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1. The zCOSMOS survey

Author

Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova, #269, Lilly S., Tresse L., Tasca L., Cassata P., Halliday C., Vergani D., Caputi K., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., Coppa G., 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., Abbas U., Bottini D., Cappi A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, MORESCO, MICHELE ENNIO MARIA, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (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), INAF- Milano, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Tokai University, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], California Institute of Technology (CALTECH), Sea Mammal Research Unit, St Andrews, Astronomy, Zucca E., Bardelli S., Bolzonella M., Zamorani G., Ilbert O., Pozzetti L., Mignoli M., Kova&#269, K., Lilly S., Tresse L., Tasca L., Cassata P., Halliday C., Vergani D., Caputi K., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Scodeggio M., Bongiorno A., 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., Abbas U., Bottini D., Cappi A., Cimatti A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Meme, P., Meneux B., Moresco M., Oesch P., Porciani C., Scaramella R., Arnouts S., Aussel H., Capak P., Kartaltepe J., Salvato M., Sanders D., Scoville N., Taniguchi Y., Thompson D., Università di Bologna, Dipartimento di Astronomia, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-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, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, 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
Normalization (statistics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), High density, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MORPHOLOGICAL CLASSIFICATION, 1ST EPOCH DATA, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Density field, FIELD, 10. No inequality, 010303 astronomy & astrophysics, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, galaxies: statistics, Luminosity function (astronomy), Physics, REDSHIFT SURVEY, LEGACY SURVEY, 010308 nuclear & particles physics, Galaxies: evolution, Galaxies: luminosity function, mass function, Galaxies: statistics, Astronomy and Astrophysics, Space and Planetary Science, VLT DEEP SURVEY, B band, Galaxy, galaxies: luminosity function, mass function, COLOR-DENSITY RELATION, galaxies: luminosity function, mass function, DIGITAL SKY SURVEY, galaxies: evolution, Cosmic time, SURVEY COSMOS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

(Abridged) We studied the evolution in the B band luminosity function to z~1 in the zCOSMOS 10k sample, for which both accurate galaxy classifications and a detailed description of the local density field are available. The global LF exhibits a brightening of ~0.7 mag in M* from z~0.2 to z~0.9. At low z, late types dominate at faint magnitudes, while the bright end is populated mainly by early types. At higher z, late-type galaxies evolve significantly and, at z~1, the contribution from the various types to the bright end of the LF is comparable. The evolution for early types is in both luminosity and normalization. A similar behaviour is exhibited by late types, but with an opposite trend for the normalization. Studying the role of the environment, we find that the global LF of galaxies in overdense regions has always a brighter M* and a flatter slope. In low density environments, the main contribution to the LF is from blue galaxies, while for high density environments there is an important contribution from red galaxies to the bright end. The differences between the global LF in the two environments are not due to only a difference in the relative numbers of red and blue galaxies, but also to their relative luminosity distributions: the value of M* for both types in underdense regions is always fainter than in overdense environments. The "specular" evolution of late- and early-type galaxies is consistent with a scenario where a part of blue galaxies is transformed in red galaxies with increasing cosmic time, without significant changes in the fraction of intermediate-type galaxies. The bulk of this tranformation in overdense regions probably happened before z~1, while it is still ongoing at lower z in underdense environments., Comment: 18 pages, 10 figures, A&A in press

Published
2009
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2. Tracking the impact of environment on the galaxy stellar mass function up to z ∼ 1 in the 10 k zCOSMOS sample

Author

Bolzonella M., Kova, #269, Pozzetti L., Zucca E., Lilly S. J., Peng Y., Iovino A., Zamorani G., Vergani D., Tasca L. A. M., Lamareille F., Oesch P., Caputi K., Kampczyk P., Bardelli S., Maier C., Abbas U., Knobel C., Scodeggio M., Carollo C. M., Contini T., Kneib J. P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J. F., Le Brun V., Mignoli M., Pelló R., Perez Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Bottini D., Cappi A., Cassata P., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Aussel H., Capak P., Halliday C., Ilbert O., Kartaltepe J., Salvato M., Sanders D., Scarlata C., Scoville N., Taniguchi Y., Thompson D., CUCCIATI, OLGA, CIMATTI, ANDREA, Bolzonella M., Kova&#269, K., Pozzetti L., Zucca E., Cucciati O., Lilly S. J., Peng Y., Iovino A., Zamorani G., Vergani D., Tasca L. A. M., Lamareille F., Oesch P., Caputi K., Kampczyk P., Bardelli S., Maier C., Abbas U., Knobel C., Scodeggio M., Carollo C. M., Contini T., Kneib J.-P., Le Fèvre O., Mainieri V., Renzini A., Bongiorno A., Coppa G., de la Torre S., de Ravel L., Franzetti P., Garilli B., Le Borgne J.-F., Le Brun V., Mignoli M., Pelló R., Perez-Montero E., Ricciardelli E., Silverman J. D., Tanaka M., Tresse L., Bottini D., Cappi A., Cassata P., Cimatti A., Guzzo L., Koekemoer A. M., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Porciani C., Scaramella R., Aussel H., Capak P., Halliday C., Ilbert O., Kartaltepe J., Salvato M., Sanders D., Scarlata C., Scoville N., Taniguchi Y., Thompson D., INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF- Milano, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Brera (OAB), 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), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (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), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Human Genetics Center, The University of Texas Health Science Center at Houston (UTHealth), School of Biotechnology and Biomolecular Sciences, University of New South Wales [Sydney] (UNSW), Space Telescope Science Institute (STSci), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Materials & Process technology, Boeing Company [Chicago], Sea Mammal Research Unit, St Andrews, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-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, 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), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Galaxy formation and evolution, Density contrast, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, galaxies: fundamental parameters, Astronomy and Astrophysics, Redshift, Galaxy, Bimodality, galaxies: luminosity function, mass function, Space and Planetary Science, cosmology: observations, galaxies: evolution, galaxies: luminosity function, mass function, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the impact of the environment on the evolution of galaxies in the zCOSMOS 10k sample in the redshift range 0.1, Comment: 17 pages, 11 figures. Version accepted for publication in Astronomy and Astrophysics, including referee's suggestions, a new section with comparison with literature data, and updated references

Published
2010
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3. Extended Lymanαhaloes around individual high-redshift galaxies revealed by MUSE

Author

Wisotzki, L., primary, Bacon, R., additional, Blaizot, J., additional, Brinchmann, J., additional, Herenz, E. C., additional, Schaye, J., additional, Bouché, N., additional, Cantalupo, S., additional, Contini, T., additional, Carollo, C. M., additional, Caruana, J., additional, Courbot, J.-B., additional, Emsellem, E., additional, Kamann, S., additional, Kerutt, J., additional, Leclercq, F., additional, Lilly, S. J., additional, Patrício, V., additional, Sandin, C., additional, Steinmetz, M., additional, Straka, L. A., additional, Urrutia, T., additional, Verhamme, A., additional, Weilbacher, P. M., additional, and Wendt, M., additional

Published
2016
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4. Extreme emission-line galaxies out toz~ 1 in zCOSMOS

Author

Amorín, R., primary, Pérez-Montero, E., additional, Contini, T., additional, Vílchez, J. M., additional, Bolzonella, M., additional, Tasca, L. A. M., additional, Lamareille, F., additional, Zamorani, G., additional, Maier, C., additional, Carollo, C. M., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Lilly, S., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Bongiorno, A., additional, Caputi, K., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Mignoli, M., additional, Pellò, R., additional, Peng, Y., additional, Presotto, V., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tresse, L., additional, Vergani, D., additional, and Zucca, E., additional

Published
2015
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5. Passive galaxies as tracers of cluster environments atz~ 2

Author

Strazzullo, V., primary, Daddi, E., additional, Gobat, R., additional, Garilli, B., additional, Mignoli, M., additional, Valentino, F., additional, Onodera, M., additional, Renzini, A., additional, Cimatti, A., additional, Finoguenov, A., additional, Arimoto, N., additional, Cappellari, M., additional, Carollo, C. M., additional, Feruglio, C., additional, Le Floc’h, E., additional, Lilly, S. J., additional, Maccagni, D., additional, McCracken, H. J., additional, Moresco, M., additional, Pozzetti, L., additional, and Zamorani, G., additional

Published
2015
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6. The MUSE 3D view of theHubbleDeep Field South

Author

Bacon, R., primary, Brinchmann, J., additional, Richard, J., additional, Contini, T., additional, Drake, A., additional, Franx, M., additional, Tacchella, S., additional, Vernet, J., additional, Wisotzki, L., additional, Blaizot, J., additional, Bouché, N., additional, Bouwens, R., additional, Cantalupo, S., additional, Carollo, C. M., additional, Carton, D., additional, Caruana, J., additional, Clément, B., additional, Dreizler, S., additional, Epinat, B., additional, Guiderdoni, B., additional, Herenz, C., additional, Husser, T.-O., additional, Kamann, S., additional, Kerutt, J., additional, Kollatschny, W., additional, Krajnovic, D., additional, Lilly, S., additional, Martinsson, T., additional, Michel-Dansac, L., additional, Patricio, V., additional, Schaye, J., additional, Shirazi, M., additional, Soto, K., additional, Soucail, G., additional, Steinmetz, M., additional, Urrutia, T., additional, Weilbacher, P., additional, and de Zeeuw, T., additional

Published
2015
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7. The zCOSMOS redshift survey: evolution of the light in bulges and discs sincez~ 0.8

Author

Tasca, L. A. M., primary, Tresse, L., additional, Le Fèvre, O., additional, Ilbert, O., additional, Lilly, S. J., additional, Zamorani, G., additional, López-Sanjuan, C., additional, Ho, L. C., additional, Bardelli, S., additional, Cattaneo, A., additional, Cucciati, O., additional, Farrah, D., additional, Iovino, A., additional, Koekemoer, A. M., additional, Liu, C. T., additional, Massey, R., additional, Renzini, A., additional, Taniguchi, Y., additional, Welikala, N., additional, Zucca, E., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Mainieri, V., additional, Scodeggio, M., additional, Bolzonella, M., additional, Bongiorno, A., additional, Caputi, K., additional, de la Torre, S., additional, Franzetti, P., additional, Garilli, B., additional, Guzzo, L., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Mignoli, M., additional, Pello, R., additional, Peng, Y., additional, Perez Montero, E., additional, Rich, R. M., additional, Tanaka, M., additional, Vergani, D., additional, Bordoloi, R., additional, Cappi, A., additional, Cimatti, A., additional, Coppa, G., additional, McCracken, H. J., additional, Moresco, M., additional, Pozzetti, L., additional, Sanders, D., additional, and Sheth, K., additional

Published
2014
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8. Spot the difference

Author

Moresco, M., primary, Pozzetti, L., additional, Cimatti, A., additional, Zamorani, G., additional, Bolzonella, M., additional, Lamareille, F., additional, Mignoli, M., additional, Zucca, E., additional, Lilly, S. J., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Bongiorno, A., additional, Caputi, K., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pelló, R., additional, Peng, Y., additional, Perez-Montero, E., additional, Presotto, V., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Barnes, L., additional, Bordoloi, R., additional, Cappi, A., additional, Diener, C., additional, Koekemoer, A. M., additional, Le Floc’h, E., additional, López-Sanjuan, C., additional, McCracken, H. J., additional, Nair, P., additional, Oesch, P., additional, Scarlata, C., additional, Scoville, N., additional, and Welikala, N., additional

Published
2013
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9. Obscured AGN atz ~ 1 from the zCOSMOS-Bright Survey

Author

Mignoli, M., primary, Vignali, C., additional, Gilli, R., additional, Comastri, A., additional, Zamorani, G., additional, Bolzonella, M., additional, Bongiorno, A., additional, Lamareille, F., additional, Nair, P., additional, Pozzetti, L., additional, Lilly, S. J., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Caputi, K., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pellò, R., additional, Peng, Y., additional, Perez Montero, E., additional, Presotto, V., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Zucca, E., additional, Bordoloi, R., additional, Cappi, A., additional, Cimatti, A., additional, Koekemoer, A. M., additional, McCracken, H. J., additional, Moresco, M., additional, and Welikala, N., additional

Published
2013
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10. Investigating the relationship between AGN activity and stellar mass in zCOSMOS galaxies at 0 < z < 1 using emission-line diagnostic diagrams

Author

Vitale, M., primary, Mignoli, M., additional, Cimatti, A., additional, Lilly, S. J., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fevre, O., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Zamorani, G., additional, Bardelli, S., additional, Barnes, L., additional, Bolzonella, M., additional, Bongiorno, A., additional, Bordoloi, R., additional, Bschorr, T. J., additional, Cappi, A., additional, Caputi, K., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Koekemoer, A. M., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, López-Sanjuan, C., additional, Maier, C., additional, McCracken, H. J., additional, Moresco, M., additional, Nair, P., additional, Oesch, P. A., additional, Pello, R., additional, Peng, Y., additional, Pérez Montero, E., additional, Pozzetti, L., additional, Presotto, V., additional, Silverman, J., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Welikala, N., additional, and Zucca, E., additional

Published
2013
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11. The cosmic evolution of oxygen and nitrogen abundances in star-forming galaxies over the past 10 Gyr

Author

Pérez-Montero, E., primary, Contini, T., additional, Lamareille, F., additional, Maier, C., additional, Carollo, C. M., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Lilly, S., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Zamorani, G., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Caputi, K., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Mignoli, M., additional, Pellò, R., additional, Peng, Y., additional, Presotto, V., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L. A. M., additional, Tresse, L., additional, Vergani, D., additional, and Zucca, E., additional

Published
2012
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12. The dominant role of mergers in the size evolution of massive early-type galaxies sincez ~ 1

Author

López-Sanjuan, C., primary, Le Fèvre, O., additional, Ilbert, O., additional, Tasca, L. A. M., additional, Bridge, C., additional, Cucciati, O., additional, Kampczyk, P., additional, Pozzetti, L., additional, Xu, C. K., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Lilly, S. J., additional, Mainieri, V., additional, Renzini, A., additional, Sanders, D., additional, Scodeggio, M., additional, Scoville, N. Z., additional, Taniguchi, Y., additional, Zamorani, G., additional, Aussel, H., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Capak, P., additional, Caputi, K., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Le Floc’h, E., additional, Maier, C., additional, McCracken, H. J., additional, Mignoli, M., additional, Pelló, R., additional, Peng, Y., additional, Pérez-Montero, E., additional, Presotto, V., additional, Ricciardelli, E., additional, Salvato, M., additional, Silverman, J. D., additional, Tanaka, M., additional, Tresse, L., additional, Vergani, D., additional, Zucca, E., additional, Barnes, L., additional, Bordoloi, R., additional, Cappi, A., additional, Cimatti, A., additional, Coppa, G., additional, Koekemoer, A., additional, Liu, C. T., additional, Moresco, M., additional, Nair, P., additional, Oesch, P., additional, Schawinski, K., additional, and Welikala, N., additional

Published
2012
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13. A journey from the outskirts to the cores of groups

Author

Presotto, V., primary, Iovino, A., additional, Scodeggio, M., additional, Cucciati, O., additional, Knobel, C., additional, Bolzonella, M., additional, Oesch, P., additional, Finoguenov, A., additional, Tanaka, M., additional, Kovač, K., additional, Peng, Y., additional, Zamorani, G., additional, Bardelli, S., additional, Pozzetti, L., additional, Kampczyk, P., additional, López-Sanjuan, C., additional, Vergani, D., additional, Zucca, E., additional, Tasca, L. A. M., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Lilly, S., additional, Mainieri, V., additional, Renzini, A., additional, Bongiorno, A., additional, Caputi, K., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Mignoli, M., additional, Pellò, R., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tresse, L., additional, Barnes, L., additional, Bordoloi, R., additional, Cappi, A., additional, Cimatti, A., additional, Coppa, G., additional, Koekemoer, A. M., additional, McCracken, H. J., additional, Moresco, M., additional, Nair, P., additional, and Welikala, N., additional

Published
2012
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14. The bimodality of the 10k zCOSMOS-bright galaxies up toz ~ 1: a new statistical and portable classification based on optical galaxy properties

Author

Coppa, G., primary, Mignoli, M., additional, Zamorani, G., additional, Bardelli, S., additional, Lilly, S. J., additional, Bolzonella, M., additional, Scodeggio, M., additional, Vergani, D., additional, Nair, P., additional, Pozzetti, L., additional, Cimatti, A., additional, Zucca, E., additional, Carollo, C. M., additional, Contini, T., additional, Le Fèvre, O., additional, Renzini, A., additional, Mainieri, V., additional, Bongiorno, A., additional, Caputi, K. I., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Memeo, P., additional, Iovino, A., additional, Kampczyk, P., additional, Kneib, J.-P., additional, Knobel, C., additional, Koekemoer, A. M., additional, Kovač, K., additional, Lamareille, F., additional, le Borgne, J.-F., additional, le Brun, V., additional, Maier, C., additional, Pellò, R., additional, Peng, Y., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Scarlata, C., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Abbas, U., additional, Bottini, D., additional, Capak, P., additional, Cappi, A., additional, Cassata, P., additional, Fumana, M., additional, Guzzo, L., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, Meneux, B., additional, Oesch, P., additional, Porciani, C., additional, Scaramella, R., additional, and Scoville, N., additional

Published
2011
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15. Tracking the impact of environment on the galaxy stellar mass function up toz ~ 1 in the 10 k zCOSMOS sample

Author

Bolzonella, M., primary, Kovač, K., additional, Pozzetti, L., additional, Zucca, E., additional, Cucciati, O., additional, Lilly, S. J., additional, Peng, Y., additional, Iovino, A., additional, Zamorani, G., additional, Vergani, D., additional, Tasca, L. A. M., additional, Lamareille, F., additional, Oesch, P., additional, Caputi, K., additional, Kampczyk, P., additional, Bardelli, S., additional, Maier, C., additional, Abbas, U., additional, Knobel, C., additional, Scodeggio, M., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Bongiorno, A., additional, Coppa, G., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Mignoli, M., additional, Pelló, R., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tresse, L., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Guzzo, L., additional, Koekemoer, A. M., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Porciani, C., additional, Scaramella, R., additional, Aussel, H., additional, Capak, P., additional, Halliday, C., additional, Ilbert, O., additional, Kartaltepe, J., additional, Salvato, M., additional, Sanders, D., additional, Scarlata, C., additional, Scoville, N., additional, Taniguchi, Y., additional, and Thompson, D., additional

Published
2010
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16. The zCOSMOS 10k-sample: the role of galaxy stellar mass in the colour-density relation up toz ~ 1

Author

Cucciati, O., primary, Iovino, A., additional, Kovač, K., additional, Scodeggio, M., additional, Lilly, S. J., additional, Bolzonella, M., additional, Bardelli, S., additional, Vergani, D., additional, Tasca, L. A. M., additional, Zucca, E., additional, Zamorani, G., additional, Pozzetti, L., additional, Knobel, C., additional, Oesch, P., additional, Lamareille, F., additional, Caputi, K., additional, Kampczyk, P., additional, Tresse, L., additional, Maier, C., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Bongiorno, A., additional, Coppa, G., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Mignoli, M., additional, Pellò, R., additional, Peng, Y., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Koekemoer, A. M., additional, Scoville, N., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Guzzo, L., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Porciani, C., additional, and Scaramella, R., additional

Published
2010
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17. The [O iii] emission line luminosity function of optically selected type-2 AGN from zCOSMOS$^{\rm,}$

Author

Bongiorno, A., primary, Mignoli, M., additional, Zamorani, G., additional, Lamareille, F., additional, Lanzuisi, G., additional, Miyaji, T., additional, Bolzonella, M., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J. P., additional, Le Fèvre, O., additional, Lilly, S. J., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Brusa, M., additional, Caputi, K., additional, Civano, F., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Halliday, C., additional, Hasinger, G., additional, Koekemoer, A. M., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Le Borgne, J. -F., additional, Le Brun, V., additional, Maier, C., additional, Merloni, A., additional, Nair, P., additional, Pello, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Salvato, M., additional, Silverman, J., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Zucca, E., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Guzzo, L., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Porciani, C., additional, Pozzetti, L., additional, and Scaramella, R., additional

Published
2010
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18. Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey

Author

Bardelli, S., primary, Schinnerer, E., additional, Smolčic, V., additional, Zamorani, G., additional, Zucca, E., additional, Mignoli, M., additional, Halliday, C., additional, Kovač, K., additional, Ciliegi, P., additional, Caputi, K., additional, Koekemoer, A. M., additional, Bongiorno, A., additional, Bondi, M., additional, Bolzonella, M., additional, Vergani, D., additional, Pozzetti, L., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Lilly, S., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pellò, R., additional, Peng, Y., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Guzzo, L., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Porciani, C., additional, Scaramella, R., additional, Capak, P., additional, Sanders, D., additional, Scoville, N., additional, Taniguchi, Y., additional, and Jahnke, K., additional

Published
2010
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19. The zCOSMOS redshift survey: how group environment alters global downsizing trends

Author

Iovino, A., primary, Cucciati, O., additional, Scodeggio, M., additional, Knobel, C., additional, Kovač, K., additional, Lilly, S., additional, Bolzonella, M., additional, Tasca, L. A. M., additional, Zamorani, G., additional, Zucca, E., additional, Caputi, K., additional, Pozzetti, L., additional, Oesch, P., additional, Lamareille, F., additional, Halliday, C., additional, Bardelli, S., additional, Finoguenov, A., additional, Guzzo, L., additional, Kampczyk, P., additional, Maier, C., additional, Tanaka, M., additional, Vergani, D., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Bongiorno, A., additional, Coppa, G., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Mignoli, M., additional, Pellò, R., additional, Peng, Y., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tresse, L., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Koekemoer, A. M., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Porciani, C., additional, Scaramella, R., additional, Schiminovich, D., additional, and Scoville, N., additional

Published
2009
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20. K+a galaxies in the zCOSMOS survey

Author

Vergani, D., primary, Zamorani, G., additional, Lilly, S., additional, Lamareille, F., additional, Halliday, C., additional, Scodeggio, M., additional, Vignali, C., additional, Ciliegi, P., additional, Bolzonella, M., additional, Bondi, M., additional, Kovač, K., additional, Knobel, C., additional, Zucca, E., additional, Caputi, K., additional, Pozzetti, L., additional, Bardelli, S., additional, Mignoli, M., additional, Iovino, A., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Bongiorno, A., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Kampczyk, P., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pello, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Guzzo, L., additional, Koekemoer, A. M., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Porciani, C., additional, Scaramella, R., additional, Capak, P., additional, Sanders, D., additional, Scoville, N., additional, and Taniguchi, Y., additional

Published
2009
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21. The zCOSMOS survey: the role of the environment in the evolution of the luminosity function of different galaxy types

Author

Zucca, E., primary, Bardelli, S., additional, Bolzonella, M., additional, Zamorani, G., additional, Ilbert, O., additional, Pozzetti, L., additional, Mignoli, M., additional, Kovač, K., additional, Lilly, S., additional, Tresse, L., additional, Tasca, L., additional, Cassata, P., additional, Halliday, C., additional, Vergani, D., additional, Caputi, K., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Bongiorno, A., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pellò, R., additional, Peng, Y., additional, Perez-Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cimatti, A., additional, Guzzo, L., additional, Koekemoer, A. M., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Moresco, M., additional, Oesch, P., additional, Porciani, C., additional, Scaramella, R., additional, Arnouts, S., additional, Aussel, H., additional, Capak, P., additional, Kartaltepe, J., additional, Salvato, M., additional, Sanders, D., additional, Scoville, N., additional, Taniguchi, Y., additional, and Thompson, D., additional

Published
2009
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22. The zCOSMOS survey. The dependence of clustering on luminosity and stellar mass at $z=0.2$–1

Author

Meneux, B., primary, Guzzo, L., additional, de la Torre, S., additional, Porciani, C., additional, Zamorani, G., additional, Abbas, U., additional, Bolzonella, M., additional, Garilli, B., additional, Iovino, A., additional, Pozzetti, L., additional, Zucca, E., additional, Lilly, S. J., additional, Le Fèvre, O., additional, Kneib, J.-P., additional, Carollo, C. M., additional, Contini, T., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Bongiorno, A., additional, Caputi, K., additional, Coppa, G., additional, Cucciati, O., additional, de Ravel, L., additional, Franzetti, P., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pellò, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Bottini, D., additional, Cappi, A., additional, Cimatti, A., additional, Cassata, P., additional, Fumana, M., additional, Koekemoer, A. M., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Oesch, P., additional, and Scaramella, R., additional

Published
2009
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23. The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Author

Tasca, L. A. M., primary, Kneib, J.-P., additional, Iovino, A., additional, Le Fèvre, O., additional, Kovač, K., additional, Bolzonella, M., additional, Lilly, S. J., additional, Abraham, R. G., additional, Cassata, P., additional, Cucciati, O., additional, Guzzo, L., additional, Tresse, L., additional, Zamorani, G., additional, Capak, P., additional, Garilli, B., additional, Scodeggio, M., additional, Sheth, K., additional, Zucca, E., additional, Carollo, C. M., additional, Contini, T., additional, Mainieri, V., additional, Renzini, A., additional, Bardelli, S., additional, Bongiorno, A., additional, Caputi, K., additional, Coppa, G., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Kampczyk, P., additional, Knobel, C., additional, Koekemoer, A. M., additional, Lamareille, F., additional, Le Borgne, J. -F., additional, Le Brun, V., additional, Maier, C., additional, Mignoli, M., additional, Pello, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Silverman, J. D., additional, Vergani, D., additional, Tanaka, M., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cimatti, A., additional, Ilbert, O., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Porciani, C., additional, Pozzetti, L., additional, Scaramella, R., additional, and Scarlata, C., additional

Published
2009
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24. The spatial clustering of X-ray selected AGN in the XMM-COSMOS field

Author

Gilli, R., primary, Zamorani, G., additional, Miyaji, T., additional, Silverman, J., additional, Brusa, M., additional, Mainieri, V., additional, Cappelluti, N., additional, Daddi, E., additional, Porciani, C., additional, Pozzetti, L., additional, Civano, F., additional, Comastri, A., additional, Finoguenov, A., additional, Fiore, F., additional, Salvato, M., additional, Vignali, C., additional, Hasinger, G., additional, Lilly, S., additional, Impey, C., additional, Trump, J., additional, Capak, P., additional, McCracken, H., additional, Scoville, N., additional, Taniguchi, Y., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fevre, O., additional, Renzini, A., additional, Scodeggio, M., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Caputi, K., additional, Cimatti, A., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Mignoli, M., additional, Pellò, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Zucca, E., additional, Abbas, U., additional, Bottini, D., additional, Cappi, A., additional, Cassata, P., additional, Fumana, M., additional, Guzzo, L., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Scaramella, R., additional, and Walcher, J., additional

Published
2008
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25. The zCOSMOS redshift survey: the three-dimensional classification cube and bimodality in galaxy physical properties

Author

Mignoli, M., primary, Zamorani, G., additional, Scodeggio, M., additional, Cimatti, A., additional, Halliday, C., additional, Lilly, S. J., additional, Pozzetti, L., additional, Vergani, D., additional, Carollo, C. M., additional, Contini, T., additional, Le Févre, O., additional, Mainieri, V., additional, Renzini, A., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Caputi, K., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Iovino, A., additional, Kampczyk, P., additional, Kneib, J.-P., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Maier, C., additional, Pellò, R., additional, Peng, Y., additional, Perez Montero, E., additional, Ricciardelli, E., additional, Scarlata, C., additional, Silverman, J. D., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Zucca, E., additional, Abbas, U., additional, Bottini, D., additional, Capak, P., additional, Cappi, A., additional, Cassata, P., additional, Fumana, M., additional, Guzzo, L., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H. J., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Porciani, C., additional, Scaramella, R., additional, and Scoville, N., additional

Published
2008
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26. Supermassive black holes in the Sbc spiral galaxies NGC 3310, NGC 4303 and NGC 4258

Author

Pastorini, G., primary, Marconi, A., additional, Capetti, A., additional, Axon, D. J., additional, Alonso-Herrero, A., additional, Atkinson, J., additional, Batcheldor, D., additional, Carollo, C. M., additional, Collett, J., additional, Dressel, L., additional, Hughes, M. A., additional, Macchetto, D., additional, Maciejewski, W., additional, Sparks, W., additional, and van der Marel, R., additional

Published
2007
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27. Extreme emission-line galaxies out to z ~ 1 in zCOSMOS.

Author

Amorín, R., Pérez-Montero, E., Contini, T., Vílchez, J. M., Bolzonella, M., Tasca, L. A. M., Lamareille, F., Zamorani, G., Maier, C., Carollo, C. M., Kneib, J.-P., Le Fèvre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., and Cucciati, O.

Subjects
EMISSION-line galaxies, GALACTIC evolution, STARBURSTS, GALACTIC redshift, LOW mass stars, STELLAR mass, ASTRONOMICAL photometry
Abstract

Context. The study of large and representative samples of low-metallicity star-forming galaxies at different cosmic epochs is of great interest to the detailed understanding of the assembly history and evolution of low-mass galaxies. Aims. We present a thorough characterization of a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 ≤ z ≤ 0.93 selected from the 20k zCOSMOS bright survey because of their unusually large emission line equivalent widths. Methods. We use multiwavelength COSMOS photometry, HST-ACS I-band imaging, and optical zCOSMOS spectroscopy to derive the main global properties of star-forming EELGs, such as sizes, stellar masses, star formation rates (SFR), and reliable oxygen abundances using both Â"directÂ" and Â"strong-lineÂ" methods. Results. The EELGs are extremely compact (r50 ~ 1.3 kpc), low-mass (M* ~ 107-1010 M⊙) galaxies forming stars at unusually high specific star formation rates (sSFR = SFR/M* up to 10-7 yr-1) compared to main sequence star-forming galaxies of the same stellar mass and redshift. At rest-frame UV wavelengths, the EELGs are luminous and show high surface brightness and include strong Lya emitters, as revealed by GALEX spectroscopy. We show that zCOSMOS EELGs are high-ionization, low-metallicity systems, with median 12+ log(O/H) = 8.16 ± 0.21 (0.2 ⊙) including a handful of extremely metal-deficient (<0.1 Z⊙) EELGs. While ~80% of the EELGs show non-axisymmetric morphologies, including clumpy and cometary or tadpole galaxies, we find that ~29% of them show additional low-surface-brightness features, which strongly suggests recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are most often found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. Conclusions. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building up a significant fraction of their present-day stellar mass in an ongoing, galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low- and high-redshift low-mass star-forming galaxies. [ABSTRACT FROM AUTHOR]

Published
2015
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28. The MUSE 3D view of the Hubble Deep Field South.

Author

Bacon, R., Brinchmann, J., Richard, J., Contini, T., Drake, A., Franx, M., Tacchella, S., Vernet, J., Wisotzki, L., Blaizot, J., Bouché, N., Bouwens, R., Cantalupo, S., Carollo, C. M., Carton, D., Caruana, J., Clément, B., Dreizler, S., Epinat, B., and Guiderdoni, B.

Subjects
HUBBLE deep field, SPECTROGRAPHS, SURFACE brightness (Astronomy), EMISSION-line galaxies, REDSHIFT, ASTRONOMICAL observations
Abstract

We observed Hubble Deep Field South with the new panoramic integral-field spectrograph MUSE that we built and have just commissioned at the VLT. The data cube resulting from 27 h of integration covers one arcmin2 field of view at an unprecedented depth with a 1σ emission-line surface brightness limit of 1 × 10-19 erg s-1 cm-2 arcsec-2, and contains ~90?000 spectra. We present the combined and calibrated data cube, and we performed a first-pass analysis of the sources detected in the Hubble Deep Field South imaging. We measured the redshifts of 189 sources up to a magnitude I814?=?29.5, increasing the number of known spectroscopic redshifts in this field by more than an order of magnitude. We also discovered 26 Lyα emitting galaxies that are not detected in the HST WFPC2 deep broad-band images. The intermediate spectral resolution of 2.3 Å allows us to separate resolved asymmetric Lyα emitters, [O?ii]3727 emitters, and C?iii]1908 emitters, and the broad instantaneous wavelength range of 4500 Å helps to identify single emission lines, such as [O?iii]5007, Hβ, and Hα, over a very wide redshift range. We also show how the three-dimensional information of MUSE helps to resolve sources that are confused at ground-based image quality. Overall, secure identifications are provided for 83% of the 227 emission line sources detected in the MUSE data cube and for 32% of the 586 sources identified in the HST catalogue. The overall redshift distribution is fairly flat to z = 6.3, with a reduction between z = 1.5 to 2.9, in the well-known redshift desert. The field of view of MUSE also allowed us to detect 17 groups within the field. We checked that the number counts of [O?ii]3727 and Lyα emitters are roughly consistent with predictions from the literature. Using two examples, we demonstrate that MUSE is able to provide exquisite spatially resolved spectroscopic information on the intermediate-redshift galaxies present in the field. This unique data set can be used for a wide range of follow-up studies. We release the data cube, the associated products, and the source catalogue with redshifts, spectra, and emission-line fluxes. [ABSTRACT FROM AUTHOR]

Published
2015
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29. Spot the difference: Impact of different selection criteria on observed properties of passive galaxies in zCOSMOS-20k sample.

Author

Moresco, M., Pozzetti, L., Cimatti, A., Zamorani, G., Bolzonella, M., Lamareille, F., Mignoli, M., Zucca, E., Lilly, S. J., Carollo, C. M., Contini, T., Kneib, J.-P., Le Fèvre, O., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., Bongiorno, A., Caputi, K., and Cucciati, O.

Subjects
GALACTIC evolution, ASTRONOMICAL observations, STELLAR mass, SPECTRAL energy distribution, EARLY stars
Abstract

Aims. We present the analysis of photometric, spectroscopic, and morphological properties for differently selected samples of passive galaxies up to z = 1 extracted from the zCOSMOS-20k spectroscopic survey. This analysis intends to explore the dependence of galaxy properties on the selection criterion adopted, study the degree of contamination due to star-forming outliers, and provide a comparison between different commonly used selection criteria. This work is a first step to fully investigating the selection effects of passive galaxies for future massive surveys such as Euclid. Methods. We extracted from the zCOSMOS-20k catalog six different samples of passive galaxies, based on morphology (3336 "morphological" early-type galaxies), optical colors (4889 "red-sequence" galaxies and 4882 "red UVJ" galaxies), specific star-formation rate (2937 "quiescent" galaxies), a best fit to the observed spectral energy distribution (2603 "red SED" galaxies), and a criterion that combines morphological, spectroscopic, and photometric information (1530 "red & passive early-type galaxies"). For all the samples, we studied optical and infrared colors, morphological properties, specific star-formation rates (SFRs), and the equivalent widths of the residual emission lines; this analysis was performed as a function of redshift and stellar mass to inspect further possible dependencies. Results. We find that each passive galaxy sample displays a certain level of contamination due to blue/star-forming/nonpassive outliers. The morphological sample is the one that presents the higher percentage of contamination, with ~12-65% (depending on the mass range) of galaxies not located in the red sequence, ~25-80% of galaxies with a specific SFR up to ~25 times higher than the adopted definition of passive, and significant emission lines found in the median stacked spectra, at least for log (M/M☉) < 10.25. The red & passive ETGs sample is the purest, with a percentage of contamination in color <10% for stellar masses log (M/M☉) > 10.25, very limited tails in sSFR, a median value ~20% higher than the chosen passive cut, and equivalent widths of emission lines mostly compatible with no star-formation activity. However, it is also the less economic criterion in terms of information used. Among the other criteria, we found that the best performing are the red SED and the quiescent ones, providing a percentage of contamination only slightly higher than the red & passive ETGs criterion (on average of a factor of ~2) but with absolute values of the properties of contaminants still compatible with a red, passively evolving population. We also find a strong dependence of the contamination on the stellar mass and conclude that, almost irrespective of the adopted selection criteria, a cut at log (M/M☉) > 10.75 provides a significantly purer sample in terms of star-forming contaminants. By studying the restframe color-mass and color-color diagrams, we provided two revised definitions of passive galaxies based on these criteria that better reproduce the observed bimodality in the properties of zCOSMOS-20k galaxies. The analysis of the number densities of the various samples shows evidences of mass-assembly "downsizing", with galaxies at 10.25 < log (M/M☉) < 10.75 increasing their number by a factor ~2-4 from z = 0.6 to z = 0.2, by a factor ~2-3 from z = 1 to z = 0.2 at 10.75 < log (M/M☉) < 11, and by only ~10-50% from z = 1 to z = 0.2 at 11 < log (M/M☉) < 11.5. [ABSTRACT FROM AUTHOR]

Published
2013
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30. Obscured AGN at z ∼ 1 from the zCOSMOS-Bright Survey.

Author

Mignoli, M., Vignali, C., Gilli, R., Comastri, A., Zamorani, G., Bolzonella, M., Bongiorno, A., Lamareille, F., Nair, P., Pozzetti, L., Lilly, S. J., Carollo, C. M., Contini, T., Kneib, J.-P., Le Fèvre, O., Mainieri, V., Renzini, A., Scodeggio, M., Bardelli, S., and Caputi, K.

Subjects
ACTIVE galactic nuclei, OPTICAL spectroscopy, SEYFERT galaxies, X-ray emission spectroscopy, STELLAR mass, X-ray detection
Abstract

Aims. The application of multi-wavelength selection techniques is essential for obtaining a complete and unbiased census of active galactic nuclei (AGN). We present here a method for selecting z ∼ 1 obscured AGN from optical spectroscopic surveys. Methods. A sample of 94 narrow-line AGN with 0:65 < z < 1:20 was selected from the 20k-Bright zCOSMOS galaxy sample by detection of the high-ionization [Ne v] λ3426 line. The presence of this emission line in a galaxy spectrum is indicative of nuclear activity, although the selection is biased toward low absorbing column densities on narrow-line region or galactic scales. A similar sample of unobscured (type 1 AGN) was collected applying the same analysis to zCOSMOS broad-line objects. This paper presents and compares the optical spectral properties of the two AGN samples. Taking advantage of the large amount of data available in the COSMOS field, the properties of the [Ne v]-selected type 2 AGN were investigated, focusing on their host galaxies, X-ray emission, and optical line-flux ratios. Finally, a previously developed diagnostic, based on the X-ray-to-[Ne v] luminosity ratio, was exploited to search for the more heavily obscured AGN. Results. We found that [Ne v]-selected narrow-line AGN have Seyfert 2-like optical spectra, although their emission line ratios are diluted by a star-forming component. The ACS morphologies and stellar component in the optical spectra indicate a preference for our type 2 AGN to be hosted in early-type spirals with stellar masses greater than 109:5-10 M , on average higher than those of the galaxy parent sample. The fraction of galaxies hosting [Ne v]-selected obscured AGN increases with the stellar mass, reaching a maximum of about 3% at ≈2 × 1011 M . A comparison with other selection techniques at z ∼ 1, namely the line-ratio diagnostics and X-ray detections, shows that the detection of the [Ne v] λ3426 line is an effective method for selecting AGN in the optical band, in particular the most heavily obscured ones, but cannot provide a complete census of type 2 AGN by itself. Finally, the high fraction of [Ne v]-selected type 2 AGN not detected in medium-deep (≈100-200 ks) Chandra observations (67%) is suggestive of the inclusion of Compton-thick (i.e., with NH > 1024 cm-2) sources in our sample. The presence of a population of heavily obscured AGN is corroborated by the X-ray-to-[Ne v] ratio; we estimated, by means of an X-ray stacking technique and simulations, that the Comptonthick fraction in our sample of type 2 AGN is 43 ± 4% (statistical errors only), which agrees well with standard assumptions by XRB synthesis models. [ABSTRACT FROM AUTHOR]

Published
2013
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31. Investigating the relationship between AGN activity and stellar mass in zCOSMOS galaxies at 0<z <1 using emission-line diagnostic diagrams.

Author

Vitale, M., Mignoli, M., Cimatti, A., Lilly, S. J., Carollo, C. M., Contini, T., Kneib, J.-P., Le Fevre, O., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Barnes, L., Bolzonella, M., Bongiorno, A., Bordoloi, R., Bschorr, T. J., Cappi, A., and Caputi, K.

Subjects
STELLAR mass, EMISSION-line galaxies, ACTIVE galactic nuclei, STELLAR populations, REDSHIFT
Abstract

Context. Active galactic nuclei (AGN) are thought to play an important role in galaxy evolution. It has been suggested that AGN feedback could be partly responsible for quenching star-formation in the hosts, leading to transition from the blue cloud to the red sequence. The transition seems to occur faster for the most massive galaxies, where traces of AGN activity have been found as early as at z < 0.1. The correlation between AGN activity, aging of the stellar populations, and stellar mass still needs to be fully understood, especially at high redshifts. Aims. Our aim is to investigate the link between AGN activity, star-formation, and stellar mass of the host galaxy at 0 < z < 1, looking for spectroscopic traces of AGN and aging of the host. This work provides an extension of the existing studies at z < 0.1 and contributes to shed light on galaxy evolution at intermediate redshifts. Methods. We used the zCOSMOS 20k data to create a sample of galaxies at z < 1. We divided the sample into several mass-redshift bins to obtain stacked galaxy spectra with an improved signal-to-noise ratio (S/N).We exploited emission-line diagnostic diagrams to separate AGN from star-forming galaxies. Results. We found an indication of a role for the total galaxy stellar mass in leading galaxy classification. Stacked spectra show AGN signatures above the log M*/M⊙ > 10.2 threshold. Moreover, the stellar populations of AGN hosts are found to be older than star-forming and composite galaxies. This could be due to the the tendency of AGN to reside in massive hosts. Conclusions. The dependence of the AGN classification on the stellar mass agrees with what has been found in previous research. Together with the evidence of older stellar populations inhabiting the AGN-like galaxies, it is consistent with the downsizing scenario. In particular, our evidence points to an evolutionary scenario where the AGN-feedback is capable of quenching the star formation in the most massive galaxies. Therefore, the AGN-feedback is the best candidate for initiating the passive evolutionary phase of galaxies. [ABSTRACT FROM AUTHOR]

Published
2013
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32. The cosmic evolution of oxygen and nitrogen abundances in star-forming galaxies over the past 10 Gyr.

Author

Pérez-Montero, E., Contini, T., Lamareille, F., Maier, C., Carollo, C. M., Kneib, J.-P., Le Fèvre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Caputi, K., Cucciati, O., de la Torre, S., de Ravel, L., and Franzetti, P.

Subjects
GALACTIC evolution, GALAXY formation, STELLAR mass, STELLAR evolution, STAR formation, ASTRONOMICAL spectroscopy
Abstract

Aims. The chemical evolution of galaxies on a cosmological timescale is still a matter of debate despite the increasing number of available data provided by spectroscopic surveys of star-forming galaxies at different redshifts. The fundamental relations involving metallicity, such as the mass—metallicity relation (MZR) or the fundamental metallicity relation, give controversial results about the reality of evolution of the chemical content of galaxies at a given stellar mass. In this work we shed some light on this issue using the completeness reached by the 20 k bright sample of the zCOSMOS survey and using for the first time the nitrogen-to-oxygen ratio (N/O) as a tracer of the gas phase chemical evolution of galaxies that is independent of the star formation rate. Methods. Emission-line galaxies both in the SDSS and 20 k zCOSMOS bright survey were used to study the evolution from the local Universe of the MZR up to a redshift of ∼1.32, and the relation between stellar mass and N/O (MNOR) up to a redshift of ∼0.42 using the N2S2 parameter. All the physical properties derived from stellar continuum and gas emission-lines, including stellar mass, star formation rates, metallicity and N/O, were calculated in a self-consistent way over the full redshift range. Results. We confirm the trend to find lower metallicities in galaxies of a given stellar mass in a younger Universe. This trend is even observed when taking possible effects into account that are due to the observed larger median star formation rates for galaxies at higher redshifts. We also find a significant evolution of the MNOR up to z ∼ 0.4. Taking the slope of the O/H vs. N/O relation into account for the secondary-nitrogen production regime, the observed evolution of the MNOR is consistent with the trends found for both the MZR and its equivalent relation using new expressions to reduce its dependence on star formation rate. [ABSTRACT FROM AUTHOR]

Published
2013
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33. The dominant role of mergers in the size evolution of massive early-type galaxies since z ~ 1.

Author

López-Sanjua, C., Le Fèvre, O., Ilbert, O., Tasca, L. A. M., Bridge, C., Cucciati, O., Kampczyk, P., Pozzetti, L., Xu, C. K., Carollo, C. M., Contini, T., Kneib, J. -P., Lilly, S. J., Mainieri, V., Renzini, A., Sanders, D., Scodeggio, M., Scoville, N. Z., Taniguchi, Y., and Zamorani, G.

Subjects
GALACTIC evolution, STELLAR mergers, EARLY stars, COSMOS satellites, ASTRONOMICAL photometry, DIAGNOSTIC use of spectrum analysis, STELLAR mass, COOL stars (Astronomy)
Abstract

Aims. The role of galaxy mergers in massive galaxy evolution, and in particular to mass assembly and size growth, remains an open question. In this paper we measure the merger fraction and rate, both minor and major, of massive early-type galaxies (M ⋆ ≥ 1011 Mʘ) in the COSMOS field, and study their role in mass and size evolution. Methods. We used the 30-band photometric catalogue in COSMOS, complemented with the spectroscopy of the zCOSMOS survey, to define close pairs with a separation on the sky plane 10 h-1 kpc ≤ rp ≤ 30 h-1 kpc and a relative velocity Δv ≤ 500 km s-1 in redshift space. We measured both major (stellar mass ratio μ ≡ M ⋆ ,2/M ⋆ ,1 ≥ 1/4) and minor (1/10 ≤ μ < 1/4) merger fractions of massive galaxies, and studied their dependence on redshift and on morphology (early types vs. late types). Results. The merger fraction and rate of massive galaxies evolves as a power-law (1 + z)n, with major mergers increasing with redshift, nMM = 1.4, and minor mergers showing little evolution, nmm ~ 0. When split by their morphology, the minor merger fraction for early-type galaxies (ETGs) is higher by a factor of three than that for late-type galaxies (LTGs), and both are nearly constant with redshift. The fraction of major mergers for massive LTGs evolves faster (nMMLT ~ 4 ) than for ETGs (nMMET= 1.8). Conclusions. Our results show that massive ETGs have undergone 0.89 mergers (0.43 major and 0.46 minor) since z ~ 1, leading to a mass growth of ~30%. We find that μ ≥ 1/10 mergers can explain ~55% of the observed size evolution of these galaxies since z ~ 1. Another ~20% is due to the progenitor bias (younger galaxies are more extended) and we estimate that very minor mergers (μ < 1/10) could contribute with an extra ~20%. The remaining ~5% should come from other processes (e.g., adiabatic expansion or observational effects). This picture also reproduces the mass growth and the velocity dispersion evolution of these galaxies. We conclude from these results, and after exploring all the possible uncertainties in our picture, that merging is the main contributor to the size evolution of massive ETGs at z ≲ 1, accounting for ~50−75% of that evolution in the last 8 Gyr. Nearly half of the evolution due to mergers is related to minor (μ < 1/4) events. [ABSTRACT FROM AUTHOR]

Published
2012
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34. The dominant role of mergers in the size evolution of massive early-type galaxies since z ∼ 1.

Author

López-Sanjuan, C., Le Fèvre, O., Ilbert, O., Tasca, L. A. M., Bridge, C., Cucciati, O., Kampczyk, P., Pozzetti, L., Xu, C. K., Carollo, C. M., Contini, T., Kneib, J.-P., Lilly, S. J., Mainieri, V., Renzini, A., Sanders, D., Scodeggio, M., Scoville, N. Z., Taniguchi, Y., and Zamorani, G.

Subjects
GALAXIES, PHOTOMETRY, SPECTRUM analysis, REDSHIFT, STELLAR mass
Abstract

Aims. The role of galaxy mergers in massive galaxy evolution, and in particular to mass assembly and size growth, remains an open question. In this paper we measure the merger fraction and rate, both minor and major, of massive early-type galaxies (M⋆ ⩾ 1011 M☉) in the COSMOS field, and study their role in mass and size evolution. Methods. We used the 30-band photometric catalogue in COSMOS, complemented with the spectroscopy of the zCOSMOS survey, to define close pairs with a separation on the sky plane 10 h-1 kpc ⩽ rp ⩽ 30 h-1 kpc and a relative velocity Δv ⩽ 500 km s-1 in redshift space. We measured both major (stellar mass ratio μ ≡ M⋆,2/M⋆,1 ⩾ 1/4) and minor (1/10 ⩽ μ < 1/4) merger fractions of massive galaxies, and studied their dependence on redshift and on morphology (early types vs. late types). Results. The merger fraction and rate of massive galaxies evolves as a power-law (1+z)n, with major mergers increasing with redshift, nMM = 1.4, and minor mergers showing little evolution, nmm ∼ 0. When split by their morphology, the minor merger fraction for early-type galaxies (ETGs) is higher by a factor of three than that for late-type galaxies (LTGs), and both are nearly constant with redshift. The fraction of major mergers for massive LTGs evolves faster (nLTMM ∼ 4) than for ETGs (nETMM = 1.8). Conclusions. Our results show that massive ETGs have undergone 0.89 mergers (0.43 major and 0.46 minor) since z ∼ 1, leading to a mass growth of ∼30%.We find that μ ⩾ 1/10 mergers can explain ∼55% of the observed size evolution of these galaxies since z ∼ 1. Another ∼20% is due to the progenitor bias (younger galaxies are more extended) and we estimate that very minor mergers (μ < 1/10) could contribute with an extra ∼20%. The remaining ∼5% should come from other processes (e.g., adiabatic expansion or observational effects). This picture also reproduces the mass growth and the velocity dispersion evolution of these galaxies. We conclude from these results, and after exploring all the possible uncertainties in our picture, that merging is the main contributor to the size evolution of massive ETGs at z ⋆ 1, accounting for ∼50-75% of that evolution in the last 8 Gyr. Nearly half of the evolution due to mergers is related to minor (μ < 1/4) events [ABSTRACT FROM AUTHOR]

Published
2012
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