D. Masters, M. Frailis, Andrew Humphrey, Leonardo Corcione, A. Secroun, Mark Cropper, Ismael Tereno, G. Polenta, V. Capobianco, Jason Rhodes, L. Valenziano, Ivan Lloro, S. Serrano, Peter Schneider, Elisabetta Maiorano, L. Conversi, Fabio Pasian, Ole Marggraf, G. Congedo, P. B. Lilje, S. Dusini, S. Paltani, Y. Mellier, Valeria Pettorino, P. Franzetti, C. J. Conselice, F. Raison, B. Garilli, Yu Wang, Marco Castellano, M. Fumana, O. Le Fevre, Richard Massey, Knud Jahnke, Pierre-Alain Duc, Stefano Cavuoti, Emanuel Rossetti, C. Padilla, Julien Zoubian, Zoubian, J, Wetzstein, M, Wang, Y, Valenziano, L, Toledo-Moreo, R, Tereno, I, Taylor, A N, Sureau, F, Serrano, S, Secroun, A, Schneider, P, Sauvage, M, Saglia, R, Rossetti, E, Roncarelli, M, Rhodes, J, Raison, F, Poncet, M, Polenta, G, Pires, S, Pettorino, V, Pasian, F, Paltani, S, Padilla, C, Meylan, G, Mellier, Y, Mei, S, Masters, D C, Massey, R, Marggraf, O, Maiorano, E, Lloro, I, Lilje, P B, Ligori, S, Le Fèvre, O, Kunz, M, Kubik, B, Kohley, R, Kitching, T, Kermiche, S, Jahnke, K, Israel, H, Hormuth, F, Fumana, M, Franzetti, P, Franceschi, E, Frailis, M, Dusini, S, Cropper, M S, Corcione, L, Conversi, L, Congedo, G, Cledassou, R, Cimatti, A, Cavuoti, S, Castellano, M, Castander, F J, Carretero, J, Capobianco, V, Brinchmann, J, Auricchio, N, Zamorani, G, Tortora, C, Pozzetti, L, Moresco, M, Maraston, C, Humphrey, A, Garilli, B, Duc, P-A, Bolzonella, M, Andreon, S, Conselice, C J, Kuchner, U, Bisigello, L, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), Université Paris Diderot - Paris 7 (UPD7), 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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), 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), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
photometric redshifts, challenge lightcone simulation, Sample (material), FOS: Physical sciences, Astrophysics, Star (graph theory), 01 natural sciences, law.invention, Telescope, environmental dependence, law, 0103 physical sciences, Galaxy formation and evolution, formation rates, luminosity function, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, legacy survey, evolution survey cosmos, Astrophysics - Astrophysics of Galaxies, galaxies: general, red sequence, Galaxy, Redshift, galaxies: photometry, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), magnitude distribution, stellar mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution
Abstract

The Euclid mission will observe well over a billion galaxies out to $z\sim6$ and beyond. This will offer an unrivalled opportunity to investigate several key questions for understanding galaxy formation and evolution. The first step for many of these studies will be the selection of a sample of quiescent and star-forming galaxies, as is often done in the literature by using well known colour techniques such as the `UVJ' diagram. However, given the limited number of filters available for the Euclid telescope, the recovery of such rest-frame colours will be challenging. We therefore investigate the use of observed Euclid colours, on their own and together with ground-based u-band observations, for selecting quiescent and star-forming galaxies. The most efficient colour combination, among the ones tested in this work, consists of the (u-VIS) and (VIS-J) colours. We find that this combination allows users to select a sample of quiescent galaxies complete to above $\sim70\%$ and with less than 15$\%$ contamination at redshifts in the range $0.7565\%$ completeness level and contamination below 20$\%$ at $1, Comment: 19 pages, 15 figures, 5 tables, accepted for publication in MNRAS

Published
2020
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2. Bright Lyman-alpha emitters among Spitzer SMUVS galaxies in the MUSE/COSMOS field

Author

S. Deshmukh, G. Rosani, Karina Caputi, G. B. Caminha, and Astronomy

Subjects
EMITTING GALAXIES, Stellar mass, Extinction (astronomy), REDSHIFT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ESCAPE, 01 natural sciences, Spectral line, STAR-FORMATION, STELLAR POPULATIONS, LY-ALPHA, galaxies: high-redshift, 0103 physical sciences, SPECTRA, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, EVOLUTION SURVEY COSMOS, Mass distribution, 010308 nuclear & particles physics, Star formation, CONSTRAINTS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, observations [cosmology], STARBURSTS, Space and Planetary Science, galaxies: star formation, cosmology: observations, Spectral energy distribution, star formation [galaxies], high-redshift [galaxies]
Abstract

We search for bright Ly$\rm \alpha$ emitters among Spitzer SMUVS galaxies at z > 2.9 with homogeneous MUSE data. Although it only covers a small region of COSMOS, MUSE has the unique advantage of providing spectral information over the entire field, without the need of target pre-selection. This gives an unbiased detection of all the brightest Ly$\rm \alpha$ emitters among SMUVS sources, which by design are stellar-mass selected galaxies. Within the studied area, ~14% of the SMUVS galaxies at z > 2.9 have Ly$\rm \alpha$ fluxes F$\rm _\lambda$ > 7 x 10$^{-18}$ erg s$^{-1}$ cm$^{-2}$. These Ly$\rm \alpha$ emitters are characterized by three types of emission, 47% show a single line profile, 19% present a double peak or a blue bump and 31% show a red tail. One object (3%) shows both a blue bump and a red tail. We also investigate the spectral energy distribution (SED) properties of the SMUVS MUSE-detected galaxies and MUSE non-detections. After stellar-mass matching both populations, we find that MUSE detected galaxies have generally lower extinction than SMUVS-only objects, while there is no clear intrinsic difference in the mass and age distributions. For the MUSE-detected SMUVS galaxies, we compare the instantaneous SFR lower limit given by Ly$\rm \alpha$ flux with its past average derived from SED fitting, and find evidence for rejuvenation in some of our oldest objects. We also study the spectra of those Ly$\rm \alpha$ emitters which are not detected in SMUVS in the same field. We find different distributions of the emission line profiles, which could be ascribed to the fainter Ly$\rm \alpha$ luminosities of the MUSE-only sources and an intrinsically different mass distribution. Finally, we search for the presence of galaxy associations. MUSE's integral coverage is 20 times more likely to find associations than all other existing spectral data in COSMOS, biased by target pre-selection., Comment: 14 pages, 7 figures, 5 tables, re-submitted to A&A after addressing the referee's report

Published
2020
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3. The ALPINE-ALMA [CII] survey: Survey strategy, observations and sample properties of 118 star-forming galaxies at $4 < z < 6$

Author

M. Bethermin, Carlotta Gruppioni, Shoubaneh Hemmati, Lin Yan, G. Zamorani, Michele Ginolfi, Andreas L. Faisst, E. Zucca, Fabian Walter, G. Lagache, Francesca Pozzi, F. Loiacono, Edo Ibar, Médéric Boquien, Ricardo Amorín, Nick Scoville, Daniel Schaerer, Anton M. Koekemoer, Y. Khusanova, Pascal Oesch, Dominik Riechers, Desika Narayanan, Andrea Cimatti, John D. Silverman, Nimish P. Hathi, Sune Toft, Brian C. Lemaux, Livia Vallini, Chiara Mancini, Miroslava Dessauges-Zavadsky, H. Mendez-Hernandez, R. Thomas, L. Morselli, G. C. Jones, Mauro Giavalisco, L. A. M. Tasca, Paolo Cassata, Roberto Maiolino, Peter Capak, O. Le Fevre, M. Romano, D. Vergani, S. Bardelli, Margherita Talia, Seiji Fujimoto, Y. Fudamoto, 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), 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), ALPINE Team, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université 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), Le Fevre, O., Bethermin, M., Faisst, A., Jones, G. C., Capak, P., Cassata, P., Silverman, J. D., Schaerer, D., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Giavalisco, M., Hathi, N. P., Fudamoto, Y., Fujimoto, S., Ginolfi, M., Gruppioni, C., Hemmati, S., Ibar, E., Koekemoer, A., Khusanova, Y., Lagache, G., Lemaux, B. C., Loiacono, F., Maiolino, R., Mancini, C., Narayanan, D., Morselli, L., Mendez-Hernandez, H., Oesch, P. A., Pozzi, F., Romano, M., Riechers, D., Scoville, N., Talia, M., Tasca, L. A. M., Thomas, R., Toft, S., Vallini, L., Vergani, D., Walter, F., Zamorani, G., Zucca, E., Le Fevre O., Bethermin M., Faisst A., Jones G.C., Capak P., Cassata P., Silverman J.D., Schaerer D., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Giavalisco M., Hathi N.P., Fudamoto Y., Fujimoto S., Ginolfi M., Gruppioni C., Hemmati S., Ibar E., Koekemoer A., Khusanova Y., Lagache G., Lemaux B.C., Loiacono F., Maiolino R., Mancini C., Narayanan D., Morselli L., Mendez-Hernandez H., Oesch P.A., Pozzi F., Romano M., Riechers D., Scoville N., Talia M., Tasca L.A.M., Thomas R., Toft S., Vallini L., Vergani D., Walter F., Zamorani G., and Zucca E.

Subjects
formation [galaxies], Population, REDSHIFT, BILLION YEARS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, COOL GAS, Far infrared, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, galaxies: formation, MAIN-SEQUENCE, FIELD, education, 010303 astronomy & astrophysics, Reionization, BLACK-HOLES, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, EVOLUTION SURVEY COSMOS, education.field_of_study, 010308 nuclear & particles physics, James Webb Space Telescope, Astronomy and Astrophysics, FRAMEWORK, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, C II EMISSION, SIMULATIONS, Reference sample, Space and Planetary Science, galaxies: star formation, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The ALMA-ALPINE [CII] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [CII]-158$\mu$m line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 45). Based on a visual inspection of the [CII] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4, Comment: 20 pages, 13 figures, 1 table, accepted by A&A

Published
2020
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4. Molecular gas in radio galaxies in dense megaparsec-scale environments at $z =$ 0.4–2.6

Author

Gianluca Castignani, Francoise Combes, Jonathan Freundlich, P. Salomé, G. de Zotti, Marco Chiaberge, C. Benoist, 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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Collège de France (CdF (institution)), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (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 (CdF), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
photometric redshifts, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Scale (ratio), molecular data, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, spectral energy-distribution, line emission, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, legacy survey, evolution survey cosmos, star-forming galaxies, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, active galactic nuclei, Astrophysics::Earth and Planetary Astrophysics, brightest cluster galaxies, stellar mass, hubble-deep-field, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Context. Low luminosity radio galaxies (LLRGs) typically reside in dense megaparsec-scale environments and are often associated with brightest cluster galaxies (BCGs). They are an excellent tool to study the evolution of molecular gas reservoirs in giant ellipticals, even close to the active galactic nucleus., Aims. We investigate the role of dense megaparsec-scale environment in processing molecular gas in LLRGs in the cores of galaxy (proto-)clusters. To this aim we selected within the COSMOS and DES surveys a sample of five LLRGs at z = 0.4-2.6 that show evidence of ongoing star formation on the basis of their far-infrared (FIR) emission., Methods. We assembled and modeled the FIR-to-UV spectral energy distributions (SEDs) of the five radio sources to characterize their host galaxies in terms of stellar mass and star formation rate. We observed the LLRGs with the IRAM-30m telescope to search for CO emission. We then searched for dense megaparsec-scale overdensities associated with the LLRGs using photometric redshifts of galaxies and the Poisson Probability Method, which we have upgraded using an approach based on the wavelet-transform (wPPM), to ultimately characterize the overdensity in the projected space and estimate the radio galaxy miscentering. Color-color and colormagnitude plots were then derived for the fiducial cluster members, selected using photometric redshifts., Results. Our IRAM-30m observations yielded upper limits to the CO emission of the LLRGs, at z = 0 : 39, 0.61, 0.91, 0.97, and 2.6. For the most distant radio source, COSMOS-FRI 70 at z = 2 : 6, a hint of CO(7 -> 6) emission is found at 2.2 sigma. The upper limits found for the molecular gas content M(H-2) = M-star< 0 : 11, 0.09, 1.8, 1.5, and 0.29, respectively, and depletion time tau(dep) less than or similar to (0.2-7) Gyr of the five LLRGs are overall consistent with the corresponding values of main sequence field galaxies. Our SED modeling implies large stellar-mass estimates in the range log(M-star/M-Theta) = 10.9-11.5, typical for giant ellipticals. Both our wPPM analysis and the cross-matching of the LLRGs with existing cluster/group catalogs suggest that the megaparsec-scale overdensities around our LLRGs are rich (less than or similar to 10(14) M-Theta) groups and show a complex morphology. The color-color and color-magnitude plots suggest that the LLRGs are consistent with being star forming and on the high-luminosity tail of the red sequence. The present study thus increases the still limited statistics of distant cluster core galaxies with CO observations., Conclusions. The radio galaxies of this work are excellent targets for ALMA as well as next-generation telescopes such as the James Webb Space Telescope.

Published
2019
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5. Group connectivity in COSMOS: a tracer of mass assembly history

Author

F. Sarron, Sébastien Peirani, Christophe Pichon, Julien Devriendt, Yohan Dubois, Ghassem Gozaliasl, Alexis Finoguenov, K. Kraljic, Adrianne Slyz, Stéphane Arnouts, Clotilde Laigle, E. Darragh Ford, Richard E. Griffiths, H. C. Pan, 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), 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, and Helsinki Institute of Physics

Subjects
HALO MASS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, STAR-FORMATION, methods: numerical, SUPERMASSIVE BLACK-HOLES, GALAXY EVOLUTION, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, DARK-MATTER, galaxies: formation, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, ComputingMilieux_MISCELLANEOUS, Physics, EVOLUTION SURVEY COSMOS, Supermassive black hole, GALACTIC CONFORMITY, 010308 nuclear & particles physics, Group (mathematics), Star formation, FILAMENTARY STRUCTURE, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: photometry, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), DIGITAL SKY SURVEY, large-scale structure of Universe, methods: observational, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Cosmic filaments are the channel through which galaxy groups assemble their mass. Cosmic connectivity, namely the number of filaments connected to a given group, is therefore expected to be an important ingredient in shaping group properties. The local connectivity is measured in COSMOS around X-Ray detected groups between redshift 0.5 and 1.2. To this end, large-scale filaments are extracted using the accurate photometric redshifts of the COSMOS2015 catalogue in two-dimensional slices of thickness 120 comoving Mpc centred on the group's redshift. The link between connectivity, group mass and the properties of the brightest group galaxy (BGG) is investigated. The same measurement is carried out on mocks extracted from the lightcone of the hydrodynamical simulation Horizon-AGN in order to control systematics. More massive groups are on average more connected. At fixed group mass in low-mass groups, BGG mass is slightly enhanced at high connectivity, while in high mass groups BGG mass is lower at higher connectivity. Groups with a star-forming BGG have on average a lower connectivity at given mass. From the analysis of the Horizon-AGN simulation, we postulate that different connectivities trace different paths of group mass assembly: at high group mass, groups with higher connectivity are more likely to have grown through a recent major merger, which might be in turn the reason for the quenching of the BGG. Future large-field photometric surveys, such as Euclid and LSST, will be able to confirm and extend these results by probing a wider mass range and a larger variety of environment., 14 pages, 10 figures, 1 table; submitted to MNRAS; Comments are welcome!

Published
2019
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6. Spitzer bright ultravista faint sources in cosmos

Author

O. Le Fèvre, H. J. McCracken, Mara Salvato, Bo Milvang-Jensen, Olivier Ilbert, Clotilde Laigle, Yoshiaki Taniguchi, Peter Capak, Karina Caputi, Johan P. U. Fynbo, Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], 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), 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), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), University of Copenhagen = Københavns Universitet (UCPH), Spitzer Science Center, California Institute of Technology (CALTECH), Max-Planck-Institut für Extraterrestrische Physik (MPE), Ehime University [Matsuyama, Japon], ANR-14-CE33-0004,SAGACE,Recensement de la masse stellaire et des galaxies dans les premiers 2 milliards d'années de l'Univers(2014), European Project: 278202,EC:FP7:ERC,ERC-2011-StG_20101014,EGGS(2011), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), University of Copenhagen = Københavns Universitet (KU), Ehime University [Matsuyama], and Astronomy

Subjects
ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, [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, 01 natural sciences, galaxies [infrared], HIGH-REDSHIFT GALAXIES, infrared: galaxies, galaxies: high-redshift, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, education, EXTRAGALACTIC LEGACY SURVEY, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, STAR-FORMATION HISTORIES, S-SELECTED GALAXIES, Physics, EVOLUTION SURVEY COSMOS, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, DUST-OBSCURED GALAXIES, EXTREMELY RED H, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Cosmos (category theory), Spectral energy distribution, DEEP-FIELD-SOUTH, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Cosmic time, high-redshift [galaxies], LESS-THAN 7, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have analysed a sample of 574 Spitzer 4.5 micron-selected galaxies with [4.5]24 (AB) over the UltraVISTA ultra-deep COSMOS field. Our aim is to investigate whether these mid-IR bright, near-IR faint sources contribute significantly to the overall population of massive galaxies at redshifts z>=3. By performing a spectral energy distribution (SED) analysis using up to 30 photometric bands, we have determined that the redshift distribution of our sample peaks at redshifts z~2.5-3.0, and ~32% of the galaxies lie at z>=3. We have studied the contribution of these sources to the galaxy stellar mass function (GSMF) at high redshifts. We found that the [4.5]24 galaxies produce a negligible change to the GSMF previously determined for Ks_auto~50% of the galaxies with stellar masses Mst>~6 x 10^10 Msun. We also constrained the GSMF at the highest-mass end (Mst>~2 x 10^11 Msun) at z>=5. From their presence at 5=, Comment: 18 pages, 15 figures, 4 tables. Updated to match version in press at the ApJ

Published
2015
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7. ZFOURGE: Using Composite Spectral Energy Distributions to Characterize Galaxy Populations at 1 < z < 4

Author

Michael J. Cowley, Rebecca Allen, Glenn G. Kacprzak, Lalitwadee Kawinwanichakij, Kim-Vy Tran, Casey Papovich, Lee R. Spitler, Ben Forrest, Themiya Nanayakkara, Jonathan Cohn, Robert C. Kennicutt, Karl Glazebrook, Adam Broussard, Caroline M. S. Straatman, and Brett Salmon

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, HUBBLE-DEEP-FIELD, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, MULTIWAVELENGTH PHOTOMETRY, education, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, EVOLUTION SURVEY COSMOS, Physics, education.field_of_study, Number density, 010308 nuclear & particles physics, Star formation, POST-STARBURST GALAXIES, Spectral density, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Billion years, Galaxy, LYMAN-BREAK GALAXIES, Physics and Astronomy, Space and Planetary Science, COLOR-MAGNITUDE DIAGRAM, DIGITAL SKY SURVEY, O III, STELLAR MASS, Equivalent width, high-redshift [galaxies]
Abstract

We investigate the properties of galaxies as they shut off star formation over the 4 billion years surrounding peak cosmic star formation. To do this we categorize $\sim7000$ galaxies from $1, Comment: Accepted for publication in The Astrophysical Journal

Published
2018
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8. The Dependence of Star Formation Activity on Stellar Mass Surface Density and Sersic Index in zCOSMOS Galaxies at 0.5 <z <0.9 Compared with SDSS Galaxies at 0.04 <z <0.08

Author

M. T. Sargent, D. Bottini, Daniela Vergani, P. Franzetti, Olga Cucciati, Andrea Cimatti, A. Iovino, Simon J. Lilly, Christian Maier, A. Cappi, J. F. Le Borgne, S. de la Torre, Christian Marinoni, Karina Caputi, C. Knobel, U. Abbas, L. de Ravel, Y. Peng, E. Ricciardelli, Alvio Renzini, C. Halliday, M. Scodeggio, Claudia Scarlata, V. Le Brun, M. Mignoli, Angela Bongiorno, Anton M. Koekemoer, Pascal Oesch, A. Leauthaud, S. Bardelli, Cristiano Porciani, P. Kampczyk, Laurence Tresse, Lidia Tasca, Thierry Contini, B. Meneux, Paolo Cassata, Masayuki Tanaka, Bianca Garilli, P. Memeo, V. Mainieri, Roser Pello, Lucia Pozzetti, C. M. Carollo, O. Le Fèvre, M. Bolzonella, G. Zamorani, John D. Silverman, Jean-Paul Kneib, E. Perez Montero, H. J. McCracken, Graziano Coppa, D. Maccagni, E. Zucca, Luigi Guzzo, F. Lamareille, M. Fumana, Roberto Scaramella, K. Kovac, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), 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), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Maier C., Lilly S. J., Zamorani G., Scodeggio M., Lamareille F., Contini T., Sargent M. T., Scarlata C., Oesch P., Carollo C. M., Le Fèvre O., Renzini A., Kneib J.-P., Mainieri V., Bardelli S., Bolzonella M., 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., Kova&#269, K., Le Borgne J.-F., Le Brun V., Mignoli M., Pello R., Peng Y., Montero E. Perez, Ricciardelli E., Silverman J. D., Tanaka M., Tasca L., Tresse L., Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo L., Halliday C., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Pozzetti L., and Scaramella R.

Subjects
Surface (mathematics), 010504 meteorology & atmospheric sciences, Stellar mass, Population, PHYSICAL-PROPERTIES, POPULATION SYNTHESIS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, 10. No inequality, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, LOCAL UNIVERSE, Physics, EVOLUTION SURVEY COSMOS, REDSHIFT SURVEY, education.field_of_study, Galaxies: evolution, Galaxies: high-redshift, Astronomy and Astrophysics, Space and Planetary Science, FORMING GALAXIES, Star formation, ASSEMBLY HISTORY, DISK GALAXIES, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, LUMINOSITY FUNCTION, DIGITAL SKY SURVEY, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies: evolution, Surface mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

One of the key unanswered questions in the study of galaxy evolution is what physical processes inside galaxies drive the changes in the SFRs in individual galaxies that, taken together, produce the large decline in the global star-formation rate density (SFRD) to redshifts since z~2. Many studies of the SFR at intermediate redshifts have been made as a function of the integrated stellar mass of galaxies but these did not use information on the internal structural properties of the galaxies. In this paper we present a comparative study of the dependence of SFRs on the average surface mass densities (SigmaM) of galaxies of different morphological types up to z~1 using the zCOSMOS and SDSS surveys. The main findings about the evolution of these relatively massive galaxies are: 1) There is evidence that, for both SDSS ans zCOSMOS galaxies, the mean specific SFR within a given population (either disk-dominated or bulge-dominated) is independent of SigmaM; 2) The observed SSFR - SigmaM step-function relation is due, at all investigated redshifts, to the changing mix of disk-dominated and bulge-dominated galaxies as surface density increases and the strong difference in the average SSFR between disks and bulges. We also find a modest differential evolution in the size-mass relations of disk and spheroid galaxies; 3) The shape of the median SSFR - SigmaM relation is similar, but with median SSFR values that are about 5-6 times higher in zCOSMOS galaxies than for SDSS, across the whole range of SigmaM, and in both spheroid and disk galaxies. This increase matches that of the global SFRD of the Universe as a whole, emphasizing that galaxies of all types are contributing, proportionally, to the global increase in SFRD in the Universe back to these redshifts (abridged)., Comment: Published 2009 in ApJ, 694, 1099

Published
2009
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9. The STAGES view of red spirals and dusty red galaxies: mass-dependent quenching of star formation in cluster infall

Author

Alfonso Aragón-Salamanca, John A. R. Caldwell, Marco Barden, Andy Taylor, Eric F. Bell, Michael L. Balogh, David Bacon, Klaus Meisenheimer, Casey Papovich, Eelco van Kampen, Kyle Lane, Anna Gallazzi, Meghan E. Gray, Daniel H. McIntosh, Catherine Heymans, Asmus Boehm, Xianzhong Zheng, Lutz Wisotzki, Christian Wolf, Chien Y. Peng, B. Haeussler, Fabio D. Barazza, Sebastián F. Sánchez, Shardha Jogee, and Knud Jahnke

Subjects
Cosmology and Gravitation, galaxies: spiral, Digital Sky Survey, Stellar mass, Population, Color-Magnitude Relation, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Low-Redshift Clusters, 01 natural sciences, infrared: galaxies, Large-Scale Structure, surveys, Morphology-Density Relation, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, education, Evolution Survey Cosmos, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, stars: formation, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), Sigma, Active Galactic Nuclei, Astronomy and Astrophysics, Luminosity Function, Redshift, Galaxy, Virgo Cluster, Stars, galaxies: clusters: general, Environmental Dependence, Space and Planetary Science, galaxies: evolution
Abstract

We investigate the properties of optically passive spirals and dusty red galaxies in the A901/2 cluster complex at redshift ~0.17 using restframe near-UV-optical SEDs, 24 micron IR data and HST morphologies from the STAGES dataset. The cluster sample is based on COMBO-17 redshifts with an rms precision of sigma_cz~2000 km/sec. We find that 'dusty red galaxies' and 'optically passive spirals' in A901/2 are largely the same phenomenon, and that they form stars at a substantial rate, which is only 4x lower than that in blue spirals at fixed mass. This star formation is more obscured than in blue galaxies and its optical signatures are weak. They appear predominantly in the stellar mass range of log M*/Msol=[10,11] where they constitute over half of the star-forming galaxies in the cluster; they are thus a vital ingredient for understanding the overall picture of star formation quenching in clusters. We find that the mean specific SFR of star-forming galaxies in the cluster is clearly lower than in the field, in contrast to the specific SFR properties of blue galaxies alone, which appear similar in cluster and field. Such a rich red spiral population is best explained if quenching is a slow process and morphological transformation is delayed even more. At log M*/Msol, Accepted for publication in MNRAS

Published
2009
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10. The Chandra COSMOS Legacy survey: optical/IR identifications

Author

Stephanie M. LaMassa, Takamitsu Miyaji, Vernesa Smolčić, Knud Jahnke, Hyewon Suh, Ezequiel Treister, Piero Ranalli, Kevin Schawinski, Benny Trakhtenbrot, Viola Allevato, C. Cardamone, Alexis Finoguenov, Mara Salvato, Clotilde Laigle, Alexander Karim, Günther Hasinger, G. Zamorani, S. Marchesi, Martin Elvis, Marcella Brusa, Nico Cappelluti, Cristian Vignali, Richard E. Griffiths, John D. Silverman, Giorgio Lanzuisi, Andrea Comastri, Eva Schinnerer, Roberto Gilli, C. M. Urry, Francesca Civano, ITA, USA, FRA, DEU, CHL, HRV, FIN, JPN, MEX, SWE, CHE, Marchesi, S., Civano, F., Elvis, M., Salvato, M., Brusa, M., Comastri, A., Gilli, R., Hasinger, G., Lanzuisi, G., Miyaji, T., Treister, E., Urry, C.M., Vignali, C., Zamorani, G., Allevato, V., Cappelluti, N., Cardamone, C., Finoguenov, A., Griffiths, R.E., Karim, A., Laigle, C., Lamassa, S.M., Jahnke, K., Ranalli, P., Schawinski, K., Schinnerer, E., Silverman, J.D., Smolcic, V., Suh, H., Trakhtenbrot, B., Urry, C. M., Griffiths, R. E., Lamassa, S. M., Silverman, J. D., and Department of Physics

Subjects
catalogs, cosmology: observations, galaxies: active, galaxies: evolution, surveys, X-rays: general, COMPTON-THICK AGN, catalog, Infrared, X-RAY SOURCES, Astrophysics, 01 natural sciences, Luminosity, general [X-rays], 010303 astronomy & astrophysics, Photometric redshift, Physics, observations [cosmology], PRIRODNE ZNANOSTI. Fizika, ROSAT DEEP SURVEY, active [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics, WIDE-FIELD SURVEY, observation [cosmology], ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometry (optics), SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, STAR-FORMING GALAXIES, survey, evolution [galaxies], Astrophysics::Galaxy Astrophysics, EVOLUTION SURVEY COSMOS, Supermassive black hole, cosmology: observation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, NATURAL SCIENCES. Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MEDIUM-SENSITIVITY SURVEY
Abstract

We present the catalog of optical and infrared counterparts of the Chandra COSMOS-Legacy Survey, a 4.6 Ms Chandra program on the 2.2 square degrees of the COSMOS field, combination of 56 new overlapping observations obtained in Cycle 14 with the previous C-COSMOS survey. In this Paper we report the i, K, and 3.6 micron identifications of the 2273 X-ray point sources detected in the new Cycle 14 observations. We use the likelihood ratio technique to derive the association of optical/infrared (IR) counterparts for 97% of the X-ray sources. We also update the information for the 1743 sources detected in C-COSMOS, using new K and 3.6 micron information not available when the C-COSMOS analysis was performed. The final catalog contains 4016 X-ray sources, 97% of which have an optical/IR counterpart and a photometric redshift, while 54% of the sources have a spectroscopic redshift. The full catalog, including spectroscopic and photometric redshifts and optical and X-ray properties described here in detail, is available online. We study several X-ray to optical (X/O) properties: with our large statistics we put better constraints on the X/O flux ratio locus, finding a shift towards faint optical magnitudes in both soft and hard X-ray band. We confirm the existence of a correlation between X/O and the the 2-10 keV luminosity for Type 2 sources. We extend to low luminosities the analysis of the correlation between the fraction of obscured AGN and the hard band luminosity, finding a different behavior between the optically and X-ray classified obscured fraction., Comment: 28 pages, 14 figures, accepted to ApJ

Published
2016
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11. The Chandra COSMOS-Legacy Survey: Source X-Ray Spectral Properties

Author

John D. Silverman, Kazushi Iwasawa, Giorgio Lanzuisi, Francesca Civano, C. M. Urry, G. Zamorani, Andrea Comastri, Stefano Marchesi, Richard E. Griffiths, Piero Ranalli, Viola Allevato, Mara Salvato, Takamitsu Miyaji, Hyewon Suh, Ezequiel Treister, Kevin Schawinski, Cristian Vignali, Department of Physics, ITA, USA, DEU, ESP, CHL, FIN, JPN, MEX, SWE, CHE, Universitat de Barcelona, Marchesi, S., Lanzuisi, G., Civano, F., Iwasawa, K., Suh, H., Comastri, A., Zamorani, G., Allevato, V., Griffiths, R., Miyaji, T., Ranalli, P., Salvato, M., Schawinski, K., Silverman, J., Treister, E., Urry, C.M., Vignali, C., and Urry, C. M.

Subjects
galaxie [X-rays], ACTIVE GALACTIC NUCLEI, COMPTON-THICK AGN, Photon, Active galactic nucleus, HEAVILY OBSCURED AGN, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, nuclei [galaxies], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Beta ray spectrometry, 0103 physical sciences, STAR-FORMING GALAXIES, Emission spectrum, DEEP FIELD-SOUTH, Absorption (electromagnetic radiation), SEYFERT 2 GALAXIES, 010303 astronomy & astrophysics, XMM-NEWTON OBSERVATIONS, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, Physics, EVOLUTION SURVEY COSMOS, Cosmologia, 010308 nuclear & particles physics, Star formation, ABSORBING COLUMN DENSITIES, X-ray, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Espectrometria de raigs beta, Cosmology, X-rays: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], galaxies: nuclei
Abstract

We present the X-ray spectral analysis of the 1855 extragalactic sources in the Chandra COSMOS-Legacy survey catalog having more than 30 net counts in the 0.5-7 keV band. 38% of the sources are optically classified Type 1 active galactic nuclei (AGN), 60% are Type 2 AGN and 2% are passive, low-redshift galaxies. We study the distribution of AGN photon index and of the intrinsic absorption N(H,z) based on the sources optical classification: Type 1 have a slightly steeper mean photon index than Type 2 AGN, which on the other hand have average intrinsic absorption ~3 times higher than Type 1 AGN. We find that ~15% of Type 1 AGN have N(H,z)>1E22 cm^(-2), i.e., are obscured according to the X-ray spectral fitting; the vast majority of these sources have L(2-10keV)>$1E44 erg/s. The existence of these objects suggests that optical and X-ray obscuration can be caused by different phenomena, the X-ray obscuration being for example caused by dust-free material surrounding the inner part of the nuclei. ~18% of Type 2 AGN have N(H,z), Comment: 23 pages, 16 figures. Accepted for publication on ApJ

Published
2016

12. HSTImaging of the Brightestz∼ 8–9 Galaxies from UltraVISTA: The Extreme Bright End of the UV Luminosity Function

Author

Dan Magee, Adam Muzzin, Bo Milvang-Jensen, Pascal Oesch, Ivo Labbé, Gabriel B. Brammer, Benne W. Holwerda, Karina Caputi, H. J. McCracken, Renske Smit, Garth D. Illingworth, Mauro Stefanon, Olivier Le Fevre, Johan P. U. Fynbo, Marijn Franx, Rychard Bouwens, 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), 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), Astronomy, Smit, Renske [0000-0001-8034-7802], and Apollo - University of Cambridge Repository

Subjects
STELLAR MASSES, formation [galaxies], FOS: Physical sciences, Phot, Astrophysics, Astronomy & Astrophysics, Atomic, 01 natural sciences, HIGH-REDSHIFT GALAXIES, Volume density, Particle and Plasma Physics, Optical imaging, galaxies: high-redshift, galaxies: high, redshift, 0103 physical sciences, STAR-FORMING GALAXIES, PHOTOMETRY, galaxies: formation, Nuclear, 010303 astronomy & astrophysics, evolution [galaxies], luminosity function [galaxies], EVOLUTION SURVEY COSMOS, Physics, Effective radius, high [galaxies], 010308 nuclear & particles physics, HUBBLE DEEP FIELD, REIONIZATION, Molecular, Spectral density, Astronomy and Astrophysics, redshift, Astrophysics - Astrophysics of Galaxies, FORMATION RATES, Galaxy, galaxies: luminosity function, FRONTIER FIELDS, mass function, [SDU]Sciences of the Universe [physics], Space and Planetary Science, DENSITY, Astrophysics of Galaxies (astro-ph.GA), galaxies: luminosity function, mass function, galaxies: evolution, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We report on the discovery of three especially bright candidate $z_{phot} \gtrsim 8$ galaxies. Five sources were targeted for follow-up with HST/WFC3, selected from a larger sample of 16 bright ($24.8 \lesssim H\lesssim25.5$~mag) candidate $z\gtrsim 8$ LBGs identified over the 1.6 degrees$^2$ of the COSMOS/UltraVISTA field. These were identified as Y and J dropouts by leveraging the deep (Y-to-$K_{S} \sim 25.3-24.8$~mag, $5\sigma$) NIR data from the UltraVISTA DR3 release, deep ground based optical imaging from the CFHTLS and Subaru Suprime Cam programs and Spitzer/IRAC mosaics combining observations from the SMUVS and SPLASH programs. Through the refined spectral energy distributions, which now also include new HyperSuprime Cam g, r, i, z and Y band data, we confirm that 3/5 galaxies have robust $z_{phot}\sim8.0-8.7$, consistent with the initial selection. The remaining 2/5 galaxies have a nominal $z_{phot}\sim2$. However, if we use the HST data alone, these objects have increased probability of being at $z\sim9$. Furthermore, we measure mean UV continuum slopes $\beta=-1.91\pm0.26$ for the three $z\sim8-9$ galaxies, marginally bluer than similarly luminous $z\sim4-6$ in CANDELS but consistent with previous measurements of similarly luminous galaxies at $z\sim7$. The circularized effective radius for our brightest source is $0.9\pm0.2$ kpc, similar to previous measurements for a bright $z\sim11$ galaxy and bright $z\sim7$ galaxies. Finally, enlarging our sample to include the six brightest $z\sim8$ LBGs identified over UltraVISTA (i.e., including three other sources from Labbe et al. 2017, in prep.) we estimate for the first time the volume density of galaxies at the extreme bright ($M_{UV}\sim-22$~mag) end of the $z\sim8$ UV LF. Despite this exceptional result, the still large statistical uncertainties do not allow us to discriminate between a Schechter and a double power-law form., Comment: Resubmitting after addressing the referee's comments. Appendix B includes the additional 3 sources from Labbe+2017, used for the LF estimate

Published
2017
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13. 3D-HST WFC3-selected Photometric Catalogs in the Five CANDELS/3D-HST Fields: Photometry, Photometric Redshifts and Stellar Masses

Author

Mariska Kriek, Camilla Pacifici, Gabriel B. Brammer, Danilo Marchesini, Pascal Oesch, Britt Lundgren, Elisabete da Cunha, Shannon G. Patel, Arjen van der Wel, Joel Leja, Rachel Bezanson, Stijn Wuyts, Marijn Franx, Katherine E. Whitaker, Sedona H. Price, Natascha M. Förster Schreiber, David A. Wake, Erica J. Nelson, Rosalind E. Skelton, Ivelina Momcheva, Hans-Walter Rix, Daniel Magee, Mattia Fumagalli, Ivo Labbé, Michael V. Maseda, Tomer Tal, and Pieter G. van Dokkum

Subjects
Point spread function, SIMILAR-TO 2, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, analysis, FOS: Physical sciences, Astrophysics, HUBBLE-DEEP-FIELD, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Imaging data, PASSIVELY EVOLVING GALAXIES, data [methods], Photometry (optics), photometric [techniques], 0103 physical sciences, STAR-FORMING GALAXIES, data analysis [methods], Astrophysics::Solar and Stellar Astrophysics, EXTRAGALACTIC LEGACY SURVEY, 010303 astronomy & astrophysics, YALE-CHILE, evolution [galaxies], Astrophysics::Galaxy Astrophysics, MUSYC, Physics, EVOLUTION SURVEY COSMOS, 010308 nuclear & particles physics, Wavelength range, Astrophysics::Instrumentation and Methods for Astrophysics, STRIP, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Grism, LYMAN-BREAK GALAXIES, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), EXTENDED GROTH, Astrophysics::Earth and Planetary Astrophysics, Derived Data, catalogs, Astrophysics - Cosmology and Nongalactic Astrophysics, general [galaxies]
Abstract

The 3D-HST and CANDELS programs have provided WFC3 and ACS spectroscopy and photometry over ~900 square arcminutes in five fields: AEGIS, COSMOS, GOODS-North, GOODS-South, and the UKIDSS UDS field. All these fields have a wealth of publicly available imaging datasets in addition to the HST data, which makes it possible to construct the spectral energy distributions (SEDs) of objects over a wide wavelength range. In this paper we describe a photometric analysis of the CANDELS and 3D-HST HST imaging and the ancillary imaging data at wavelengths 0.3um to 8um. Objects were selected in the WFC3 near-IR bands, and their SEDs were determined by carefully taking the effects of the point spread function in each observation into account. A total of 147 distinct imaging datasets were used in the analysis. The photometry is made available in the form of six catalogs: one for each field, as well as a master catalog containing all objects in the entire survey. We also provide derived data products: photometric redshifts, determined with the EAZY code, and stellar population parameters determined with the FAST code. We make all the imaging data that were used in the analysis available, including our reductions of the WFC3 imaging in all five fields. 3D-HST is a spectroscopic survey with the WFC3 and ACS grisms, and the photometric catalogs presented here constitute a necessary first step in the analysis of these grism data. All the data presented in this paper are available through the 3D-HST website., Comment: Catalogs and images described are publicly available at the 3D-HST website: http://3dhst.research.yale.edu. v2: Updated to match version accepted by ApJS. v3: Added to acknowledgements

Published
2014
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14. The Star Formation History of Mass-selected Galaxies in the COSMOS Field

Author

Vernesa Smolčić, Olivier Ilbert, Chris Carilli, Mark Sargent, Alexander Karim, Anton M. Koekemoer, Maurilio Pannella, Arjen van der Wel, A. Martinez-Sansigre, Eva Schinnerer, Mara Salvato, Eric F. Bell, and Hans-Walter Rix

Subjects
ACTIVE GALACTIC NUCLEI, Cosmology and Nongalactic Astrophysics (astro-ph.CO), LESS-THAN 2, FOS: Physical sciences, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Flattening, HIGH-REDSHIFT GALAXIES, surveys, galaxies: evolution, galaxies: star formation, radio continuum: galaxies, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, QB, Physics, EVOLUTION SURVEY COSMOS, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, Galaxy, galaxies [radio continuum], LYMAN-BREAK GALAXIES, Physics and Astronomy, Space and Planetary Science, COLOR-MAGNITUDE DIAGRAM, FUNCTIONS, INFRARED LUMINOSITY, FORMATION RATE DENSITY, star formation [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We explore the evolution of the specific star formation rate (SSFR) for 3.6um-selected galaxies of different M_* in the COSMOS field. The average SFR for sub-sets of these galaxies is estimated with stacked 1.4GHz radio continuum emission. We separately consider the total sample and a subset of galaxies (SF) that shows evidence for substantive recent star formation in the rest-frame optical SED. At 0.22, at least above 4x10^10M_Sun where our conclusions are most robust. We find a tight correlation with power-law dependence, SSFR (M_*)^beta, between SSFR and M_* at all z. It tends to flatten below ~10^10M_Sun if quiescent galaxies are included; if they are excluded a shallow index beta_SFG -0.4 fits the correlation. On average, higher M_* objects always have lower SSFRs, also among SF galaxies. At z>1.5 there is tentative evidence for an upper SSFR-limit that an average galaxy cannot exceed. It is suggested by a flattening of the SSFR-M_* relation (also for SF sources), but affects massive (>10^10M_Sun) galaxies only at the highest z. Below z=1.5 there thus is no direct evidence that galaxies of higher M_* experience a more rapid waning of their SSFR than lower M_* SF systems. In this sense, the data rule out any strong 'downsizing'. We combine our results with recent measurements of the galaxy (stellar) mass function in order to determine the characteristic mass of a SF galaxy (M_*=10^(10.6\pm0.4)M_Sun). In this sense, too, there is no 'downsizing'. Our analysis constitutes the most extensive SFR density determination with a single technique to z=3. Recent Herschel results are consistent with our results, but rely on far smaller samples., Comment: 37 pages, 14 figures, 7 tables; accepted for publication in the Astrophysical Journal; High resolution versions of all figures available at www.mpia-hd.mpg.de/homes/karim/research.html

Published
2011
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15. The spatial clustering of X-ray selected AGN in the XMM-COSMOS field

Author

E. Zucca, Andrea Comastri, C. Knobel, O. Le Fèvre, S. de la Torre, N. Z. Scoville, Francesca Civano, Fabrizio Fiore, Alexie Leauthaud, J. F. Le Borgne, Roberto Gilli, Chris Impey, L. de Ravel, M. Mignoli, Alessandro Cimatti, F. Lamareille, M. Bolzonella, Roberto Scaramella, Takamitsu Miyaji, G. Zamorani, Günther Hasinger, J. Walcher, Lidia Tasca, M. Fumana, Jean-Paul Kneib, P. Memeo, V. Le Brun, D. Maccagni, Angela Bongiorno, K. Kovac, S. Bardelli, Christian Maier, M. Scodeggio, Daniela Vergani, Nico Cappelluti, P. Franzetti, Christian Marinoni, H. J. McCracken, D. Bottini, A. Iovino, P. Kampczyk, E. Perez Montero, Olga Cucciati, Laurence Tresse, R. Pello, Jonathan R. Trump, Y. Peng, Luigi Guzzo, E. Ricciardelli, Emanuele Daddi, Cristiano Porciani, Cristian Vignali, Thierry Contini, Mara Salvato, Masayuki Tanaka, Alexis Finoguenov, Graziano Coppa, Paolo Cassata, Lucia Pozzetti, John D. Silverman, Vincenzo Mainieri, Peter Capak, C. M. Carollo, Marcella Brusa, Bianca Garilli, B. Meneux, Simon J. Lilly, Karina Caputi, Alvio Renzini, Pascal Oesch, A. Cappi, U. Abbas, Yoshiaki Taniguchi, Astronomy, California Institute of Technology (CALTECH), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 6207 (CPT), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), R. Gilli, G. Zamorani, T. Miyaji, J. Silverman, M. Brusa, V. Mainieri, N. Cappelluti, E. Daddi, C. Porciani, L. Pozzetti, F. Civano, A. Comastri, A. Finoguenov, F. Fiore, M. Salvato, C. Vignali, G. Hasinger, S. Lilly, C. Impey, J. Trump, P. Capak, H. McCracken, N. Scoville, Y. Taniguchi, C.M. Carollo, T. Contini, J.-P. Kneib, O. LeFevre, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, A. Cimatti, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovac, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello', Y. Peng, E. Perez Montero, E. Ricciardelli, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, E. Zucca, U. Abba, D. Bottini, A. Cappi, P. Cassata, M. Fumana, L. Guzzo, A. Leauthaud, D. Maccagni, C. Marinoni, P. Memeo, B. Meneux, P. Oesch, R. Scaramella, and J. Walcher

Subjects
QSOS, ACTIVE GALACTIC NUCLEI, Stellar mass, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, 2-POINT CORRELATION-FUNCTION, Large-scale structure of universe, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, Luminosity, SUPERMASSIVE BLACK-HOLES, GALAXY REDSHIFT SURVEY, 0103 physical sciences, STAR-FORMING GALAXIES, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, EVOLUTION SURVEY COSMOS, galaxies: active – cosmology: large-scale structure of Universe – cosmology: observations – X-rays: galaxies, 010308 nuclear & particles physics, Cosmology, Cosmology: observations, Galaxies: active, X-rays: galaxies, Astronomy and Astrophysics, Space and Planetary Science, POINT-SOURCE CATALOGS, cosmology: large-scale structure of Universe, Universe, Galaxy, Redshift, Correlation function (statistical mechanics), LUMINOSITY FUNCTION, cosmology: observations, DIGITAL SKY SURVEY, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], ANGULAR-CORRELATION
Abstract

We study the spatial clustering of 538 X-ray selected AGN in the 2 deg^2 XMM-COSMOS field that are spectroscopically identified to I_{AB} 3 x 10^{10} M_sun) at the same redshift. This suggests that AGN at z~1 are preferentially hosted by massive galaxies, as observed both in the local and in the distant (z~2) Universe. (shortened), Comment: 16 pages, 11 figures; accepted for publication in A&A. Language edited version

Published
2009
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16. X-ray groups of galaxies at 0.5 < z < 1 in zCOSMOS: Increased AGN activities in high redshift groups

Author

Masayuki Tanaka, Marco Scodeggio, P. Nair, John D. Silverman, Pascal Oesch, Angela Bongiorno, Alexis Finoguenov, E. Perez Montero, Graziano Coppa, A. Iovino, Niraj Welikala, E. Zucca, O. Cucciati, Vincenzo Mainieri, S. de la Torre, S. J. Lilly, L. de Ravel, O. Le Fevre, Jean-Paul Kneib, C. M. Carollo, Anton M. Koekemoer, J. F. Le Borgne, Michele Moresco, P. Kampczyk, M. Bolzonella, Lucia Pozzetti, Y. Peng, T. Contini, Katarina Kovac, Alvio Renzini, R. Pello, P. Franzetti, V. Le Brun, Andrea Cimatti, M. Mignoli, Karina Caputi, Rongmon Bordoloi, S. Bardelli, A. Cappi, L. A. M. Tasca, B. Garilli, L. Tresse, C. Knobel, V. Presotto, C. Lopez-Sanjuan, F. Lamareille, Luke A. Barnes, Christian Maier, G. Zamorani, H. J. McCracken, D. Vergani, Astronomy, 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), Tanaka Masayuki, Finoguenov Alexi, Lilly Simon J., Bolzonella Micol, Carollo C. Marcella, Contini Thierry, Iovino Angela, Kneib Jean-Paul, Lamareille Fabrice, Le Fevre Olivier, Mainieri Vincenzo, Presotto Valentina, Renzini Alvio, Scodeggio Marco, Silverman John D., Zamorani Gianni, Bardelli Sandro, Bongiorno Angela, Caputi Karina, Cucciati Olga, de la Torre Sylvain, de Ravel Loic, Franzetti Paolo, Garilli Bianca, Kampczyk Pawel, Knobel Christian, Kovac Katarina, Le Borgne Jean-Francoi, Le Brun Vincent, López-Sanjuan Carlo, Maier Christian, Mignoli Marco, Pello Roser, Peng Yingjie, Perez-Montero Enrique, Tasca Lidia, Tresse Laurence, Vergani Daniela, Zucca Elena, Barnes Luke, Bordoloi Rongmon, Cappi Alberto, Cimatti Andrea, Coppa Graziano, Koekemoer Anton M., McCracken Henry J., Moresco Michele, Nair Preethi, Oesch Pascal, Pozzetti Lucia, and Welikala Niraj

Subjects
Active galactic nucleus, 010504 meteorology & atmospheric sciences, Stellar population, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Astrophysical investigations, Photometry (optics), surveys, 0103 physical sciences, LARGE-SCALE STRUCTURE, COLOR-MAGNITUDE RELATION, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, STAR-FORMATION HISTORIES, Physics, EVOLUTION SURVEY COSMOS, Group membership, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, BAND OPTICAL-PROPERTIES, Galaxy, Redshift, PANORAMIC H-ALPHA, RED-SEQUENCE GALAXIES, Space and Planetary Science, galaxies: clusters: general, DIGITAL SKY SURVEY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: evolution, MORPHOLOGY-DENSITY RELATION, Astrophysics - Cosmology and Nongalactic Astrophysics, WIDE-FIELD SURVEY
Abstract

We present a photometric and spectroscopic study of galaxies at 0.5, Comment: 11 pages, 7 figures, accepted for publication in PASJ

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17. The Chandra COSMOS Legacy survey: overview and point source catalog

Author

Meg Urry, Antonella Fruscione, Giorgio Lanzuisi, Heng Hao, Takamitsu Miyaji, Fiona A. Harrison, Nico Cappelluti, Andrea Comastri, Peter Capak, S. Marchesi, Günther Hasinger, Eva Schinnerer, Tom Aldcroft, Sune Toft, Daniel Stern, Jeyhan S. Kartaltepe, Alexander Karim, Cristian Vignali, Roberto Gilli, Vernesa Smolčić, Simonetta Puccetti, B. Trakhenbrot, F. Civano, Ezequiel Treister, N. J. Scoville, G. Zamorani, Knud Jahnke, Alexis Finoguenov, Mara Salvato, Martin Elvis, Marcella Brusa, Mark Sargent, K. Glotfelty, John D. Silverman, David M. Alexander, Viola Allevato, Fabrizio Fiore, Hermann Brunner, Stephanie M. LaMassa, Richard E. Griffiths, Piero Ranalli, Kevin Schawinski, ITA, USA, GBR, DEU, CHL, HRV, DNK, FIN, JPN, GRC, MEX, CHE, Civano, F., Marchesi, S., Comastri, A., Urry, M.C., Elvis, M., Cappelluti, N., Puccetti, S., Brusa, M., Zamorani, G., Hasinger, G., Aldcroft, T., Alexander, D.M., Allevato, V., Brunner, H., Capak, P., Finoguenov, A., Fiore, F., Fruscione, A., Gilli, R., Glotfelty, K., Griffiths, R.E., Hao, H., Harrison, F.A., Jahnke, K., Kartaltepe, J., Karim, A., Lamassa, S.M., Lanzuisi, G., Miyaji, T., Ranalli, P., Salvato, M., Sargent, M., Scoville, N.J., Schawinski, K., Schinnerer, E., Silverman, J., Smolcic, V., Stern, D., Toft, S., Trakhenbrot, B., Treister, E., Vignali, C., Department of Physics, Urry, M. C., Alexander, D. M., Griffiths, R. E., Harrison, F. A., Lamassa, S. M., and Scoville, N. J.

Subjects
ACTIVE GALACTIC NUCLEI, catalog, PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, Point source, catalogs, cosmology: observations, galaxies: evolution, quasars: general, surveys, X-rays: general, FOS: Physical sciences, Astrophysics, 01 natural sciences, X-RAY SURVEY, general [X-rays], 0103 physical sciences, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, survey, STRIPE 82, NUMBER COUNTS, 010303 astronomy & astrophysics, evolution [galaxies], QB, Physics, EVOLUTION SURVEY COSMOS, MS SOURCE CATALOGS, XMM-NEWTON, cosmology: observation, general [quasars], 010308 nuclear & particles physics, Hardness ratio, Astronomy and Astrophysics, Limiting, Astronomy and Astrophysic, LOG S, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, observations [cosmology], Large sample, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), BLACK-HOLE, observation [cosmology], WIDE-FIELD SURVEY
Abstract

The COSMOS-Legacy survey is a 4.6 Ms Chandra program that has imaged 2.2 deg$^2$ of the COSMOS field with an effective exposure of $\simeq$160 ks over the central 1.5 deg$^2$ and of $\simeq$80 ks in the remaining area. The survey is the combination of 56 new observations, obtained as an X-ray Visionary Project, with the previous C-COSMOS survey. We describe the reduction and analysis of the new observations and the properties of 2273 point sources detected above a spurious probability of 2$\times 10^{-5}$. We also present the updated properties of the C-COSMOS sources detected in the new data. The whole survey includes 4016 point sources (3814, 2920 and 2440 in the full, soft and hard band). The limiting depths are 2.2 $\times$ 10$^{-16}$, 1.5 $\times$ 10$^{-15}$ and 8.9$\times$ 10$^{-16}$ ${\rm erg~cm}^{-2}~{\rm s}^{-1}$ in the 0.5-2, 2-10 and 0.5-10 keV bands, respectively. The observed fraction of obscured AGN with column density $> 10^{22}$ cm$^{-2}$ from the hardness ratio (HR) is $\sim$50$^{+17}_{-16}$%. Given the large sample, we compute source number counts in the hard and soft bands, significantly reducing the uncertainties of 5-10%. For the first time, we compute number counts for obscured (HR$>$-0.2) and unobscured (HR$, Comment: 20 pages, 16 figures, accepted for publication on ApJ on December 24, 2015

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18. The Stellar-to-halo Mass Ratios of Passive and Star-forming Galaxies at z ∼ 2–3 from the SMUVS Survey

Author

Giovanni G. Fazio, Olivier Le Fevre, S. Deshmukh, Olivier Ilbert, Bo Milvang-Jensen, Karina Caputi, Matthew L. N. Ashby, Johan P. U. Fynbo, W. I. Cowley, Astronomy, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cold dark matter, 010504 meteorology & atmospheric sciences, Stellar mass, Dark matter, FOS: Physical sciences, STATISTICAL-ANALYSIS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, DARK-MATTER, Satellite galaxy, galaxies: formation, RED SEQUENCE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminosity function (astronomy), large-scale structure of universe, EVOLUTION SURVEY COSMOS, Physics, methods: statistical, ENVIRONMENT RELATIONSHIPS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ULTRA DEEP SURVEY, Accretion (astrophysics), Galaxy, MODEL, RESOLUTION, [SDU]Sciences of the Universe [physics], LUMINOSITY FUNCTION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DIGITAL SKY SURVEY, Halo, galaxies: evolution
Abstract

In this work, we use measurements of galaxy stellar mass and two-point angular correlation functions to constrain the stellar-to-halo mass ratios (SHMRs) of passive and \np\ galaxies at $z\sim2-3$, as identified in the \emph{Spitzer} Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS). We adopt a sophisticated halo modeling approach to statistically divide our two populations into central and satellite galaxies. For central galaxies, we find that the normalization of the SHMR is greater for our passive population. Through the modeling of $\Lambda$ cold dark matter halo mass accretion histories, we show that this can only arise if the conversion of baryons into stars was more efficient at higher redshifts and additionally that passive galaxies can be plausibly explained as residing in halos with the highest formation redshifts (i.e., those with the lowest accretion rates) at a given halo mass. At a fixed stellar mass, satellite galaxies occupy host halos with a greater mass than central galaxies, and we find further that the fraction of passive galaxies that are satellites is higher than for the combined population. This, and our derived satellite quenching timescales, combined with earlier estimates from the literature, support dynamical/environmental mechanisms as the dominant process for satellite quenching at $z\lesssim3$., Comment: 17 pages, 9 Figures, 1 Table. Accepted for publication in ApJ. Minor changes to previous version

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